Science.gov

Sample records for 10-5 msun yr-1

  1. Separation in 5 Msun Binaries

    NASA Astrophysics Data System (ADS)

    Evans, Nancy R.; Bond, H. E.; Schaefer, G.; Mason, B. D.; Karovska, M.; Tingle, E.

    2013-01-01

    Cepheids (5 Msun stars) provide an excellent sample for determining the binary properties of fairly massive stars. International Ultraviolet Explorer (IUE) observations of Cepheids brighter than 8th magnitude resulted in a list of ALL companions more massive than 2.0 Msun uniformly sensitive to all separations. Hubble Space Telescope Wide Field Camera 3 (WFC3) has resolved three of these binaries (Eta Aql, S Nor, and V659 Cen). Combining these separations with orbital data in the literature, we derive an unbiased distribution of binary separations for a sample of 18 Cepheids, and also a distribution of mass ratios. The distribution of orbital periods shows that the 5 Msun binaries prefer shorter periods than 1 Msun stars, reflecting differences in star formation processes.

  2. 46 CFR 59.10-5 - Cracks.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... 46 Shipping 2 2012-10-01 2012-10-01 false Cracks. 59.10-5 Section 59.10-5 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY (CONTINUED) MARINE ENGINEERING REPAIRS TO BOILERS, PRESSURE VESSELS AND APPURTENANCES Welding Repairs to Boilers and Pressure Vessels in -Service § 59.10-5 Cracks. (a) Cracks extending from the calking edge of plates...

  3. 10 CFR 10.5 - Definitions.

    Code of Federal Regulations, 2014 CFR

    2014-01-01

    ... 10 Energy 1 2014-01-01 2014-01-01 false Definitions. 10.5 Section 10.5 Energy NUCLEAR REGULATORY COMMISSION CRITERIA AND PROCEDURES FOR DETERMINING ELIGIBILITY FOR ACCESS TO RESTRICTED DATA OR NATIONAL SECURITY INFORMATION OR AN EMPLOYMENT CLEARANCE General Provisions § 10.5 Definitions. Access authorization means an administrative...

  4. 10 CFR 10.5 - Definitions.

    Code of Federal Regulations, 2011 CFR

    2011-01-01

    ... 10 Energy 1 2011-01-01 2011-01-01 false Definitions. 10.5 Section 10.5 Energy NUCLEAR REGULATORY COMMISSION CRITERIA AND PROCEDURES FOR DETERMINING ELIGIBILITY FOR ACCESS TO RESTRICTED DATA OR NATIONAL SECURITY INFORMATION OR AN EMPLOYMENT CLEARANCE General Provisions § 10.5 Definitions. Access authorization means an administrative...

  5. 10 CFR 10.5 - Definitions.

    Code of Federal Regulations, 2012 CFR

    2012-01-01

    ... 10 Energy 1 2012-01-01 2012-01-01 false Definitions. 10.5 Section 10.5 Energy NUCLEAR REGULATORY COMMISSION CRITERIA AND PROCEDURES FOR DETERMINING ELIGIBILITY FOR ACCESS TO RESTRICTED DATA OR NATIONAL SECURITY INFORMATION OR AN EMPLOYMENT CLEARANCE General Provisions § 10.5 Definitions. Access authorization means an administrative...

  6. 10 CFR 10.5 - Definitions.

    Code of Federal Regulations, 2010 CFR

    2010-01-01

    ... 10 Energy 1 2010-01-01 2010-01-01 false Definitions. 10.5 Section 10.5 Energy NUCLEAR REGULATORY COMMISSION CRITERIA AND PROCEDURES FOR DETERMINING ELIGIBILITY FOR ACCESS TO RESTRICTED DATA OR NATIONAL SECURITY INFORMATION OR AN EMPLOYMENT CLEARANCE General Provisions § 10.5 Definitions. Access authorization means an administrative...

  7. 46 CFR 2.10-5 - Exemptions.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 46 Shipping 1 2010-10-01 2010-10-01 false Exemptions. 2.10-5 Section 2.10-5 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY PROCEDURES APPLICABLE TO THE PUBLIC VESSEL INSPECTIONS Fees § 2.10-5 Exemptions. (a) Vessels owned or operated by a non-profit organization may be exempted from payment of...

  8. 49 CFR 10.5 - Definitions.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... its own Privacy Act regulations (49 CFR Part 1007), except to the extent that any system of records... 49 Transportation 1 2011-10-01 2011-10-01 false Definitions. 10.5 Section 10.5 Transportation... Applicability and Policy § 10.5 Definitions. Unless the context requires otherwise, the following...

  9. 49 CFR 10.5 - Definitions.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... its own Privacy Act regulations (49 CFR Part 1007), except to the extent that any system of records... 49 Transportation 1 2014-10-01 2014-10-01 false Definitions. 10.5 Section 10.5 Transportation... Applicability and Policy § 10.5 Definitions. Unless the context requires otherwise, the following...

  10. 49 CFR 10.5 - Definitions.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... its own Privacy Act regulations (49 CFR Part 1007), except to the extent that any system of records... 49 Transportation 1 2013-10-01 2013-10-01 false Definitions. 10.5 Section 10.5 Transportation... Applicability and Policy § 10.5 Definitions. Unless the context requires otherwise, the following...

  11. 49 CFR 10.5 - Definitions.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... its own Privacy Act regulations (49 CFR Part 1007), except to the extent that any system of records... 49 Transportation 1 2012-10-01 2012-10-01 false Definitions. 10.5 Section 10.5 Transportation... Applicability and Policy § 10.5 Definitions. Unless the context requires otherwise, the following...

  12. 49 CFR 10.5 - Definitions.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... its own Privacy Act regulations (49 CFR Part 1007), except to the extent that any system of records... 49 Transportation 1 2010-10-01 2010-10-01 false Definitions. 10.5 Section 10.5 Transportation... Applicability and Policy § 10.5 Definitions. Unless the context requires otherwise, the following...

  13. 46 CFR 56.10-5 - Pipe.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... design limits of stress and temperature indicated in ASME B31.1 (incorporated by reference; see 46 CFR 56... 46 Shipping 2 2010-10-01 2010-10-01 false Pipe. 56.10-5 Section 56.10-5 Shipping COAST GUARD... § 56.10-5 Pipe. (a) General. Pipe and tubing shall be selected as described in Table 56.60-1(a)....

  14. 46 CFR 2.10-5 - Exemptions.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... 46 Shipping 1 2012-10-01 2012-10-01 false Exemptions. 2.10-5 Section 2.10-5 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY PROCEDURES APPLICABLE TO THE PUBLIC VESSEL INSPECTIONS Fees § 2.10-5 Exemptions. (a) Vessels owned or operated by a non-profit organization may be exempted from payment of the fees required by this subpart, only if...

  15. 46 CFR 2.10-5 - Exemptions.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... 46 Shipping 1 2011-10-01 2011-10-01 false Exemptions. 2.10-5 Section 2.10-5 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY PROCEDURES APPLICABLE TO THE PUBLIC VESSEL INSPECTIONS Fees § 2.10-5 Exemptions. (a) Vessels owned or operated by a non-profit organization may be exempted from payment of the fees required by this subpart, only if...

  16. 32 CFR 10.5 - Construction.

    Code of Federal Regulations, 2012 CFR

    2012-07-01

    ... with 32 CFR part 9, and Military Order of November 13, 2001, “Detention, Treatment, and Trial of... event of an inconsistency, the provisions of 32 CFR part 9, and Military Order of November 13, 2001... 32 National Defense 1 2012-07-01 2012-07-01 false Construction. 10.5 Section 10.5 National...

  17. 32 CFR 10.5 - Construction.

    Code of Federal Regulations, 2014 CFR

    2014-07-01

    ... with 32 CFR part 9, and Military Order of November 13, 2001, “Detention, Treatment, and Trial of... event of an inconsistency, the provisions of 32 CFR part 9, and Military Order of November 13, 2001... 32 National Defense 1 2014-07-01 2014-07-01 false Construction. 10.5 Section 10.5 National...

  18. 44 CFR 10.5 - Responsibilities.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... 44 Emergency Management and Assistance 1 2012-10-01 2011-10-01 true Responsibilities. 10.5 Section... SECURITY GENERAL ENVIRONMENTAL CONSIDERATIONS Agency Implementing Procedures § 10.5 Responsibilities. (a... impact statements and assign lead agency responsibility when more than one FEMA office or...

  19. 44 CFR 10.5 - Responsibilities.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 44 Emergency Management and Assistance 1 2010-10-01 2010-10-01 false Responsibilities. 10.5... Responsibilities. (a) The Regional Administrators shall, for each action not categorically excluded from this... impact statements and assign lead agency responsibility when more than one FEMA office or...

  20. 44 CFR 10.5 - Responsibilities.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... 44 Emergency Management and Assistance 1 2013-10-01 2013-10-01 false Responsibilities. 10.5... Responsibilities. (a) The Regional Administrators shall, for each action not categorically excluded from this... impact statements and assign lead agency responsibility when more than one FEMA office or...

  1. 44 CFR 10.5 - Responsibilities.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... 44 Emergency Management and Assistance 1 2011-10-01 2011-10-01 false Responsibilities. 10.5... Responsibilities. (a) The Regional Administrators shall, for each action not categorically excluded from this... impact statements and assign lead agency responsibility when more than one FEMA office or...

  2. Effects of carbon source on expression of alcohol oxidase activity and on morphologic pattern of YR-1 Strain, a filamentous fungus isolated from petroleum-contaminated soils.

    PubMed

    Robelo, Carmen Rodríguez; Novoa, Vanesa Zazueta; Zazueta-Sandoval, Roberto

    2004-01-01

    Soluble alcohol oxidase (AO) activity was detected in the supernatant fraction of a high-speed centrifugation procedure after ballistic cellular homo-genization to break the mycelium from a filamentous fungus strain named YR-1, isolated from petroleum-contaminated soils. AO activity from aerobically grown mycelium was detected in growth media containing different carbon sources, including alcohols and hydrocarbons but not in glucose. In previous work, zymogram analysis conducted with crude extracts from aerobic mycelium of YR-1 strain indicated the existence of two AO enzymes originally named AO-1 and AO-2. In the present study, we were able to separate the AO-1 band into two bands depending on culture conditions, carbon source, and polyacrylamide gel electrophoresis (PAGE) separation conditions; the enzyme activity pattern in zymograms from cell-free extracts exhibited three different bands after native PAGE. New nomenclature was used for upper bands AO-1 and AO-2 and lower band AO-3, respectively. The expression of AO activity was studied in the absence of glucose in the culture media and in the presence of hydrocarbons or petroleum as sole carbon source, suggesting that AO expression could be subjected to two regulatory possibilities: carbon catabolite regulation by glucose and induction by hydrocarbons. The possibility of catabolic inhibition of AO by glucose in the active enzyme was also tested, and the results confirm that this kind of regulatory mechanism is not present in AO activity. PMID:15054203

  3. The Solar Neighborhood. XIII. Parallax Results from the CTIOPI 0.9 Meter Program: Stars with μ >= 1.0" yr-1 (MOTION Sample)

    NASA Astrophysics Data System (ADS)

    Jao, Wei-Chun; Henry, Todd J.; Subasavage, John P.; Brown, Misty A.; Ianna, Philip A.; Bartlett, Jennifer L.; Costa, Edgardo; Méndez, René A.

    2005-04-01

    We present the first set of definitive trigonometric parallaxes and proper motions from the Cerro Tololo Inter-American Observatory Parallax Investigation. Full astrometric reductions for the program are discussed, including methods of reference star selection, differential color refraction corrections, and conversion of relative to absolute parallax. Using data acquired at the 0.9 m telescope at CTIO, full astrometric solutions and VRIJHKs photometry are presented for 36 red and white dwarf stellar systems with proper motions faster than 1.0" yr-1. Of these, 33 systems have their first ever trigonometric parallaxes, which comprise 41% of MOTION systems (those reported to have proper motions greater than 1.0" yr-1) south of δ=0deg that have no parallaxes. Four of the systems are new members of the RECONS 10 pc sample for which the first accurate trigonometric parallaxes are published here: DENIS J1048-3956 (4.04+/-0.03 pc), GJ 1128 (LHS 271, 6.53+/-0.10 pc), GJ 1068 (LHS 22, 6.97+/-0.09 pc), and GJ 1123 (LHS 263, 9.02+/-0.16 pc). In addition, two red subdwarf-white dwarf pairs, LHS 193AB and LHS 300AB, are identified. The white dwarf secondaries fall in a previously uncharted region of the H-R diagram.

  4. On the Evolution of Stars That Form Electron-degenerate Cores Processed by Carbon Burning. II. Isotope Abundances and Thermal Pulses in a 10 Msun Model with an ONe Core and Applications to Long-Period Variables, Classical Novae, and Accretion-induced Collapse

    NASA Astrophysics Data System (ADS)

    Ritossa, Claudio; Garcia-Berro, Enrique; Iben, Icko, Jr.

    1996-03-01

    long-period variables in the Galaxy and in the Magellanic Clouds. Perhaps the major signature of a TPSAGB star is a brightness greater than the "classical limit" of Mbol = -7.1. Betelgeuse in our Galaxy and four stars in the Magellanic Clouds are brighter than the supposed limit, but they exhibit abundance characteristics which can be accounted for in the framework of TPSAGB theory. Assuming that a superwind removes mass from the surface at a rate of ˜10-4 Msun yr-1, the final mass of the ONe white dwarf formed by our TPSAGB model is ˜1.26 Msun, the outer 0.06 Msun of which is composed primarily of carbon and oxygen.

  5. 33 CFR 66.10-5-66.10-10 - [Reserved

    Code of Federal Regulations, 2012 CFR

    2012-07-01

    ... 33 Navigation and Navigable Waters 1 2012-07-01 2012-07-01 false 66.10-5-66.10-10 Section 66.10-5-66.10-10 Navigation and Navigable Waters COAST GUARD, DEPARTMENT OF HOMELAND SECURITY AIDS TO NAVIGATION PRIVATE AIDS TO NAVIGATION Uniform State Waterway Marking System §§ 66.10-5—66.10-10...

  6. 33 CFR 66.10-5-66.10-10 - [Reserved

    Code of Federal Regulations, 2010 CFR

    2010-07-01

    ... 33 Navigation and Navigable Waters 1 2010-07-01 2010-07-01 false 66.10-5-66.10-10 Section 66.10-5-66.10-10 Navigation and Navigable Waters COAST GUARD, DEPARTMENT OF HOMELAND SECURITY AIDS TO NAVIGATION PRIVATE AIDS TO NAVIGATION Uniform State Waterway Marking System §§ 66.10-5—66.10-10...

  7. 46 CFR 95.10-5 - Fire pumps.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... 46 Shipping 4 2011-10-01 2011-10-01 false Fire pumps. 95.10-5 Section 95.10-5 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY (CONTINUED) CARGO AND MISCELLANEOUS VESSELS FIRE PROTECTION EQUIPMENT Fire Main System, Details § 95.10-5 Fire pumps. (a) Vessels shall be equipped with independently driven...

  8. 46 CFR 76.10-5 - Fire pumps.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 46 Shipping 3 2010-10-01 2010-10-01 false Fire pumps. 76.10-5 Section 76.10-5 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY (CONTINUED) PASSENGER VESSELS FIRE PROTECTION EQUIPMENT Fire Main System, Details § 76.10-5 Fire pumps. (a) Vessels shall be equipped with independently driven fire pumps...

  9. 46 CFR 95.10-5 - Fire pumps.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 46 Shipping 4 2010-10-01 2010-10-01 false Fire pumps. 95.10-5 Section 95.10-5 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY (CONTINUED) CARGO AND MISCELLANEOUS VESSELS FIRE PROTECTION EQUIPMENT Fire Main System, Details § 95.10-5 Fire pumps. (a) Vessels shall be equipped with independently driven...

  10. 46 CFR 61.10-5 - Pressure vessels in service.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 46 Shipping 2 2010-10-01 2010-10-01 false Pressure vessels in service. 61.10-5 Section 61.10-5... INSPECTIONS Tests and Inspections of Pressure Vessels § 61.10-5 Pressure vessels in service. (a) Basic requirements. Each pressure vessel must be examined or tested every 5 years. The extent of the test...

  11. 46 CFR 61.10-5 - Pressure vessels in service.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... 46 Shipping 2 2011-10-01 2011-10-01 false Pressure vessels in service. 61.10-5 Section 61.10-5... INSPECTIONS Tests and Inspections of Pressure Vessels § 61.10-5 Pressure vessels in service. (a) Basic requirements. Each pressure vessel must be examined or tested every 5 years. The extent of the test...

  12. 46 CFR 61.10-5 - Pressure vessels in service.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... 46 Shipping 2 2014-10-01 2014-10-01 false Pressure vessels in service. 61.10-5 Section 61.10-5... INSPECTIONS Tests and Inspections of Pressure Vessels § 61.10-5 Pressure vessels in service. (a) Basic requirements. Each pressure vessel must be examined or tested every 5 years. The extent of the test...

  13. 33 CFR 67.10-5 - Location requirements.

    Code of Federal Regulations, 2011 CFR

    2011-07-01

    ... 33 Navigation and Navigable Waters 1 2011-07-01 2011-07-01 false Location requirements. 67.10-5 Section 67.10-5 Navigation and Navigable Waters COAST GUARD, DEPARTMENT OF HOMELAND SECURITY AIDS TO... signals § 67.10-5 Location requirements. The sound signal required by §§ 67.20-10, 67.25-10, and...

  14. 33 CFR 67.10-5 - Location requirements.

    Code of Federal Regulations, 2014 CFR

    2014-07-01

    ... 33 Navigation and Navigable Waters 1 2014-07-01 2014-07-01 false Location requirements. 67.10-5 Section 67.10-5 Navigation and Navigable Waters COAST GUARD, DEPARTMENT OF HOMELAND SECURITY AIDS TO... signals § 67.10-5 Location requirements. The sound signal required by §§ 67.20-10, 67.25-10, and...

  15. 33 CFR 67.10-5 - Location requirements.

    Code of Federal Regulations, 2010 CFR

    2010-07-01

    ... 33 Navigation and Navigable Waters 1 2010-07-01 2010-07-01 false Location requirements. 67.10-5 Section 67.10-5 Navigation and Navigable Waters COAST GUARD, DEPARTMENT OF HOMELAND SECURITY AIDS TO... signals § 67.10-5 Location requirements. The sound signal required by §§ 67.20-10, 67.25-10, and...

  16. 33 CFR 67.10-5 - Location requirements.

    Code of Federal Regulations, 2012 CFR

    2012-07-01

    ... 33 Navigation and Navigable Waters 1 2012-07-01 2012-07-01 false Location requirements. 67.10-5 Section 67.10-5 Navigation and Navigable Waters COAST GUARD, DEPARTMENT OF HOMELAND SECURITY AIDS TO... signals § 67.10-5 Location requirements. The sound signal required by §§ 67.20-10, 67.25-10, and...

  17. 33 CFR 67.10-5 - Location requirements.

    Code of Federal Regulations, 2013 CFR

    2013-07-01

    ... 33 Navigation and Navigable Waters 1 2013-07-01 2013-07-01 false Location requirements. 67.10-5 Section 67.10-5 Navigation and Navigable Waters COAST GUARD, DEPARTMENT OF HOMELAND SECURITY AIDS TO... signals § 67.10-5 Location requirements. The sound signal required by §§ 67.20-10, 67.25-10, and...

  18. 46 CFR 92.10-5 - Two means required.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 46 Shipping 4 2010-10-01 2010-10-01 false Two means required. 92.10-5 Section 92.10-5 Shipping... AND ARRANGEMENT Means of Escape § 92.10-5 Two means required. (a) There shall be at least two means of... quartered or normally employed. At least one of these two means of escape shall be independent of...

  19. 46 CFR 168.10-5 - Civilian nautical school.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 46 Shipping 7 2010-10-01 2010-10-01 false Civilian nautical school. 168.10-5 Section 168.10-5 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY (CONTINUED) NAUTICAL SCHOOLS CIVILIAN NAUTICAL SCHOOL VESSELS Definitions of Terms Used in This Part § 168.10-5 Civilian nautical school. The term...

  20. 46 CFR 111.10-5 - Multiple energy sources.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... 46 Shipping 4 2014-10-01 2014-10-01 false Multiple energy sources. 111.10-5 Section 111.10-5...-GENERAL REQUIREMENTS Power Supply § 111.10-5 Multiple energy sources. Failure of any single generating set energy source such as a boiler, diesel, gas turbine, or steam turbine must not cause all generating...

  1. 46 CFR 72.10-5 - Two means required.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... 46 Shipping 3 2011-10-01 2011-10-01 false Two means required. 72.10-5 Section 72.10-5 Shipping... Means of Escape § 72.10-5 Two means required. (a) There shall be at least two means of escape from all... least one of these two means of escape shall be independent of watertight doors. For stairway...

  2. 46 CFR 92.10-5 - Two means required.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... 46 Shipping 4 2013-10-01 2013-10-01 false Two means required. 92.10-5 Section 92.10-5 Shipping... AND ARRANGEMENT Means of Escape § 92.10-5 Two means required. (a) There shall be at least two means of... quartered or normally employed. At least one of these two means of escape shall be independent of...

  3. 46 CFR 190.10-5 - Two means required.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... 46 Shipping 7 2011-10-01 2011-10-01 false Two means required. 190.10-5 Section 190.10-5 Shipping... ARRANGEMENT Means of Escape § 190.10-5 Two means required. (a) There shall be at least two means of escape... least one of these two means of escape shall be independent of watertight doors and hatches, except...

  4. 46 CFR 190.10-5 - Two means required.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... 46 Shipping 7 2013-10-01 2013-10-01 false Two means required. 190.10-5 Section 190.10-5 Shipping... ARRANGEMENT Means of Escape § 190.10-5 Two means required. (a) There shall be at least two means of escape... least one of these two means of escape shall be independent of watertight doors and hatches, except...

  5. 46 CFR 72.10-5 - Two means required.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... 46 Shipping 3 2013-10-01 2013-10-01 false Two means required. 72.10-5 Section 72.10-5 Shipping... Means of Escape § 72.10-5 Two means required. (a) There shall be at least two means of escape from all... least one of these two means of escape shall be independent of watertight doors. For stairway...

  6. 46 CFR 190.10-5 - Two means required.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... 46 Shipping 7 2012-10-01 2012-10-01 false Two means required. 190.10-5 Section 190.10-5 Shipping... ARRANGEMENT Means of Escape § 190.10-5 Two means required. (a) There shall be at least two means of escape... least one of these two means of escape shall be independent of watertight doors and hatches, except...

  7. 46 CFR 92.10-5 - Two means required.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... 46 Shipping 4 2012-10-01 2012-10-01 false Two means required. 92.10-5 Section 92.10-5 Shipping... AND ARRANGEMENT Means of Escape § 92.10-5 Two means required. (a) There shall be at least two means of... quartered or normally employed. At least one of these two means of escape shall be independent of...

  8. 46 CFR 72.10-5 - Two means required.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... 46 Shipping 3 2012-10-01 2012-10-01 false Two means required. 72.10-5 Section 72.10-5 Shipping... Means of Escape § 72.10-5 Two means required. (a) There shall be at least two means of escape from all... least one of these two means of escape shall be independent of watertight doors. For stairway...

  9. 46 CFR 190.10-5 - Two means required.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 46 Shipping 7 2010-10-01 2010-10-01 false Two means required. 190.10-5 Section 190.10-5 Shipping... ARRANGEMENT Means of Escape § 190.10-5 Two means required. (a) There shall be at least two means of escape... least one of these two means of escape shall be independent of watertight doors and hatches, except...

  10. 46 CFR 72.10-5 - Two means required.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... 46 Shipping 3 2014-10-01 2014-10-01 false Two means required. 72.10-5 Section 72.10-5 Shipping... Means of Escape § 72.10-5 Two means required. (a) There shall be at least two means of escape from all... least one of these two means of escape shall be independent of watertight doors. For stairway...

  11. 46 CFR 72.10-5 - Two means required.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 46 Shipping 3 2010-10-01 2010-10-01 false Two means required. 72.10-5 Section 72.10-5 Shipping... Means of Escape § 72.10-5 Two means required. (a) There shall be at least two means of escape from all... least one of these two means of escape shall be independent of watertight doors. For stairway...

  12. 46 CFR 92.10-5 - Two means required.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... 46 Shipping 4 2014-10-01 2014-10-01 false Two means required. 92.10-5 Section 92.10-5 Shipping... AND ARRANGEMENT Means of Escape § 92.10-5 Two means required. (a) There shall be at least two means of... quartered or normally employed. At least one of these two means of escape shall be independent of...

  13. 46 CFR 190.10-5 - Two means required.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... 46 Shipping 7 2014-10-01 2014-10-01 false Two means required. 190.10-5 Section 190.10-5 Shipping... ARRANGEMENT Means of Escape § 190.10-5 Two means required. (a) There shall be at least two means of escape... least one of these two means of escape shall be independent of watertight doors and hatches, except...

  14. 46 CFR 30.10-5 - Cargo-TB/ALL.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... 46 Shipping 1 2014-10-01 2014-10-01 false Cargo-TB/ALL. 30.10-5 Section 30.10-5 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY TANK VESSELS GENERAL PROVISIONS Definitions § 30.10-5 Cargo—TB/ALL. The term cargo means combustible liquid, flammable liquid, or liquefied flammable gas...

  15. 46 CFR 30.10-5 - Cargo-TB/ALL.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... 46 Shipping 1 2012-10-01 2012-10-01 false Cargo-TB/ALL. 30.10-5 Section 30.10-5 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY TANK VESSELS GENERAL PROVISIONS Definitions § 30.10-5 Cargo—TB/ALL. The term cargo means combustible liquid, flammable liquid, or liquefied flammable gas...

  16. 46 CFR 30.10-5 - Cargo-TB/ALL.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... 46 Shipping 1 2013-10-01 2013-10-01 false Cargo-TB/ALL. 30.10-5 Section 30.10-5 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY TANK VESSELS GENERAL PROVISIONS Definitions § 30.10-5 Cargo—TB/ALL. The term cargo means combustible liquid, flammable liquid, or liquefied flammable gas...

  17. 46 CFR 95.10-5 - Fire pumps.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... 46 Shipping 4 2014-10-01 2014-10-01 false Fire pumps. 95.10-5 Section 95.10-5 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY (CONTINUED) CARGO AND MISCELLANEOUS VESSELS FIRE PROTECTION EQUIPMENT Fire Main System, Details § 95.10-5 Fire pumps. (a) Vessels shall be equipped with independently driven...

  18. 46 CFR 95.10-5 - Fire pumps.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... 46 Shipping 4 2013-10-01 2013-10-01 false Fire pumps. 95.10-5 Section 95.10-5 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY (CONTINUED) CARGO AND MISCELLANEOUS VESSELS FIRE PROTECTION EQUIPMENT Fire Main System, Details § 95.10-5 Fire pumps. (a) Vessels shall be equipped with independently driven...

  19. 46 CFR 111.10-5 - Multiple energy sources.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... 46 Shipping 4 2012-10-01 2012-10-01 false Multiple energy sources. 111.10-5 Section 111.10-5...-GENERAL REQUIREMENTS Power Supply § 111.10-5 Multiple energy sources. Failure of any single generating set energy source such as a boiler, diesel, gas turbine, or steam turbine must not cause all generating...

  20. 46 CFR 111.10-5 - Multiple energy sources.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 46 Shipping 4 2010-10-01 2010-10-01 false Multiple energy sources. 111.10-5 Section 111.10-5...-GENERAL REQUIREMENTS Power Supply § 111.10-5 Multiple energy sources. Failure of any single generating set energy source such as a boiler, diesel, gas turbine, or steam turbine must not cause all generating...

  1. 46 CFR 111.10-5 - Multiple energy sources.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... 46 Shipping 4 2011-10-01 2011-10-01 false Multiple energy sources. 111.10-5 Section 111.10-5...-GENERAL REQUIREMENTS Power Supply § 111.10-5 Multiple energy sources. Failure of any single generating set energy source such as a boiler, diesel, gas turbine, or steam turbine must not cause all generating...

  2. 46 CFR 111.10-5 - Multiple energy sources.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... 46 Shipping 4 2013-10-01 2013-10-01 false Multiple energy sources. 111.10-5 Section 111.10-5...-GENERAL REQUIREMENTS Power Supply § 111.10-5 Multiple energy sources. Failure of any single generating set energy source such as a boiler, diesel, gas turbine, or steam turbine must not cause all generating...

  3. 46 CFR 30.10-5 - Cargo-TB/ALL.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... 46 Shipping 1 2011-10-01 2011-10-01 false Cargo-TB/ALL. 30.10-5 Section 30.10-5 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY TANK VESSELS GENERAL PROVISIONS Definitions § 30.10-5 Cargo—TB/ALL. The term cargo means combustible liquid, flammable liquid, or liquefied flammable gas...

  4. 46 CFR 30.10-5 - Cargo-TB/ALL.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 46 Shipping 1 2010-10-01 2010-10-01 false Cargo-TB/ALL. 30.10-5 Section 30.10-5 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY TANK VESSELS GENERAL PROVISIONS Definitions § 30.10-5 Cargo—TB/ALL. The term cargo means combustible liquid, flammable liquid, or liquefied flammable gas...

  5. 46 CFR 113.10-5 - Common return.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 46 Shipping 4 2010-10-01 2010-10-01 false Common return. 113.10-5 Section 113.10-5 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY (CONTINUED) ELECTRICAL ENGINEERING COMMUNICATION AND ALARM SYSTEMS AND EQUIPMENT Fire and Smoke Detecting and Alarm Systems § 113.10-5 Common return. A...

  6. 46 CFR 113.10-5 - Common return.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... 46 Shipping 4 2011-10-01 2011-10-01 false Common return. 113.10-5 Section 113.10-5 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY (CONTINUED) ELECTRICAL ENGINEERING COMMUNICATION AND ALARM SYSTEMS AND EQUIPMENT Fire and Smoke Detecting and Alarm Systems § 113.10-5 Common return. A...

  7. 46 CFR 113.10-5 - Common return.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... 46 Shipping 4 2012-10-01 2012-10-01 false Common return. 113.10-5 Section 113.10-5 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY (CONTINUED) ELECTRICAL ENGINEERING COMMUNICATION AND ALARM SYSTEMS AND EQUIPMENT Fire and Smoke Detecting and Alarm Systems § 113.10-5 Common return. A...

  8. 46 CFR 113.10-5 - Common return.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... 46 Shipping 4 2014-10-01 2014-10-01 false Common return. 113.10-5 Section 113.10-5 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY (CONTINUED) ELECTRICAL ENGINEERING COMMUNICATION AND ALARM SYSTEMS AND EQUIPMENT Fire and Smoke Detecting and Alarm Systems § 113.10-5 Common return. A...

  9. 46 CFR 113.10-5 - Common return.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... 46 Shipping 4 2013-10-01 2013-10-01 false Common return. 113.10-5 Section 113.10-5 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY (CONTINUED) ELECTRICAL ENGINEERING COMMUNICATION AND ALARM SYSTEMS AND EQUIPMENT Fire and Smoke Detecting and Alarm Systems § 113.10-5 Common return. A...

  10. Registration of cotton germplasm line md 10-5

    Technology Transfer Automated Retrieval System (TEKTRAN)

    MD 10-5 (Reg. No. ______, PI 675077) is a noncommercial breeding line of cotton (Gossypium hirsutum L.) released by the USDA-ARS at Stoneville, MS in 2015. MD 10-5 was selected in F4 progenies from a cross between MD 15 (PI 642769) and JJ 1145ne. MD 10-5 has a desirable combination between lint yi...

  11. The Solar Neighborhood. XXIV. Parallax Results from the CTIOPI 0.9 m Program: Stars with μ >= 1farcs0 yr-1 (MOTION Sample) and Subdwarfs

    NASA Astrophysics Data System (ADS)

    Jao, Wei-Chun; Henry, Todd J.; Subasavage, John P.; Winters, Jennifer G.; Riedel, Adric R.; Ianna, Philip A.

    2011-04-01

    We present 41 trigonometric parallaxes of 37 stellar systems, most of which have proper motions greater than 1farcs0 yr-1. These are the first trigonometric parallaxes for 24 systems. Overall, there are 15 red dwarf systems and 22 red subdwarf systems in the sample. Five of the systems are multiples with directly detected companions, and we have discovered perturbations caused by unseen companions in two additional cases, the dwarf LHS 501 and the subdwarf LHS 440. The latter system may eventually provide important dynamical mass points on the subdwarf mass-luminosity relation. Two additional stars of note are LHS 272, the third closest M-type subdwarf at a distance of only 13.6 pc, and LHS 2734 AB, a high-velocity subdwarf binary with V tan> 700 km s-1, which likely exceeds the escape velocity of the Milky Way. We also report the first long-term variability study of cool subdwarfs indicating that cool subdwarfs are less photometrically variable than their main-sequence counterparts.

  12. 46 CFR 193.10-5 - Fire main system, details.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... of a total flooding system using carbon dioxide or a clean agent complying with 46 CFR subpart 95.16... 46 Shipping 7 2012-10-01 2012-10-01 false Fire main system, details. 193.10-5 Section 193.10-5 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY (CONTINUED) OCEANOGRAPHIC RESEARCH VESSELS...

  13. 27 CFR 10.5 - Delegations of the Administrator.

    Code of Federal Regulations, 2010 CFR

    2010-04-01

    ... Administrator's Authorities in 27 CFR Part 10, Commercial Bribery. You may obtain a copy of this order by... Administrator. 10.5 Section 10.5 Alcohol, Tobacco Products and Firearms ALCOHOL AND TOBACCO TAX AND TRADE BUREAU... Administrator. Most of the regulatory authorities of the Administrator contained in this part are delegated...

  14. 27 CFR 10.5 - Delegations of the Administrator.

    Code of Federal Regulations, 2013 CFR

    2013-04-01

    ... Administrator's Authorities in 27 CFR Part 10, Commercial Bribery. You may obtain a copy of this order by... Administrator. 10.5 Section 10.5 Alcohol, Tobacco Products and Firearms ALCOHOL AND TOBACCO TAX AND TRADE BUREAU... Administrator. Most of the regulatory authorities of the Administrator contained in this part are delegated...

  15. 27 CFR 10.5 - Delegations of the Administrator.

    Code of Federal Regulations, 2014 CFR

    2014-04-01

    ... Administrator's Authorities in 27 CFR Part 10, Commercial Bribery. You may obtain a copy of this order by... Administrator. 10.5 Section 10.5 Alcohol, Tobacco Products and Firearms ALCOHOL AND TOBACCO TAX AND TRADE BUREAU... Administrator. Most of the regulatory authorities of the Administrator contained in this part are delegated...

  16. 27 CFR 10.5 - Delegations of the Administrator.

    Code of Federal Regulations, 2012 CFR

    2012-04-01

    ... Administrator's Authorities in 27 CFR Part 10, Commercial Bribery. You may obtain a copy of this order by... Administrator. 10.5 Section 10.5 Alcohol, Tobacco Products and Firearms ALCOHOL AND TOBACCO TAX AND TRADE BUREAU... Administrator. Most of the regulatory authorities of the Administrator contained in this part are delegated...

  17. 33 CFR 49.10-5 - Payment of moneys due.

    Code of Federal Regulations, 2010 CFR

    2010-07-01

    ... 33 Navigation and Navigable Waters 1 2010-07-01 2010-07-01 false Payment of moneys due. 49.10-5... PAYMENT OF AMOUNTS DUE MENTALLY INCOMPETENT COAST GUARD PERSONNEL Reports and Moneys § 49.10-5 Payment of moneys due. Upon the appointment of a trustee or trustees to receive moneys due an incompetent,...

  18. 33 CFR 49.10-5 - Payment of moneys due.

    Code of Federal Regulations, 2011 CFR

    2011-07-01

    ... 33 Navigation and Navigable Waters 1 2011-07-01 2011-07-01 false Payment of moneys due. 49.10-5... PAYMENT OF AMOUNTS DUE MENTALLY INCOMPETENT COAST GUARD PERSONNEL Reports and Moneys § 49.10-5 Payment of moneys due. Upon the appointment of a trustee or trustees to receive moneys due an incompetent,...

  19. 33 CFR 49.10-5 - Payment of moneys due.

    Code of Federal Regulations, 2014 CFR

    2014-07-01

    ... 33 Navigation and Navigable Waters 1 2014-07-01 2014-07-01 false Payment of moneys due. 49.10-5... PAYMENT OF AMOUNTS DUE MENTALLY INCOMPETENT COAST GUARD PERSONNEL Reports and Moneys § 49.10-5 Payment of moneys due. Upon the appointment of a trustee or trustees to receive moneys due an incompetent,...

  20. 33 CFR 49.10-5 - Payment of moneys due.

    Code of Federal Regulations, 2013 CFR

    2013-07-01

    ... 33 Navigation and Navigable Waters 1 2013-07-01 2013-07-01 false Payment of moneys due. 49.10-5... PAYMENT OF AMOUNTS DUE MENTALLY INCOMPETENT COAST GUARD PERSONNEL Reports and Moneys § 49.10-5 Payment of moneys due. Upon the appointment of a trustee or trustees to receive moneys due an incompetent,...

  1. 33 CFR 49.10-5 - Payment of moneys due.

    Code of Federal Regulations, 2012 CFR

    2012-07-01

    ... 33 Navigation and Navigable Waters 1 2012-07-01 2012-07-01 false Payment of moneys due. 49.10-5... PAYMENT OF AMOUNTS DUE MENTALLY INCOMPETENT COAST GUARD PERSONNEL Reports and Moneys § 49.10-5 Payment of moneys due. Upon the appointment of a trustee or trustees to receive moneys due an incompetent,...

  2. 15 CFR 10.5 - Development of a recommended standard.

    Code of Federal Regulations, 2010 CFR

    2010-01-01

    ... 15 Commerce and Foreign Trade 1 2010-01-01 2010-01-01 false Development of a recommended standard... DEVELOPMENT OF VOLUNTARY PRODUCT STANDARDS § 10.5 Development of a recommended standard. (a) The Standard... Department or the chairman of this committee. If conducted by the chairman, a report of the vote shall...

  3. 15 CFR 10.5 - Development of a recommended standard.

    Code of Federal Regulations, 2011 CFR

    2011-01-01

    ... 15 Commerce and Foreign Trade 1 2011-01-01 2011-01-01 false Development of a recommended standard... DEVELOPMENT OF VOLUNTARY PRODUCT STANDARDS § 10.5 Development of a recommended standard. (a) The Standard... Department or the chairman of this committee. If conducted by the chairman, a report of the vote shall...

  4. 46 CFR 58.10-5 - Gasoline engine installations.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... MACHINERY AND RELATED SYSTEMS Internal Combustion Engine Installations § 58.10-5 Gasoline engine... flame arrester complying with SAE J-1928 (incorporated by reference; see 46 CFR 58.03-1) or UL 1111 (incorporated by reference; see 46 CFR 58.03-1) and marked accordingly. The flame arrester must be...

  5. 46 CFR 58.10-5 - Gasoline engine installations.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... MACHINERY AND RELATED SYSTEMS Internal Combustion Engine Installations § 58.10-5 Gasoline engine... flame arrester complying with SAE J-1928 (incorporated by reference; see 46 CFR 58.03-1) or UL 1111 (incorporated by reference; see 46 CFR 58.03-1) and marked accordingly. The flame arrester must be...

  6. 46 CFR 58.10-5 - Gasoline engine installations.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... MACHINERY AND RELATED SYSTEMS Internal Combustion Engine Installations § 58.10-5 Gasoline engine... flame arrester complying with SAE J-1928 (incorporated by reference; see 46 CFR 58.03-1) or UL 1111 (incorporated by reference; see 46 CFR 58.03-1) and marked accordingly. The flame arrester must be...

  7. 46 CFR 58.10-5 - Gasoline engine installations.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... MACHINERY AND RELATED SYSTEMS Internal Combustion Engine Installations § 58.10-5 Gasoline engine... flame arrester complying with SAE J-1928 (incorporated by reference; see 46 CFR 58.03-1) or UL 1111 (incorporated by reference; see 46 CFR 58.03-1) and marked accordingly. The flame arrester must be...

  8. 46 CFR 58.10-5 - Gasoline engine installations.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... MACHINERY AND RELATED SYSTEMS Internal Combustion Engine Installations § 58.10-5 Gasoline engine... flame arrester complying with SAE J-1928 (incorporated by reference; see 46 CFR 58.03-1) or UL 1111 (incorporated by reference; see 46 CFR 58.03-1) and marked accordingly. The flame arrester must be...

  9. 28 CFR 10.5 - Incorporation of papers previously filed.

    Code of Federal Regulations, 2013 CFR

    2013-07-01

    ... 28 Judicial Administration 1 2013-07-01 2013-07-01 false Incorporation of papers previously filed... CARRYING ON ACTIVITIES WITHIN THE UNITED STATES Registration Statement § 10.5 Incorporation of papers previously filed. Papers and documents already filed with the Attorney General pursuant to the said act...

  10. 28 CFR 10.5 - Incorporation of papers previously filed.

    Code of Federal Regulations, 2010 CFR

    2010-07-01

    ... 28 Judicial Administration 1 2010-07-01 2010-07-01 false Incorporation of papers previously filed... CARRYING ON ACTIVITIES WITHIN THE UNITED STATES Registration Statement § 10.5 Incorporation of papers previously filed. Papers and documents already filed with the Attorney General pursuant to the said act...

  11. 28 CFR 10.5 - Incorporation of papers previously filed.

    Code of Federal Regulations, 2012 CFR

    2012-07-01

    ... 28 Judicial Administration 1 2012-07-01 2012-07-01 false Incorporation of papers previously filed... CARRYING ON ACTIVITIES WITHIN THE UNITED STATES Registration Statement § 10.5 Incorporation of papers previously filed. Papers and documents already filed with the Attorney General pursuant to the said act...

  12. 28 CFR 10.5 - Incorporation of papers previously filed.

    Code of Federal Regulations, 2011 CFR

    2011-07-01

    ... 28 Judicial Administration 1 2011-07-01 2011-07-01 false Incorporation of papers previously filed... CARRYING ON ACTIVITIES WITHIN THE UNITED STATES Registration Statement § 10.5 Incorporation of papers previously filed. Papers and documents already filed with the Attorney General pursuant to the said act...

  13. 28 CFR 10.5 - Incorporation of papers previously filed.

    Code of Federal Regulations, 2014 CFR

    2014-07-01

    ... 28 Judicial Administration 1 2014-07-01 2014-07-01 false Incorporation of papers previously filed... CARRYING ON ACTIVITIES WITHIN THE UNITED STATES Registration Statement § 10.5 Incorporation of papers previously filed. Papers and documents already filed with the Attorney General pursuant to the said act...

  14. 46 CFR 34.10-5 - Fire pumps-T/ALL.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... 46 Shipping 1 2014-10-01 2014-10-01 false Fire pumps-T/ALL. 34.10-5 Section 34.10-5 Shipping COAST... § 34.10-5 Fire pumps—T/ALL. (a) Tankships shall be equipped with independently driven fire pumps in accordance with table 34.10-5(a). Table 34.10-5(a)—Fire Pumps Size vessel,L.O.A. (feet) Over— Not...

  15. 46 CFR 50.10-5 - Coast Guard District Commander or District Commander.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 46 Shipping 2 2010-10-01 2010-10-01 false Coast Guard District Commander or District Commander. 50.10-5 Section 50.10-5 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY (CONTINUED) MARINE ENGINEERING GENERAL PROVISIONS Definition of Terms Used in This Subchapter § 50.10-5 Coast Guard District Commander or District Commander. The term...

  16. 46 CFR 50.10-5 - Coast Guard District Commander or District Commander.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... 46 Shipping 2 2014-10-01 2014-10-01 false Coast Guard District Commander or District Commander. 50.10-5 Section 50.10-5 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY (CONTINUED) MARINE ENGINEERING GENERAL PROVISIONS Definition of Terms Used in This Subchapter § 50.10-5 Coast Guard District Commander or District Commander. The term...

  17. 46 CFR 50.10-5 - Coast Guard District Commander or District Commander.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... 46 Shipping 2 2013-10-01 2013-10-01 false Coast Guard District Commander or District Commander. 50.10-5 Section 50.10-5 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY (CONTINUED) MARINE ENGINEERING GENERAL PROVISIONS Definition of Terms Used in This Subchapter § 50.10-5 Coast Guard...

  18. 46 CFR 50.10-5 - Coast Guard District Commander or District Commander.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... 46 Shipping 2 2012-10-01 2012-10-01 false Coast Guard District Commander or District Commander. 50.10-5 Section 50.10-5 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY (CONTINUED) MARINE ENGINEERING GENERAL PROVISIONS Definition of Terms Used in This Subchapter § 50.10-5 Coast Guard...

  19. 46 CFR 50.10-5 - Coast Guard District Commander or District Commander.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... 46 Shipping 2 2011-10-01 2011-10-01 false Coast Guard District Commander or District Commander. 50.10-5 Section 50.10-5 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY (CONTINUED) MARINE ENGINEERING GENERAL PROVISIONS Definition of Terms Used in This Subchapter § 50.10-5 Coast Guard...

  20. 46 CFR 34.10-5 - Fire pumps-T/ALL.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 46 Shipping 1 2010-10-01 2010-10-01 false Fire pumps-T/ALL. 34.10-5 Section 34.10-5 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY TANK VESSELS FIREFIGHTING EQUIPMENT Fire Main System, Details § 34.10-5 Fire pumps—T/ALL. (a) Tankships shall be equipped with independently driven fire pumps...

  1. 46 CFR 38.10-5 - Filling and discharge pipes-TB/ALL.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 46 Shipping 1 2010-10-01 2010-10-01 false Filling and discharge pipes-TB/ALL. 38.10-5 Section 38.10-5 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY TANK VESSELS LIQUEFIED FLAMMABLE GASES Piping, Valves, Fittings, and Accessory Equipment § 38.10-5 Filling and discharge pipes—TB/ALL....

  2. 46 CFR 30.10-5b - Cargo control station-TB/ALL.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... 46 Shipping 1 2011-10-01 2011-10-01 false Cargo control station-TB/ALL. 30.10-5b Section 30.10-5b Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY TANK VESSELS GENERAL PROVISIONS Definitions § 30.10-5b Cargo control station—TB/ALL. The term cargo control station means a location that is...

  3. 46 CFR 30.10-5b - Cargo control station-TB/ALL.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 46 Shipping 1 2010-10-01 2010-10-01 false Cargo control station-TB/ALL. 30.10-5b Section 30.10-5b Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY TANK VESSELS GENERAL PROVISIONS Definitions § 30.10-5b Cargo control station—TB/ALL. The term cargo control station means a location that is...

  4. 46 CFR 31.10-5 - Inspection of new tank vessels-TB/ALL.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... 46 Shipping 1 2011-10-01 2011-10-01 false Inspection of new tank vessels-TB/ALL. 31.10-5 Section 31.10-5 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY TANK VESSELS INSPECTION AND CERTIFICATION Inspections § 31.10-5 Inspection of new tank vessels—TB/ALL. (a) Plans. Triplicate copies...

  5. 46 CFR 39.10-5 - Incorporation by reference-TB/ALL.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... 46 Shipping 1 2012-10-01 2012-10-01 false Incorporation by reference-TB/ALL. 39.10-5 Section 39.10-5 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY TANK VESSELS VAPOR CONTROL SYSTEMS General § 39.10-5 Incorporation by reference—TB/ALL. (a) Certain materials are incorporated by reference...

  6. 46 CFR 39.10-5 - Incorporation by reference-TB/ALL.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... 46 Shipping 1 2011-10-01 2011-10-01 false Incorporation by reference-TB/ALL. 39.10-5 Section 39.10-5 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY TANK VESSELS VAPOR CONTROL SYSTEMS General § 39.10-5 Incorporation by reference—TB/ALL. (a) Certain materials are incorporated by reference...

  7. 46 CFR 31.10-5 - Inspection of new tank vessels-TB/ALL.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 46 Shipping 1 2010-10-01 2010-10-01 false Inspection of new tank vessels-TB/ALL. 31.10-5 Section 31.10-5 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY TANK VESSELS INSPECTION AND CERTIFICATION Inspections § 31.10-5 Inspection of new tank vessels—TB/ALL. (a) Plans. Triplicate copies...

  8. 33 CFR 1.10-5 - Public availability of records and documents.

    Code of Federal Regulations, 2012 CFR

    2012-07-01

    ... and documents. 1.10-5 Section 1.10-5 Navigation and Navigable Waters COAST GUARD, DEPARTMENT OF HOMELAND SECURITY GENERAL GENERAL PROVISIONS Public Availability of Information § 1.10-5 Public..., 2100 2nd St. SW., Stop 7101, Washington, DC 20593-7101. (b) Each person desiring to inspect a record...

  9. 46 CFR 31.10-5 - Inspection of new tank vessels-TB/ALL.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... 46 Shipping 1 2012-10-01 2012-10-01 false Inspection of new tank vessels-TB/ALL. 31.10-5 Section 31.10-5 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY TANK VESSELS INSPECTION AND CERTIFICATION Inspections § 31.10-5 Inspection of new tank vessels—TB/ALL. (a) Plans. Triplicate copies...

  10. 33 CFR 1.10-5 - Public availability of records and documents.

    Code of Federal Regulations, 2013 CFR

    2013-07-01

    ... and documents. 1.10-5 Section 1.10-5 Navigation and Navigable Waters COAST GUARD, DEPARTMENT OF HOMELAND SECURITY GENERAL GENERAL PROVISIONS Public Availability of Information § 1.10-5 Public..., 2100 2nd St. SW., Stop 7101, Washington, DC 20593-7101. (b) Each person desiring to inspect a record...

  11. 33 CFR 1.10-5 - Public availability of records and documents.

    Code of Federal Regulations, 2011 CFR

    2011-07-01

    ... and documents. 1.10-5 Section 1.10-5 Navigation and Navigable Waters COAST GUARD, DEPARTMENT OF HOMELAND SECURITY GENERAL GENERAL PROVISIONS Public Availability of Information § 1.10-5 Public..., 2100 2nd St. SW., Stop 7101, Washington, DC 20593-7101. (b) Each person desiring to inspect a record...

  12. 33 CFR 1.10-5 - Public availability of records and documents.

    Code of Federal Regulations, 2010 CFR

    2010-07-01

    ... and documents. 1.10-5 Section 1.10-5 Navigation and Navigable Waters COAST GUARD, DEPARTMENT OF HOMELAND SECURITY GENERAL GENERAL PROVISIONS Public Availability of Information § 1.10-5 Public..., 2100 2nd St. SW., Stop 7101, Washington, DC 20593-7101. (b) Each person desiring to inspect a record...

  13. 46 CFR 39.10-5 - Incorporation by reference-TB/ALL.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 46 Shipping 1 2010-10-01 2010-10-01 false Incorporation by reference-TB/ALL. 39.10-5 Section 39.10-5 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY TANK VESSELS VAPOR CONTROL SYSTEMS General § 39.10-5 Incorporation by reference—TB/ALL. (a) Certain materials are incorporated by reference...

  14. 33 CFR 1.10-5 - Public availability of records and documents.

    Code of Federal Regulations, 2014 CFR

    2014-07-01

    ... and documents. 1.10-5 Section 1.10-5 Navigation and Navigable Waters COAST GUARD, DEPARTMENT OF HOMELAND SECURITY GENERAL GENERAL PROVISIONS Public Availability of Information § 1.10-5 Public..., 2100 2nd St. SW., Stop 7101, Washington, DC 20593-7101. (b) Each person desiring to inspect a record...

  15. 46 CFR 38.10-5 - Filling and discharge pipes-TB/ALL.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... 46 Shipping 1 2013-10-01 2013-10-01 false Filling and discharge pipes-TB/ALL. 38.10-5 Section 38.10-5 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY TANK VESSELS LIQUEFIED FLAMMABLE GASES Piping, Valves, Fittings, and Accessory Equipment § 38.10-5 Filling and discharge pipes—TB/ALL. (a) Filling and discharge connections shall be...

  16. 46 CFR 38.10-5 - Filling and discharge pipes-TB/ALL.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... 46 Shipping 1 2012-10-01 2012-10-01 false Filling and discharge pipes-TB/ALL. 38.10-5 Section 38.10-5 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY TANK VESSELS LIQUEFIED FLAMMABLE GASES Piping, Valves, Fittings, and Accessory Equipment § 38.10-5 Filling and discharge pipes—TB/ALL. (a) Filling and discharge connections shall be...

  17. 46 CFR 35.10-5 - Muster lists, emergency signals, and manning-T/ALL.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... 46 Shipping 1 2013-10-01 2013-10-01 false Muster lists, emergency signals, and manning-T/ALL. 35.10-5 Section 35.10-5 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY TANK VESSELS OPERATIONS Fire and Emergency Requirements § 35.10-5 Muster lists, emergency signals, and manning—T/ALL. The requirements for muster lists, emergency signals,...

  18. 46 CFR 35.10-5 - Muster lists, emergency signals, and manning-T/ALL.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... 46 Shipping 1 2014-10-01 2014-10-01 false Muster lists, emergency signals, and manning-T/ALL. 35.10-5 Section 35.10-5 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY TANK VESSELS OPERATIONS Fire and Emergency Requirements § 35.10-5 Muster lists, emergency signals, and manning—T/ALL. The requirements for muster lists, emergency signals,...

  19. 46 CFR 35.10-5 - Muster lists, emergency signals, and manning-T/ALL.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 46 Shipping 1 2010-10-01 2010-10-01 false Muster lists, emergency signals, and manning-T/ALL. 35.10-5 Section 35.10-5 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY TANK VESSELS OPERATIONS Fire and Emergency Requirements § 35.10-5 Muster lists, emergency signals, and manning—T/ALL. The requirements for muster lists, emergency signals,...

  20. 46 CFR 35.10-5 - Muster lists, emergency signals, and manning-T/ALL.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... 46 Shipping 1 2011-10-01 2011-10-01 false Muster lists, emergency signals, and manning-T/ALL. 35.10-5 Section 35.10-5 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY TANK VESSELS OPERATIONS Fire and Emergency Requirements § 35.10-5 Muster lists, emergency signals, and manning—T/ALL. The requirements for muster lists, emergency signals,...

  1. 46 CFR 35.10-5 - Muster lists, emergency signals, and manning-T/ALL.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... 46 Shipping 1 2012-10-01 2012-10-01 false Muster lists, emergency signals, and manning-T/ALL. 35.10-5 Section 35.10-5 Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY TANK VESSELS OPERATIONS Fire and Emergency Requirements § 35.10-5 Muster lists, emergency signals, and manning—T/ALL. The requirements for muster lists, emergency signals,...

  2. 46 CFR 30.10-5a - Cargo area-TB/ALL.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... 46 Shipping 1 2011-10-01 2011-10-01 false Cargo area-TB/ALL. 30.10-5a Section 30.10-5a Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY TANK VESSELS GENERAL PROVISIONS Definitions § 30.10-5a Cargo area—TB/ALL. The term cargo area means that part of a vessel that includes the cargo tanks...

  3. 46 CFR 30.10-5a - Cargo area-TB/ALL.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 46 Shipping 1 2010-10-01 2010-10-01 false Cargo area-TB/ALL. 30.10-5a Section 30.10-5a Shipping COAST GUARD, DEPARTMENT OF HOMELAND SECURITY TANK VESSELS GENERAL PROVISIONS Definitions § 30.10-5a Cargo area—TB/ALL. The term cargo area means that part of a vessel that includes the cargo tanks...

  4. 41 CFR 302-10.5 - May I transport a mobile home over water?

    Code of Federal Regulations, 2013 CFR

    2013-07-01

    ... 41 Public Contracts and Property Management 4 2013-07-01 2012-07-01 true May I transport a mobile home over water? 302-10.5 Section 302-10.5 Public Contracts and Property Management Federal Travel... transport a mobile home over water? Yes, you may transport a mobile home over water when both the points...

  5. 41 CFR 302-10.5 - May I transport a mobile home over water?

    Code of Federal Regulations, 2014 CFR

    2014-07-01

    ... 41 Public Contracts and Property Management 4 2014-07-01 2014-07-01 false May I transport a mobile home over water? 302-10.5 Section 302-10.5 Public Contracts and Property Management Federal Travel... transport a mobile home over water? Yes, you may transport a mobile home over water when both the points...

  6. 41 CFR 302-10.5 - May I transport a mobile home over water?

    Code of Federal Regulations, 2012 CFR

    2012-07-01

    ... 41 Public Contracts and Property Management 4 2012-07-01 2012-07-01 false May I transport a mobile home over water? 302-10.5 Section 302-10.5 Public Contracts and Property Management Federal Travel Regulation System RELOCATION ALLOWANCES TRANSPORTATION AND STORAGE OF PROPERTY 10-ALLOWANCES FOR TRANSPORTATION OF MOBILE HOMES AND BOATS USED AS...

  7. 41 CFR 302-10.5 - May I transport a mobile home over water?

    Code of Federal Regulations, 2010 CFR

    2010-07-01

    ... 41 Public Contracts and Property Management 4 2010-07-01 2010-07-01 false May I transport a mobile home over water? 302-10.5 Section 302-10.5 Public Contracts and Property Management Federal Travel... transport a mobile home over water? Yes, you may transport a mobile home over water when both the points...

  8. 41 CFR 302-10.5 - May I transport a mobile home over water?

    Code of Federal Regulations, 2011 CFR

    2011-07-01

    ... 41 Public Contracts and Property Management 4 2011-07-01 2011-07-01 false May I transport a mobile home over water? 302-10.5 Section 302-10.5 Public Contracts and Property Management Federal Travel Regulation System RELOCATION ALLOWANCES TRANSPORTATION AND STORAGE OF PROPERTY 10-ALLOWANCES...

  9. 20 CFR 10.5 - What definitions apply to the regulations in this subchapter?

    Code of Federal Regulations, 2014 CFR

    2014-04-01

    ... 20 Employees' Benefits 1 2014-04-01 2012-04-01 true What definitions apply to the regulations in this subchapter? 10.5 Section 10.5 Employees' Benefits OFFICE OF WORKERS' COMPENSATION PROGRAMS, DEPARTMENT OF LABOR FEDERAL EMPLOYEES' COMPENSATION ACT CLAIMS FOR COMPENSATION UNDER THE FEDERAL EMPLOYEES' COMPENSATION ACT, AS AMENDED...

  10. 46 CFR 34.10-5 - Fire pumps-T/ALL.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... at least 2 fire pumps. 3 From hydrants having greatest pressure drop between fire-pump(s) and nozzles... of water required by table 34.10-5(a) from the outlets having the greatest pressure drop between fire... international voyage, each required fire pump, while delivering water through the fire main system at a......

  11. 46 CFR 34.10-5 - Fire pumps-T/ALL.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... at least 2 fire pumps. 3 From hydrants having greatest pressure drop between fire-pump(s) and nozzles... of water required by table 34.10-5(a) from the outlets having the greatest pressure drop between fire... international voyage, each required fire pump, while delivering water through the fire main system at a......

  12. 19 CFR 10.5 - Shooks and staves; cloth boards; port director's account.

    Code of Federal Regulations, 2010 CFR

    2010-04-01

    ... 19 Customs Duties 1 2010-04-01 2010-04-01 false Shooks and staves; cloth boards; port director's... Provisions Articles Exported and Returned § 10.5 Shooks and staves; cloth boards; port director's account. (a... returned as boxes or barrels shall file in triplicate with the director of the port of exportation,...

  13. 46 CFR 54.10-5 - Maximum allowable working pressure (reproduces UG-98).

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... ENGINEERING PRESSURE VESSELS Inspection, Reports, and Stamping § 54.10-5 Maximum allowable working pressure... reference; see 46 CFR 54.01-1.) (b) The maximum allowable working pressure for a vessel part is the maximum... loadings listed in UG-22 of section VIII of the ASME Boiler and Pressure Vessel Code (see 46 CFR...

  14. 46 CFR 54.10-5 - Maximum allowable working pressure (reproduces UG-98).

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... ENGINEERING PRESSURE VESSELS Inspection, Reports, and Stamping § 54.10-5 Maximum allowable working pressure... reference; see 46 CFR 54.01-1.) (b) The maximum allowable working pressure for a vessel part is the maximum... loadings listed in UG-22 of section VIII of the ASME Boiler and Pressure Vessel Code (see 46 CFR...

  15. Evidence for upper Great Lakes waters in the Erie Basin until 10. 5 ka

    SciTech Connect

    Tinkler, K.J. . Dept. of Geology) Lewis, C.F.M. ); Anderson, T.W. ); Cameron, G.D.M.

    1992-01-01

    Modern recession at Niagara Falls suggests that Erie basin flow alone produces a narrower gorge with recession reduced by an order of magnitude. Gorge interpretations relate dimensions to stages of Great Lakes evolution. A published date of 9.8 ka, for upper river shells at Whirlpool State Park favors an interpretation implying 3.5 kilometers of gorge were cut in the period 12.5 ka to 10.5 ka at a rate of 1.75 m/a, a value consistent with the pre-twentieth century rate of 1.37--1.52 m/a. Erie basin discharge alone would be insufficient to excavate the length of gorge seen. Stratigraphic studies of offshore sediments in lake Erie north-east of Long Point based on seismic profiles and core samples show evidence of lake level change. Following decline of the post-Whittlesey (< 13 ka) southwestward-draining proglacial lakes in the Erie basin and the establishment of Lake Iroquois at about 12.5 ka water levels fell to a control on the Niagara Peninsula. Glacial meltwater continued to pass through the Erie basin until 10.5 ka. Negative shifts in delta O-18 suggest increased meltwater flow through the Erie basin and increased lake level between 11 ka and 10.5 ka. An erosional unconformity, lag sediments, and a distinct former shoreface suggest that lake level subsequently fell in the Long Point area of eastern Lake Erie to about 30m below present by about 10.5 ka when meltwater runoff from the upper Great Lakes by-passed Erie basin. Both the lake cores and the gorge recession are consistent with a computational model of flow out to the Erie basin. According to the model great Lakes outflow, augmented by inflow from Lake Agassiz between 11 to 10.5 ka, would yield shorelines at the height attributed to Lake Tonawanda (180--182m), the immediate source of the Niagara River.

  16. 31 CFR 10.5 - Application to become an enrolled agent, enrolled retirement plan agent, or registered tax return...

    Code of Federal Regulations, 2014 CFR

    2014-07-01

    ... 31 Money and Finance: Treasury 1 2014-07-01 2014-07-01 false Application to become an enrolled agent, enrolled retirement plan agent, or registered tax return preparer. 10.5 Section 10.5 Money and Finance: Treasury Office of the Secretary of the Treasury PRACTICE BEFORE THE INTERNAL REVENUE SERVICE Rules Governing Authority to Practice §...

  17. The rise and fall of Lake Bonneville between 45 and 10.5 ka

    USGS Publications Warehouse

    Benson, L.V.; Lund, S.P.; Smoot, J.P.; Rhode, D.E.; Spencer, R.J.; Verosub, K.L.; Louderback, L.A.; Johnson, C.A.; Rye, R.O.; Negrini, R.M.

    2011-01-01

    A sediment core taken from the western edge of the Bonneville Basin has provided high-resolution proxy records of relative lake-size change for the period 45.1-10.5 calendar ka (hereafter ka). Age control was provided by a paleomagnetic secular variation (PSV)-based age model for Blue Lake core BL04-4. Continuous records of ??18O and total inorganic carbon (TIC) generally match an earlier lake-level envelope based on outcrops and geomorphic features, but with differences in the timing of some hydrologic events/states. The Stansbury Oscillation was found to consist of two oscillations centered on 25 and 24 ka. Lake Bonneville appears to have reached its geomorphic highstand and began spilling at 18.5 ka. The fall from the highstand to the Provo level occurred at 17.0 ka and the lake intermittently overflowed at the Provo level until 15.2 ka, at which time the lake fell again, bottoming out at ~14.7 ka. The lake also fell briefly below the Provo level at ~15.9 ka. Carbonate and ??18O data indicate that between 14.7 and 13.1 ka the lake slowly rose to the Gilbert shoreline and remained at about that elevation until 11.6 ka, when it fell again. Chemical and sedimentological data indicate that a marsh formed in the Blue Lake area at 10.5 ka.Relatively dry periods in the BL04-4 records are associated with Heinrich events H1-H4, suggesting that either the warming that closely followed a Heinrich event increased the evaporation rate in the Bonneville Basin and (or) that the core of the polar jet stream (PJS) shifted north of the Bonneville Basin in response to massive losses of ice from the Laurentide Ice Sheet (LIS) during the Heinrich event. The second Stansbury Oscillation occurred during Heinrich event H2, and the Gilbert wet event occurred during the Younger Dryas cold interval. Several relatively wet events in BL04-4 occur during Dansgaard-Oeschger (DO) warm events.The growth of the Bear River glacier between 32 and 17 ka paralleled changes in the values of proxy

  18. Mach-Zehnder interferometry at framing rates of 10. 5--21 GHz

    SciTech Connect

    Houtman, H.; Legault, L.E.; Meyer, J.

    1987-03-15

    A simple beam splitter arrangement is used to divide a single ultrashort optical pulse into four beams of accurately known jitter-free delay. The 50-ps ruby laser beams are used in a Mach-Zehnder interferometer to produce four interferograms in one shot of the CO/sub 2/-laser-irradiated plasma at an interframe delay of 95 ps. Fringe straightness of <1/10 wave error is attained in all four frames by overlapping reference and scene beams precisely on the film while relaxing the constraint of the high spatial coherence necessary in shearing and folding shear interferometry. Such high fringe quality is required to record properly the observed fractional fringe shifts in a plasma of electron density up to n/sub e/ = 5 x 10/sup 18/ cm/sup -3/. The four-frame interferogram, recorded on Polaroid-type 667 film, is available immediately after the shot is taken. Neither a streak camera for recording timing sequences nor wavelength filters for rejection of plasma light was required. Simple rearrangement of optical components allows framing rates of 10.5 or 21.0 GHz.

  19. Pion interference correlations in pion-nucleus collisions at 10. 5 GeV/c

    SciTech Connect

    Wong, R.

    1983-01-01

    Inclusive reactions of pion, Ne collisions at 10.5 GeV/c have been studied. The pion intensity interference effect has been observed in identical pion (..pi../sup +/, ..pi../sup -/, and ..pi../sup -/, ..pi../sup -/) as well as non-identical (..pi../sup +/, ..pi../sup -/) pion pair correlations. A momentum dependence is observed in the interference correlation function at small momentum differences. Previously only the identical pion interference correlations have been reported. In this thesis, the non-identical pion pair correlation is also studied. The momentum dependence is also new. For (..pi../sup -/,..pi../sup +/) and (..pi../sup -/,..pi../sup -/) pairs, the enhancement is due mostly to pions with mom/sup */>600 MeV/c. However for (..pi../sup +/, ..pi../sup +/) pairs, the peak is due primarily to pions with mom<200 MeV/c. Using the method of Kopylov and Podgoretsky the identical pion source region is determined to be 4.1 +/- 2.3 fermis. Also the influence on the final state correlations by the Bose statistics, Coulomb, and nuclear forces is observed. The possibility of using the (..pi../sup +/,..pi../sup -/) pion pair correlations to examine the pions produced in the quark-gluon perturbative vacuum of high-energy nucleus-nucleus collisions is suggested.

  20. Production of PET radionuclides using a 10.5 MeV 3He RFQ accelerator

    NASA Astrophysics Data System (ADS)

    Link, Jeanne M.; Krohn, Kenneth A.; Bida, Jerry T.; DeHaas, Richard; Larson, Delbert J.; Johanning, Jeff; Young, Phillip E.; Pasquinelli, Ralph J.

    1999-06-01

    An RFQ linac has been built that accelerates 3He to 10.5 MeV for production of C, N, O, F isotopes for PET. The accelerator produces 70 μs pulses, at 360 Hz, a 2.5% duty cycle, with a peak current of ˜6 mAe. The RFQ delivers ˜100 μAe. A recirculating water target has been evaluated for production of 18F and low specific activity 15O. Recoil chemistry within the target has been evaluated to improve 15O specific activity. Gas targets have also been tested for production of 15O. 13N is made from carbon. Several target materials have been evaluated for producing 11C, including C, B and Be. The challenges of targetry for this high current, low energy machine led us to evaluate large, high aspect ratio windows and grid supports. The 3He RFQ is a useful research machine for testing targets for pulsed, high power density, low LET beams.

  1. Effect of 10.5 M Aqueous Urea on Helicobacter pylori Urease: A Molecular Dynamics Study.

    PubMed

    Minkara, Mona S; Weaver, Michael N; Merz, Kenneth M

    2015-07-01

    The effects of a 10.5 M solution of aqueous urea on Helicobacter pylori urease were investigated over the course of a 500 ns molecular dynamics (MD) simulation. The enzyme was solvated by 25321 water molecules, and additionally, 4788 urea molecules were added to the solution. Although concentrated urea solutions are known laboratory denaturants, the protein secondary structure is retained throughout the simulation largely because of the short simulation time (urea denaturation occurs on the millisecond time scale). The relatively constant solvent accessible surface area over the last 400 ns of the simulation further confirms the overall lack of denaturation. The wide-open flap state observed previously in Klebsiella areogenes urease [Roberts, B. P., et al. (2012) J. Am. Chem. Soc. 134, 9934] and H. pylori [Minkara, M. S., et al. (2014) J. Chem. Theory Comput. 10, 1852-1862] was also identified in this aqueous urea simulation. Over the course of the trajectory, we were able to observe urea molecules entering the active site in proportions related to the extent of opening of the active site-covering flap. Furthermore, urea molecules were observed to approach the pentacoordinate Ni(2+) ion in position to bind in a manner consistent with the proposed initial coordination step of the hydrolysis mechanism. We also observed a specific and unique pattern in the regions of the protein with a high root-mean-square fluctuation (rmsf). The high-rmsf regions in the β-chain form a horseshoelike arrangement surrounding the active site-covering flap on the surface of the protein. We hypothesize that the function of these regions is to both attract and shuttle urea toward the loop of the active site-covering flap before entry into the cavity. Indeed, urea is observed to interact with these regions for extended periods of simulation time before active site ingress. PMID:26057619

  2. Distributed Energy Resources Customer Adoption Model (DER-CAM), Investment & Planing Version 3.10.5.m

    2014-04-01

    Version 3.10.5 is a multi-year Decision Support tool for Distributed Generation (DG). DER-CAM was initially created as an exclusively economic energy model, able to find the cost minimizing combination and operation profile of a set of DER technologies that meet heat and electric loads of a single building or microgrid for a typical test year. Now, version 3.10.5.m solves for a multiple-year horizon the technology choice question, the appropriate capacity for each selected technology asmore » well as the operational and investment schedule. Optimized investment decisions are based on techno-economic criteria, along with site information such as energy loads, economic forecast, and technology characterization. Version 3.10.5 contains: 1. a PV and battery degradation model and 2. variable performance for technologies. Efficiency, investment costs, etc. can vary over time and model technology breakthroughs and advancements.« less

  3. Distributed Energy Resources Customer Adoption Model (DER-CAM), Investment & Planing Version 3.10.5.m

    SciTech Connect

    2014-04-01

    Version 3.10.5 is a multi-year Decision Support tool for Distributed Generation (DG). DER-CAM was initially created as an exclusively economic energy model, able to find the cost minimizing combination and operation profile of a set of DER technologies that meet heat and electric loads of a single building or microgrid for a typical test year. Now, version 3.10.5.m solves for a multiple-year horizon the technology choice question, the appropriate capacity for each selected technology as well as the operational and investment schedule. Optimized investment decisions are based on techno-economic criteria, along with site information such as energy loads, economic forecast, and technology characterization. Version 3.10.5 contains: 1. a PV and battery degradation model and 2. variable performance for technologies. Efficiency, investment costs, etc. can vary over time and model technology breakthroughs and advancements.

  4. Single mode operation with mid-IR hollow fibers in the range 5.1-10.5 µm.

    PubMed

    Sampaolo, Angelo; Patimisco, Pietro; Kriesel, Jason M; Tittel, Frank K; Scamarcio, Gaetano; Spagnolo, Vincenzo

    2015-01-12

    Single mode beam delivery in the mid-infrared spectral range 5.1-10.5 μm employing flexible hollow glass waveguides of 15 cm and 50 cm lengths, with metallic/dielectric internal layers and a bore diameter of 200 μm were demonstrated. Three quantum cascade lasers were coupled with the hollow core fibers. For a fiber length of 15 cm, we measured losses down to 1.55 dB at 5.4 μm and 0.9 dB at 10.5 μm. The influence of the launch conditions in the fiber on the propagation losses and on the beam profile at the waveguide exit was analyzed. At 10.5 µm laser wavelength we found near perfect agreement between measured and theoretical losses, while at ~5 µm and ~6 µm wavelengths the losses were higher than expected. This discrepancy can be explained considering an additional scattering loss effect, which scales as 1/λ(2) and is due to surface roughness of the metallic layer used to form the high-reflective internal layer structure of the hollow core waveguide. PMID:25835666

  5. Spin-Hall-Effect-Assisted Electroresistance in Antiferromagnets via 10(5) A/cm(2) dc Current.

    PubMed

    Han, Jiahao; Wang, Yuyan; Pan, Feng; Song, Cheng

    2016-01-01

    Antiferromagnet (AFM) spintronics with reduced electrical current is greatly expected to process information with high integration and low power consumption. In Pt/FeMn and Ta/FeMn hybrids, we observe significant resistance variation (up to 7% of the total resistance) manipulated by 10(5) A/cm(2) dc current. We have excluded the contribution of isotropic structural effects, and confirmed the critical role of the spin Hall injection from Pt (or Ta) to FeMn. This electrical current-manipulated resistance (i.e. electroresistance) is proposed to be attributed to the spin-Hall-effect-induced spin-orbit torque in FeMn. Similar results have also been detected in plain IrMn films, where the charge current generates spin current via the spin Hall effect with the existence of Ir atoms. All the measurements are free from external magnetic fields and ferromagnets. Our findings present an interesting step towards high-efficiency spintronic devices. PMID:27546199

  6. Thermal emission spectra of Mars (5.4-10.5 microns) - Evidence for sulfates, carbonates, and hydrates

    NASA Technical Reports Server (NTRS)

    Pollack, James B.; Roush, Ted; Witteborn, Fred; Bregman, Jesse; Wooden, Diane; Stoker, Carol; Toon, Owen B.

    1990-01-01

    Spectra of the Martian thermal emission in the 5.4-10.5 micron region are reported. Emission features at 7.8 and 9.7 microns are attributed to surface silicates, and an emission feature at 6.1 micron is attributed to a molecular water component of the surface material. An absorption band at 8.7 micron and a possible one at 9.8 microns is attributed to sulfate or bisulfate anions probably located at a distorted crystalline site, and an absorption band at 6.7 microns is attributed to carbonate or bicarbonate anions located in a distorted crystalline site. Spectral simulations indicate that the sulfate- and carbonate-bearing minerals are contained in the same particles of airborne dust as the dominant silicate minerals, that the dust optical depth is about 0.6 at a reference wavelength of 0.3 micron over the area of the observed spots, and that sulfates and carbonates constitute 10-15 percent and 1-3 percent by volume of the airborne dust, respectively.

  7. Extrasolar Giant Magnetospheric Response to Steady-state Stellar Wind Pressure at 10, 5, 1, and 0.2 au

    NASA Astrophysics Data System (ADS)

    Tilley, Matt A.; Harnett, Erika M.; Winglee, Robert M.

    2016-08-01

    A three-dimensional, multifluid simulation of a giant planet’s magnetospheric interaction with steady-state stellar wind from a Sun-like star was performed for four different orbital semimajor axes—10, 5, 1, and 0.2 au. We simulate the effect of the increasing, steady-state stellar wind pressure related to the planetary orbital semimajor axis on the global magnetospheric dynamics for a Saturn-like planet, including an Enceladus-like plasma torus. Mass-loss processes are shown to vary with orbital distance, with the centrifugal interchange instability displayed only in the 10 and 5 au cases, which reach a state of mass-loss equilibrium more slowly than the 1 or 0.2 au cases. The compression of the magnetosphere in the 1 and 0.2 au cases contributes to the quenching of the interchange process by increasing the ratio of total plasma thermal energy to corotational energy. The strength of field-aligned currents, associated with auroral radio emissions, is shown to increase in magnitude and latitudinal coverage with a corresponding shift equatorward from increased dynamic ram pressure experienced in the hotter orbits. Similar to observed hot Jovian planets, the warm exo-Saturn simulated in the current work shows enhanced ion density in the magnetosheath and magnetopause regions, as well as the plasma torus, which could contribute to altered transit signals, suggesting that for planets in warmer (>0.1 au) orbits, planetary magnetic field strengths and possibly exomoons—via the plasma torus—could be observable with future missions.

  8. Synthesis of CeFe10.5Mo1.5 with ThMn12-type structure by melt spinning

    SciTech Connect

    Zhou, C; Tessema, M; Meyer, MS; Pinkerton, FE

    2013-06-01

    Rare earth compounds RFe12_xMx with tetragonal ThMn12-type structure are of great research interest for potential applications as permanent magnets. These materials are known to serve as the precursors for nitriding and hydriding processes which in certain conditions can dramatically increase the Curie temperature, spontaneous magnetization, and affect the magnetic anisotropy. In this paper, we report the phase study of CeFe10.5Mo1.5 samples melt spun at various surface wheel speeds vs between 5 m/s and 60 m/s. The results from quantitative Rietveld analysis indicate that the as-spun ribbons are a mixture of primary CeFe10.5Mo1.5 phase with impurity phases such as Ce2Fe17, Fe-Mo alloy and CeFe2. When the wheel speed vs is below 25 m/s, CeFe10.5Mo1.5 phase accounts for greater than 85 wt% in the as-spun ribbons, while the Fe-Mo alloy is the only detectable impurity phase. Above v(s)=25 m/s, as the wheel speed increases, CeFe10.5Mo1.5 phase decreases monotonically to about 60 wt% at v(s)=6O m/s while the amounts of impurity phases increase. Thermogravimetric measurement indicates that the Curie temperature T-c. corresponding to CeFe10.5Mo1.5 phase is 341 K. As a result, the best performing sample melt spun at v(s),=15 m/s only exhibits an energy product BHmax=0.121 MGOe at room temperature. Although such a number is modest for a permanent magnet, further nitriding is expected to greatly enhance the Curie temperature, and hence the magnetic performance. (C) 2013 Elsevier B.V. All rights reserved.

  9. Deposition of calcium phosphate coatings using condensed phosphates (P2O7(4-) and P3O10(5-)) as phosphate source through induction heating.

    PubMed

    Zhou, Huan; Hou, Saisai; Zhang, Mingjie; Yang, Mengmeng; Deng, Linhong; Xiong, Xinbo; Ni, Xinye

    2016-12-01

    In present work condensed phosphates (P2O7(4-) and P3O10(5-)) were used as phosphate source in induction heating to deposit calcium phosphate coatings. The phase, morphology, and composition of different phosphate-related coatings were characterized and compared using XRD, FTIR, and SEM analyses. Results showed that P2O7(4-)formed calcium pyrophosphate hydrate coatings with interconnected cuboid-like particles. The as-deposited calcium tripolyphosphate hydrate coating with P3O10(5-) was mainly composed of flower-like particles assembled by plate-like crystals. The bioactivity and cytocompatibility of the coatings were also studied. Moreover, the feasibility of using hybrid phosphate sources for preparing and depositing coatings onto magnesium alloy was investigated. PMID:27612721

  10. Mirex residues in nontarget organisms after application of 10-5 bait for fire ant control, northeast Florida--1972-74.

    PubMed

    Wheeler, W B; Jouvenaz, D P; Wojcik, D P; Banks, W A; VanMiddelem, C H; Lofgren, C S; Nesbitt, S; Williams, L; Brown, R

    1977-12-01

    The 10-5 bait formulation of mirex insecticide was applied to a 20,000-acre area of northeast Florida. For 24 months after application, samples of a wide variety of fauna were collected and analyzed for mirex content. Insects accumulated mirex to the greatest extent in the first 6 months after application; most residues had decreased greatly by 12 months. Other invertebrates showed low mirex levels during the first 9 months after application and none after 12 months. Fish possessed low levels of insecticides for 9 months; amphibians showed mirex residues for 12 months after application. In general, reptiles had low levels throughout the 24-month period and mammals had higher levels, particularly in fat tissues. Birds consistently had low to moderate mirex levels. After a single application of 10-5 mirex bait, only relatively low levels of insecticide were detected in exposed fauna. After 24-months, mirex was found infrequently and at low levels. PMID:609513

  11. Synthesis and structure of a new halophosphate Sr3P3O10Cl with the flexible [P3O10]5- anions

    NASA Astrophysics Data System (ADS)

    Gao, Jianhua; Liu, Xi; Song, Limei; Sha, Xunshan; Zhao, Pan; Guo, Ping

    2016-05-01

    A new halophosphate crystal Sr3P3O10Cl was grown in molten chloride flux media. It crystallizes in the centrosymmetric orthorhombic space group Pnma (No. 62) with a = 10.617(2) Å, b = 10.736(2) Å, and c = 8.7354(17) Å. In the structure, the basic building unit is the [P3O10]5- anion, which is consist of three PO4 tetrahedra by sharing the corner oxygen atoms. The two Sr atoms and the Cl atom are linked to construct an infinite [Sr3Cl]5+ chain. The [P3O10]5- anions are interconnected with the [Sr3Cl]5+ chains to form a three-dimensional frameworks. Additionally, the first-principle calculation was employed to obtain the band structures and densities of states.

  12. Reducing the linewidth of a diode laser below 30 Hz by stabilization to a reference cavity with a finesse above 10(5).

    PubMed

    Schoof, A; Grünert, J; Ritter, S; Hemmerich, A

    2001-10-15

    An extended-cavity diode laser operating in the Littrow configuration emitting near 657 nm is stabilized through its injection current to a reference cavity with a finesse of more than 10(5) and a corresponding resonance linewidth of 14 kHz. The laser linewidth is reduced from a few megahertz to a value below 30 Hz. The compact and robust setup appears ideal as a portable optical frequency standard that uses the calcium intercombination line. PMID:18049663

  13. Heat transfer investigation of two Langley Research Center delta wing configurations at a Mach number of 10.5, volume 1

    NASA Technical Reports Server (NTRS)

    Eaves, R. H.; Buchanan, T. D.; Warmbrod, J. D.; Johnson, C. B.

    1972-01-01

    Heat transfer tests for two delta wing configurations were conducted in the hypervelocity wind tunnel. The 24-inch long models were tested at a Mach number of approximately 10.5 and at angles of attack of 20, 40, and 60 degrees over a length Reynolds number range from 5 million to 23 million on 4 May to 4 June 1971. Heat transfer results were obtained from model surface heat gage measurements and thermographic phosphor paint.

  14. Space shuttle: Heat transfer investigation of the McDonnell-Douglas delta wing orbiter at a nominal Mach number of 10.5

    NASA Technical Reports Server (NTRS)

    Eaves, R. H.; Buchanan, T. D.

    1972-01-01

    Heat transfer tests for the delta wing orbiter were conducted in a hypervelocity wind tunnel. A 1.1 percent scale model was tested at a Mach number of approximately 10.5 over an angle of attack range from 10 to 60 degrees over a length Reynolds number range from 5 times 10 to the 6th power to 24 times 10 to the 6th power. Heat transfer results were obtained from model surface heat gage measurements and thermographic phosphor paint. Limited pressure measurements were obtained.

  15. Effect of ball milling and thermal treatment on exchange bias and magnetocaloric properties of Ni48Mn39.5Sn10.5Al2 ribbons

    NASA Astrophysics Data System (ADS)

    Czaja, P.; Przewoźnik, J.; Fitta, M.; Bałanda, M.; Chrobak, A.; Kania, B.; Zackiewicz, P.; Wójcik, A.; Szlezynger, M.; Maziarz, W.

    2016-03-01

    The combined effect of ball milling and subsequent heat treatment on microstructure, magnetic, magnetocaloric and exchange bias properties of Ni48Mn39.5Sn10.5Al2 ribbons is reported. The annealing treatment results in the increase of the critical martensitic transformation temperature. The magnetic entropy change ΔSM of the order of 7.9 and -2.3 J kg K-1 for the annealed 50-32 μm powder fraction is determined. This is less than in the as melt spun ribbon but appears at a considerably higher temperature. At the same time EB is decreased due to annealing treatment. This decrease is attributed to the strengthened ferromagnetic exchange coupling due heat induced stress and structural relaxation.

  16. Research on fast fault identification method of 10.5 kV/1.5 kA superconducting fault current limiter

    NASA Astrophysics Data System (ADS)

    Zhang, Zhifeng; Sun, Qiang; Xiao, Liye; Liu, Daqian; Qiu, Ming; Qiu, Qinquan; Zhang, Guomin; Dai, Shaotao; Lin, Liangzhen

    2014-09-01

    Superconducting fault current limiter (SFCL) is a prospective electric devices connected in series in power grid to limit short-circuit current. A 10.5 kV/1.5 kA 3-phase SFCL with HTS coil of 6.24 mH was developed at IEECAS in China in 2005, which was operated in a local power grid in Hunan province for more than 11,000 h, and integrated lately in a superconducting power substation in Baiyin city in 2011 and is still running safely and reliably. In order to reduce the fault response time and enhance the performance of the SFCL, we analyzed the structure characteristics of the SFCL and discussed the variation of currents and voltages of the HTS coil and the bridge during the fault time. The simulation and tests results of power system validate the feasibility of the fast fault identification method.

  17. Coupled anion and cation ordering in Sr{sub 3}RFe{sub 4}O{sub 10.5} (R=Y, Ho, Dy) anion-deficientperovskites

    SciTech Connect

    Abakumov, Artem M.; D'Hondt, Hans; Rossell, Marta D.; Tsirlin, Alexander A.; Gutnikova, Olga; Filimonov, Dmitry S.; Schnelle, Walter; Rosner, Helge; Hadermann, Joke; Van Tendeloo, Gustaaf; Antipov, Evgeny V.

    2010-12-15

    The Sr{sub 3}RFe{sub 4}O{sub 10.5} (R=Y, Ho, Dy) anion-deficient perovskites were prepared using a solid-state reaction in evacuated sealed silica tubes. Transmission electron microscopy and {sup 57}Fe Moessbauer spectroscopy evidenced a complete A-cations and oxygen vacancies ordering. The structure model was further refined by ab initio structure relaxation, based on density functional theory calculations. The compounds crystallize in a tetragonal a{approx}2{radical}2a{sub p{approx}}11.3 A, c{approx}4c{sub p{approx}}16 A unit cell (a{sub p}: parameter of the perovskite subcell) with the P4{sub 2}/mnm space group. Oxygen vacancies reside in the (FeO{sub 5/4{open_square}3/4}) layers, comprising corner-sharing FeO{sub 4} tetrahedra and FeO{sub 5} tetragonal pyramids, which are sandwiched between the layers of the FeO{sub 6} octahedra. Smaller R atoms occupy the 9-fold coordinated position, whereas the 10-fold coordinated positions are occupied by larger Sr atoms. The Fe sublattice is ordered aniferromagnetically up to at least 500 K, while the rare-earth sublattice remains disordered down to 2 K. -- Graphical abstract: The Sr{sub 3}RFe{sub 4}O{sub 10.5} (R=Y, Ho, Dy) anion-deficient perovskites with a complete ordering of the A-cations and oxygen vacancies have been prepared using a solid-state reaction in evacuated sealed silica tubes. Oxygen vacancies reside in the (FeO{sub 5/43/4}) layers, comprising corner-sharing FeO{sub 4} tetrahedra and FeO{sub 5} tetragonal pyramids, which are sandwiched between the layers of the FeO{sub 6} octahedra. Smaller R atoms occupy the 9-fold coordinated position, whereas the 10-fold coordinated positions are occupied by larger Sr atoms.

  18. Evolution and CNO yields of Z = 10-5 stars and possible effects on carbon-enhanced metal-poor production

    NASA Astrophysics Data System (ADS)

    Gil-Pons, P.; Doherty, C. L.; Lau, H.; Campbell, S. W.; Suda, T.; Guilani, S.; Gutiérrez, J.; Lattanzio, J. C.

    2013-09-01

    Aims: Our main goals are to get a deeper insight into the evolution and final fates of intermediate-mass, extremely metal-poor (EMP) stars. We also aim to investigate the C, N, and O yields of these stars. Methods: Using the Monash University Stellar Evolution code MONSTAR we computed and analysed the evolution of stars of metallicity Z = 10-5 and masses between 4 and 9 M⊙, from their main sequence until the late thermally pulsing (super) asymptotic giant branch, TP-(S)AGB phase. Results: Our model stars experience a strong C, N, and O envelope enrichment either due to the second dredge-up process, the dredge-out phenomenon, or the third dredge-up early during the TP-(S)AGB phase. Their late evolution is therefore similar to that of higher metallicity objects. When using a standard prescription for the mass loss rates during the TP-(S)AGB phase, the computed stars are able to lose most of their envelopes before their cores reach the Chandrasekhar mass (mCh), so our standard models do not predict the occurrence of SNI1/2 for Z = 10-5 stars. However, we find that the reduction of only one order of magnitude in the mass-loss rates, which are particularly uncertain at this metallicity, would prevent the complete ejection of the envelope, allowing the stars to either explode as an SNI1/2 or become an electron-capture SN. Our calculations stop due to an instability near the base of the convective envelope that hampers further convergence and leaves remnant envelope masses between 0.25 M⊙ for our 4 M⊙ model and 1.5 M⊙ for our 9 M⊙ model. We present two sets of C, N, and O yields derived from our full calculations and computed under two different assumptions, namely, that the instability causes a practically instant loss of the remnant envelope or that the stars recover and proceed with further thermal pulses. Conclusions: Our results have implications for the early chemical evolution of the Universe and might provide another piece for the puzzle of the carbon

  19. Remote sounding of the tropical cirrus cloud temperature and optical depth using 6.5 and 10.5-micron radiometers during STEP

    NASA Technical Reports Server (NTRS)

    Liou, K. N.; Ou, S. C.; Takano, Y.; Valero, F. P. J.; Ackerman, T. P.

    1990-01-01

    A dual-channel retrieval technique involving the water vapor band at 6.5 microns and the window region at 10.5 microns has been developed to infer the temperature and emissivity of tropical anvils. This technique has been applied to data obtained from the ER-2 narrow field-of-view radiometers during two flights in the field observation of the Stratosphere-Troposphere Exchange Project near Darwin, Australia, January-February 1987. The retrieved cloud temperatures are between 190 and 240 K, while the cloud emissivities derived from the retrieval algorithm range from about 0.2 to 1. Moreover, the visible optical depths have been obtained from the cloud emissivity through a theoretical parameterization with values of 0.5-10. A significant portion of tropical cirrus clouds are found to have optical depths greater than about 6. Because of the parameterization, the present technique is unable to precisely determine the optical depth values for optically thick cirrus clouds.

  20. Molecular simulation of fluids with non-identical intermolecular potentials: Thermodynamic properties of 10-5 + 12-6 Mie potential binary mixtures

    NASA Astrophysics Data System (ADS)

    Stiegler, Thomas; Sadus, Richard J.

    2015-02-01

    General methods for combining interactions between particles characterised by non-identical intermolecular potentials are investigated. The combination methods are tested by performing molecular dynamics simulations to determine the pressure, energy, isochoric and isobaric heat capacities, thermal expansion coefficient, isothermal compressibility, Joule-Thomson coefficient, and speed of sound of 10-5 + 12-6 Mie potential binary mixtures. In addition to the two non-identical Mie potentials, mixtures are also studied with non-identical intermolecular parameters. The combination methods are compared with results obtained by simply averaging the Mie exponents. When either the energy or size parameters are non-identical, very significant differences emerge in the thermodynamic properties predicted by the alternative combination methods. The isobaric heat capacity is the thermodynamic property that is most affected by the relative magnitude of the intermolecular potential parameters and the method for combining non-identical potentials. Either the arithmetic or geometric combination of potentials provides a simple and effective way of performing simulations involving mixtures of components characterised by non-identical intermolecular potentials, which is independent of their functional form.

  1. A New Niobium Cluster Oxychloride Built from Interconnected Nb 6Cl 12O 6 Units: Na 0.21Nb 6Cl 10.5O 3

    NASA Astrophysics Data System (ADS)

    Gulo, Fakhili; Perrin, Christiane

    2002-01-01

    The new Na0.21Nb6Cl10.5O3 oxychloride was synthesized by a solid state route, from NaCl, Nb2O5, NbCl5, and Nb, heated at 680°C for 2 weeks. The structure was determined by single-crystal X-ray diffraction. It crystallizes in the trigonal system (Roverline3c space group, a=11.5048(1) Å, c=44.9446(7) Å, V=5151.88(10) Å3, Z=12). The structure is built from [(Nb6Cli9Oi3) Oa3Cla3] units, which share their inner and apical oxygens forming pseudolayers with short Nb-Nb intercluster distances (3.399 Å). Along the c axis, these layers are interconnected by apical-apical chlorines. The sodium atoms are randomly distributed in the voids arranged between two adjacent layers, in a deformed chlorine prismatic coordination. The developed formula Na0.21 [(Nb6Cli9Oi-a3/2)Oa-i3/2Cla-a3/2] leads to a number of valence electrons per cluster close to 14. This oxychloride will be compared to CsNb6Cl12O2 which we have previously isolated and which was the first example of a Nb6 oxyhalide involving Oi-a, Oa-i interunit connections.

  2. Molecular simulation of fluids with non-identical intermolecular potentials: Thermodynamic properties of 10-5 + 12-6 Mie potential binary mixtures

    SciTech Connect

    Stiegler, Thomas; Sadus, Richard J.

    2015-02-28

    General methods for combining interactions between particles characterised by non-identical intermolecular potentials are investigated. The combination methods are tested by performing molecular dynamics simulations to determine the pressure, energy, isochoric and isobaric heat capacities, thermal expansion coefficient, isothermal compressibility, Joule-Thomson coefficient, and speed of sound of 10-5 + 12-6 Mie potential binary mixtures. In addition to the two non-identical Mie potentials, mixtures are also studied with non-identical intermolecular parameters. The combination methods are compared with results obtained by simply averaging the Mie exponents. When either the energy or size parameters are non-identical, very significant differences emerge in the thermodynamic properties predicted by the alternative combination methods. The isobaric heat capacity is the thermodynamic property that is most affected by the relative magnitude of the intermolecular potential parameters and the method for combining non-identical potentials. Either the arithmetic or geometric combination of potentials provides a simple and effective way of performing simulations involving mixtures of components characterised by non-identical intermolecular potentials, which is independent of their functional form.

  3. Magneto-optical properties of Fe-Pt alloy films in the range 1.55-10.5 eV

    NASA Astrophysics Data System (ADS)

    Sugimoto, Toshio; Katayama, Toshikazu; Suzuki, Yoshishige; Koide, Tsuneharu; Sidara, Tetsuo; Yuri, Masatada; Itoh, Akiyoshi; Kawanishi, Kenji

    1993-12-01

    The optical and magneto-optical properties of as-deposited and annealed Fe51Pt49 films were investigated in the photon energy range 1.55-10.5 eV. The magneto-optical Kerr rotation (θK) spectra of both films were found to show a dispersion-type structure in the 4.6-7.8 eV region: they have large negative and broad positive peaks at around 4.8 and 7.8 eV, respectively. The θK spectra showed a tendency that is essentially quite similar to that of bulk Fe. The Kerr ellipticity (ηK) spectra are bell shaped, exhibiting a large negative peak at 6.3 eV. Plasma edges were observed at 6.9 eV for the as-deposited film and at 7.3 eV for the annealed film. The absolute value of the real part of the off-diagonal dielectric element (ɛ'XY) of both films at ~4.8 eV are almost the same as that of bulk Fe. This leads to the conclusion that the θK enhancement at 4.8 eV is mainly due to a decrease in ɛ''XX and a peak shift in ɛ'XY towards lower energy, but not to a plasma-resonance effect.

  4. Absolute VUV Photoionization Spectra for Hcho, HO{_2}, and H{_2}O{_2} from 10.5-12.0 eV

    NASA Astrophysics Data System (ADS)

    Dodson, Leah G.; Shen, Linhan; Eddingsaas, Nathan C.; Takematsu, Kana; Savee, John D.; Welz, Oliver; Taatjes, Craig A.; Osborn, David L.; Sander, Stanley P.; Okumura, Mitchio

    2013-06-01

    The absolute vacuum ultraviolet (VUV) photoionization spectra of formaldehyde (HCHO), the hydroperoxy radical (HO{_2}) and hydrogen peroxide (H{_2}O{_2}) have been measured. The ability to quantify these species is critical for photoionization mass spectrometry studies of the kinetics of atmospheric and combustion reactions, which require accurate cross sections over a wide range of ionization energies. Experiments were performed at the Advanced Light Source (ALS) synchrotron at the Lawrence Berkeley National Laboratory. HCHO, HO{_2}, and H{_2}O{_2} were generated from the oxidation of methanol which is initiated by pulsed-laser-photolysis of Cl{_2} in a low pressure flow cell. Sampled gas was ionized by tunable VUV radiation from the ALS synchrotron and detected by time-resolved multiplexed photoionization mass spectrometry using the Sandia Multiplexed Chemical Kinetics Reactor. The photoionization spectra were obtained by scanning the photon energy from 10.5 to 12.0 eV. Absolute cross sections were determined relative to methanol from measurements of the depletion of precursors and kinetic modeling of the initial chemistry ({<} 10 ms). The absolute photoionization spectrum of HCHO and the relative photoionization spectra of HO{_2} and H{_2}O{_2} are in good agreement with previous work. D. L. Osborn, P. Zou, H. Johnson, C. C. Hayden, C. A. Taatjes, V. D. Knyazev, S. W. North, D. S. Peterka, M. Ahmed, S. R. Leone. Rev. Sci. Inst. 2008, 79, 104103. G. Cooper, J. E. Anderson, C. E. Brion. Chem. Phys. 1996, 209, 61. M. Litorja, B. J. Ruscic. Electron Spectrosc. Relat. Phenom. 1998, 97, 131.

  5. Lake ecosystem dynamics and links to climate change inferred from a stable isotope and organic palaeorecord from a mountain lake in southwestern China (ca. 22.6-10.5 cal ka BP)

    NASA Astrophysics Data System (ADS)

    Cook, Charlotte G.; Leng, Melanie J.; Jones, Richard T.; Langdon, Peter G.; Zhang, Enlou

    2012-01-01

    A detailed understanding of long-term climatic and environmental change in southwestern China is hampered by a lack of long-term regional palaeorecords. Organic analysis (%TOC, %TN, C/N ratios and δ13C values) of a sediment sequence from Lake Shudu, Yunnan Province (ca. 22.6-10.5 cal ka BP) indicates generally low aquatic palaeoproductivity rates over millennial timescales in response to cold, dry climatic conditions. However, the record is punctuated by two marked phases of increased aquatic productivity from ca. 17.7 to 17.1 cal ka BP and from ca. 11.9 to 10.5 cal ka BP. We hypothesise that these shifts reflect a marked, stepwise lacustrine response to Asian summer monsoon strengthening during the last deglaciation.

  6. 32 CFR 10.5 - Construction.

    Code of Federal Regulations, 2013 CFR

    2013-07-01

    ... with 32 CFR part 9, and Military Order of November 13, 2001, “Detention, Treatment, and Trial of... event of an inconsistency, the provisions of 32 CFR part 9, and Military Order of November 13, 2001... Certain Non-Citizens in the War Against Terrorism.” Pronouns referring to the male gender shall...

  7. 32 CFR 10.5 - Construction.

    Code of Federal Regulations, 2010 CFR

    2010-07-01

    ... with 32 CFR part 9, and Military Order of November 13, 2001, “Detention, Treatment, and Trial of... event of an inconsistency, the provisions of 32 CFR part 9, and Military Order of November 13, 2001... Certain Non-Citizens in the War Against Terrorism.” Pronouns referring to the male gender shall...

  8. 32 CFR 10.5 - Construction.

    Code of Federal Regulations, 2011 CFR

    2011-07-01

    ... with 32 CFR part 9, and Military Order of November 13, 2001, “Detention, Treatment, and Trial of... event of an inconsistency, the provisions of 32 CFR part 9, and Military Order of November 13, 2001... Certain Non-Citizens in the War Against Terrorism.” Pronouns referring to the male gender shall...

  9. 43 CFR 10.5 - Consultation.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... REPATRIATION REGULATIONS Human Remains, Funerary Objects, Sacred Objects, or Objects of Cultural Patrimony From... inadvertent discovery of human remains, funerary objects, sacred objects, or objects of cultural patrimony on... likely to be, culturally affiliated with the human remains, funerary objects, sacred objects, or......

  10. 43 CFR 10.5 - Consultation.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... REPATRIATION REGULATIONS Human Remains, Funerary Objects, Sacred Objects, or Objects of Cultural Patrimony From... inadvertent discovery of human remains, funerary objects, sacred objects, or objects of cultural patrimony on... likely to be, culturally affiliated with the human remains, funerary objects, sacred objects, or......

  11. 46 CFR 59.10-5 - Cracks.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... CFR 59.01-2). For thicknesses exceeding three-fourths inch, suitable U grooves should be employed. A... the total length of any crack or series of consecutive cracks does not exceed two staybolt pitches. (d) Cracks in plain, circular or Adamson ring or similar type furnaces may be welded provided any one...

  12. 46 CFR 59.10-5 - Cracks.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... CFR 59.01-2). For thicknesses exceeding three-fourths inch, suitable U grooves should be employed. A... the total length of any crack or series of consecutive cracks does not exceed two staybolt pitches. (d) Cracks in plain, circular or Adamson ring or similar type furnaces may be welded provided any one...

  13. 46 CFR 59.10-5 - Cracks.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... CFR 59.01-2). For thicknesses exceeding three-fourths inch, suitable U grooves should be employed. A... the total length of any crack or series of consecutive cracks does not exceed two staybolt pitches. (d) Cracks in plain, circular or Adamson ring or similar type furnaces may be welded provided any one...

  14. 46 CFR 59.10-5 - Cracks.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... CFR 59.01-2). For thicknesses exceeding three-fourths inch, suitable U grooves should be employed. A... the total length of any crack or series of consecutive cracks does not exceed two staybolt pitches. (d) Cracks in plain, circular or Adamson ring or similar type furnaces may be welded provided any one...

  15. 43 CFR 10.5 - Consultation.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... Lands: Interior Office of the Secretary of the Interior NATIVE AMERICAN GRAVES PROTECTION AND... prior to making recommendations. Indian tribe officials are under no obligation to reveal the identity... discovery has been made; and (2) From Indian tribes and Native Hawaiian organizations that are, or...

  16. 43 CFR 10.5 - Consultation.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... Lands: Interior Office of the Secretary of the Interior NATIVE AMERICAN GRAVES PROTECTION AND... official shall notify in writing: (i) Any known lineal descendants of the deceased Native American... prior to making recommendations. Indian tribe officials are under no obligation to reveal the...

  17. 43 CFR 10.5 - Consultation.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... Lands: Interior Office of the Secretary of the Interior NATIVE AMERICAN GRAVES PROTECTION AND... official shall notify in writing: (i) Any known lineal descendants of the deceased Native American... prior to making recommendations. Indian tribe officials are under no obligation to reveal the...

  18. 46 CFR 56.10-5 - Pipe.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... design limits of stress and temperature indicated in ASME B31.1 (incorporated by reference; see 46 CFR 56..., DEPARTMENT OF HOMELAND SECURITY (CONTINUED) MARINE ENGINEERING PIPING SYSTEMS AND APPURTENANCES Components... and steam service may be used for design pressures up to 250 pounds per square inch and for...

  19. 46 CFR 56.10-5 - Pipe.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... design limits of stress and temperature indicated in ASME B31.1 (incorporated by reference; see 46 CFR 56..., DEPARTMENT OF HOMELAND SECURITY (CONTINUED) MARINE ENGINEERING PIPING SYSTEMS AND APPURTENANCES Components... and steam service may be used for design pressures up to 250 pounds per square inch and for...

  20. 46 CFR 56.10-5 - Pipe.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... found from Table 56.60-1(a). (3) Copper-nickel alloys may be used for water and steam service within the design limits of stress and temperature indicated in ASME B31.1 (incorporated by reference; see 46 CFR 56... specifically permitted by this part. (6) Aluminum-alloy pipe or tube along with similar junction equipment...

  1. 46 CFR 56.10-5 - Pipe.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... found from table 56.60-1(a). (3) Copper-nickel alloys may be used for water and steam service within the design limits of stress and temperature indicated in ASME B31.1 (incorporated by reference; see 46 CFR 56... specifically permitted by this part. (6) Aluminum-alloy pipe or tube along with similar junction equipment...

  2. L-shell X-ray production cross sections of Ce, Nd, Sm, Eu, Gd, and Dy by impact of 14N2+ ions with energies between 7.0 MeV and 10.5 MeV

    NASA Astrophysics Data System (ADS)

    Murillo, G.; Méndez, B.; López-Monroy, J.; Miranda, J.; Villaseñor, P.

    2016-09-01

    L-shell X-ray production cross sections from the lanthanoid elements Ce, Nd, Sm, Eu, Gd, and Dy, induced by the impact of 14N2+ ions with energies in the interval 7.0 MeV to 10.5 MeV (0.50 MeV/μ to 0.75 MeV/μ), were measured and then compared with theoretical calculations obtained with the ECPSSR model with exact limits of integration (eCPSSR) and related corrections. These include the electron capture by the incoming ion and multiple ionizations of higher shells. Data from this work were contrasted with previously published L X-ray production cross sections for 14N2+ ion impact. As with other ions, a universal behavior is found when Lα and Lγ X-ray production cross sections are plotted as a function of reduced velocity parameters. The agreement with theoretical predictions was very good when the corrections were applied to the eCPSSR model.

  3. Structural and relaxor-like dielectric properties of unfilled tungsten bronzes Ba5-5xSm5xTi5xNb10-5xO30

    NASA Astrophysics Data System (ADS)

    Wei, T.; Dong, Z.; Zhao, C. Z.; Guo, Y. Y.; Zhou, Q. J.; Li, Z. P.

    2016-03-01

    New unfilled tetragonal tungsten bronze (TTB) oxides, Ba5-5xSm5xTi5xNb10-5xO30 (BSTN-x), where 0.10 ≤ x ≤ 0.35, have been synthesized in this work. Their crystal structure was determined and analyzed based on Rietveld structural refinement. It is found that single TTB phase can be formed in a particular x range (i.e., 0.15 ≤ x ≤ 0.3) due to the competition interaction between tolerance factor and electronegativity difference. Furthermore, dielectric and ferroelectric results indicate that phase transitions and ferroelectric states are sensitive to x. Referring to the local chemistry, we suggest that the raise of vacancies at the A2-site compared with that of A1-site will intensely depress the normal ferroelectric phase and is in favor of relaxor ferroelectric state. Macroscopically, previous A-site size difference standpoint on fill TTB compounds cannot give a reasonable explanation about the variation of dielectric maximum temperature (Tm) for present BSTN-x compounds. Alternatively, tetragonality (c/a) is adopted which can well describe the variation of Tm in whole x range. In addition, one by one correspondence between tetragonality and electrical features can be found, and the compositions involving high c/a are usually stabilized in normal ferroelectric phase. It is believed that c/a is a more appropriate parameter to illustrate the variation of ferroelectric properties for unfilled TTB system.

  4. Core electron excitations in U(4+): modelling of the nd(10)5f(2)→nd(9)5f(3) transitions with n = 3, 4 and 5 by ligand field tools and density functional theory.

    PubMed

    Ramanantoanina, Harry; Kuri, Goutam; Daul, Claude; Bertsch, Johannes

    2016-07-28

    Ligand field density functional theory (LFDFT) calculations have been used to model the uranium M4,5, N4,5 and O4,5-edge X-ray absorption near edge structure (XANES) in UO2, characterized by the promotion of one electron from the core and the semi-core 3d, 4d and 5d orbitals of U(4+) to the valence 5f. The model describes the procedure to resolve non-empirically the multiplet energy levels originating from the two-open-shell system with d and f electrons and to calculate the oscillator strengths corresponding to the dipole allowed d(10)f(2)→ d(9)f(3) transitions appropriate to represent the d electron excitation process. In the first step, the energy and UO2 unit-cell volume corresponding to the minimum structures are determined using the Hubbard model (DFT+U) approach. The model of the optical properties due to the uranium nd(10)5f(2)→nd(9)5f(3) transitions, with n = 3, 4 and 5, has been tackled by means of electronic structure calculations based on the ligand field concept emulating the Slater-Condon integrals, the spin-orbit coupling constants and the parameters of the ligand field potential needed by the ligand field Hamiltonian from Density Functional Theory. A deep-rooted theoretical procedure using the LFDFT approach has been established for actinide-bearing systems that can be valuable to compute targeted results, such as spectroscopic details at the electronic scale. As a case study, uranium dioxide has been considered because it is a nuclear fuel material, and both atomic and electronic structure calculations are indispensable for a deeper understanding of irradiation driven microstructural changes occurring in this material. PMID:27356168

  5. Pervasive and Persistent Large-Volume, low delta 18O Silicic Magma Generation at the Yellowstone Hotspot, 12.7-10.5 Ma: Ion Microprobe Analyses of Zircon in the Cougar Point Tuff

    NASA Astrophysics Data System (ADS)

    Cathey, H. E.; Nash, B. P.; Valley, J. W.; Kita, N.; Ushikubo, T.; Spicuzza, M.

    2007-12-01

    High precision analyses of oxygen isotopes measured by ion microprobe in cores and rims of 111 zircon crystals from the voluminous Cougar Point Tuff (CPT) of the Bruneau-Jarbidge eruptive center in southern Idaho, USA, confirm the presence of the largest low δ18O silicic volcanic province yet discovered (c.f. Boroughs, 2005). These data provide an unprecedented, high resolution view into details of large-volume magma generation and source materials at a major eruptive center of the Yellowstone hotspot. The CPT consists of at least ten members of high-temperature (800-1000 °C) ignimbrites erupted from 12.7-10.5 Ma with a collective eruptive volume estimated at ≥ 7000 km3. Analyses of zircon were performed on the University of Wisconsin Cameca IMS-1280 using a spot diameter of 10 microns, with an average analytical precision for δ18O on the KIM5 standard of 0.3‰ (2 s.d.). Core and rim spot locations were carefully selected using cathodoluminescence and secondary electron imaging to evaluate zoning patterns, identify core locations and avoid inclusions. All but two zircon grains display rims that are depleted in 18O, and ~60 % of crystals display core-rim zonation of 0.5 to 7.4‰. The total range of δ18OVSMOW in cores of the 109 zircons with low δ18O rims is from -1.8 to 6.4 ‰; rims of these zircons range from -3.1 to 3.3 ‰. Within individual units, cores of zoned zircons are generally more variable than rims and vary over a minimum of 1.5 ‰ (Unit IX) and up to 8.2 ‰ (Unit VII). Rims vary 0.4 (Unit IX) to 5.2‰ (Unit XII). Our data indicate that the vast majority of zircons (96%) grew in low δ18O crustal melts, and that multiple discrete lowδ18O sources were involved in magma generation for most eruptive units. Whereas zircon cores display the most variable compositions, rims in several units converge to a more restricted range of δ18O values, although all units but IX show rim variability > 0.8 ‰. The presence of multiple discrete magma

  6. VizieR Online Data Catalog: 4yr 1.3mm VLBI observations of SgrA* with EHT (Fish+, 2016)

    NASA Astrophysics Data System (ADS)

    Fish, V. L.; Johnson, M. D.; Doeleman, S. S.; Broderick, A. E.; Psaltis, D.; Lu, R.-S.; Akiyama, K.; Alef, W.; Algaba, J. C.; Asada, K.; Beaudoin, C.; Bertarini, A.; Blackburn, L.; Blundell, R.; Bower, G. C.; Brinkerink, C.; Cappallo, R.; Chael, A. A.; Chamberlin, R.; Chan, C.-K.; Crew, G. B.; Dexter, J.; Dexter, M.; Dzib, S. A.; Falcke, H.; Freund, R.; Friberg, P.; Greer, C. H.; Gurwell, M. A.; Ho, P. T. P.; Honma, M.; Inoue, M.; Johannsen, T.; Kim, J.; Krichbaum, T. P.; Lamb, J.; Leon-Tavares, J.; Loeb, A.; Loinard, L.; MacMahon, D.; Marrone, D. P.; Moran, J. M.; Moscibrodzka, M.; Ortiz-Leon, G. N.; Oyama, T.; Ozel, F.; Plambeck, R. L.; Pradel, N.; Primiani, R. A.; Rogers, A. E. E.; Rosenfeld, K.; Rottmann, H.; Roy, A. L.; Ruszczyk, C.; Smythe, D. L.; Soohoo, J.; Spilker, J.; Stone, J.; Strittmatter, P.; Tilanus, R. P. J.; Titus, M.; Vertatschitsch, L.; Wagner, J.; Wardle, J. F. C.; Weintroub, J.; Woody, D.; Wright, M.; Yamaguchi, P.; Young, A.; Young, K. H.; Zensus, J. A.; Ziurys, L. M.

    2016-06-01

    The Event Horizon Telescope (EHT) obtained detections of Sgr A* on closed triangles of baselines among stations in Arizona, California, and Hawaii in 2009, 2011, 2012, and 2013. In all cases, two 480MHz bands, centered at 229.089GHz and 229.601GHz (hereafter, low and high bands, respectively), were observed. One or more telescopes from each of three sites in Arizona, California, and Hawaii participated in each set of observations. The Arizona Radio Observatory (ARO) Submillimeter Telescope (SMT) on Mt. Graham, Arizona, was used in all cases. Over the years of data analyzed here, the configuration of VLBI recording at these sites evolved as described in section 2.1. (1 data file).

  7. 46 CFR 194.10-5 - Type and location.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... requirements of 49 CFR part 176. (c) Magazine chests. (1) Magazine chests shall be located on the weather decks in a position suitable for jettisoning the contents. (2) Magazine chests shall be set off at least 4... utilized shall not be used for stowage of other hazardous materials covered by 49 CFR parts 171-179....

  8. 46 CFR 194.10-5 - Type and location.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... requirements of 49 CFR part 176. (c) Magazine chests. (1) Magazine chests shall be located on the weather decks in a position suitable for jettisoning the contents. (2) Magazine chests shall be set off at least 4... utilized shall not be used for stowage of other hazardous materials covered by 49 CFR parts 171-179....

  9. 46 CFR 194.10-5 - Type and location.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... requirements of 49 CFR part 176. (c) Magazine chests. (1) Magazine chests shall be located on the weather decks in a position suitable for jettisoning the contents. (2) Magazine chests shall be set off at least 4... utilized shall not be used for stowage of other hazardous materials covered by 49 CFR parts 171-179....

  10. 46 CFR 194.10-5 - Type and location.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... requirements of 49 CFR part 176. (c) Magazine chests. (1) Magazine chests shall be located on the weather decks in a position suitable for jettisoning the contents. (2) Magazine chests shall be set off at least 4... utilized shall not be used for stowage of other hazardous materials covered by 49 CFR parts 171-179....

  11. 46 CFR 194.10-5 - Type and location.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... requirements of 49 CFR part 176. (c) Magazine chests. (1) Magazine chests shall be located on the weather decks in a position suitable for jettisoning the contents. (2) Magazine chests shall be set off at least 4... utilized shall not be used for stowage of other hazardous materials covered by 49 CFR parts 171-179....

  12. 46 CFR 193.10-5 - Fire pumps.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... tube pressure may not be less than 35 p.s.i. (d) Fire pumps shall be fitted on the discharge side with... and over on an international voyage, each required fire pump, while delivering water through the fire... Pitot tube pressure of not less than 50 p.s.i. Where 11/2-inch hose is permitted in lieu of...

  13. 46 CFR 95.10-5 - Fire pumps.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... on an international voyage, each required fire pump, while delivering water thru the fire main system... pressure of approximately 50 p.s.i. Where 11/2-inch hose is permitted in lieu of 21/2-inch hose by footnote... be only 35 p.s.i. (d) Fire pumps shall be fitted on the discharge side with relief valves set...

  14. 46 CFR 76.10-5 - Fire pumps.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... capable of delivering water simultaneously from the two highest outlets at a Pitot tube pressure of...) Fire pumps shall be fitted on the discharge side with relief valves set to relieve at 25 p. s. i. in... conditions, are not capable of developing a pressure exceeding this amount. (e) Fire pumps shall be...

  15. 46 CFR 76.10-5 - Fire pumps.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... capable of delivering water simultaneously from the two highest outlets at a Pitot tube pressure of...) Fire pumps shall be fitted on the discharge side with relief valves set to relieve at 25 p. s. i. in... conditions, are not capable of developing a pressure exceeding this amount. (e) Fire pumps shall be...

  16. 46 CFR 193.10-5 - Fire main system, details.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ..., while delivering water through the fire main system at a pressure corresponding to that required by...(a), the Pitot tube pressure may not be less than 35 p.s.i. (d) Fire pumps shall be fitted on the... highest outlets, at a Pitot tube pressure of not less than 50 p.s.i. Where 11/2-inch hose is permitted...

  17. 46 CFR 61.10-5 - Pressure vessels in service.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... examination should be that necessary to determine that the pressure vessel's condition is satisfactory and... tested except when a defect is found that, in the marine inspector's opinion, may affect the safety of... pressure vessels used in refrigeration service. (2) If your vessel's Certificate of Inspection is...

  18. 46 CFR 61.10-5 - Pressure vessels in service.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... examination should be that necessary to determine that the pressure vessel's condition is satisfactory and... tested except when a defect is found that, in the marine inspector's opinion, may affect the safety of... pressure vessels used in refrigeration service. (2) If your vessel's Certificate of Inspection is...

  19. 46 CFR 193.10-5 - Fire pumps.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... tube pressure may not be less than 35 p.s.i. (d) Fire pumps shall be fitted on the discharge side with... and over on an international voyage, each required fire pump, while delivering water through the fire... Pitot tube pressure of not less than 50 p.s.i. Where 11/2-inch hose is permitted in lieu of...

  20. 46 CFR 76.10-5 - Fire pumps.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... capable of delivering water simultaneously from the two highest outlets at a Pitot tube pressure of...) Fire pumps shall be fitted on the discharge side with relief valves set to relieve at 25 p. s. i. in... conditions, are not capable of developing a pressure exceeding this amount. (e) Fire pumps shall be...

  1. 46 CFR 193.10-5 - Fire main system, details.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ..., while delivering water through the fire main system at a pressure corresponding to that required by...(a), the Pitot tube pressure may not be less than 35 p.s.i. (d) Fire pumps shall be fitted on the... highest outlets, at a Pitot tube pressure of not less than 50 p.s.i. Where 11/2-inch hose is permitted...

  2. 46 CFR 76.10-5 - Fire pumps.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... capable of delivering water simultaneously from the two highest outlets at a Pitot tube pressure of...) Fire pumps shall be fitted on the discharge side with relief valves set to relieve at 25 p. s. i. in... conditions, are not capable of developing a pressure exceeding this amount. (e) Fire pumps shall be...

  3. Observation by two-photon laser spectroscopy of the 4d{sup 10}5s {sup 2}S{sub 1/2}{yields}4d{sup 9}5s{sup 2} {sup 2}D{sub 5/2} clock transition in atomic silver

    SciTech Connect

    Badr, T.; Plimmer, M. D.; Juncar, P.; Himbert, M. E.; Louyer, Y.; Knight, D. J. E.

    2006-12-15

    We report the observation of the very narrow 4d{sup 10}5s {sup 2}S{sub 1/2}{yields}4d{sup 9}5s{sup 2} {sup 2}D{sub 5/2} transition in atomic silver. The frequencies of the hyperfine components in {sup 107}Ag and {sup 109}Ag have been measured using Doppler-free two-photon laser spectroscopy of a thermal beam and heterodyne calibration with respect to the a{sub 1} component of the 62P(4-5) line in molecular iodine near 661 nm. For the center of gravity of a mixture of natural abundance, we deduce the value 906 641 295.77(19) MHz. For the isotope shift, we obtain {nu}({sup 109}Ag)-{nu}({sup 107}Ag)=564.15(37) MHz, from which we deduce the frequency and isotope shift of the 4d{sup 10}5s {sup 2}S{sub 1/2}{yields}4d{sup 10}6p {sup 2}P{sub 3/2} transition at 206 nm.

  4. Single crystal studies on Co-containing {tau}-borides Co{sub 23-x}M{sub x}B{sub 6} (M=Al, Ga, Sn, Ti, V, Ir) and the boron-rich {tau}-boride Co{sub 12.3}Ir{sub 8.9}B{sub 10.5}

    SciTech Connect

    Kotzott, Dominik; Ade, Martin; Hillebrecht, Harald

    2009-03-15

    Single crystals of the cubic {tau}-Borides Co{sub 23-x}M{sub x}B{sub 6} (M=Al, Ga, Sn) were synthesised from the elements at temperatures between 1200 and 1500 deg. C. According to the structure refinements one (Ga, Sn: 8c) or two (Al: 4a and 8c) of the four independent metal sites show a mixed occupation Co/M resulting in the compositions Co{sub 20.9}Al{sub 2.1}B{sub 6}, Co{sub 21.9}Ga{sub 1.1}B{sub 6}, and Co{sub 21.4}Sn{sub 1.6}B{sub 6}, respectively. Melts with Indium gave access to Co{sub 23}B{sub 6} as the first binary {tau}-boride (Fm3-barm,a=10.4618(13) A, 104 refl., 14 param., R{sub 1}(F)=0.0132, wR{sub 2}(F{sup 2})=0.0210). With M=Ir mixed occupations occur for all sites and the boron content varies. The composition for the boron-poor single crystal was Co{sub 16.2}Ir{sub 6.8}B{sub 6}. A higher Ir-content enables the uptake of additional boron resulting in a composition Co{sub 12.3}Ir{sub 8.9}B{sub 10.5}. This can be explained be the substitution of metal atoms on the 8c-site by B{sub 4}-tetrahedra. A boron-rich phase was observed for the first time for a {tau}-boride of cobalt. All compositions were confirmed by EDX measurements. - Graphical Abstract: Single crystal investigations on {tau}-borides Co/M/B with M = Al, Ga, In, Sn, V, Ti, Ir explained the substitution processes. Furthermore the yielded the first binary boride, Co{sub 23}B{sub 6}, and a boron-rich Co{sub 12.3}Ir{sub 8.9}B{sub 10.5} containing B{sub 4}-tetrahedra.

  5. Massive Star Formation at Millimeter and Submillimeter Wavelengths

    NASA Astrophysics Data System (ADS)

    Su, Yu-Nung

    2004-06-01

    associated with luminous young stellar objects have been studied in high angular resolutions (<10"). I find that the outflow associated with each IRAS source shows a clear bipolar morphology in 12CO, with properties (i.e., total mass of order 10-100 M_sun, mass-outflow rate >10^-3 M_sun yr^-1, dynamical timescale 10^4-10^5 yrs, and energetics) comparable with those of other massive outflows associated with luminous young stellar objects. Each outflow appears to be centered on a dust and gas condensation with a mass of 200-300 M_sun, likely marking the location of the driving source. The mass-velocity diagrams of both outflows change in slope at a velocity of ~10 km s^-1, suggesting that the high-velocity component (HVC) may drive the low-velocity component (LVC). Neither HVC has a momentum supply rate sufficient to drive their corresponding LVCs, and as for other molecular outflows the primary driving agent cannot be ionized gas, leaving atomic gas as the other remaining candidate. Finally, I present a first glimpse at the small-scale distribution of dust around UC HII regions and high-mass protostellar objects (HMPOs) at 0.85 mm made with the Submillimeter Array (SMA), and investigate whether HMPOs and UC HII regions can serve as useful gain calibrators for the SMA. The SMA observations with an angular resolution of ~3" reveal that although a large fraction of the dust emission originates from an extended ``halo' component, a compact unresolved component often remains that when sufficiently strong may serve as a useful calibrator. I discuss the origin of the core-halo structure seen in many sources and conclude with suggestions for future searches for calibrators with the SMA.

  6. Suppression of star formation in the galaxy NGC 253 by a starburst-driven molecular wind

    NASA Astrophysics Data System (ADS)

    Warren, Steven R.; Bolatto, A. D.; Leroy, A. K.; Walter, F.; Veilleux, S.; Ostriker, E. C.; Ott, J.; Zwaan, M.; Fisher, D. B.; Weiss, A.; Rosolowsky, E.; Hodge, J.

    2014-01-01

    We present Atacama Large (Sub)Millimeter Array (ALMA) CO (J=1-0) observations of the nearby, nuclear starburst galaxy NGC 253. NGC 253 is host to a "superwind" emanating from the central ~200 pc. Galaxy superwinds are thought to help shape the galactic mass function, play a critical role in galaxy evolution, and pollute the intergalactic medium with heavy metals. Detailed studies of nearby systems frequently focus on the warm or hot phases of the wind, visible in X-ray or Halpha emission. However, most of the mass in the outflowing material is thought to be in the form of neutral atomic and molecular gas. We use the observed CO luminosities and velocities to estimate the mass, mass loss rate, and energetics of the molecular wind. We compute an outflow mass of M_mo 6.6x10^6 Msun. The observed projected velocities of the CO filaments range from ~30-60 km s^-1 resulting in a mass loss rate of ~9 Msun yr^-1. The nuclear region of NGC 253 has a star formation rate of ~3 Msun yr^-1 resulting in a mass loading parameter 1-3. It is not immediately clear if the outflowing gas will escape the halo or eventually rain back onto the disk. What is clear is that NGC 253 will exhaust its nuclear star forming gas in ~60-120 Myr at its current mass loss rate, cementing the superwind as an important contributor in the evolution of NGC 253.

  7. 20 CFR 10.5 - What definitions apply to these regulations?

    Code of Federal Regulations, 2011 CFR

    2011-04-01

    ... vertebrae which must be demonstrable on any x-ray film to an individual trained in the reading of x-rays... examinations (and related laboratory tests), x-rays performed to diagnose a subluxation of the spine and... who has not been excluded under the provisions of subpart I of this part. (x) Recurrence of...

  8. 20 CFR 10.5 - What definitions apply to the regulations in this subchapter?

    Code of Federal Regulations, 2012 CFR

    2012-04-01

    ... related laboratory tests), x-rays performed to diagnose a subluxation of the spine and treatment..., fixation or abnormal spacing of the vertebrae which must be demonstrable on any x-ray film to an individual trained in the reading of x-rays. (cc) Surviving spouse means the husband or wife living with or...

  9. 20 CFR 10.5 - What definitions apply to the regulations in this subchapter?

    Code of Federal Regulations, 2013 CFR

    2013-04-01

    ... related laboratory tests), x-rays performed to diagnose a subluxation of the spine and treatment..., fixation or abnormal spacing of the vertebrae which must be demonstrable on any x-ray film to an individual trained in the reading of x-rays. (cc) Surviving spouse means the husband or wife living with or...

  10. 46 CFR 54.10-5 - Maximum allowable working pressure (reproduces UG-98).

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... reference; see 46 CFR 54.01-1.) (b) The maximum allowable working pressure for a vessel part is the maximum... loadings listed in UG-22 of section VIII of the ASME Boiler and Pressure Vessel Code (see 46 CFR 54.01-30... thickness specified as corrosion allowance. (See UG-25 of section VIII of the ASME Boiler and...

  11. 46 CFR 54.10-5 - Maximum allowable working pressure (reproduces UG-98).

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... reference; see 46 CFR 54.01-1.) (b) The maximum allowable working pressure for a vessel part is the maximum... loadings listed in UG-22 of section VIII of the ASME Boiler and Pressure Vessel Code (see 46 CFR 54.01-30... thickness specified as corrosion allowance. (See UG-25 of section VIII of the ASME Boiler and...

  12. 46 CFR 54.10-5 - Maximum allowable working pressure (reproduces UG-98).

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... reference; see 46 CFR 54.01-1.) (b) The maximum allowable working pressure for a vessel part is the maximum... loadings listed in UG-22 of section VIII of the ASME Boiler and Pressure Vessel Code (see 46 CFR 54.01-30... thickness specified as corrosion allowance. (See UG-25 of section VIII of the ASME Boiler and...

  13. General Counsel`s office FY 1995 site support program plan WBS 6.10.5

    SciTech Connect

    Moreno, S.R.

    1994-09-01

    The General Counsel`s office provides legal counsel to all levels of WHC management; administers the intellectual property program; coordinates all WHC investigative activity and supports WHC activities to ensure compliance with all applicable federal, state, and local laws, DOE directives, contractual provisions, and other requirements. In so doing, the Office of General Counsel supports the Hanford site mission of transforming the Hanford site into an environmentally attractive and economically sustainable community. This document briefs the FY95 site support plan.

  14. 20 CFR 10.5 - What definitions apply to these regulations?

    Code of Federal Regulations, 2010 CFR

    2010-04-01

    ... does not include continuation of pay. (b) Beneficiary means an individual who is entitled to a benefit... vertebrae which must be demonstrable on any x-ray film to an individual trained in the reading of...

  15. Millwright Apprenticeship. Related Training Modules. 10.1-10.5 Combustion.

    ERIC Educational Resources Information Center

    Lane Community Coll., Eugene, OR.

    This packet, part of the instructional materials for the Oregon apprenticeship program for millwright training, contains five modules covering combustion. The modules provide information on the following topics: the combustion process, types of fuel, air and fuel gases, heat transfer, and combustion in wood. Each module consists of a goal,…

  16. Stationary Engineers Apprenticeship. Related Training Modules. 10.1-10.5 Machine Components.

    ERIC Educational Resources Information Center

    Lane Community Coll., Eugene, OR.

    This packet of five learning modules on machine components is one of 20 such packets developed for apprenticeship training for stationary engineers. Introductory materials are a complete listing of all available modules and a supplementary reference list. Each module contains some or all of these components: goal, performance indicators, statement…

  17. 46 CFR 34.10-5 - Fire pumps-T/ALL.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    .... (Refer to table 34.50-5(c).) 2 Vessels of 1,000 gross tons and over on an international voyage shall have... international voyage, each required fire pump, while delivering water through the fire main system at a pressure... required for an independent bilge pump if no length correction is taken for the cargo tank space....

  18. Radiology Technician, 10-5. Military Curriculum Materials for Vocational and Technical Education.

    ERIC Educational Resources Information Center

    Ohio State Univ., Columbus. National Center for Research in Vocational Education.

    These five volumes of student materials for a secondary/postsecondary level course in radiology technology comprise one of a number of military-developed curriculum packages selected for adaptation to vocational instruction and curriculum development in a civilian setting. The purpose stated for the course is to provide the theory portion of…

  19. 25 CFR 10.5 - Where can I find the policies and standards for the administration, operation, services, and...

    Code of Federal Regulations, 2011 CFR

    2011-04-01

    ... administration, operation, services, and physical plant/construction of Indian country detention, community... policies and standards for the administration, operation, services, and physical plant/construction of Indian country detention, community residential, and holding facilities? The Bureau of Indian...

  20. 25 CFR 10.5 - Where can I find the policies and standards for the administration, operation, services, and...

    Code of Federal Regulations, 2010 CFR

    2010-04-01

    ... administration, operation, services, and physical plant/construction of Indian country detention, community... policies and standards for the administration, operation, services, and physical plant/construction of Indian country detention, community residential, and holding facilities? The Bureau of Indian...

  1. 25 CFR 10.5 - Where can I find the policies and standards for the administration, operation, services, and...

    Code of Federal Regulations, 2014 CFR

    2014-04-01

    ... administration, operation, services, and physical plant/construction of Indian country detention, community... policies and standards for the administration, operation, services, and physical plant/construction of Indian country detention, community residential, and holding facilities? The Bureau of Indian...

  2. 25 CFR 10.5 - Where can I find the policies and standards for the administration, operation, services, and...

    Code of Federal Regulations, 2012 CFR

    2012-04-01

    ... administration, operation, services, and physical plant/construction of Indian country detention, community... policies and standards for the administration, operation, services, and physical plant/construction of Indian country detention, community residential, and holding facilities? The Bureau of Indian...

  3. 25 CFR 10.5 - Where can I find the policies and standards for the administration, operation, services, and...

    Code of Federal Regulations, 2013 CFR

    2013-04-01

    ... administration, operation, services, and physical plant/construction of Indian country detention, community... policies and standards for the administration, operation, services, and physical plant/construction of Indian country detention, community residential, and holding facilities? The Bureau of Indian...

  4. 31 CFR 10.5 - Application to become an enrolled agent, enrolled retirement plan agent, or registered tax return...

    Code of Federal Regulations, 2012 CFR

    2012-07-01

    ... tax return preparer. See 26 CFR part 300. (c) Additional information; examination. The Internal... applicant's tax liabilities. (e) Temporary recognition. On receipt of a properly executed application, the Commissioner, or delegate, may grant the applicant temporary recognition to practice pending a determination...

  5. 31 CFR 10.5 - Application for enrollment as an enrolled agent or enrolled retirement plan agent.

    Code of Federal Regulations, 2011 CFR

    2011-07-01

    ... accordance with 26 CFR 300.5. A reasonable nonrefundable fee will be charged for each application for... agent, or registered tax return preparer. See 26 CFR part 300. (c) Additional information; examination... enrollment. (d) Temporary recognition. On receipt of a properly executed application, the Director of...

  6. 31 CFR 10.5 - Application to become an enrolled agent, enrolled retirement plan agent, or registered tax return...

    Code of Federal Regulations, 2013 CFR

    2013-07-01

    ... tax return preparer. See 26 CFR part 300. (c) Additional information; examination. The Internal... applicant's tax liabilities. (e) Temporary recognition. On receipt of a properly executed application, the Commissioner, or delegate, may grant the applicant temporary recognition to practice pending a determination...

  7. 31 CFR 10.5 - Application for enrollment as an enrolled agent or enrolled retirement plan agent.

    Code of Federal Regulations, 2010 CFR

    2010-07-01

    ... Professional Responsibility in accordance with 26 CFR 300.5. A reasonable nonrefundable fee will be charged for... his or her application for enrollment. (d) Temporary recognition. On receipt of a properly executed... recognition to practice pending a determination as to whether enrollment to practice should be...

  8. 22 CFR 19.10-5 - Reduced annuity with additional survivor annuity to spouse or former spouse.

    Code of Federal Regulations, 2014 CFR

    2014-04-01

    ... effective prior to the principal's retirement, shall be reduced as necessary by PER/ER/RET after the... the regular survivor annuity because the participant is required to pay it's full cost by deduction... principal's full annuity counting any supplemental annuity or recomputation of annuity because of...

  9. 22 CFR 19.10-5 - Reduced annuity with additional survivor annuity to spouse or former spouse.

    Code of Federal Regulations, 2013 CFR

    2013-04-01

    ... effective prior to the principal's retirement, shall be reduced as necessary by PER/ER/RET after the... the regular survivor annuity because the participant is required to pay it's full cost by deduction... principal's full annuity counting any supplemental annuity or recomputation of annuity because of...

  10. 22 CFR 19.10-5 - Reduced annuity with additional survivor annuity to spouse or former spouse.

    Code of Federal Regulations, 2010 CFR

    2010-04-01

    ... effective prior to the principal's retirement, shall be reduced as necessary by PER/ER/RET after the... the regular survivor annuity because the participant is required to pay it's full cost by deduction... principal's full annuity counting any supplemental annuity or recomputation of annuity because of...

  11. 22 CFR 19.10-5 - Reduced annuity with additional survivor annuity to spouse or former spouse.

    Code of Federal Regulations, 2012 CFR

    2012-04-01

    ... effective prior to the principal's retirement, shall be reduced as necessary by PER/ER/RET after the... the regular survivor annuity because the participant is required to pay it's full cost by deduction... principal's full annuity counting any supplemental annuity or recomputation of annuity because of...

  12. 22 CFR 19.10-5 - Reduced annuity with additional survivor annuity to spouse or former spouse.

    Code of Federal Regulations, 2011 CFR

    2011-04-01

    ... effective prior to the principal's retirement, shall be reduced as necessary by PER/ER/RET after the... the regular survivor annuity because the participant is required to pay it's full cost by deduction... principal's full annuity counting any supplemental annuity or recomputation of annuity because of...

  13. General Counsel`s Office FY 1996 Site Support Program Plan: WBS 6.10.5. Revision 1

    SciTech Connect

    Moreno, S.R.

    1995-09-01

    This is the General Counsel`s Office site support program plan for the US DOE Hanford site. The topics addressed in the program plan include a mission statement, description of activities, program objectives, planning assumptions, program constraints, work breakdown structure, milestone list, milestone description sheets, and activity detail.

  14. Formation and Evolution of Binary Planetary Nebula Nuclei and Related Objects

    NASA Astrophysics Data System (ADS)

    Iben, Icko, Jr.; Tutukov, Alexander V.

    1993-11-01

    A study is made of the evolution of close binaries in which the primary first fills its Roche lobe after the exhaustion of helium at its center and before the onset of thermal pulses. Initial masses are in the range 3-6 M0. Also examined is the evolution of a 1 Msun model which fills its Roche lobe on the first giant branch when the mass of its helium degenerate core reaches 0.4 M0. In all cases, a common envelope scenario is assumed, and mass is removed from the model primary on a timescale shorter than the initial thermal timescale of the envelope of the primary until the model contracts within a final Roche lobe of predetermined size. After the removal of the common envelope, systems are very close binaries in which the evolved remnant has either a carbon-oxygen (CO) core and a helium-burning shell (progenitor of mass 2.3-8 Msun) or a helium core and a hydrogen-burning shell (progenitor of mass 1-2.3 Msun). The more massive remnants fill their Roche lobes for an extended period, transferring first hydrogen-rich material at a rate ˜10-8±1 Msun yr-1 for up to 106 yr, and then helium at a rate ˜10-6±1 Msun yr-1 for (1-4) × 105 yr. As much as ˜0.4 Msun of nearly pure helium can be transferred to an accretor. A possible real analog of the hydrogen-transferring models is U Sco, although, in many instances, a hydrogen-transferring episode may be bypassed or considerably shortened if the hot remnant blows a strong enough wind. Possible observational analogs of helium transferring models are bright ultrasoft X-ray sources like CAL 83 and CAL 87 in the Large Magellanic Cloud and some classes of supernova precursors. Our models help to explain the number and properties of hot helium OB subdwarfs. A method for estimating initial orbital periods of binary planetary nebula nuclei is introduced and used to infer the initial characteristics of binary systems which have produced close binary central stars, precataclysmic variables, and related systems. Using existing

  15. The Far-IR View of an Ultra-Hard X-ray Selected Sample of AGN

    NASA Astrophysics Data System (ADS)

    Shimizu, Thomas; Melendez, M.; Mushotzky, R.; Barger, A. J.; Cowie, L. L.

    2014-01-01

    We present early results of the Herschel PACS (70 and 160 μm) and SPIRE (250, 350, and 500 μm) survey of 313 low redshift (z < 0.05), ultra-hard X-ray (14-195 keV) selected AGN from the 58 month Swift/BAT catalog. Selection of AGN from ultra-hard X-rays avoids bias from obscuration that are unavoidable at other wavelengths (eg optical, infrared, and radio) providing the most complete sample of AGN to study the connection between nuclear activity and star formation in host galaxies. With the high angular resolution of PACS, we find that ~35% and ~20% of the sources are 'point-like' at 70 and 160 μm respectively with another 20% that have their flux dominated by a point source located at the nucleus. The inferred star formation rates (SFR) of 0.1 - 100 Msun yr-1 using the 70 and 160 μm flux densities and the calibration of Calzettti et al (2010) are consistent with those inferred from Spitzer NeII fluxes, but we find that 11.25 μm PAH data give ~3x lower SFR. Using GALFIT to measure the size of the FIR emitting regions, we determined the SFR density [Msun yr-1 kpc-2] for our sample, finding a significant fraction to exist above the threshold for star formation driven winds (0.1 Msun yr-1 kpc-2, Heckman 2001). Analysis of the SPIRE colors (250/350 and 350/500) also reveals evidence for the presence of nonthermal synchrotron emission from a radio jet significantly affecting the FIR emission at long wavelengths and altering the shape of the spectral energy distribution (SED). We also will present the broad band Herschel 70-500m SEDS for our sample and include archival Spitzer, WISE, FIRST and NVSS data to extend the SED down to near-IR and up to radio wavelengths. The SEDs will be fit using multiple models to attempt to determine the AGN contribution to the FIR (indirect or direct) and ultimately its effect on nuclear star formation.

  16. Three Millimeter Molecular Line Observations of Sagittarius B2. II. High-Resolution Studies of C 18O, HNCO, NH 2CHO, and HCOOCH 3

    NASA Astrophysics Data System (ADS)

    Kuan, Yi-Jehng; Snyder, Lewis E.

    1996-10-01

    High-resolution imaging of C18O, HNCO, NR2CHO, and RCOOCH3 in Sgr B2 are presented in this study. The C18O emission comes mainly from the Sgr B2(M) and Sgr B2(N) dense cores and the western gas clump RNO(M). Toward Sgr B2(M), the C18O column density is 2 times higher and the fractional abundance is 80 times higher than toward Sgr B2(N). In HNO(M), the narrow line width implies that the C18O emission arises from the diffuse gas. The complex molecules NR2CHO and HCOOCR3 were detected only toward the Sgr B2(N) core. The HNCO K-1 = 2 emission is detected only in Sgr B2(N) and is attributed to efficient radiative pumping, which indicates the significant presence of far-infrared field and warm dust grains. Only 4% of the HNCO was found in the K-1 = 0 ladders in Sgr B2(N). The nondetection of the K-1 = 2 emission toward Sgr B2(M) is caused by excitation and low abundance. In contrast, the HNCO K-1 = 0 emission comes mainly from the extended gas component: the far northern region and HNCO(SW). For the K-1 = 0 transitions, Trot = ˜7 K. The low Trot and the apparent ubiquity of RNCO suggest that abundant HNCO exists in the Sgr B2 envelope. The HNCO K-1 = 0 emission unveiled two spatially extended velocity components; the velocity gap between them covers the same LSR velocities of the Sgr B2 dense cores. If HNCO is formed via surface reactions, the pervasive detection of HNCO in the outer edges of Sgr B2 cloud core leads to the cloud-cloud collision postulate. A north-south C18O bipolar structure was seen in Sgr B2(M) centered at the compact H II region F. The bipolar structure appears asymmetric and thus favors the outflow interpretation. The sharp outer edges of the C18O line profiles of the two lobes further support the outflow picture. The estimated outflow age is ˜2±1 x 104 yr, and the total mass is ˜1700 Msun. The outflow masses for the blue and red lobes are <360 Msun and <410 Msun, respectively. The mass-loss rate is thus <0.037 Msun yr-1. The detection of

  17. Photon loss from the helium Lyα line - the key to the acceleration of Wolf-Rayet winds.

    NASA Astrophysics Data System (ADS)

    Schmutz, W.

    1997-05-01

    It is demonstrated that the ionization equilibrium of helium in non-LTE atmospheres for Wolf-Rayet stars is very sensitive to photon loss from the Heii Lyα line. A removal of 0.001% of the photons is sufficient to initiate an abruptly recombining ionization equilibrium. The assumption of photon loss allows to address the wind momentum problem of Wolf-Rayet stars. It is possible for the first time to construct a line blanketed non-LTE model of a Wolf-Rayet star that reproduces the observed spectrum and simultaneously, provides the radiation force to drive its outer velocity structure. A method is developed to determine the free model parameters L, R_phot_, ˙(M), vinfinity_, v_phot_, C (clumping factor), and f (photon loss factor), by an analysis of an observed Wolf-Rayet spectrum. The method is applied to the spectrum of the WN5 star HD 50896 resulting in good fits in shape and strength to the observed helium emission lines. In particular the profile of the Hei λ10830 line, which is a tracer of the outer velocity structure, is reproduced remarkably well. The hydrodynamically calculated velocity law differs significantly from the commonly adopted β-law with β=1. The outer part can be approximated by a β-law with β=3 if the core radius of the atmosphere model is used, or by β=8, if the velocity law is calculated referring to the hydrostatic radius of a stellar evolution model in the Wolf-Rayet phase. Close to the photosphere the velocity structure is flat with an expansion velocity of v_phot_ =~1100 km/s. The resulting luminosity L= 5.5x10^5^ Lsun_ and terminal wind velocity vinfinity_=2060 km/s are found to be considerably larger than the values from previous determinations. On the other hand, the mass loss rate is lower ˙(M)=3.2x10^-5^ Msun_yr^-1^ due to an inhomogeneous wind with a clumping factor C=~4. There is evidence for a decrease of the clumping factor with distance from the star. The photon loss factor is determined empirically to have a value of f

  18. Performance of beef heifers grazing stockpiled fescue as influenced by supplemental whole cottonseed.

    PubMed

    Poore, M H; Scott, M E; Green, J T

    2006-06-01

    greater (P < 0.05) for supplemented heifers. Supplemented heifers had greater serum urea nitrogen in yr 1 (9.5 vs. 10.5 mg/dL; P < 0.07) and yr 2 (7.2 vs. 8.6 mg/dL; P < 0.01). Forage disappearance was similar between supplemented and unsupplemented heifers (3.19 vs. 3.39 kg.heifer(-1).d(-1) in yr 1 and 4.14 vs. 4.17 kg.heifer(-1).d(-1) in yr 2, respectively). Heifers responded to supplementation, but performance was lower than expected based on forage nutrient content. PMID:16699119

  19. Climatic variability, hydrologic anomaly, and methane emission can turn productive freshwater marshes into net carbon sources.

    PubMed

    Chu, Housen; Gottgens, Johan F; Chen, Jiquan; Sun, Ge; Desai, Ankur R; Ouyang, Zutao; Shao, Changliang; Czajkowski, Kevin

    2015-03-01

    Freshwater marshes are well-known for their ecological functions in carbon sequestration, but complete carbon budgets that include both methane (CH4 ) and lateral carbon fluxes for these ecosystems are rarely available. To the best of our knowledge, this is the first full carbon balance for a freshwater marsh where vertical gaseous [carbon dioxide (CO2 ) and CH4 ] and lateral hydrologic fluxes (dissolved and particulate organic carbon) have been simultaneously measured for multiple years (2011-2013). Carbon accumulation in the sediments suggested that the marsh was a long-term carbon sink and accumulated ~96.9 ± 10.3 (±95% CI) g C m(-2)  yr(-1) during the last ~50 years. However, abnormal climate conditions in the last 3 years turned the marsh to a source of carbon (42.7 ± 23.4 g C m(-2)  yr(-1) ). Gross ecosystem production and ecosystem respiration were the two largest fluxes in the annual carbon budget. Yet, these two fluxes compensated each other to a large extent and led to the marsh being a CO2 sink in 2011 (-78.8 ± 33.6 g C m(-2)  yr(-1) ), near CO2 -neutral in 2012 (29.7 ± 37.2 g C m(-2)  yr(-1) ), and a CO2 source in 2013 (92.9 ± 28.0 g C m(-2)  yr(-1) ). The CH4 emission was consistently high with a three-year average of 50.8 ± 1.0 g C m(-2)  yr(-1) . Considerable hydrologic carbon flowed laterally both into and out of the marsh (108.3 ± 5.4 and 86.2 ± 10.5 g C m(-2)  yr(-1) , respectively). In total, hydrologic carbon fluxes contributed ~23 ± 13 g C m(-2)  yr(-1) to the three-year carbon budget. Our findings highlight the importance of lateral hydrologic inflows/outflows in wetland carbon budgets, especially in those characterized by a flow-through hydrologic regime. In addition, different carbon fluxes responded unequally to climate variability/anomalies and, thus, the total carbon budgets may vary drastically among years. PMID:25287051

  20. Mass accretion flows in the high-mass star forming complex NGC 6334

    NASA Astrophysics Data System (ADS)

    Sánchez-Monge, Á.; Schilke, P.; Zernickel, A.; Schmiedeke, A.; Möller, Th.; Qin, S.-L.

    2016-05-01

    The formation of high-mass stars is one of the major topics of astrophysical research, in particular the process of accretion from large-scale clouds down to small-scale cores. We have selected the nearby, filamentary, high-mass star forming complex NGC 6334 to study the gas velocity at different scales and probe the infall rates onto the protostellar cores embedded in the NGC 6334-I and I(N) clusters. This study makes use of single-dish and interferometric submillimeter observations, complemented with 3D numerical non-LTE radiative transfer modeling. We measure a mass accretion rate of 10-5 M⊙ yr-1 throughout the filament increasing up to 10-3 M⊙ yr-1 towards the densest regions where high-mass stars are forming. At smaller scales, our 3D model is consistent with accretion rates of 10-3 M⊙ yr-1 towards the clusters, and 10-4 M⊙ yr-1 onto the protostars.

  1. Aerodynamics of a sphere and an oblate spheroid for Mach numbers from 0.6 to 10.5 including some effects of test conditions

    NASA Technical Reports Server (NTRS)

    Spearman, M. Leroy; Braswell, Dorothy O.

    1993-01-01

    Wind-tunnel tests were made for spheres of various sizes over a range of Mach numbers and Reynolds numbers. The results indicated some conditions where the drag was affected by changes in the afterbody pressure due to a shock reflection from the tunnel wall. This effect disappeared when the Mach number was increased for a given sphere size or when the sphere size was decreased for a given Mach number. Drag measurements and Schlieren photographs are presented that show the possibility of obtaining inaccurate data when tests are made with a sphere too large for the test section size and Mach number. Tests were also made of an oblate spheroid. The results indicated a region at high Mach numbers where inherent positive static stability might occur with the oblate-face forward. The drag results are compared with those for a sphere as well as those for various other shapes. The drag results for the oblate spheroid and the sphere are also compared with some calculated results.

  2. Lateral distribution of high energy muons in EAS of sizes Ne approximately equals 10(5) and Ne approximately equals 10(6)

    NASA Technical Reports Server (NTRS)

    Bazhutov, Y. N.; Ermakov, G. G.; Fomin, G. G.; Isaev, V. I.; Jarochkina, Z. V.; Kalmykov, N. N.; Khrenov, B. A.; Khristiansen, G. B.; Kulikov, G. V.; Motova, M. V.

    1985-01-01

    Muon energy spectra and muon lateral distribution in EAS were investigated with the underground magnetic spectrometer working as a part of the extensive air showers (EAS) array. For every registered muon the data on EAS are analyzed and the following EAS parameters are obtained, size N sub e, distance r from the shower axis to muon, age parameter s. The number of muons with energy over some threshold E associated to EAS of fixed parameters are measured, I sub reg. To obtain traditional characteristics, muon flux densities as a function of the distance r and muon energy E, muon lateral distribution and energy spectra are discussed for hadron-nucleus interaction model and composition of primary cosmic rays.

  3. Hadronic components of EAS by rigorous saddle point method in the energy range between 10(5) and 10(8) GeV

    NASA Technical Reports Server (NTRS)

    Roy, S.; Sinha, M.

    1985-01-01

    The study of hadronic components in the high energy range between 10 to the 5 and 10 to the 8 Gev exhibits by far the strongest mass sensitivity since the primary energy spectrum as discussed by Linsley and measured by many air shower experimental groups indicates a change of slope from -1.7 to 2.0 in this energy range. This change of slope may be due to several reasons such as a genuine spectral feature of astrophysical origin, a confinement effect of galactic component or a rather rapid change of mass, a problem which we have attempted to study here in detail.

  4. Impedance spectroscopy study with Ca(UO{sub 2}PO{sub 4}){sub 2}10.5H{sub 2}O films

    SciTech Connect

    Ramos-Barrado, J.R.; Benavente, J.; Bruque, S.; Martinez, M.

    1995-03-15

    Calcium uranyl phosphate (CaUP) films were prepared and characterized both chemically and structurally. The electrical behavior of the films, as a solid phase (dry film) and in contact with aqueous solutions of electrolytes containing the generating ions (wet film), was studied by impedance spectroscopy. These last measurements made it possible to determine the contribution of both the bulk film and film/electrolyte interface. For both dry and wet films, the equivalent circuits are a parallel combination of resistance and a nonideal capacitor. Temperature dependence of the impedance of the CAUP solid films was considered, while concentration dependence of the film resistance when it is in contact with the electrolyte solutions was determined. In this case, the contribution of both the bulk film and electrolyte/film interface to the total impedance was also studied.

  5. FINAL REPORT INTEGRATED DM1200 MELTER TESTING OF BUBBLER CONFIGURATIONS USING HLW AZ-101 SIMULANTS VSL-04R4800-4 REV 0 10/5/04

    SciTech Connect

    KRUGER AA; MATLACK KS; GONG W; BARDAKCI T; D'ANGELO NA; LUTZE W; CALLOW RA; BRANDYS M; KOT WK; PEGG IL

    2011-12-29

    This report documents melter and off-gas performance results obtained on the DM1200 HLW Pilot Melter during processing of AZ-101 HLW simulants. The tests reported herein are a subset of six tests from a larger series of tests described in the Test Plan for the work; results from the other tests have been reported separately. The solids contents of the melter feeds were based on the WTP baseline value for the solids content of the feeds from pretreatment which changed during these tests from 20% to 15% undissolved solids resulting in tests conducted at two feed solids contents. Based on the results of earlier tests with single outlet 'J' bubblers, initial tests were performed with a total bubbling rate of 651 pm. The first set of tests (Tests 1A-1E) addressed the effects of skewing this total air flow rate back and forth between the two installed bubblers in comparison to a fixed equal division of flow between them. The second set of tests (2A-2D) addressed the effects of bubbler depth. Subsequently, as the location, type and number of bubbling outlets were varied, the optimum bubbling rate for each was determined. A third (3A-3C) and fourth (8A-8C) set of tests evaluated the effects of alternative bubbler designs with two gas outlets per bubbler instead of one by placing four bubblers in positions simulating multiple-outlet bubblers. Data from the simulated multiple outlet bubblers were used to design bubblers with two outlets for an additional set of tests (9A-9C). Test 9 was also used to determine the effect of small sugar additions to the feed on ruthenium volatility. Another set of tests (10A-10D) evaluated the effects on production rate of spiking the feed with chloride and sulfate. Variables held constant to the extent possible included melt temperature, plenum temperature, cold cap coverage, the waste simulant composition, and the target glass composition. The feed rate was increased to the point that a constant, essentially complete, cold cap was achieved, which was used as an indicator of a maximized feed rate for each test. The first day of each test was used to build the cold cap and decrease the plenum temperature. The remainder of each test was split into two- to six-day segments, each with a different bubbling rate, bubbler orientation, or feed concentration of chloride and sulfur.

  6. Recent evolution of river discharges in the Gulf of Trieste and their potential response to climate changes and anthropogenic pressure

    NASA Astrophysics Data System (ADS)

    Cozzi, Stefano; Falconi, Claus; Comici, Cinzia; Čermelj, Branko; Kovac, Nives; Turk, Valentina; Giani, Michele

    2012-12-01

    Freshwater and nutrient discharges by rivers were analysed in the northeastern Adriatic continental shelf from 1998 to 2008, in order to assess their role in the biogeochemistry of this coastal zone, as well as their potential future changes due to the effects of climate variability and anthropogenic pressure. River water loads (up to 6.05 km3 yr-1) and transport of nutrients (up to 13,200 t N yr-1 for TN, 86 t P yr-1 for TP and 12,400 t Si yr-1 for Si(OH)4) were high from 1998 to 2002, but they decreased by over 70% during the driest years 2003, 2005, 2006 and 2007. The precipitation in the surrounding continental region (average of 1371 mm yr-1) is the major forcing that regulates the runoff in this area, with peaks in early spring and autumn that are associated respectively to negative phases of Mediterranean Oscillation index and positive phases of West Mediterranean Oscillation index. This finding, together with the minor contribution of snowmelt in early spring (up to 3.2·10-5 kg m-2 s-1), indicates that the dynamics of the natural water cycle still overtake in this coastal zone the effects of anthropogenic usage of continental waters. During the last four decades, the northeastern Adriatic continental shelf has been subjected to an increasing pressure due to a high river transport of nitrogen and, currently, only a deep phosphorus deficiency in total (TN/TP = 49-405) and inorganic (DIN/PO4 = 37-418) river nutrient pools prevents its severe eutrophication. By contrast, the decrease of river loads of nutrients from 2003 to 2007 indicates that recurrent water crisis might significantly lower the trophic level in this coastal zone in the future. In this perspective, other allochthonous sources of nutrients, like sewage loads, atmospheric deposition and benthic fluxes might become more important for their balance, with possible implications on the structure of this ecosystem.

  7. Astronomical constraints on the cosmic evolution of the fine structure constant and possible quantum dimensions.

    PubMed

    Carilli, C L; Menten, K M; Stocke, J T; Perlman, E; Vermeulen, R; Briggs, F; de Bruyn, A G; Conway, J; Moore, C P

    2000-12-25

    We present measurements of absorption by the 21 cm hyperfine transition of neutral hydrogen toward radio sources at substantial look-back times. These data are used in combination with observations of rotational transitions of common interstellar molecules to set limits on the evolution of the fine structure constant: alpha/ alpha<3.5x10(-15) yr(-1), to a look-back time of 4.8 Gyr. In the context of string theory, the limit on the secular evolution of the scale factor of the compact dimensions, R, is &Rdot/ R<10(-15) yr(-1). Including terrestrial and other astronomical measurements places 2sigma limits on slow oscillations of R from the present to the epoch of cosmic nucleosynthesis, just seconds after the big bang, of DeltaR /R<10(-5). PMID:11136034

  8. The global gas and dust budget of the Small Magellanic Cloud

    NASA Astrophysics Data System (ADS)

    Matsuura, Mikako; Woods, Paul M.; Owen, Patrick J.

    2013-03-01

    In order to understand the evolution of the interstellar medium (ISM) of a galaxy, we have analysed the gas and dust budget of the Small Magellanic Cloud (SMC). Using the Spitzer Space Telescope, we measured the integrated gas mass-loss rate across asymptotic giant branch (AGB) stars and red supergiants (RSGs) in the SMC, and obtained a rate of 1.4 × 10-3 M⊙ yr-1. This is much smaller than the estimated gas ejection rate from Type II supernovae (SNe) (2-4 × 10-2 M⊙ yr-1). The SMC underwent an increase in star formation rate in the last 12 Myr, and consequently the galaxy has a relatively high SN rate at present. Thus, SNe are more important gas sources than AGB stars in the SMC. The total gas input from stellar sources into the ISM is 2-4 × 10-2 M⊙ yr-1. This is slightly smaller than the ISM gas consumed by star formation (˜8 × 10-2 M⊙ yr-1). Star formation in the SMC relies on a gas reservoir in the ISM, but eventually the star formation rate will decline in this galaxy, unless gas infalls into the ISM from an external source. The dust injection rate from AGB and RSG candidates is 1 × 10-5 M⊙ yr-1. Dust injection from SNe is in the range 0.2-11 × 10-4 M⊙ yr-1, although the SN contribution is rather uncertain. Stellar sources could be important for ISM dust (3 × 105 M⊙) in the SMC, if the dust lifetime is about 1.4 Gyr. We found that the presence of poly-aromatic hydrocarbons (PAHs) in the ISM cannot be explained entirely by carbon-rich AGB stars. Carbon-rich AGB stars could inject only 7 × 10-9 M⊙ yr-1 of PAHs at most, which could contribute up to 100 M⊙ of PAHs in the lifetime of a PAH. The estimated PAH mass of 1800 M⊙ in the SMC cannot be explained. Additional PAH sources, or ISM reprocessing should be needed.

  9. Direct Detections of Young Stars in Nearby Elliptical Galaxies

    NASA Astrophysics Data System (ADS)

    Ford, H. Alyson; Bregman, Joel N.

    2013-06-01

    Small amounts of star formation in elliptical galaxies are suggested by several results: surprisingly young ages from optical line indices, cooling X-ray gas, and mid-infrared dust emission. Such star formation has previously been difficult to directly detect, but using ultraviolet Hubble Space Telescope Wide Field Camera 3 imaging, we have identified individual young stars and star clusters in four nearby ellipticals. Ongoing star formation is detected in all galaxies, including three ellipticals that have previously exhibited potential signposts of star-forming conditions (NGC 4636, NGC 4697, and NGC 4374), as well as the typical "red and dead" NGC 3379. The current star formation in our closest targets, where we are most complete, is between 2.0 and 9.8 × 10-5 M ⊙ yr-1. The star formation history was roughly constant from 0.5 to 1.5 Gyr (at (3-5) × 10-4 M ⊙ yr-1), but decreased by a factor of several in the past 0.3 Gyr. Most star clusters have a mass between 102 and 104 M ⊙. The specific star formation rates of ~10-16 yr-1 (at the present day) or ~10-14 yr-1 (when averaging over the past Gyr) imply that a fraction 10-8 of the stellar mass is younger than 100 Myr and 10-5 is younger than 1 Gyr, quantifying the level of frosting of recent star formation over the otherwise passive stellar population. There is no obvious correlation between either the presence or spatial distribution of postulated star formation indicators and the star formation we detect. Based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with program 11583.

  10. On the lack of X-ray bright Type IIP supernovae

    NASA Astrophysics Data System (ADS)

    Dwarkadas, V. V.

    2014-05-01

    Type IIP supernovae (SNe) are expected to arise from red supergiant stars (RSGs). These stars have observed mass-loss rates that span more than two orders of magnitude, from less than 10^{-6} M_{⊙} yr-1 to almost 10^{-4} M_{⊙} yr-1. Thermal bremsstrahlung X-ray emission from at least some IIPs should reflect the larger end of the high mass-loss rates. Strangely, no IIP SNe are seen where the X-ray luminosity is large enough to suggest mass-loss rates greater than about 10^{-5} M_{⊙} yr-1. We investigate if this could be due to absorption of the X-ray emission. After carefully studying all the various aspects, we conclude that absorption would not be large enough to prevent us from having detected X-ray emission from high mass-loss rate IIPs. This leads us to the conclusion that there may be an upper limit of ˜10^{-5} M_{⊙} yr-1 to the mass-loss rate of Type IIP progenitors, and therefore to the luminosity of RSGs that explode to form Type IIPs. This in turn suggests an upper limit of ≲ 19 M_{⊙} for the progenitor mass of a Type IIP SN. This limit is close to that obtained by direct detection of IIP progenitors, as well as that suggested by recent stellar evolution calculations. Although the statistics need to be improved, many current indicators support the notion that RSGs above ˜ 19 M_{⊙} do not explode to form Type IIP SNe.

  11. The Nature of Irac-selected Extremely Red Objects

    NASA Astrophysics Data System (ADS)

    Wang, Tao; Huang, J.; Gu, Q.

    2010-05-01

    Using deep U-8um photometry from GEMs, MUSYC and SIMPLE surveys, we investigate properties of a large sample of IRAC-selected extremely red galaxies(IEROs). The sample comprises 304 brightest IEROs distributed over the GEMS field with a total area of 800 arcmin2, which satisfy ([3.6]+[4.5]/2)<21.2 and z-[3.6] > 3.25). Combined with the deepest Chandra and Spitzer surveys in this field, we are able to determine relative contributions of AGNs, (dusty) star-forming galaxies and passively evolving systems to the RED population; 51 sources are detected in at least one of three X-ray bands, leaving 253 non-Xray sources with 179 detected in 24um( 20uJy, 3sigma), indicating that at most 25% of these IEROs are passively evolving.We derive and examine photometric redshift using different methods; their redshift range from 1 to 2.6 with the median value at 1.5. Stellar masses of non-Xray sources are also derived with SED fitting methods, achieving a median value of 0.4*1011 Msun for a chrabrier initial mass function. The properties of best-fitting BC03 models are consistent with templates used for estimating redshifts, which have on average E(B-V) of 0.5 for 24um-deteced galaxies. The corresponding star-formation rates of these star-forming galaxies through SED fitting are within 40-100 Msun yr-1, consistent with that derived from their 24μm flux, which show a median total infrared luminosity 1*1011Lsun. We argue that such selected IEROs may represent a transient population from ULIRGs to LIRGs, and are likely descents of SMGs or DOGs.

  12. The VIRUS-P Exploration of Nearby Galaxies (VENGA): Radial Gas Inflow and Shock Excitation in NGC 1042

    NASA Astrophysics Data System (ADS)

    Luo, Rongxin; Hao, Lei; Blanc, Guillermo A.; Jogee, Shardha; van den Bosch, Remco C. E.; Weinzirl, Tim

    2016-06-01

    NGC 1042 is a late-type bulgeless disk galaxy that hosts low-luminosity active galactic nuclei (AGNs) coincident with a massive nuclear star cluster. In this paper, we present the integral field spectroscopy studies of this galaxy, based on the data obtained with the Mitchell spectrograph on the 2.7 m Harlan J. Smith telescope. In the central 100–300 pc region of NGC 1042, we find a circumnuclear ring structure of gas with enhanced ionization, which we suggest is mainly induced by shocks. Combining this with the harmonic decomposition analysis of the velocity field of the ionized gas, we propose that the shocked gas is the result of gas inflow driven by the inner spiral arms. The inflow velocity is ˜ 32+/- 10 {km} {{{s}}}-1, and the estimated mass-inflow rate is ˜ 1.1+/- 0.3× {10}-3 {M}ȯ {{yr}}-1. The mass-inflow rate is about one hundred times the black hole’s mass-accretion rate (˜ 1.4× {10}-5 {M}ȯ {{yr}}-1) and slightly larger than the star-formation rate in the nuclear star cluster (7.94× {10}-4 {M}ȯ {{yr}}-1), implying that the inflow material is enough to feed both the AGN activity and star formation in the nuclear star cluster. Our study highlights that secular evolution can be important in late-type unbarred galaxies like NGC 1042.

  13. The VIRUS-P Exploration of Nearby Galaxies (VENGA): Radial Gas Inflow and Shock Excitation in NGC 1042

    NASA Astrophysics Data System (ADS)

    Luo, Rongxin; Hao, Lei; Blanc, Guillermo A.; Jogee, Shardha; van den Bosch, Remco C. E.; Weinzirl, Tim

    2016-06-01

    NGC 1042 is a late-type bulgeless disk galaxy that hosts low-luminosity active galactic nuclei (AGNs) coincident with a massive nuclear star cluster. In this paper, we present the integral field spectroscopy studies of this galaxy, based on the data obtained with the Mitchell spectrograph on the 2.7 m Harlan J. Smith telescope. In the central 100–300 pc region of NGC 1042, we find a circumnuclear ring structure of gas with enhanced ionization, which we suggest is mainly induced by shocks. Combining this with the harmonic decomposition analysis of the velocity field of the ionized gas, we propose that the shocked gas is the result of gas inflow driven by the inner spiral arms. The inflow velocity is ∼ 32+/- 10 {km} {{{s}}}-1, and the estimated mass-inflow rate is ∼ 1.1+/- 0.3× {10}-3 {M}ȯ {{yr}}-1. The mass-inflow rate is about one hundred times the black hole’s mass-accretion rate (∼ 1.4× {10}-5 {M}ȯ {{yr}}-1) and slightly larger than the star-formation rate in the nuclear star cluster (7.94× {10}-4 {M}ȯ {{yr}}-1), implying that the inflow material is enough to feed both the AGN activity and star formation in the nuclear star cluster. Our study highlights that secular evolution can be important in late-type unbarred galaxies like NGC 1042.

  14. Environmental impact from mountainous olive orchards under different soil-management systems (SE Spain).

    PubMed

    Francia Martínez, José R; Durán Zuazo, Víctor H; Martínez Raya, Armando

    2006-04-01

    Soil erosion, runoff and nutrient-loss patterns over a two-year period (1999-2000) were monitored in erosion plots on a mountainside with olive (Olea europaea cv. Picual) trees under three different types of soil management: (1) non-tillage with barley (Hordeum vulgare) strips of 4 m width (BS); (2) conventional tillage (CT); (3) non-tillage without plant strips (NT). The erosion plots, located in Lanjaron (Alpujarras) on the southern flank of the Sierra Nevada Mountains in south-eastern Spain, had 30% slope at an altitude of 565 m and 192 m(2) (24x8 m) in area. The highest erosion and runoff values, ranging from 10.5 to 40.7 t ha(-1) yr(-1) and from 26.5 to 51.5 mm yr(-1), respectively, over the entire study period, were measured under NT. In CT, erosion ranged from 1.0 to 10.4 t ha(-1) yr(-1) and runoff from 6.7 to 15.2 mm yr(-1), while under BS, erosion ranged from 1.7 to 2.4 t ha(-1) yr(-1) and runoff from 19.6 to 20.0 mm yr(-1). It is concluded that the BS and CT reduced the soil erosion by 92% and 78%, with respect to the NT, and the runoff by 49% and 72%, respectively. The total NPK losses (sediments and runoff) from BS averaged 0.87, 0.07 and 0.72 kg ha(-1), from CT 1.82, 0.11 and 0.97 kg ha(-1) and from NT 3.15, 0.29 and 2.45 kg ha(-1), respectively. In addition, nutrient concentrations in the surface runoff were higher than the recommended level for standard water quality for N-NO(3), N-NH(4) and soluble P, particularly from NT and CT. These results support the recommendation of non-tillage with barley strips for sloped agricultural land in order to reduce erosion and pollution. PMID:15990157

  15. Probing the mass-loss history of AGB and red supergiant stars from CO rotational line profiles. II. CO line survey of evolved stars: derivation of mass-loss rate formulae

    NASA Astrophysics Data System (ADS)

    De Beck, E.; Decin, L.; de Koter, A.; Justtanont, K.; Verhoelst, T.; Kemper, F.; Menten, K. M.

    2010-11-01

    Context. The evolution of intermediate and low-mass stars on the asymptotic giant branch is dominated by their strong dust-driven winds. More massive stars evolve into red supergiants with a similar envelope structure and strong wind. These stellar winds are a prime source for the chemical enrichment of the interstellar medium. Aims: We aim to (1) set up simple and general analytical expressions to estimate mass-loss rates of evolved stars, and (2) from those calculate estimates for the mass-loss rates of the asymptotic giant branch, red supergiant, and yellow hypergiant stars in our galactic sample. Methods: The rotationally excited lines of carbon monoxide (CO) are a classic and very robust diagnostic in the study of circumstellar envelopes. When sampling different layers of the circumstellar envelope, observations of these molecular lines lead to detailed profiles of kinetic temperature, expansion velocity, and density. A state-of-the-art, nonlocal thermal equilibrium, and co-moving frame radiative transfer code that predicts CO line intensities in the circumstellar envelopes of late-type stars is used in deriving relations between stellar and molecular-line parameters, on the one hand, and mass-loss rate, on the other. These expressions are applied to our extensive CO data set to estimate the mass-loss rates of 47 sample stars. Results: We present analytical expressions for estimating the mass-loss rates of evolved stellar objects for 8 rotational transitions of the CO molecule and thencompare our results to those of previous studies. Our expressions account for line saturation and resolving of the envelope, thereby allowing accurate determination of very high mass-loss rates. We argue that, for estimates based on a single rotational line, the CO(2-1) transition provides the most reliable mass-loss rate. The mass-loss rates calculated for the asympotic giant branch stars range from 4 × 10-8 M⊙ yr-1 up to 8 × 10-5 M⊙ yr-1. For red supergiants they reach

  16. The Biogeochemical Role of Antarctic Krill and Baleen Whales in Southern Ocean Nutrient Cycling.

    NASA Astrophysics Data System (ADS)

    Ratnarajah, L.

    2015-12-01

    Iron limits primary productivity in large areas of the Southern Ocean. It has been suggested that baleen whales form a crucial part of biogeochemical cycling processes through the consumption of nutrient-rich krill and subsequent defecation, but evidence on their contribution is scarce. We analysed the concentration of iron in Antarctic krill and baleen whale faeces and muscle. Iron concentrations in Antarctic krill were over 1 million times higher, and whale faecal matter were almost 10 million times higher than typical Southern Ocean High Nutrient Low Chlorophyll seawater concentrations. This suggests that Antarctic krill act as a reservoir of in in Southern Ocean surface waters, and that baleen whales play an important role in converting this fixed iron into a liquid form in their faeces. We developed an exploratory model to examine potential contribution of blue, fin and humpback whales to the Southern Ocean iron cycle to explore the effect of the recovery of great whales to historical levels. Our results suggest that pre-exploitation populations of blue whales and, to a lesser extent fin and humpback whales, could have contributed to the more effective recycling of iron in surface waters, resulting in enhanced phytoplankton production. This enhanced primary productivity is estimated to be: 8.3 x 10-5 to 15 g C m-2 yr-1 (blue whales), 7 x 10-5 to 9 g C m-2 yr-1 (fin whales), and 10-5 to 1.7 g C m-2 yr-1 (humpback whales). To put these into perspective, current estimates of primary production in the Southern Ocean from remotely sensed ocean colour are in the order of 57 g C m-2 yr-1 (south of 50°). The high degree of uncertainty around the magnitude of these increases in primary productivity is mainly due to our limited quantitative understanding of key biogeochemical processes including iron content in krill, krill consumption rates by whales, persistence of iron in the photic zone, bioavailability of retained iron, and carbon-to-iron ratio of phytoplankton

  17. An abnormal radiant luminosity of the contact binary GZ Andromedae and its possible explanation

    NASA Astrophysics Data System (ADS)

    Yang, Y.; Liu, Q.

    2003-04-01

    Complete BV light curves of the W UMa type binary GZ And is presented in this paper. From the present times of minimum light and those collected from the references, the changes in the orbital period of the system are analyzed. The result reveals that the orbital period of GZ And continuously increased at a period change rate of (dp)/(p)=2.00*E-10. The observed orbital period increase of GZ And may be explained by a mass transfer rate from the smaller to the larger component of Delta m=1.05x10-7 Msun yr-1. The present light curves are analyzed by means of the latest version of the Wilson-Devinney code. The results suggest that GZ And is a W-subtype W UMa contact binary with a mass ratio of 0.511. The present photometric mass ratio is in agreement with that obtained spectroscopically by Lu & Rucinski (\\cite{Lu99}). Combining the present photometric solution with the spectroscopic orbital elements by Lu & Rucinski (\\cite{Lu99}), we give absolute dimensions of GZ And. The determined masses and radii of the components show that GZ And is an unevolved main-sequence binary, but the luminosity of the primary is abnormally low for the same mass main-sequence star. The low luminosity of the primary may be explained by transformation between gravitational energy and thermal energy of the system.

  18. Effect of the percentage of SF6 (100% 10% 5%) on the decomposition of SF6 N2 mixtures under negative dc coronas in the presence of water vapour or oxygen

    NASA Astrophysics Data System (ADS)

    Diaz, J.; Casanovas, A. M.; Casanovas, J.

    2003-07-01

    Low SF6 content SF6-N2 mixtures have recently been proposed as a replacement for pure SF6 in the insulation of gas insulated lines (GIL). Among the areas of investigation of such gas mixtures, their electrical decomposition under corona discharges must be studied considering the possible occurrence of such stress in GIL. This paper presents data concerning the decomposition of high-pressure SF6-N2 (5 : 95) mixtures (400 kPa) submitted to negative dc coronas in the absence or presence of 0.3% H2O or 0.3% O2. The chemical stability of these mixtures is compared with that of SF6-N2 (10 : 90) mixtures or undiluted SF6 investigated in the same conditions in a previous paper. The corona discharges were generated with a point-to-plane set-up and the gaseous by-products were assayed by gas chromatography at the end of each run carried out over a range of transported charge covering 0-13 C. The following by-products were detected and assayed: SOF4, SO2F2, (SF4 + SOF2), SO2, S2F10, S2O2F10, S2O3F6, (SF5)2NF, NF3 and N2O. Whatever the type or the concentration of impurity added to the SF6-N2 mixtures the major compound groups, (SOF4 + SO2F2) and (SF4 + SOF2 + SO2), were formed with 5% SF6 in quantities very close to those observed with 10% SF6. However, the lesser production rates of S2F10, (SF5)2NF and NF3 measured with the most dilute SF6-N2 mixtures makes the use of SF6-N2 (5 : 95) more advantageous than that of SF6-N2 (10 : 90) in all cases. Considering the overall quantity of by-products formed in the presence of water or without any impurity added, it appears that SF6-N2 mixtures are, from this point of view, preferable to pure SF6.

  19. Gas Poor Galaxies in MKW/AWM Clusters

    NASA Astrophysics Data System (ADS)

    Williams, B. A.

    1995-03-01

    Follow-up observations were made of the neutral hydrogen content of 129 galaxies near the cores of MKW 4, MKW 8, MKW 11, AWM 4, and AWM 5. The neutral hydrogen content of these galaxies appears to be lower than that of galaxies of similar type in the field or in loose groups and are more consistent with those of galaxies in the richer Abell clusters. Of the 14 galaxies that appear to be spirals in MKW 4, only one was detected above a sensitivity limit of ~ 10(5) Msun /Mpc(2) . The low detection rate of galaxies in MKW 4 suggest that its core is truly deficient in neutral hydrogen gas.

  20. Determination of atmospheric nitrogen deposition to a semi-natural peat bog site in an intensively managed agricultural landscape

    NASA Astrophysics Data System (ADS)

    Hurkuck, Miriam; Brümmer, Christian; Mohr, Karsten; Grünhage, Ludger; Flessa, Heinz; Kutsch, Werner L.

    2014-11-01

    Rising levels of atmospheric nitrogen (N) deposition have been found to affect the primary productivity and species composition of most terrestrial ecosystems. Highly vulnerable ecosystems such as nutrient-poor bogs are expected to respond to increasing N input rates with a decrease in plant species diversity. Our study site - a moderately drained raised bog and one of only very few remaining protected peatland areas in Northwestern Germany - is surrounded by highly fertilised agricultural land and intensive livestock production. We quantified the annual deposition of atmospheric N over a period of two years. Dry deposition rates of different N species and their reactants were calculated from day and night-time concentrations measured by a KAPS denuder filter system. Dry N deposition amounted to 10.9 ± 1.0 kg N ha-1 yr-1 (year 1) and 10.5 ± 1.0 kg N ha-1 yr-1 (year 2). More than 80% of total deposited N was attributed to ammonia (NH3). A strong seasonality in NH3 concentrations and depositions could be observed. Day and night-time concentrations and depositions, however, did not differ significantly. Total N deposition including bulk N deposition resulted in about 25 kg N ha-1 yr-1. Our results suggest that the intensive agricultural land management of surrounding areas and strongly emitting animal husbandry lead to N inputs into the protected peatland area that exceed the ecosystem's specific critical load up to fivefold. This gives rise to the assumption that a further shift in plant species composition with a subsequent alteration of the local hydrological regime can be expected.

  1. The Cretaceous Okhotsk-Chukotka Volcanic Belt (NE Russia): Geology, geochronology, magma output rates, and implications on the genesis of silicic LIPs

    NASA Astrophysics Data System (ADS)

    Tikhomirov, P. L.; Kalinina, E. A.; Moriguti, T.; Makishima, A.; Kobayashi, K.; Cherepanova, I. Yu.; Nakamura, E.

    2012-04-01

    The Cretaceous Okhotsk-Chukotka volcanic belt (OCVB) is a prominent subduction-related magmatic province, having the remarkably high proportion of silicic rocks (ca. 53% of the present-day crop area, and presumably over 70% of the total volcanic volume). Its estimated total extrusive volume ranges between 5.5 × 105 km3 (the most conservative estimate) and over 106 km3. This article presents a brief outline of the geology of OCVB, yet poorly described in international scientific literature, and results of a geochronological study on the northern part of the volcanic belt. On the base of new and published U-Pb and 40Ar/39Ar age determinations, a new chronological model is proposed. Our study indicates that the activity of the volcanic belt was highly discontinuous and comprised at least five main episodes at 106-98 Ma, 94-91 Ma, 89-87 Ma, 85.5-84 Ma, and 82-79 Ma. The new data allow a semi-quantitative estimate of the volcanic output rate for the observed part of the OCVB (area and volume approximately 105 km2 and 2.5 × 105 km3, respectively). The average extrusion rate for the entire lifetime of the volcanic belt ranges between 1.6 and 3.6 × 10- 5 km3yr- 1 km- 1, depending on the assumed average thickness of the volcanic pile; the optimal value is 2.6 × 10- 5 km3yr- 1 km- 1. Despite imprecise, such estimates infer the time-averaged volcanic productivity of the OCVB is similar to that of silicic LIPs and most active recent subduction-related volcanic areas of the Earth. However, the most extensive volcanic flare-ups at 89-87 and 85.5-84 Ma had higher rates of over 9.0 × 10- 5 km3yr- 1 km- 1. The main volumetric, temporal and compositional parameters of the OCVB are similar to those of silicic LIPs. This gives ground for discussion about the geodynamic setting of the latters, because the widely accepted definition of a LIP implies a strictly intraplate environment. Considering the genesis of the OCVB and other large provinces of silicic volcanism, we propose that

  2. Structure and Stability of Steady Protostellar Accretion Flows - Part Three - Nonlinear Instabilities

    NASA Astrophysics Data System (ADS)

    Balluch, M.

    1991-03-01

    Recently, a global, linear stability analysis of the structure of spherically symmetric steady protostellar accretion flows with a shock discontinuity has been made (Balluch 1990b). A detailed non-linear time-dependent radiation hydrodynamics calculation is presented to complement this study. In the `ideal-case' with constant opacity, the shock front around the second, inner core appears unstable with respect to oscillation due to critical cooling, starting at the instant, when a cooling region occurs in the calculation (due to its resolution in the late stages of accretion) and lasting as long as the mass flow rate is larger than M ≥ 2.8 10-6 Msun yr-1. This is in best agreement with the results of the linear analysis. Next, a detailed calculation of the formation of the first, outer core using quasimolecular artificial viscosity length scales, is presented. In about twice the e-folding time of the unstable mode in the linear analysis, a significant growth of a disturbance can be seen. It appears first in the velocity and the radiation flux in the settling zone, accompanied by an oscillation of the radiation flux in the region upstream from the shock up to r = 1014 cm. Some time later, the shock front starts to move. Again, these characteristics are in best concordance with the linear results. In addition, the calculation shows the growth of these oscillations deep in the non-linear regime until the beginning of a rapid expansion of the whole protostellar core. At last, a calculation of the global evolution of this expansion of the first, outer core is presented. It is shown that the expansion is stopped when about twice the core mass is involved. Then another collapse follows, and the whole scenario of formation and expansion of the outer core starts anew. During this evolution, up to 3 shock fronts were present at the same time in the flow. The largest expansion leads to central physical quantities comparable to the initial ones of the interstellar medium. At

  3. Primary productivity and the prospects for biofuels in the United Kingdom

    NASA Astrophysics Data System (ADS)

    Lawson, G. J.; Callaghan, T. V.

    1983-09-01

    Estimates of land use and plant productivity are combined to predict total annual primary production in the UK as 252 million tonnes dry matter (10.5 t ha-1yr-1). Annual above ground production is predicted to be 165 Mt (6.9 t ha-1yr-1). Within these totals, intensive agriculture contributes 60%, productive woodland 8%, natural vegetation 26% and urban vegetation 5%. However, only 25% of total plant production is cropped by man and animals, and most of this is subsequently discarded as wastes and residues. 2112 PJ of organic material is available for fuel without reducing food or fibre production, but since much of this could not be economically collected, 859 PJ is calculated as a more realistic biofuel contribution by the year 2000. After deducting 50% conversion losses, this could save P1 billion (1979 prices) in oil imports. Short rotation energy plantations, forest residues, coppice woodlands, animal and crop wastes, industrial and domestic wastes, catch crops, natural vegetation and urban vegetation all have immediate or short term potential as biofuel sources. Sensitive planning is required to reduce environmental impact, but in some cases more diverse wildlife habitats may be created.

  4. Interprovincial Reliance for Improving Air Quality in China: A Case Study on Black Carbon Aerosol.

    PubMed

    Li, Yun; Meng, Jing; Liu, Junfeng; Xu, Yuan; Guan, Dabo; Tao, Wei; Huang, Ye; Tao, Shu

    2016-04-01

    Black carbon (BC) is of global concern because of its adverse effects on climate and human health. It can travel long distances via atmospheric movement and can be geographically relocated through trade. Here, we explored the integrated patterns of BC transport within 30 provinces in China from the perspective of meteorology and interprovincial trade using the Weather Research and Forecasting with Chemistry (WRF/Chem) model and multiregional input-output analysis. In general, cross-border BC transport, which accounts for more than 30% of the surface concentration, occurs mainly between neighboring provinces. Specifically, Hebei contributes 1.2 μg·m(-3) BC concentration in Tianjin. By contrast, trade typically drives virtual BC flows from developed provinces to heavily industrial provinces, with the largest net flow from Beijing to Hebei (4.2 Gg). Shanghai is most vulnerable to domestic consumption with an average interprovincial consumption influence efficiency of 1.5 × 10(-4) (μg·m(-3))/(billion Yuan·yr(-1)). High efficiencies (∼8 × 10(-5) (μg·m(-3))/(billion Yuan·yr(-1))) are also found from regions including Beijing, Jiangsu, and Shanghai to regions including Hebei, Shandong, and Henan. The above source-receptor relationship indicates two control zones: Huabei and Huadong. Both mitigating end-of-pipe emissions and rationalizing the demand for pollution-intense products are important within the two control zones to reduce BC and other pollutants. PMID:26950657

  5. The rate of Type Ia supernovae at z ~ 0.2 from SDSS-I overlapping fields

    NASA Astrophysics Data System (ADS)

    Horesh, A.; Poznanski, D.; Ofek, E. O.; Maoz, D.

    2008-10-01

    In the course of the Sloan Digital Sky Survey (SDSS-I), a large fraction of the surveyed area was observed more than once due to field tiling overlap, usually at different epochs. We utilize some of these data to perform a supernova (SN) survey at a mean redshift of z = 0.2. Our archival search, in ~5 per cent of the SDSS-I overlap area, produces 29 SN candidates clearly associated with host galaxies. Using the Bayesian photometric classification algorithm of Poznanski et al., and correcting for classification bias, we find 17 of the 29 candidates are likely Type Ia SNe. Accounting for the detection efficiency of the survey and for host extinction, this implies a Type Ia SN rate of rIa = (14.0+2.5+1.4-2.5-1.1 +/- 2.5) × 10-14h270yr-1L-1solar,g, where the errors are Poisson error, systematic detection efficiency error and systematic classification error, respectively. The volumetric rate is RIa = (1.89+0.42+0.18-0.34-0.15 +/- 0.42) × 10-5yr-1h370Mpc-3. Our measurement is consistent with other rate measurements at low redshift. An order of magnitude increase in the number of SNe is possible by analysing the full SDSS-I data base.

  6. Methane emissions from vehicles.

    PubMed

    Nam, E K; Jensen, T E; Wallington, T J

    2004-04-01

    Methane (CH4) is an important greenhouse gas emitted by vehicles. We report results of a laboratory study of methane emissions using a standard driving cycle for 30 different cars and trucks (1995-1999 model years) from four different manufacturers. We recommend the use of an average emission factor for the U.S. on-road vehicle fleet of (g of CH/g of CO2) = (15 +/- 4) x 10(-5) and estimate that the global vehicle fleet emits 0.45 +/- 0.12 Tg of CH4 yr(-1) (0.34 +/- 0.09 Tg of C yr(-1)), which represents < 0.2% of anthropogenic CH4 emissions. This estimate includes the effects of vehicle aging, cold start, and hot running emissions. The contribution of CH4 emissions from vehicles to radiative forcing of climate change is 0.3-0.4% of that of CO2 emissions from vehicles. The environmental impact of CH4 emissions from vehicles is negligible and is likely to remain so for the foreseeable future. PMID:15112800

  7. Near-infrared Observations of SiO Maser-emitting Asymptotic Giant Branch (AGB) Stars

    NASA Astrophysics Data System (ADS)

    Chibueze, James O.; Miyahara, Takeshi; Omodaka, Toshihiro; Ohta, Takashi; Fujii, Takahiro; Tanaka, Masuo; Motohara, Kentaro; Makoto, Miyoshi

    2016-02-01

    Near-infrared (NIR) monitoring observations of asymptotic giant branch stars exciting bright SiO masers have been made with the 1 m telescope of Kagoshima University. In order to investigate the properties of these stars and their envelopes, we combined our NIR photometric data with mid- and far-infrared flux data obtained by the IRAS satellite, SiO maser flux data provided by the Nobeyama Radio Observatory, visual magnitude data provided by the AAVSO, and the reported data on the expansion velocities of the circumstellar envelopes. The absolute magnitudes at the K-band and the distances are estimated using the period-luminosity relation of Mira variables determined by Feast et al. Then, mass-loss rates and isotropic luminosities of an SiO maser are estimated. The mass-loss rates range from approximately 10-8 {M}⊙ \\{{yr}}-1 to over 10-5 {M}⊙ {{yr}}-1. We found that the NIR pulsation amplitudes are correlated with the pulsation periods and the observed wavelengths. We also found correlations of the isotropic luminosities of SiO masers with the mass-loss rates and absolute magnitudes at the K-band. These results will help us to understand the pumping mechanism of SiO masers. We measured, for the first time, the periods and/or NIR magnitudes of TX Cam, BW Cam, IRAS 06297+4045, IRAS 18387-0423, and RT Cep.

  8. Physical Properties of Emission-Line Galaxies at 2 from Near-Infrared Spectroscopy with Magellan FIRE

    NASA Astrophysics Data System (ADS)

    Masters, Daniel C.; McCarthy, P. J.; Malkan, M. A.; Siana, B. D.; Scarlata, C.; Hathi, N. P.; Atek, H.; Henry, A. L.; WISP Team

    2014-01-01

    We present results from near-infrared spectroscopy with Magellan FIRE of 26 strong emission-line galaxies at 2.2 and 1.5. The sample was selected from the WFC3 Infrared Spectroscopic Parallels (WISP) survey, which uses the near-infrared grism capability of the Hubble Space Telescope Wide Field Camera 3 to detect emission-line galaxies over 0.5 < z < 2.3. High-resolution ( 5000) follow-up spectroscopy with Magellan FIRE over 1.0--2.5 microns resolves important rest-frame optical emission lines, allowing us to measure physical properties such as dust obscuration, metal abundance, star formation rate, ionization parameter, and emission line kinematics. We also analyze the properties of composite spectra derived from the FIRE-observed sample. With this relatively large sample of rest-frame optical spectra we can make statistical inferences about the population of emission-line galaxies at 2. We find that the galaxies are low metallicity ( 1/5-1/2 Z_solar) as determined from the R23 calibration. The galaxies are low dust extinction on average (E(B-V 0.2) but with significant scatter. The dust-corrected H-alpha star formation rates range from ~10--150 M_sun yr^-1 with a mean of 50 M_su yr^-1. The average ionization parameter for the sample, log U ~ -2.5, is higher than typically found for star-forming galaxies in the local universe but consistent with those found in more intense starbursting regions in galaxies such as M82. Emission line velocity dispersions are measured to be 71 +- 38 km s^-1, in good agreement with other studies that have probed the H-alpha kinematics of star-forming galaxies at similar redshift. The galaxies are compact, with half-light radii of < 2 kpc, and ~50% show evidence for multiple structures or asymmetries in the WFC3 imaging. Based on the line velocity dispersions and the location of the galaxies on BPT diagnostic plots, there is little evidence for significant AGN contribution to most emission-line galaxies at 2.

  9. On the use of the correction factor with Japanese ozonesonde data

    NASA Astrophysics Data System (ADS)

    Morris, G. A.; Labow, G.; Akimoto, H.; Takigawa, M.; Fujiwara, M.; Hasebe, F.; Hirokawa, J.; Koide, T.

    2012-06-01

    In submitting data to the World Meteorological Organization (WMO) World Ozone and Ultraviolet Data Center (WOUDC), numerous ozonesonde stations include a correction factor (CF) that multiplies ozone concentration profile data so that the columns computed agree with column measurements from co-located ground-based and/or overpassing satellite instruments. We evaluate this practice through an examination of data from 4 Japanese ozonesonde stations: Kagoshima, Naha, Sapporo, and Tsukuba. While agreement between the sonde columns and Total Ozone Mapping Spectrometer (TOMS) or Ozone Mapping Instrument (OMI) is improved by use of the CF, agreement between the sonde ozone concentrations reported near the surface and data from surface monitors near the launch sites is negatively impacted. In addition, the agreement between the mean sonde columns without the CF and the ground-based Dobson instrument columns is improved by ~1.5% by using the McPeters et al. (1997) balloon burst climatology rather than the constant mixing ratio assumption for the above burst height column estimate. Limited comparisons of coincident ozonesonde profiles from Hokkaido University with those in the WOUDC database suggest that while the application of the CFs in the stratosphere improves agreement, it negatively impacts the agreement in the troposphere. Finally, unexplained trends and changing trends in the CFs appear over the last 20 yr. The overall trend in the CFs for the four Japanese ozonesonde stations from 1990-2010 is (-0.157 ± 0.032) × 10-2 yr-1; but from 1993-1999 the trend is (-2.21 ± 0.14) × 10-2 yr-1 and from 1999-2009 is (1.180 ± 0.059) × 10-2 yr-1, resulting in a statistically significant difference in CF trends between these two periods of (3.39 ± 0.15) × 10-2 yr-1. Given our analysis, we recommend the following: (1) use of the balloon burst climatology is preferred to a constant mixing ratio assumption for determining total column ozone with sonde data; (2) if CFs are

  10. Wet and dry deposition of mineral dust particles in Japan: factors related to temporal variation and spatial distribution

    NASA Astrophysics Data System (ADS)

    Osada, K.; Ura, S.; Kagawa, M.; Mikami, M.; Tanaka, T. Y.; Matoba, S.; Aoki, K.; Shinoda, M.; Kurosaki, Y.; Hayashi, M.; Shimizu, A.; Uematsu, M.

    2013-08-01

    Data of temporal variations and spatial distributions of mineral dust deposition fluxes are very limited in terms of duration, location, and processes of deposition. To ascertain temporal variations and spatial distributions of mineral dust deposition by wet and dry processes, weekly deposition samples were obtained at Sapporo, Toyama, Nagoya, Tottori, Fukuoka, and Cape Hedo (Okinawa) in Japan during October 2008-December 2010 using automatic wet and dry separating samplers. Mineral dust weights in water-insoluble residue were estimated from Fe contents measured using an X-ray fluorescence analyzer. For wet deposition, highest and lowest annual dust fluxes were found at Toyama (9.6 g m-2 yr-1) and at Cape Hedo (1.7 g m-2 yr-1) as average values in 2009 and 2010. Higher wet deposition fluxes were observed at Toyama and Tottori, where frequent precipitation (>60% days per month) was observed during dusty seasons. For dry deposition among Toyama, Tottori, Fukuoka, and Cape Hedo, the highest and lowest annual dust fluxes were found respectively at Fukuoka (5.2 g m-2 yr-1) and at Cape Hedo (2.0 g m-2 yr-1) as average values in 2009 and 2010. Although the seasonal tendency of the monthly dry deposition amount roughly resembled that of monthly days of Kosa dust events, the monthly amount of dry deposition was not proportional to monthly days of the events. Comparison of dry deposition fluxes with vertical distribution of dust particles deduced from Lidar data and coarse particle concentrations suggested that the maximum dust layer height or thickness is an important factor for controlling the dry deposition amount after long-range transport of dust particles. Size distributions of refractory dust particles were obtained using four-stage filtration: >20, >10, >5, and >1 μm diameter. Weight fractions of the sum of >20 μm and 10-20 μm (giant fraction) were higher than 50% for most of the event samples. Irrespective of the deposition type, the giant dust fractions were

  11. Neutral hydrogen in the vicinity of the supernova remnant HB 9

    NASA Astrophysics Data System (ADS)

    Gosachinskii, I. V.

    2013-03-01

    The neutral hydrogen emission at 21 cm has been investigated with the RATAN-600 radio telescope in the vicinity of the supernova remnant HB9. A clumpyHI shell with radial motions surrounding the remnant has been detected. Its measured parameters contradict the connection with a shock wave from a supernova explosion. The shell formation under the action of a wind from a star that exploded as a supernova at the end of its evolution seems more realistic. The characteristics of the star obtained from the observed shell parameters are the following: a wind power of 0.5 × 1038 erg s-1, a mass-loss rate of 3.7 × 10-5 M ⊙ yr-1, and an age of 3 × 106 yr. Given the measurement errors, the mass of the star is estimated to be >8 M ⊙.

  12. The NTT SUSI deep field

    NASA Astrophysics Data System (ADS)

    Arnouts, S.; D'Odorico, S.; Cristiani, S.; Zaggia, S.; Fontana, A.; Giallongo, E.

    1999-01-01

    We present a deep BVrI multicolor catalog of galaxies in a 5.62 sq.arcmin field 80 arcsec south of the high redshift (z=4.7) quasar BR 1202-0725, derived from observations with the direct CCD camera SUSI at the ESO NTT. The formal 5sigma magnitude limits (in 2x FWHM apertures) are 26.9, 26.5, 25.9 and 25.3 in B, V, r and I respectively. Counts, colors for the star and galaxy samples are discussed and a comparison with a deep HST image in the I band is presented. The percentage of merged or blended galaxies in the SUSI data to this magnitude limit is estimated to be not higher than 1%. At the same galactic latitude of the HDF but pointing toward the galactic center, the star density in this field is found to be ~ 3 times higher, with ~ 20% of the objects with V-I>3.0. Reliable colors have been measured for galaxies selected down to r=26. The choice of the optical filters has been optimized to define a robust multicolor selection of galaxies at 3.8<= z<= 4.4. Within this interval the surface density of galaxy candidates with r < 26 in this field is 2.7+/- 0.4 arcmin(-2) corresponding to a comoving density of Star Formation Rate at 3.8<= z<= 4.4 of 10(-2.00) - 10(-1.82) h(3) Msun * yr(-1) * Mpc(-3) . Based on observations collected at the NTT 3.5m of ESO, Chile The catalog is available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/Abstract.letml

  13. Six months of multiwavelength follow-up of the tidal disruption candidate ASASSN-14li and implied TDE rates from ASAS-SN

    NASA Astrophysics Data System (ADS)

    Holoien, T. W.-S.; Kochanek, C. S.; Prieto, J. L.; Stanek, K. Z.; Dong, Subo; Shappee, B. J.; Grupe, D.; Brown, J. S.; Basu, U.; Beacom, J. F.; Bersier, D.; Brimacombe, J.; Danilet, A. B.; Falco, E.; Guo, Z.; Jose, J.; Herczeg, G. J.; Long, F.; Pojmanski, G.; Simonian, G. V.; Szczygieł, D. M.; Thompson, T. A.; Thorstensen, J. R.; Wagner, R. M.; Woźniak, P. R.

    2016-01-01

    We present ground-based and Swift photometric and spectroscopic observations of the candidate tidal disruption event (TDE) ASASSN-14li, found at the centre of PGC 043234 (d ≃ 90 Mpc) by the All-Sky Automated Survey for SuperNovae (ASAS-SN). The source had a peak bolometric luminosity of L ≃ 1044 erg s-1 and a total integrated energy of E ≃ 7 × 1050 erg radiated over the ˜6 months of observations presented. The UV/optical emission of the source is well fitted by a blackbody with roughly constant temperature of T ˜ 35 000 K, while the luminosity declines by roughly a factor of 16 over this time. The optical/UV luminosity decline is broadly consistent with an exponential decline, L∝ e^{-t/t_0}, with t0 ≃ 60 d. ASASSN-14li also exhibits soft X-ray emission comparable in luminosity to the optical and UV emission but declining at a slower rate, and the X-ray emission now dominates. Spectra of the source show broad Balmer and helium lines in emission as well as strong blue continuum emission at all epochs. We use the discoveries of ASASSN-14li and ASASSN-14ae to estimate the TDE rate implied by ASAS-SN, finding an average rate of r ≃ 4.1 × 10-5 yr-1 per galaxy with a 90 per cent confidence interval of (2.2-17.0) × 10-5 yr-1 per galaxy. ASAS-SN found roughly 1 TDE for every 70 Type Ia supernovae in 2014, a rate that is much higher than that of other surveys.

  14. Antagonism of lateral saphenous vein serotonin receptors from steers grazing endophyte-free, wild-type, or novel endophyte-infected tall fescue.

    PubMed

    Klotz, J L; Aiken, G E; Johnson, J M; Brown, K R; Bush, L P; Strickland, J R

    2013-09-01

    Pharmacologic profiling of serotonin (5HT) receptors of bovine lateral saphenous vein has shown that cattle grazing endophyte-infected (Neotyphodium coenophialum) tall fescue (Lolium arundinaceum) have altered responses to ergovaline, 5HT, 5HT2A, and 5HT7 agonists. To determine if 5HT receptor activity of tall fescue alkaloids is affected by grazing endophyte-free (EF), wild-type [Kentucky-31 (KY31)], novel endophyte AR542-infected (MAXQ), or novel endophyte AR584-infected (AR584) tall fescue, contractile responses of lateral saphenous veins biopsied from cattle grazing these different fescue-endophyte combinations were evaluated in presence or absence of antagonists for 5HT2A (ketanserin) or 5HT7 (SB-269970) receptors. Biopsies were conducted over 2 yr on 35 mixed-breed steers (361.5 ± 6.3 kg) grazing EF (n = 12), KY31 (n = 12), MAXQ (n = 6), or AR584 (n = 5) pasture treatments (3 ha) between 84 and 98 d (Yr 1) or 108 to 124 d (Yr 2). Segments (2 to 3 cm) of vein were surgically biopsied, sliced into 2- to 3-mm cross-sections, and suspended in a myograph chamber containing 5 mL of oxygenated Krebs-Henseleit buffer (95% O2/5% CO2; pH = 7.4; 37°C). Veins were exposed to increasing concentrations of 5HT, ergovaline, and ergovaline + 1 × 10(-5) M ketanserin or + 1 × 10(-6) M SB-269970 in Yr 1. In Yr 2, ergotamine and ergocornine were evaluated in presence or absence of 1 × 10(-5) M ketanserin. Contractile response data were normalized to a reference addition of 1 × 10(-4) M norepinephrine. In Yr 1, contractile response to 5HT and ergovaline were least (P < 0.05) in KY31 pastures and the presence of ketanserin greatly reduced (P < 0.05) the response to ergovaline in all pastures. However, presence of SB-269970 did not (P = 0.91) alter contractile response to ergovaline. In Yr 2, there was no difference in contractile response to ergotamine (P = 0.13) or ergocornine (P = 0.99) across pasture treatments, but ketanserin reduced (P < 0.05) the contractile response to

  15. Impact of Dust Cooling on Direct-collapse Black Hole Formation

    NASA Astrophysics Data System (ADS)

    Latif, M. A.; Omukai, K.; Habouzit, M.; Schleicher, D. R. G.; Volonteri, M.

    2016-05-01

    Observations of quasars at z\\gt 6 suggest the presence of black holes with a few times {10}9\\quad {M}ȯ . Numerous models have been proposed to explain their existence, including a direct collapse, which provides massive seeds of {10}5\\quad {M}ȯ . The isothermal direct collapse requires a strong Lyman–Werner (LW) flux to quench {{{H}}}2 formation in massive primordial halos. In this study, we explore the impact of trace amounts of metals and dust enrichment. We perform three-dimensional cosmological simulations for two halos of \\gt {10}7\\quad {M}ȯ with Z/{Z}ȯ ={10}-4{--}{10}-6 illuminated by an intense LW flux of {J}21={10}5. Our results show that initially the collapse proceeds isothermally with T∼ 8000 K, but dust cooling becomes effective at densities of {10}8{--}{10}12 {{cm}}-3 and brings the gas temperature down to a few 100–1000 K for Z/{Z}ȯ ≥slant {10}-6. No gravitationally bound clumps are found in the Z/{Z}ȯ ≤slant {10}-5 cases by the end of our simulations, in contrast to the case with Z/{Z}ȯ ={10}-4. Large inflow rates of ≥slant 0.1\\quad {M}ȯ {{yr}}-1 are observed for Z/{Z}ȯ ≤slant {10}-5, similar to a zero-metallicity case, while for Z/{Z}ȯ ={10}-4 the inflow rate starts to decline earlier because of dust cooling and fragmentation. For given large inflow rates, a central star of ∼ {10}4\\quad {M}ȯ may form for Z/{Z}ȯ ≤slant {10}-5.

  16. Infrared imaging and millimetre continuum mapping of Herbig Ae/Be and FU Orionis stars

    NASA Astrophysics Data System (ADS)

    Henning, Th.; Burkert, A.; Launhardt, R.; Leinert, Ch.; Stecklum, B.

    1998-08-01

    The goal of this paper is a detailed analysis of the dusty environment of Herbig Ae/Be stars and FU Orionis objects. For this purpose we mapped 22 regions at 1.3 mm wavelength containing 25 target objects. We found that it is indispensable to perform mapping in contrast to pointed On-On measurements in order to obtain the correct distribution of cold material around young stellar objects and to relate 1.3 mm flux densities to individual sources. To get reliable information about the structure and shape of the dust configurations and their relation to the stellar sources, we superimposed the millimetre maps on near-infrared images. The comparison of the data demonstrated that some of the Herbig Ae/Be stars are not associated with the peak of the millimetre emission. This is obviously the case for V 376 Cas/LkHα 198, MWC 137, CoD-42(deg) 11721, and V 1685 Cyg/V 1686 Cyg. We found two different morphologies of the dust envelopes: 6 regions show a compact structure, whereas 12 regions are characterized by a core/envelope structure. The ``disk'' objects AB Aur and HD 163296 show only a compact core and are not surrounded by an extended envelope. We did not detect HK Ori, HD 250550, LkHα 25, and V 1515 Cyg which all have low IRAS luminosities. Based on the flux densities derived from the millimetre maps, we estimated characteristic physical parameters like density and mass assuming optically thin emission. The total masses of the circumstellar regions around the Herbig Ae/Be stars with core/envelope structure and with ``genuine" point-like millimetre sources are 80+/-60 Msun\\ and 0.15+/-0.15 Msun, respectively. The lowest and highest masses of the circumstellar material were found around AB Aur (0.03 Msun) and CoD-42(deg) 11721 (1100 Msun), respectively. The average densities in the cores range from 10(5) to 10(8) cm(-3) . The densities of the extended envelopes are of the order of 10(4) to 10(5) cm(-3) . In addition, we combined the measured millimetre flux densities

  17. Mercury emissions to the atmosphere from natural and anthropogenic sources in the Mediterranean region

    NASA Astrophysics Data System (ADS)

    Pirrone, N.; Costa, P.; Pacyna, J. M.; Ferrara, R.

    This report discusses past, current and projected mercury emissions to the atmosphere from major industrial sources, and presents a first assessment of the contribution to the regional mercury budget from selected natural sources. Emissions (1995 estimates) from fossil fuels combustion (29.8 t yr -1) , cement production (28.8 t yr -1) and incineration of solid wastes (27.6 t yr -1) , all together account for about 82% of the regional anthropogenic total (105.7 t yr -1) . Other industrial sources in the region are smelters (4.8 t yr -1) , iron-steel plants (4.8 t yr -1) and other minor sources (chlor-alkali plants, crematoria, chemicals production) that have been considered together in the miscellaneous category (9.6 t yr -1) . Regional emissions from anthropogenic sources increased at a rate of 3% yr-1 from 1983 to 1995 and are projected to increase at a rate of 1.9% yr-1 in the next 25 years, if no improvement in emission control policy occurs. On a country-by-country basis, France is the leading emitter country with 22.6 t yr -1 followed by Turkey (16.1 t yr -1) , Italy (11.4 t yr -1) , Spain (9.1 t yr -1) , the former Yugoslavia 7.9 ( t yr -1) , Morocco (6.9 t yr -1) , Bulgaria (6.8 t yr -1) , Egypt (6.1 t yr -1) , Syria (3.6 t yr -1) , Libya (2.9 t yr -1) , Tunisia (2.8 t yr -1) and Greece (2.7 t yr -1) , whereas the remaining countries account for less than 7% of the regional total. The annual emission from natural sources is 110 t yr -1, although this figure only includes the volatilisation of elemental mercury from surface waters and emissions from volcanoes, whereas the contribution due to the degassing of mercury from top soil and vegetation has not been included in this first assessment. Therefore, natural and anthropogenic sources in the Mediterranean region release annually about 215 t of mercury, which represents a significant contribution to the total mercury budget released in Europe and to the global atmosphere.

  18. The evolution of the equivalent width of the Hα emission line and specific star formation rate in star-forming galaxies at 1 < z < 5

    NASA Astrophysics Data System (ADS)

    Mármol-Queraltó, E.; McLure, R. J.; Cullen, F.; Dunlop, J. S.; Fontana, A.; McLeod, D. J.

    2016-08-01

    We present the results of a study which uses spectral energy distribution (SED) fitting to investigate the evolution of the equivalent width (EW) of the Halpha emission line in star-forming galaxies over the redshift interval 1=1 in the CANDELS UDS and GOODS-S fields. Confining our analysis to a constant stellar mass range (9.5Msun)<10.5), we find that the median EW(Ha) evolves only modestly with redshift, reaching a rest-frame value of EW(Ha)=301+/-30 Angs by redshift z~4.5. Furthermore, using estimates of star-formation rate (SFR) based on both UV luminosity and Ha line flux, we use our galaxy samples to compare the evolution of EW(Ha) and specific star-formation rate (sSFR). Our results indicate that over the redshift range 1Msun are related by: EW(Ha)/Ang=(63+/-7)sSFR/Gyr^(-1). Given the current uncertainties in measuring the SFRs of high-redshift galaxies, we conclude that EW(Ha) provides a useful independent tracer of sSFR for star-forming galaxies out to redshifts of z=5.

  19. Nitrogen transfers and air-sea N2O fluxes in the upwelling off Namibia within the oxygen minimum zone: a 3-D model approach

    NASA Astrophysics Data System (ADS)

    Gutknecht, E.; Dadou, I.; Le Vu, B.; Cambon, G.; Sudre, J.; Garçon, V.; Machu, E.; Rixen, T.; Kock, A.; Flohr, A.; Paulmier, A.; Lavik, G.

    2011-04-01

    As regions of high primary production and being often associated to Oxygen Minimum Zones (OMZs), Eastern Boundary Upwelling Systems (EBUS) represent key regions for the oceanic nitrogen (N) cycle. Indeed, by exporting the Organic Matter (OM) and nutrients produced in the coastal region to the open ocean, EBUS can play an important role in sustaining primary production in subtropical gyres. Losses of fixed inorganic N, through denitrification and anammox processes and through nitrous oxide (N2O) emissions to the atmosphere, take place in oxygen depleted environments such as EBUS, and alleviate the role of these regions as a source of N. In the present study, we developed a 3-D coupled physical/biogeochemical (ROMS/BioBUS) model for investigating the full N budget in the Namibian sub-system of the Benguela Upwelling System (BUS). The different state variables of a climatological experiment have been compared to different data sets (satellite and in situ observations) and show that the model is able to represent this biogeochemical oceanic region. The N transfer is investigated in the Namibian upwelling system using this coupled model, especially in the Walvis Bay area between 22° S and 24° S where the OMZ is well developed (O2 < 0.5 ml O2 l-1). The upwelling process advects 24.2 × 1010 mol N yr-1 of nitrate enriched waters over the first 100 m over the slope and over the continental shelf. The meridional advection by the alongshore Benguela current brings also nutrient-rich waters with 21.1 × 1010 mol N yr-1. 10.5 × 1010 mol N yr-1 of OM are exported outside of the continental shelf (between 0 and 100-m depth). 32.4% and 18.1% of this OM are exported by advection in the form of Dissolved and Particulate Organic Matters (DOM and POM), respectively, however vertical sinking of POM represents the main contributor (49.5%) to OM export outside of the first 100-m depth of the water column on the continental shelf. The continental slope also represents a net N export

  20. Experimental studies of rapid bioerosion of coral reefs in the Galápagos Islands

    NASA Astrophysics Data System (ADS)

    Reaka-Kudla, M. L.; Feingold, J. S.; Glynn, W.

    1996-06-01

    Experimental carbonate blocks of coral skeleton, Porites lobata (PL), and cathedral limestone (LS) were deployed for 14.8 months at shallow (5 6 m) and deep (11 13m) depths on a severely bioeroded coral reef, Champion Island, Galápagos Islands, Ecuador. Sea urchins ( Eucidaris thouarsii) were significantly more abundant at shallow versus deep sites. Porites lobata blocks lost an average of 25.4 kg m-2yr-1 (23.71 m-2yr-1 or 60.5% decrease yr-1). Losses did not vary significantly at depths tested. Internal bioeroders excavated an average of 2.6 kg m-2 yr-1 (2.41 m-2 yr-1 or 0.6% decrease yr-1), while external bioeroders removed an average of 22.8 kg m-2 yr-1). (21.31 m-2 yr-1). or 59.9% decrease yr-1). few encrusting organisms were observed on the PL blocks. Cathedral limestone blocks lost an average of 4.1 kg m-2 yr-1). (1.81 m-2 yr-1). or 4.6% decrease yr-'), also with no relation to depth. Internal bioeroders excavated an average of 0.6 kg m-2 yr-1). (0.31 m-2 yr-1). or 0.7% decrease yr-1). and external bioeroders removed an average of 3.5 kg m-2 yr-1). (1.51 m-2 yr-1). or 3.9% decrease yr-1). from the LS blocks. Most (57.6%) encrustation occurred on the bottom of LS blocks, and there was more accretion on block bottoms in deep (61.4 mg cm-2 yr-1). versus shallow (35.0 mg cm-2 yr-1) sites. External bioerosion reduced the average height of the reef framework by 0.2 cm yr-1). for hard substrata (represented by LS) and 2.3 cm yr-1). for soft substrata (represented by PL). The results of this study suggest that coral reef frameworks in the Galápagos Islands are in serious jeopardy. If rates of coral recruitment do not increase, and if rates of bioerosion do not decline, coral reefs in the Galápagos Islands could be eliminated entirely.

  1. NH4NO3 fertilizer induces DON leaching from Sphagnum magellanicum

    NASA Astrophysics Data System (ADS)

    Hartsock, J. A.; Vile, M. A.; Wieder, R.

    2011-12-01

    Boreal peatlands globally function as long-term sinks for atmosheric CO2. Mosses in the genus Sphagnum dominate the understory of boreal peatlands, especially in ombrotrophic bogs for which the sole sources of new nitrogen (N) is atmospheric deposition and biological N2-fixation. Sphagnum mosses in undisturbed regions generally are thought to be N-limited because of slow nutrient turnover and low rates of atmospheric N deposition. In Alberta, Canada, mean background N deposition rates are less than 1 kg N ha-1yr-1, but increasing atmospheric N deposition is occurring as a consequence of oil sands development in northern Alberta. In some European countries, anthropogenic practices have increased annual N deposition rates to levels in excess of 20 kg N ha-1yr-1. Increased rates of atmospheric N deposition have been shown to alter N cycling processes of Sphagnum mosses. Current hypotheses propose that Sphagnum mosses leach dissolved organic nitrogen (DON) from their tissues to mitigate N saturation stress in high N deposition areas. The goal of this study was to determine whether Sphagnum magellanicum leaches DON when exposed to elevated concentrations of NH4NO3 applied experimentally as synthetic rainfall. Sphagnum magellanicum was collected from a fen in Driftwood, Pennsylvania (41°13'58"N 78°11'44"W). Intact cores (10.5cm x 5.5cm) were grown in 500 mL culture flasks in a controlled environment chamber at Villanova University. Ammonium nitrate was applied to moss treatments eight times over 73 days at concentrations equivalent to 6 kg N ha-1yr-1, 12 kg N ha-1yr-1, and 18 kg N ha-1yr-1 (n=5 replicates per treatment, 400 mL H2O per N addition). Leachates (freely drained water samples) were analyzed for dissolved total nitrogen (TN), ammonium (NH4+-N), nitrate (NO3--N), and DON (TN-DIN) concentrations. Results show that after 73 days, increasing DIN resulted in: 1) a shift from net N mineralization to net NH4+ immobilization (Control: 376.3 ± 15.2 ug/g; High N: -377

  2. The price of snow: albedo valuation and a case study for forest management

    NASA Astrophysics Data System (ADS)

    Lutz, David A.; Howarth, Richard B.

    2015-06-01

    Several climate frameworks have included the role of carbon storage in natural landscapes as a potential mechanism for climate change mitigation. This has resulted in an incentive to grow and maintain intact long-lived forest ecosystems. However, recent research has suggested that the influence of albedo-related radiative forcing can impart equal and in some cases greater magnitudes of climate mitigation compared to carbon storage in forests where snowfall is common and biomass is slow-growing. While several methodologies exist for relating albedo-associated radiative forcing to carbon storage for the analysis of the tradeoffs of these ecosystem services, they are varied, and they have yet to be contrasted in a case study with implications for future forest management. Here we utilize four methodologies for calculating a shadow price for albedo radiative forcing and apply the resulting eight prices to an ecological and economic forest model to examine the effects on optimal rotation periods on two different forest stands in the White Mountain National Forest in New Hampshire, USA. These pricing methodologies produce distinctly different shadow prices of albedo, varying from a high of 9.36 × 10-4 and a low of 1.75 × 10-5 w-1yr-1 in the initial year, to a high of 0.019 and a low of 3.55 × 10-4 w-1yr-1 in year 200 of the simulation. When implemented in the forest model, optimal rotation periods also varied considerably, from a low of 2 to a high of 107 years for a spruce-fir stand and from 35 to 80 years for a maple-beech-birch stand. Our results suggest that the choice of climate metrics and pricing methodologies for use with forest albedo alter albedo prices considerably, may substantially adjust optimal rotation period length, and therefore may have consequences with respect to forest land cover change.

  3. A 3D numerical model for Kepler's supernova remnant

    NASA Astrophysics Data System (ADS)

    Toledo-Roy, J. C.; Esquivel, A.; Velázquez, P. F.; Reynoso, E. M.

    2014-07-01

    We present new 3D numerical simulations for Kepler's supernova remnant. In this work we revisit the possibility that the asymmetric shape of the remnant in X-rays is the product of a Type Ia supernova explosion which occurs inside the wind bubble previously created by an AGB companion star. Due to the large peculiar velocity of the system, the interaction of the strong AGB wind with the interstellar medium results in a bow shock structure. In this new model we propose that the AGB wind is anisotropic, with properties such as mass-loss rate and density having a latitude dependence, and that the orientation of the polar axis of the AGB star is not aligned with the direction of motion. The ejecta from the Type Ia supernova explosion is modelled using a power-law density profile, and we let the remnant evolve for 400 yr. We computed synthetic X-ray maps from the numerical results. We find that the estimated size and peculiar X-ray morphology of Kepler's supernova remnant are well reproduced by considering an AGB mass-loss rate of 10-5 M⊙ yr-1, a wind terminal velocity of 10 km s-1, an ambient medium density of 10-3 cm-3 and an explosion energy of 7 × 1050 erg. The obtained total X-ray luminosity of the remnant in this model reaches 6 × 1050 erg, which is within a factor of 2 of the observed value, and the time evolution of the luminosity shows a rate of decrease in recent decades of ˜2.4 per cent yr-1 that is consistent with the observations.

  4. Formation and Evolution of Galactic Intermediate/Low-Mass X-ray Binaries

    NASA Astrophysics Data System (ADS)

    Shao, Yong; Li, Xiang-Dong

    2015-08-01

    We investigate the formation and evolutionary sequences of Galactic intermediate- and low-mass X-ray binaries (I/LMXBs) by combining binary population synthesis (BPS) and detailed stellar evolutionary calculations. Using an updated BPS code we compute the evolution of massive binaries that leads to the formation of incipient I/LMXBs and present their distribution in the initial donor mass versus initial orbital period diagram. We then follow the evolution of the I/LMXBs until the formation of binary millisecond pulsars (BMSPs). We find that the birthrate of the I/LMXB population is in the range of 9 × 10-6-3.4 × 10-5 yr-1, compatible with that of BMSPs that are thought to descend from I/LMXBs. We show that during the evolution of I/LMXBs they are likely to be observed as relatively compact binaries with orbital periods ≲1 day and donor masses ≲0.3M⊙. The resultant BMSPs have orbital periods ranging from less than 1 day to a few hundred days. These features are consistent with observations of LMXBs and BMSPs. We also confirm the discrepancies between theoretical predictions and observations mentioned in the literature, that is, the theoretical average mass transfer rates (˜10-10 M⊙ yr-1) of LMXBs are considerably lower than observed, and the number of BMSPs with orbital periods ˜0.1-10 days is severely underestimated. These discrepancies imply that something is missing in the modeling of LMXBs, which is likely to be related to the mechanisms of the orbital angular momentum loss.

  5. Spatial and temporal effects of drought on soil CO2 efflux in a cacao agroforestry system in Sulawesi, Indonesia

    NASA Astrophysics Data System (ADS)

    van Straaten, O.; Veldkamp, E.; Köhler, M.; Anas, I.

    2010-04-01

    Climate change induced droughts pose a serious threat to ecosystems across the tropics and sub-tropics, particularly to those areas not adapted to natural dry periods. In order to study the vulnerability of cacao (Theobroma cacao) - Gliricidia sepium agroforestry plantations to droughts a large scale throughfall displacement roof was built in Central Sulawesi, Indonesia. In this 19-month experiment, we compared soil surface CO2 efflux (soil respiration) from three roof plots with three adjacent control plots. Soil respiration rates peaked at intermediate soil moisture conditions and decreased under increasingly dry conditions (drought induced), or increasingly wet conditions (as evidenced in control plots). The roof plots exhibited a slight decrease in soil respiration compared to the control plots (average 13% decrease). The strength of the drought effect was spatially variable - while some measurement chamber sites reacted strongly (responsive) to the decrease in soil water content (up to R2=0.70) (n=11), others did not react at all (non-responsive) (n=7). A significant correlation was measured between responsive soil respiration chamber sites and sap flux density ratios of cacao (R=0.61) and Gliricidia (R=0.65). Leaf litter CO2 respiration decreased as conditions became drier. The litter layer contributed approximately 3-4% of the total CO2 efflux during dry periods and up to 40% during wet periods. Within days of roof opening soil CO2 efflux rose to control plot levels. Thereafter, CO2 efflux remained comparable between roof and control plots. The cumulative effect on soil CO2 emissions over the duration of the experiment was not significantly different: the control plots respired 11.1±0.5 Mg C ha-1 yr-1, while roof plots respired 10.5±0.5 Mg C ha-1 yr-1. The relatively mild decrease measured in soil CO2 efflux indicates that this agroforestry ecosystem is capable of mitigating droughts with only minor stress symptoms.

  6. A search for ionized jets towards massive young stellar objects

    NASA Astrophysics Data System (ADS)

    Purser, S. J. D.; Lumsden, S. L.; Hoare, M. G.; Urquhart, J. S.; Cunningham, N.; Purcell, C. R.; Brooks, K. J.; Garay, G.; Gúzman, A. E.; Voronkov, M. A.

    2016-07-01

    Radio continuum observations using the Australia telescope compact array at 5.5, 9.0, 17.0 and 22.8 GHz have detected free-free emission associated with 45 of 49 massive young stellar objects and H II regions. Of these, 26 sources are classified as ionized jets (12 of which are candidates), 2 as ambiguous jets or disc winds, 1 as a disc-wind, 14 as H II regions and 2 were unable to be categorized. Classification as ionized jets is based upon morphology, radio flux and spectral index, in conjunction with previous observational results at other wavelengths. Radio luminosity and momentum are found to scale with bolometric luminosity in the same way as low-mass jets, indicating a common mechanism for jet production across all masses. In 13 of the jets, we see associated non-thermal/optically thin lobes resulting from shocks either internal to the jet and/or at working surfaces. 10 jets display non-thermal (synchrotron emission) spectra in their lobes, with an average spectral index of α = -0.55 consistent with Fermi acceleration in shocks. This shows that magnetic fields are present, in agreement with models of jet formation incorporating magnetic fields. Since the production of collimated radio jets is associated with accretion processes, the results presented in this paper support the picture of disc-mediated accretion for the formation of massive stars with an upper limit on the jet phase lasting approximately 6.5 × 104 yr. Typical mass-loss rates in the jet are found to be 1.4 × 10-5 M⊙ yr-1 with associated momentum rates of the order of (1-2) × 10-2 M⊙ km s-1 yr-1.

  7. First Very Large Telescope/X-shooter spectroscopy of early-type stars outside the Local Group

    NASA Astrophysics Data System (ADS)

    Hartoog, O. E.; Sana, H.; de Koter, A.; Kaper, L.

    2012-05-01

    As part of the Very Large Telescope (VLT)/X-shooter science verification, we obtained the first optical medium-resolution spectrum of a previously identified bright O-type object in NGC 55, a Large Magellanic Cloud (LMC)-like galaxy at a distance of ˜2.0 Mpc. Based on the stellar and nebular spectra, we investigate the nature and evolutionary status of the central object(s) and its influence on the surrounding interstellar medium. We conclude that the source, NGC 55 C1_31, is a composite object, likely a stellar cluster, which contains one or several hot (Teff≃ 50 000 K) WN stars with a high mass-loss rate (˜3 × 10-5 M⊙ yr-1) and a helium-rich composition (NHe/NH= 0.8). The visual flux is dominated by OB-type (super)giant stars with Teff≲ 35 000 K, solar helium abundance (NHe/NH= 0.1) and mass-loss rate ˜2 × 10-6 M⊙ yr-1. The surrounding H II region has an electron density of ne≤ 102 cm-3 and an electron temperature of T(O III) ≃ 11 500 ± 600 K. The oxygen abundance of this region is [O/H] = 8.18 ± 0.03, which corresponds to Z= 0.31 ± 0.04 Z⊙. We observed no significant gradients in T(O III), ne or [O/H] on a scale of 73 pc extending in four directions from the ionizing source. The properties of the H II region can be reproduced by a CLOUDY model which uses the central cluster as ionizing source, thus providing a self-consistent interpretation of the data. We also report on the serendipitous discovery of He II nebular emission associated with the nearby source NGC 55 C2_35, a feature usually associated with strong X-ray sources.

  8. A search for ionized jets towards massive young stellar objects

    NASA Astrophysics Data System (ADS)

    Purser, S. J. D.; Lumsden, S. L.; Hoare, M. G.; Urquhart, J. S.; Cunningham, N.; Purcell, C. R.; Brooks, K. J.; Garay, G.; Gúzman, A. E.; Voronkov, M. A.

    2016-05-01

    Radio continuum observations using the Australia telescope compact array at 5.5, 9.0, 17.0 and 22.8 GHz have detected free-free emission associated with 45 of 49 massive young stellar objects and HII regions. Of these, 26 sources are classified as ionized jets (12 of which are candidates), 2 as ambiguous jets or disc winds, 1 as a disc-wind, 14 as HII regions and 2 were unable to be categorised. Classification as ionized jets is based upon morphology, radio flux and spectral index, in conjunction with previous observational results at other wavelengths. Radio-luminosity and momentum are found to scale with bolometric luminosity in the same way as low-mass jets, indicating a common mechanism for jet production across all masses. In 13 of the jets, we see associated non-thermal/optically-thin lobes resulting from shocks either internal to the jet and/or at working surfaces. Ten jets display non-thermal (synchrotron emission) spectra in their lobes, with an average spectral index of α = -0.55 consistent with Fermi acceleration in shocks. This shows that magnetic fields are present, in agreement with models of jet formation incorporating magnetic fields. Since the production of collimated radio jets is associated with accretion processes, the results presented in this paper support the picture of disc-mediated accretion for the formation of massive stars with an upper-limit on the jet phase lasting approximately 6.5 × 104 yr. Typical mass loss rates in the jet are found to be 1.4× 10-5 M⊙yr-1 with associated momentum rates of the order (1-2)× 10^{-2} M_⊙ km s^{-1 yr}^{-1}.

  9. Characterization of Molecular Outflows in the Substellar Domain

    NASA Astrophysics Data System (ADS)

    Phan-Bao, Ngoc; Lee, Chin-Fei; Ho, Paul T. P.; Dang-Duc, Cuong; Li, Di

    2014-11-01

    We report here our latest search for molecular outflows from young brown dwarfs and very low-mass stars in nearby star-forming regions. We have observed three sources in Taurus with the Submillimeter Array and the Combined Array for Research in Millimeter-wave Astronomy at 230 GHz frequency to search for CO J = 2 → 1 outflows. We obtain a tentative detection of a redshifted and extended gas lobe at about 10 arcsec from the source GM Tau, a young brown dwarf in Taurus with an estimated mass of 73 M J , which is right below the hydrogen-burning limit. No blueshifted emission around the brown dwarf position is detected. The redshifted gas lobe that is elongated in the northeast direction suggests a possible bipolar outflow from the source with a position angle of about 36°. Assuming that the redshifted emission is outflow emission from GM Tau, we then estimate a molecular outflow mass in the range from 1.9 × 10-6 M ⊙ to 2.9 × 10-5 M ⊙ and an outflow mass-loss rate from 2.7 × 10-9 M ⊙ yr-1 to 4.1 × 10-8 M ⊙ yr-1. These values are comparable to those we have observed in the young brown dwarf ISO-Oph 102 of 60 M J in ρ Ophiuchi and the very low-mass star MHO 5 of 90 M J in Taurus. Our results suggest that the outflow process in very low-mass objects is episodic with a duration of a few thousand years and the outflow rate of active episodes does not significantly change for different stages of the formation process of very low-mass objects. This may provide us with important implications that clarify the formation process of brown dwarfs.

  10. The impact of mechanical AGN feedback on the formation of massive early-type galaxies

    NASA Astrophysics Data System (ADS)

    Choi, Ena; Ostriker, Jeremiah P.; Naab, Thorsten; Oser, Ludwig; Moster, Benjamin P.

    2015-06-01

    We employ cosmological hydrodynamical simulations to investigate the effects of AGN feedback on the formation of massive galaxies with present-day stellar masses of M_stel= 8.8 × 10^{10}-6.0 × 10^{11} M_{⊙}. Using smoothed particle hydrodynamics simulations with a pressure-entropy formulation that allows an improved treatment of contact discontinuities and fluid mixing, we run three sets of simulations of 20 haloes with different AGN feedback models: (1) no feedback, (2) thermal feedback, and (3) mechanical and radiation feedback. We assume that seed black holes are present at early cosmic epochs at the centre of emerging dark matter haloes and trace their mass growth via gas accretion and mergers with other black holes. Both feedback models successfully recover the observed MBH-σ relation and black hole-to-stellar mass ratio for simulated central early-type galaxies. The baryonic conversion efficiencies are reduced by a factor of 2 compared to models without any AGN feedback at all halo masses. However, massive galaxies simulated with thermal AGN feedback show a factor of ˜10-100 higher X-ray luminosities than observed. The mechanical/radiation feedback model reproduces the observed correlation between X-ray luminosities and velocity dispersion, e.g. for galaxies with σ = 200 km s- 1, the X-ray luminosity is reduced from 1042 erg s- 1 to 1040 erg s- 1. It also efficiently suppresses late-time star formation, reducing the specific star formation rate from 10-10.5 yr- 1 to 10-14 yr- 1 on average and resulting in quiescent galaxies since z = 2, whereas the thermal feedback model shows higher late-time in situ star formation rates than observed.

  11. Modelling the circumstellar medium in RS Ophiuchi and its link to Type Ia supernovae

    NASA Astrophysics Data System (ADS)

    Booth, R. A.; Mohamed, S.; Podsiadlowski, Ph.

    2016-03-01

    Recent interpretations of narrow, variable absorption lines detected in some Type Ia supernovae suggest that their progenitors are surrounded by dense, circumstellar material. Similar variations detected in the symbiotic recurrent nova system RS Oph, which undergoes thermonuclear outbursts every 20 years, making it an ideal candidate to investigate the origin of these lines. To this end, we present simulations of multiple mass transfer-nova cycles in RS Oph. We find that the quiescent mass transfer produces a dense, equatorial outflow, i.e. concentrated towards the binary orbital plane, and an accretion disc forms around the white dwarf. The interaction of a spherical nova outburst with these aspherical circumstellar structures produces a bipolar outflow, similar to that seen in Hubble Space Telescope imaging of the 2006 outburst. In order to produce an ionization structure that is consistent with observations, a mass-loss rate of 5 × 10-7 M⊙ yr-1 from the red giant is required. The simulations also produce a polar accretion flow, which may explain the broad wings of the quiescent H line and hard X-rays. By comparing simulated absorption line profiles to observations of the 2006 outburst, we are able to determine which components arise in the wind and which are due to the novae. We explore the possible behaviour of absorption line profiles as they may appear should a supernova occur in a system like RS Oph. Our models show similarities to supernovae like SN 2006X, but require a high mass-loss rate, dot{M} ˜ 10^{-6}-10-5 M⊙ yr-1, to explain the variability in SN 2006X.

  12. Testing mechanisms of N-enrichment-induced species loss in a semiarid Inner Mongolia grassland: critical thresholds and implications for long-term ecosystem responses.

    PubMed

    Lan, Zhichun; Bai, Yongfei

    2012-11-19

    The increase in nutrient availability as a consequence of elevated nitrogen (N) deposition is an important component of global environmental change. This is likely to substantially affect the functioning and provisioning of ecosystem services by drylands, where water and N are often limited. We tested mechanisms of chronic N-enrichment-induced plant species loss in a 10-year field experiment with six levels of N addition rate. Our findings on a semi-arid grassland in Inner Mongolia demonstrated that: (i) species richness (SR) declined by 16 per cent even at low levels of additional N (1.75 g N m(-2) yr(-1)), and 50-70% species were excluded from plots which received high N input (10.5-28 g N m(-2) yr(-1)); (ii) the responses of SR and above-ground biomass (AGB) to N were greater in wet years than dry years; (iii) N addition increased the inter-annual variations in AGB, reduced the drought resistance of production and hence diminished ecosystem stability; (iv) the critical threshold for chronic N-enrichment-induced reduction in SR differed between common and rare species, and increased over the time of the experiment owing to the loss of the more sensitive species. These results clearly indicate that both abundance and functional trait-based mechanisms operate simultaneously on N-induced species loss. The low initial abundance and low above-ground competitive ability may be attributable to the loss of rare species. However, shift from below-ground competition to above-ground competition and recruitment limitation are likely to be the key mechanisms for the loss of abundant species, with soil acidification being less important. Our results have important implications for understanding the impacts of N deposition and global climatic change (e.g. change in precipitation regimes) on biodiversity and ecosystem services of the Inner Mongolian grassland and beyond. PMID:23045710

  13. Does Newton’s gravitational constant vary sinusoidally with time? Orbital motions say no

    NASA Astrophysics Data System (ADS)

    Iorio, Lorenzo

    2016-02-01

    A sinusoidally time-varying pattern of the values of Newton’s constant of gravitation G measured in Earth-based laboratories over the last few decades has been recently reported in the literature. We put to the test the hypothesis that the aforementioned harmonic variation may pertain to G itself in a direct and independent way. We numerically integrated the ad hoc modified equations of motion of the major bodies of the Solar System, finding that the orbits of the planets would be altered by an unacceptably larger amount in view of the present-day high accuracy astrometric measurements. In the case of Saturn, its geocentric right ascension α, declination δ and range ρ would be affected by up to {10}4-{10}5 milliarcseconds and 105 km, respectively; the present-day residuals of such observables are as little as about 4 milliarcseconds and 10-1 km, respectively. We analytically calculated the long-term orbital effects induced by the putative harmonic variation of G at hand, finding non-zero rates of change for the semimajor axis a, the eccentricity e and the argument of pericenter ω of a test particle. For the LAGEOS satellite, an orbital increase as large as 3.9 m yr-1 is predicted, in contrast with the observed decay of -0.203 ± 0.035 m yr-1. An anomalous perihelion precession as large as 14 arcseconds per century is implied for Saturn, while latest observations constrain it to the 10-4 arcseconds per century level. The rejection level provided by the Mercury’s perihelion rate is of the same order of magnitude.

  14. Iron Emission Lines in the Spectra of Classical T Tauri Stars

    NASA Astrophysics Data System (ADS)

    Beristain, G.; Edwards, S.; Hartigan, P.

    1993-05-01

    The optical and infrared continuum emission excesses in classical T Tauri stars are frequently attributed to accretion disks with characteristic mass accretion rates of 10(-7) Msun yr(-1) . The spectra of classical T Tauri stars are also rich in emission lines, arising from both permitted and forbidden atomic species, which have been attributed to formation in regions as diverse as chromospheres, boundary layers, winds and collimated jets. We have conducted a high resolution spectroscopic survey of 48 T Tauri stars in the Tau-Aur star formation complex covering the wavelength range 3900{\\kern.2em Angstroms} to 7000{\\kern.2em Angstroms} with the aim of determining the origin of the various emission lines and report here on the most prominent metallic species present in the T Tauri spectra, Fe I and Fe II. From our spectra we have both 1) determined the level of optical continuum emission, expressed as the ratio of `veiling' to photospheric flux, and 2) extracted residual Fe emission line profiles, free of contamination from underlying photospheric features. We find that Fe I, II emission is seen only in T Tauri stars which have infrared and optical continuum emission excesses attributed to accretion disks; none of the `weak-line' T Tauri stars, with photospheric IR colors and no optical veiling, have detectable Fe emission. Correlations of Fe emission equivalent widths with both K-L and the ratio of veiling to photospheric flux, r, suggest that the Fe lines arise as a result of accretion related activity. DR Tau's rich emission line spectra permit study of the largest number of unblended Fe I,II profiles, for which we have spectra covering 5 different nights. Multiplet line ratios indicate the Fe lines are optically thick, and line luminosities imply emitting areas covering a few percent of the stellar surface. The lines are typically broad and symmetric, although inverse P Cygni structure in Fe II is seen on one night. For 4 nights, the Fe I and Fe II lines

  15. The Spitzer c2d Survey of Nearby Dense Cores. IX. Discovery of a Very Low Luminosity Object Driving a Molecular Outflow in the Dense Core L673-7

    NASA Astrophysics Data System (ADS)

    Dunham, Michael M.; Evans, Neal J.; Bourke, Tyler L.; Myers, Philip C.; Huard, Tracy L.; Stutz, Amelia M.

    2010-10-01

    We present new infrared, submillimeter, and millimeter observations of the dense core L673-7 and report the discovery of a low-luminosity, embedded Class 0 protostar driving a molecular outflow. L673-7 is seen in absorption against the mid-infrared background in 5.8, 8, and 24 μm Spitzer images, allowing for a derivation of the column density profile and total enclosed mass of L673-7, independent of dust temperature assumptions. Estimates of the core mass from these absorption profiles range from 0.2to4.5 M sun. Millimeter continuum emission indicates a mass of ~2 M sun, both from a direct calculation assuming isothermal dust and from dust radiative transfer models constrained by the millimeter observations. We use dust radiative transfer models to constrain the internal luminosity of L673-7, defined to be the luminosity of the central source and excluding the luminosity from external heating, to be L int = 0.01-0.045 L sun, with L int ~ 0.04 L sun the most likely value. L673-7 is thus classified as a very low luminosity object (VeLLO), and is among the lowest luminosity VeLLOs yet studied. We calculate the kinematic and dynamic properties of the molecular outflow in the standard manner. From the outflow properties and standard assumptions regarding the driving of outflows, we calculate the time-averaged protostellar mass accretion rate, total protostellar mass accreted, and expected accretion luminosity to be < \\dot{M}_acc > ≥ 1.2 × 10^{-6} sin i {cos}^2 i Msun yr-1, M_acc ≥ 0.07 {1}/{cos } M sun, and Lacc >= 0.36 L sun, respectively. The discrepancy between this calculated L acc and the L int derived from dust radiative transfer models indicates that the current accretion rate is much lower than the average rate over the lifetime of the outflow. Although the protostar embedded within L673-7 is consistent with currently being substellar, it is unlikely to remain as such given the substantial mass reservoir remaining in the core.

  16. Discovery of a z ˜ 6 Galaxy in the Chandra Deep Field South

    NASA Astrophysics Data System (ADS)

    Bunker, A. J.; Stanway, E. R.; Ellis, R. S.; McMahon, R. G.; McCarthy, P. J.

    2003-05-01

    We report the discovery of a luminous z=5.78 star-forming galaxy in the Chandra Deep Field South. This galaxy was selected as an ``i-drop'' from the GOODS public survey imaging with HST/ACS (object 3 in Stanway, Bunker & McMahon 2003, astro-ph/0302212). The large colour of (i'-z')AB=1.6 indicated a spectral break consistent with the Lyman-α forest absorption short-ward of Lyman-α at z≈ 6. The galaxy is very compact (marginally resolved with ACS with a half-light radius of 0.08 arcsec, so rhl<0.5 h-170 kpc). We have obtained a deep (5.5-hour) spectrum of this z'AB=24.7 galaxy with the DEIMOS optical spectrograph on Keck, and here we report the discovery of a single emission line centered on (8245+/- 1) Å detected at 20 σ with a flux of f≈ 2x 10-17 ergs cm-2 s-1. The line is clearly resolved with detectable structure at our resolution of better than 55 km s-1, and the only plausible interpretation consistent with the ACS photometry is that we are seeing Lyman-α emission from a z=5.78 galaxy. This is the highest redshift galaxy to be discovered and studied using HST data. The velocity width (Δ vFWHM=260 km s-1) and rest-frame equivalent width (Wrest Lyα =20 Å ) indicate that this line is most probably powered by star formation, as an AGN would typically have larger values. The starburst interpretation is supported by our non-detection of the high-ionization Nriptsize V λ 1240 Å emission line, and the absence of this source from the deep Chandra X-ray images. The star formation rate inferred from the rest-frame UV continuum is 33.8 h70-2 Msun yr-1 (Ω M=0.3, Ω Λ =0.7). This is the most luminous starburst known at z>5. Our spectroscopic redshift for this object confirms the validity of the i'-drop selection technique of Stanway, Bunker & McMahon (2003) to select star-forming galaxies at z≈ 6.

  17. On the use of the correction factor with Japanese ozonesonde data

    NASA Astrophysics Data System (ADS)

    Morris, G. A.; Labow, G.; Akimoto, H.; Takigawa, M.; Fujiwara, M.; Hasebe, F.; Hirokawa, J.; Koide, T.

    2013-02-01

    In submitting data to the World Meteorological Organization (WMO) World Ozone and Ultraviolet Data Center (WOUDC), numerous ozonesonde stations include a correction factor (CF) that multiplies ozone concentration profile data so that the columns computed agree with column measurements from co-located ground-based and/or overpassing satellite instruments. We evaluate this practice through an examination of data from four Japanese ozonesonde stations: Kagoshima, Naha, Sapporo, and Tsukuba. While agreement between the sonde columns and Total Ozone Mapping Spectrometer (TOMS) or Ozone Mapping Instrument (OMI) is improved by use of the CF, agreement between the sonde ozone concentrations reported near the surface and data from surface monitors near the launch sites is negatively impacted. In addition, we find the agreement between the mean sonde columns without the CF and the ground-based Dobson instrument columns is improved by ~1.5 % by using the McPeters et al. (1997) balloon burst climatology rather than the constant mixing ratio assumption (that has been used for the data in the WOUDC archive) for the above burst height column estimate. Limited comparisons of coincident ozonesonde profiles from Hokkaido University with those in the WOUDC database suggest that while the application of the CFs in the stratosphere improves agreement, it negatively impacts the agreement in the troposphere. Finally and importantly, unexplained trends and changing trends in the CFs appear over the last 20 years. The overall trend in the reported CFs for the four Japanese ozonesonde stations from 1990-2010 is (-0.264 ± 0.036) × 10-2 yr-1; but from 1993-1999 the trend is (-2.18 ± 0.14) × 10-2 yr-1 and from 1999-2009 is (1.089 ± 0.075) × 10-2 yr-1, resulting in a statistically significant difference in CF trends between these two periods of (3.26 ± 0.16) × 10-2 yr-1. Repeating the analysis using CFs derived from columns computed using the balloon-burst climatology, the trends are

  18. Wet and dry deposition of mineral dust particles in Japan: factors related to temporal variation and spatial distribution

    NASA Astrophysics Data System (ADS)

    Osada, K.; Ura, S.; Kagawa, M.; Mikami, M.; Tanaka, T. Y.; Matoba, S.; Aoki, K.; Shinoda, M.; Kurosaki, Y.; Hayashi, M.; Shimizu, A.; Uematsu, M.

    2014-01-01

    Recent ground networks and satellite remote-sensing observations have provided useful data related to spatial and vertical distributions of mineral dust particles in the atmosphere. However, measurements of temporal variations and spatial distributions of mineral dust deposition fluxes are limited in terms of their duration, location, and processes of deposition. To ascertain temporal variations and spatial distributions of mineral dust deposition using wet and dry processes, weekly deposition samples were obtained at Sapporo, Toyama, Nagoya, Tottori, Fukuoka, and Cape Hedo (Okinawa) in Japan during October 2008-December 2010 using automatic wet and dry separating samplers. Mineral dust weights in water-insoluble residue were estimated from Fe contents measured using an X-ray fluorescence analyser. Wet and dry deposition fluxes of mineral dusts were both high in spring and low in summer, showing similar seasonal variations to frequency of aeolian dust events (Kosa) in Japan. For wet deposition, highest and lowest annual dust fluxes were found at Toyama (9.6 g m-2 yr-1) and at Cape Hedo (1.7 g m-2 yr-1) as average values in 2009 and 2010. Higher wet deposition fluxes were observed at Toyama and Tottori, where frequent precipitation (> 60% days per month) was observed during dusty seasons. For dry deposition among Toyama, Tottori, Fukuoka, and Cape Hedo, the highest and lowest annual dust fluxes were found respectively at Fukuoka (5.2 g m-2 yr-1) and at Cape Hedo (2.0 g m-2 yr-1) as average values in 2009 and 2010. The average ratio of wet and dry deposition fluxes was the highest at Toyama (3.3) and the lowest at Hedo (0.82), showing a larger contribution of the dry process at western sites, probably because of the distance from desert source regions and because of the effectiveness of the wet process in the dusty season. Size distributions of refractory dust particles were obtained using four-stage filtration: > 20, > 10, > 5, and > 1 μm diameter. Weight fractions

  19. Constraints on single-degenerate Chandrasekhar mass progenitors of Type Iax supernovae

    NASA Astrophysics Data System (ADS)

    Liu, Zheng-Wei; Moriya, Takashi J.; Stancliffe, Richard J.; Wang, Bo

    2015-02-01

    Context. Type Iax supernovae (SNe Iax) are proposed as one new sub-class of SNe Ia since they present sufficiently distinct observational properties from the bulk of SNe Ia. Observationally, SNe Iax have been estimated to account for ~5%-30% of the total SN Ia rate, and most SNe Iax have been discovered in late-type galaxies. In addition, observations constrain the progenitor systems of some SN Iax progenitors that have ages of <80 Myr. Although the identity of the progenitors of SNe Iax is unclear, the weak deflagration explosions of Chandrasekhar-mass (Ch-mass) carbon/oxygen white dwarfs (C/O WDs) seem to provide a viable physical scenario. Aims: Comparing theoretical predictions from binary population synthesis (BPS) calculations with observations of SNe Iax, we put constraints on the single-degenerate (SD) Ch-mass model as a possible SN Iax progenitor. Methods: Based on the SD Ch-mass model, the SN rates and delay times are predicted by combining binary evolution calculations for the progenitor systems into a BPS model. Moreover, with current X-ray observations of SNe Iax, we constrain the pre-explosion mass-loss rates of stellar progenitor systems by using two analytic models. Results: From our calculations, the long delay times of ≳3 Gyr and low SN rates of ~3 × 10-5 yr-1 are found in the red-gaint donor channel, indicating that this channel is unlikely to produce SNe Iax. With our standard models, we predict that the Galactic SN Iax rate from the main-sequence (helium-star) donor scenario is ~1.5 × 10-3 yr-1 (~3 × 10-4 yr-1). The total rate of these two models is consistent with the observed SN Iax rate. The short delay times in the helium-star donor channel (<100 Myr) support the young host environments of SNe Iax. However, the relatively long delay times in the main-sequence donor channel (~250 Myr-1 Gyr) are less favourable for the observational constraints on the ages of SN Iax progenitors. Finally, with current X-ray observations for SNe Iax, we

  20. Effects of land use change on soil carbon cycling in the conterminous United States from 1900 to 2050

    NASA Astrophysics Data System (ADS)

    Woodbury, Peter B.; Heath, Linda S.; Smith, James E.

    2007-09-01

    We developed matrices representing historical area transitions between forest and other land uses. We projected future transitions on the basis of historical transitions and econometric model results. These matrices were used to drive a model of changes in soil and forest floor carbon stocks. Our model predicted net carbon emission from 1900 until 1982, then sequestration until 2030, with little subsequent change. However, the northeast region showed substantial carbon sequestration from 1900 to the present. From 1990 to 2004, afforestation caused sequestration averaging 17 Tg C yr-1: 6 Tg C yr-1 in soil and 11 Tg C yr-1 in forest floor. Deforestation caused emission averaging 12 Tg C yr-1: 3 Tg C yr-1 from soil and 9 Tg C yr-1 from forest floor. However, these effects were only 5% of the total change in carbon stocks in all forestland.

  1. WSRT HI imaging of candidate gas-bearing dark matter halos in the Local Group

    NASA Astrophysics Data System (ADS)

    Adams, Elizabeth A.; Oosterloo, Tom; Cannon, John M.; Giovanelli, Riccardo; Haynes, Martha P.

    2016-01-01

    A long standing problem in cosmology is the mismatch between the number of low mass dark matter halos predicted by simulations and the number of low mass galaxies observed in the Local Group. We recently presented a set of isolated ultra-compact high velocity clouds (UCHVCs) identified within the dataset of the Arecibo Legacy Fast ALFA (ALFALFA) HI line survey that are consistent with representing low mass gas-bearing dark matter halos within the Local Group (Adams+ 2013). At distances of ~1 Mpc, the UCHVCs have HI masses of ~10^5 Msun and indicative dynamical masses of ~10^7 Msun. The HI diameters of the UCHVCs range from 4' to 20', or 1 to 6 kpc at a distance of 1 Mpc. We have selected the most compact and isolated UCHVCs with the highest average column densities as representing the best galaxy candidates. These systems have been observed with the Westerbork Synthesis Radio Telescope (WSRT) to enable higher spatial resolution studies of the HI distribution. From these data, the sources break into two clear categories. Two of the sources maintain a smooth HI morphology at higher resolution, show a velocity gradient and have the highest peak column densities of the sample, indicating they are good candidates to represent gas in dark matter halos. In fact, one of these sources, AGC 198606, has a tentative stellar counterpart detection (Janesh+ 2015). Nine of the sources break into clumps at higher angular resolution, show no ordered velocity motion, and have significantly lower peak column densities, indicating they are likely Galactic halo HI clouds. One source straddles the two categories with a relatively smooth HI morphology and some evidence for ordered velocity motion while having a lower peak column density. These observations show that higher resolution HI data is a good way to address the galaxy hypothesis for isolated HI clouds, and future HI surveys with phased-array feeds on interferometers, such as Apertif, will be able to directly detect and

  2. New Techniques: Muon Glaciology and Ultrasonic Logging

    NASA Astrophysics Data System (ADS)

    Chirkin, D.; Allen, J.; Bay, R. C.; Bramall, N.; Price, P. B.

    2003-12-01

    The strain rate of cold glacial ice depends mainly on the stress tensor, temperature, grain size, and crystal habit. Lab measurements cannot be made at both the low stresses and low temperatures relevant to flow of cold glacial ice. Field studies with inclinometers measure only the horizontal components of flow. We have developed a new method for measuring the 3D strain-rate field at -40o to -15oC, using the AMANDA neutrino-detecting array frozen into deep ice at South Pole. Each strain detector consists of a photomultiplier tube (PMT) in its pressure vessel. AMANDA has ˜600 PMTs at depths 1500 to 2300 m in a ˜0.02 km3 volume. The coordinates of each PMT relative to a coordinate system moving down slope at 9 m yr-1 can be measured with s.d. <1 m in 1 day by mapping trajectories of down-going cosmic-ray muons that pass through the array. The PMTs record the arrival times of the Cherenkov light emitted along the muon trajectory. Use of maximum likelihood for 105 muon tracks allows PMT positions to be determined; their positions are then updated at six-month intervals. We will report results of strain-rate measurements in three dimensions, made in 2000, 2001, and 2002 at T ≈ -30oC. Applying the same technique to the future 1 km3 IceCube array, by averaging over subsets of the 5000 detectors, values of the strain-rate tensor as small as 3x 10-5 yr-1 can be measured as a function of temperature and lateral position. The vertical strain rate due to snow accumulation, estimated to be ˜ 3x 10-5 yr-1, can be measured and will serve as a check on the method. The second new method is designed to measure mean grain size in the ice surrounding a borehole. We will adapt an all-digital logging tool originally developed by Advanced Logic Technology (Luxembourg) for geophysics prospecting in rock boreholes. A 1.3 MHz transducer emits acoustic pulses horizontally into the ice in increments of 5o in azimuth and records the wave train back-scattered from grain boundaries. For

  3. Quantification of Carbon Fluxes in Tropical Deciduous Forests Using Satellite Data

    NASA Astrophysics Data System (ADS)

    Prasad, V. Krishna; Rajagopal, T.; Kant, Yogesh; Badarinath, K. V. S.

    Biomass burning in tropics is causing drastic changes in physical, chemical and biological properties of earth's atmosphere. Biomass burning associated with slash and burn agriculture is one of the major cause of Green House Gas emissions. In the present study, study area covering tropical deciduous forests having slash and burn agriculture practice, has been considered for studying carbon dynamics. Satellite data pertaining to IRS-1C LISS III satellite data has been used for stratification of vegetation into different communities. Second order texture measures Semivariograms, Angular Second Moment (ASM) and Inverse Difference Moment (IDM) and NDVI textural algorithm have been used to capture spatial information from forest stands. Biomass estimations have been done through regression equations by using girth measurements obtained through field studies. Satellite data has been used to quantify the amount of biomass burnt in respective vegetation types. Results of the study through textural measures suggest high heterogeneity in canopy diversity for mixed dry deciduous forests. ASM and IDM are found to be high for pure stands of dry deciduous forests. NDVI textural algorithm detected a low spatial variability with respect to mixed dry deciduous forests suggesting homogeneity in plant biomass spatial variability. The average mean carbon storage has been found to be 64.34 t ha-1 C for dry deciduous forests, 129.0 t ha-1 C for mixed dry deciduous forests and 0.02 t ha-1 C for mixed scrub forests. Potential Net primary productivity for the forests ranged from 26.07 to 11.73 t ha-1 yr-1, when compared to actual productivity of 0.1 t ha-1 yr-1 to 4.6 t ha-1 yr-1. Mean carbon storage for plantations, above ground, below ground and total carbon has been found to be 16.84, 3.36 and 20.2 t ha-1 C respectively. Dry matter burnt in gms (M) obtained from satellite derived areal estimates has been found to be 1.344 × 1012 gms. Area weighted carbon release for the total study

  4. Hydrogen consumption by methanogens on the early Earth

    NASA Technical Reports Server (NTRS)

    Kral, T. A.; Brink, K. M.; Miller, S. L.; McKay, C. P.; Bada, J. L. (Principal Investigator)

    1998-01-01

    It is possible that the first autotroph used chemical energy rather than light. This could have been the main source of primary production after the initial inventory of abiotic organic material had been depleted. The electron acceptor most readily available for use by this first chemoautotroph would have been CO2. The most abundant electron donor may have been H2 that would have been outgassing from volcanoes at a rate estimated to be as large as 10(12) moles yr-1, as well as from photo-oxidation of Fe+2. We report here that certain methanogens will consume H2 down to partial pressures as low as 4 Pa (4 x 10(-5) atm) with CO2 as the sole carbon source at a rate of 0.7 ng H2 min-1 microgram-1 cell protein. The lower limit of pH2 for growth of methanogens can be understood on the basis that the pH2 needs to be high enough for one ATP to be synthesized per CO2 reduced. The pH2 values needed for growth measured here are consistent with those measured by Stevens and McKinley for growth of methanogens in deep basalt aquifers. H2-consuming autotrophs are likely to have had a profound effect on the chemistry of the early atmosphere and to have been a dominant sink for H2 on the early Earth after life began rather than escape from the Earth's atmosphere to space.

  5. Search for gravitational waves from low mass compact binary coalescence in LIGO's sixth science run and Virgo's science runs 2 and 3

    NASA Astrophysics Data System (ADS)

    Abadie, J.; Abbott, B. P.; Abbott, R.; Abbott, T. D.; Abernathy, M.; Accadia, T.; Acernese, F.; Adams, C.; Adhikari, R.; Affeldt, C.; Agathos, M.; Ajith, P.; Allen, B.; Allen, G. S.; Amador Ceron, E.; Amariutei, D.; Amin, R. S.; Anderson, S. B.; Anderson, W. G.; Arai, K.; Arain, M. A.; Araya, M. C.; Aston, S. M.; Astone, P.; Atkinson, D.; Aufmuth, P.; Aulbert, C.; Aylott, B. E.; Babak, S.; Baker, P.; Ballardin, G.; Ballmer, S.; Barker, D.; Barone, F.; Barr, B.; Barriga, P.; Barsotti, L.; Barsuglia, M.; Barton, M. A.; Bartos, I.; Bassiri, R.; Bastarrika, M.; Basti, A.; Batch, J.; Bauchrowitz, J.; Bauer, Th. S.; Bebronne, M.; Behnke, B.; Beker, M. G.; Bell, A. S.; Belletoile, A.; Belopolski, I.; Benacquista, M.; Berliner, J. M.; Bertolini, A.; Betzwieser, J.; Beveridge, N.; Beyersdorf, P. T.; Bilenko, I. A.; Billingsley, G.; Birch, J.; Biswas, R.; Bitossi, M.; Bizouard, M. A.; Black, E.; Blackburn, J. K.; Blackburn, L.; Blair, D.; Bland, B.; Blom, M.; Bock, O.; Bodiya, T. P.; Bogan, C.; Bondarescu, R.; Bondu, F.; Bonelli, L.; Bonnand, R.; Bork, R.; Born, M.; Boschi, V.; Bose, S.; Bosi, L.; Bouhou, B.; Braccini, S.; Bradaschia, C.; Brady, P. R.; Braginsky, V. B.; Branchesi, M.; Brau, J. E.; Breyer, J.; Briant, T.; Bridges, D. O.; Brillet, A.; Brinkmann, M.; Brisson, V.; Britzger, M.; Brooks, A. F.; Brown, D. A.; Brummit, A.; Bulik, T.; Bulten, H. J.; Buonanno, A.; Burguet–Castell, J.; Burmeister, O.; Buskulic, D.; Buy, C.; Byer, R. L.; Cadonati, L.; Cagnoli, G.; Calloni, E.; Camp, J. B.; Campsie, P.; Cannizzo, J.; Cannon, K.; Canuel, B.; Cao, J.; Capano, C. D.; Carbognani, F.; Caride, S.; Caudill, S.; Cavaglià, M.; Cavalier, F.; Cavalieri, R.; Cella, G.; Cepeda, C.; Cesarini, E.; Chaibi, O.; Chalermsongsak, T.; Chalkley, E.; Charlton, P.; Chassande-Mottin, E.; Chelkowski, S.; Chen, Y.; Chincarini, A.; Chiummo, A.; Cho, H.; Christensen, N.; Chua, S. S. Y.; Chung, C. T. Y.; Chung, S.; Ciani, G.; Clara, F.; Clark, D. E.; Clark, J.; Clayton, J. H.; Cleva, F.; Coccia, E.; Cohadon, P.-F.; Colacino, C. N.; Colas, J.; Colla, A.; Colombini, M.; Conte, A.; Conte, R.; Cook, D.; Corbitt, T. R.; Cordier, M.; Cornish, N.; Corsi, A.; Costa, C. A.; Coughlin, M.; Coulon, J.-P.; Couvares, P.; Coward, D. M.; Coyne, D. C.; Creighton, J. D. E.; Creighton, T. D.; Cruise, A. M.; Cumming, A.; Cunningham, L.; Cuoco, E.; Cutler, R. M.; Dahl, K.; Danilishin, S. L.; Dannenberg, R.; D'Antonio, S.; Danzmann, K.; Dattilo, V.; Daudert, B.; Daveloza, H.; Davier, M.; Davies, G.; Daw, E. J.; Day, R.; Dayanga, T.; De Rosa, R.; DeBra, D.; Debreczeni, G.; Degallaix, J.; Del Pozzo, W.; del Prete, M.; Dent, T.; Dergachev, V.; DeRosa, R.; DeSalvo, R.; Dhurandhar, S.; Di Fiore, L.; Di Lieto, A.; Di Palma, I.; Di Paolo Emilio, M.; Di Virgilio, A.; Díaz, M.; Dietz, A.; DiGuglielmo, J.; Donovan, F.; Dooley, K. L.; Dorsher, S.; Drago, M.; Drever, R. W. P.; Driggers, J. C.; Du, Z.; Dumas, J.-C.; Dwyer, S.; Eberle, T.; Edgar, M.; Edwards, M.; Effler, A.; Ehrens, P.; Endrőczi, G.; Engel, R.; Etzel, T.; Evans, K.; Evans, M.; Evans, T.; Factourovich, M.; Fafone, V.; Fairhurst, S.; Fan, Y.; Farr, B. F.; Farr, W.; Fazi, D.; Fehrmann, H.; Feldbaum, D.; Ferrante, I.; Fidecaro, F.; Finn, L. S.; Fiori, I.; Fisher, R. P.; Flaminio, R.; Flanigan, M.; Foley, S.; Forsi, E.; Forte, L. A.; Fotopoulos, N.; Fournier, J.-D.; Franc, J.; Frasca, S.; Frasconi, F.; Frede, M.; Frei, M.; Frei, Z.; Freise, A.; Frey, R.; Fricke, T. T.; Friedrich, D.; Fritschel, P.; Frolov, V. V.; Fulda, P. J.; Fyffe, M.; Galimberti, M.; Gammaitoni, L.; Ganija, M. R.; Garcia, J.; Garofoli, J. A.; Garufi, F.; Gáspár, M. E.; Gemme, G.; Geng, R.; Genin, E.; Gennai, A.; Gergely, L. Á.; Ghosh, S.; Giaime, J. A.; Giampanis, S.; Giardina, K. D.; Giazotto, A.; Gill, C.; Goetz, E.; Goggin, L. M.; González, G.; Gorodetsky, M. L.; Goßler, S.; Gouaty, R.; Graef, C.; Granata, M.; Grant, A.; Gras, S.; Gray, C.; Gray, N.; Greenhalgh, R. J. S.; Gretarsson, A. M.; Greverie, C.; Grosso, R.; Grote, H.; Grunewald, S.; Guidi, G. M.; Guido, C.; Gupta, R.; Gustafson, E. K.; Gustafson, R.; Ha, T.; Hage, B.; Hallam, J. M.; Hammer, D.; Hammond, G.; Hanks, J.; Hanna, C.; Hanson, J.; Hardt, A.; Harms, J.; Harry, G. M.; Harry, I. W.; Harstad, E. D.; Hartman, M. T.; Haughian, K.; Hayama, K.; Hayau, J.-F.; Heefner, J.; Heidmann, A.; Heintze, M. C.; Heitmann, H.; Hello, P.; Hendry, M. A.; Heng, I. S.; Heptonstall, A. W.; Herrera, V.; Hewitson, M.; Hild, S.; Hoak, D.; Hodge, K. A.; Holt, K.; Hong, T.; Hooper, S.; Hosken, D. J.; Hough, J.; Howell, E. J.; Hughey, B.; Husa, S.; Huttner, S. H.; Huynh-Dinh, T.; Ingram, D. R.; Inta, R.; Isogai, T.; Ivanov, A.; Izumi, K.; Jacobson, M.; Jang, H.; Jaranowski, P.; Johnson, W. W.; Jones, D. I.; Jones, G.; Jones, R.; Ju, L.; Kalmus, P.; Kalogera, V.; Kamaretsos, I.; Kandhasamy, S.; Kang, G.; Kanner, J. B.; Katsavounidis, E.; Katzman, W.; Kaufer, H.; Kawabe, K.; Kawamura, S.; Kawazoe, F.; Kells, W.; Keppel, D. G.; Keresztes, Z.; Khalaidovski, A.; Khalili, F. Y.; Khazanov, E. A.; Kim, B.; Kim, C.; Kim, D.; Kim, H.; Kim, K.; Kim, N.; Kim, Y.-M.; King, P. J.; Kinsey, M.; Kinzel, D. L.; Kissel, J. S.; Klimenko, S.; Kokeyama, K.; Kondrashov, V.; Kopparapu, R.; Koranda, S.; Korth, W. Z.; Kowalska, I.; Kozak, D.; Kringel, V.; Krishnamurthy, S.; Krishnan, B.; Królak, A.; Kuehn, G.; Kumar, R.; Kwee, P.; Lam, P. K.; Landry, M.; Lang, M.; Lantz, B.; Lastzka, N.; Lawrie, C.; Lazzarini, A.; Leaci, P.; Lee, C. H.; Lee, H. M.; Leindecker, N.; Leong, J. R.; Leonor, I.; Leroy, N.; Letendre, N.; Li, J.; Li, T. G. F.; Liguori, N.; Lindquist, P. E.; Lockerbie, N. A.; Lodhia, D.; Lorenzini, M.; Loriette, V.; Lormand, M.; Losurdo, G.; Luan, J.; Lubinski, M.; Lück, H.; Lundgren, A. P.; Macdonald, E.; Machenschalk, B.; MacInnis, M.; Macleod, D. M.; Mageswaran, M.; Mailand, K.; Majorana, E.; Maksimovic, I.; Man, N.; Mandel, I.; Mandic, V.; Mantovani, M.; Marandi, A.; Marchesoni, F.; Marion, F.; Márka, S.; Márka, Z.; Markosyan, A.; Maros, E.; Marque, J.; Martelli, F.; Martin, I. W.; Martin, R. M.; Marx, J. N.; Mason, K.; Masserot, A.; Matichard, F.; Matone, L.; Matzner, R. A.; Mavalvala, N.; Mazzolo, G.; McCarthy, R.; McClelland, D. E.; McGuire, S. C.; McIntyre, G.; McIver, J.; McKechan, D. J. A.; Meadors, G. D.; Mehmet, M.; Meier, T.; Melatos, A.; Melissinos, A. C.; Mendell, G.; Menendez, D.; Mercer, R. A.; Meshkov, S.; Messenger, C.; Meyer, M. S.; Miao, H.; Michel, C.; Milano, L.; Miller, J.; Minenkov, Y.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman, R.; Miyakawa, O.; Moe, B.; Moesta, P.; Mohan, M.; Mohanty, S. D.; Mohapatra, S. R. P.; Moraru, D.; Moreno, G.; Morgado, N.; Morgia, A.; Mori, T.; Mosca, S.; Mossavi, K.; Mours, B.; Mow-Lowry, C. M.; Mueller, C. L.; Mueller, G.; Mukherjee, S.; Mullavey, A.; Müller-Ebhardt, H.; Munch, J.; Murphy, D.; Murray, P. G.; Mytidis, A.; Nash, T.; Naticchioni, L.; Nawrodt, R.; Necula, V.; Nelson, J.; Newton, G.; Nishizawa, A.; Nocera, F.; Nolting, D.; Nuttall, L.; Ochsner, E.; O'Dell, J.; Oelker, E.; Ogin, G. H.; Oh, J. J.; Oh, S. H.; Oldenburg, R. G.; O'Reilly, B.; O'Shaughnessy, R.; Osthelder, C.; Ott, C. D.; Ottaway, D. J.; Ottens, R. S.; Overmier, H.; Owen, B. J.; Page, A.; Pagliaroli, G.; Palladino, L.; Palomba, C.; Pan, Y.; Pankow, C.; Paoletti, F.; Papa, M. A.; Parisi, M.; Pasqualetti, A.; Passaquieti, R.; Passuello, D.; Patel, P.; Pedraza, M.; Peiris, P.; Pekowsky, L.; Penn, S.; Peralta, C.; Perreca, A.; Persichetti, G.; Phelps, M.; Pickenpack, M.; Piergiovanni, F.; Pietka, M.; Pinard, L.; Pinto, I. M.; Pitkin, M.; Pletsch, H. J.; Plissi, M. V.; Poggiani, R.; Pöld, J.; Postiglione, F.; Prato, M.; Predoi, V.; Price, L. R.; Prijatelj, M.; Principe, M.; Privitera, S.; Prix, R.; Prodi, G. A.; Prokhorov, L.; Puncken, O.; Punturo, M.; Puppo, P.; Quetschke, V.; Raab, F. J.; Rabeling, D. S.; Rácz, I.; Radkins, H.; Raffai, P.; Rakhmanov, M.; Ramet, C. R.; Rankins, B.; Rapagnani, P.; Raymond, V.; Re, V.; Redwine, K.; Reed, C. M.; Reed, T.; Regimbau, T.; Reid, S.; Reitze, D. H.; Ricci, F.; Riesen, R.; Riles, K.; Robertson, N. A.; Robinet, F.; Robinson, C.; Robinson, E. L.; Rocchi, A.; Roddy, S.; Rodriguez, C.; Rodruck, M.; Rolland, L.; Rollins, J.; Romano, J. D.; Romano, R.; Romie, J. H.; Rosińska, D.; Röver, C.; Rowan, S.; Rüdiger, A.; Ruggi, P.; Ryan, K.; Ryll, H.; Sainathan, P.; Sakosky, M.; Salemi, F.; Samblowski, A.; Sammut, L.; Sancho de la Jordana, L.; Sandberg, V.; Sankar, S.; Sannibale, V.; Santamaría, L.; Santiago-Prieto, I.; Santostasi, G.; Sassolas, B.; Sathyaprakash, B. S.; Sato, S.; Saulson, P. R.; Savage, R. L.; Schilling, R.; Schlamminger, S.; Schnabel, R.; Schofield, R. M. S.; Schulz, B.; Schutz, B. F.; Schwinberg, P.; Scott, J.; Scott, S. M.; Searle, A. C.; Seifert, F.; Sellers, D.; Sengupta, A. S.; Sentenac, D.; Sergeev, A.; Shaddock, D. A.; Shaltev, M.; Shapiro, B.; Shawhan, P.; Shoemaker, D. H.; Sibley, A.; Siemens, X.; Sigg, D.; Singer, A.; Singer, L.; Sintes, A. M.; Skelton, G.; Slagmolen, B. J. J.; Slutsky, J.; Smith, J. R.; Smith, M. R.; Smith, N. D.; Smith, R. J. E.; Somiya, K.; Sorazu, B.; Soto, J.; Speirits, F. C.; Sperandio, L.; Stefszky, M.; Stein, A. J.; Steinert, E.; Steinlechner, J.; Steinlechner, S.; Steplewski, S.; Stochino, A.; Stone, R.; Strain, K. A.; Strigin, S.; Stroeer, A. S.; Sturani, R.; Stuver, A. L.; Summerscales, T. Z.; Sung, M.; Susmithan, S.; Sutton, P. J.; Swinkels, B.; Tacca, M.; Taffarello, L.; Talukder, D.; Tanner, D. B.; Tarabrin, S. P.; Taylor, J. R.; Taylor, R.; Thomas, P.; Thorne, K. A.; Thorne, K. S.; Thrane, E.; Thüring, A.; Titsler, C.; Tokmakov, K. V.; Toncelli, A.; Tonelli, M.; Torre, O.; Torres, C.; Torrie, C. I.; Tournefier, E.; Travasso, F.; Traylor, G.; Trias, M.; Tseng, K.; Tucker, E.; Ugolini, D.; Urbanek, K.; Vahlbruch, H.; Vajente, G.; Vallisneri, M.; van den Brand, J. F. J.; Van Den Broeck, C.; van der Putten, S.; van Veggel, A. A.; Vass, S.; Vasuth, M.; Vaulin, R.; Vavoulidis, M.; Vecchio, A.; Vedovato, G.; Veitch, J.; Veitch, P. J.; Veltkamp, C.; Verkindt, D.; Vetrano, F.; Viceré, A.; Villar, A. E.; Vinet, J.-Y.; Vitale, S.; Vitale, S.; Vocca, H.; Vorvick, C.; Vyatchanin, S. P.; Wade, A.; Waldman, S. J.; Wallace, L.; Wan, Y.; Wang, X.; Wang, Z.; Wanner, A.; Ward, R. L.; Was, M.; Wei, P.; Weinert, M.; Weinstein, A. J.; Weiss, R.; Wen, L.; Wen, S.; Wessels, P.; West, M.; Westphal, T.; Wette, K.; Whelan, J. T.; Whitcomb, S. E.; White, D.; Whiting, B. F.; Wilkinson, C.; Willems, P. A.; Williams, H. R.; Williams, L.; Willke, B.; Winkelmann, L.; Winkler, W.; Wipf, C. C.; Wiseman, A. G.; Wittel, H.; Woan, G.; Wooley, R.; Worden, J.; Yablon, J.; Yakushin, I.; Yamamoto, H.; Yamamoto, K.; Yang, H.; Yeaton-Massey, D.; Yoshida, S.; Yu, P.; Yvert, M.; Zadroźny, A.; Zanolin, M.; Zendri, J.-P.; Zhang, F.; Zhang, L.; Zhang, W.; Zhang, Z.; Zhao, C.; Zotov, N.; Zucker, M. E.; Zweizig, J.

    2012-04-01

    We report on a search for gravitational waves from coalescing compact binaries using LIGO and Virgo observations between July 7, 2009, and October 20, 2010. We searched for signals from binaries with total mass between 2 and 25M⊙; this includes binary neutron stars, binary black holes, and binaries consisting of a black hole and neutron star. The detectors were sensitive to systems up to 40 Mpc distant for binary neutron stars, and further for higher mass systems. No gravitational-wave signals were detected. We report upper limits on the rate of compact binary coalescence as a function of total mass, including the results from previous LIGO and Virgo observations. The cumulative 90% confidence rate upper limits of the binary coalescence of binary neutron star, neutron star-black hole, and binary black hole systems are 1.3×10-4, 3.1×10-5, and 6.4×10-6Mpc-3yr-1, respectively. These upper limits are up to a factor 1.4 lower than previously derived limits. We also report on results from a blind injection challenge.

  6. The contribution of chemical abundances in nova ejecta to the interstellar medium

    NASA Astrophysics Data System (ADS)

    Li, Fanger; Zhu, Chunhua; Lü, Guoliang; Wang, Zhaojun

    2016-06-01

    According to the nova model from Yaron et al. (2005, ApJ, 418, 794) and José and Hernanz (1998, ApJ, 494, 680), and using a Monte Carlo simulation method, we investigate the contribution of chemical abundances in nova ejecta to the interstellar medium (ISM) of the Galaxy. We find that the mass ejected from classical novae is about 2.7 × 10-3 M⊙ yr-1. In the nova ejecta, the isotopic ratios of C, N, and O, that is, 13C/12C, 15N/14N, and 17O/16O, are higher by about one order of magnitude than those in red giants. We estimate that about 10%, 5%, and 20% of 13C, 15N, and 17O in the ISM of the Galaxy come from nova ejecta, respectively. However, the chemical abundances of C, N, and O calculated by our model cannot cover all observational values. This means that there is still a long way to go to understand novae.

  7. The contribution of chemical abundances in nova ejecta to the interstellar medium

    NASA Astrophysics Data System (ADS)

    Li, Fanger; Zhu, Chunhua; Lü, Guoliang; Wang, Zhaojun

    2016-04-01

    According to the nova model from Yaron et al. (2005, ApJ, 418, 794) and José and Hernanz (1998, ApJ, 494, 680), and using a Monte Carlo simulation method, we investigate the contribution of chemical abundances in nova ejecta to the interstellar medium (ISM) of the Galaxy. We find that the mass ejected from classical novae is about 2.7 × 10-3 M⊙ yr-1. In the nova ejecta, the isotopic ratios of C, N, and O, that is, 13C/12C, 15N/14N, and 17O/16O, are higher by about one order of magnitude than those in red giants. We estimate that about 10%, 5%, and 20% of 13C, 15N, and 17O in the ISM of the Galaxy come from nova ejecta, respectively. However, the chemical abundances of C, N, and O calculated by our model cannot cover all observational values. This means that there is still a long way to go to understand novae.

  8. Clump formation through colliding stellar winds in the Galactic Center

    NASA Astrophysics Data System (ADS)

    Calderón, Diego

    2016-07-01

    The gas cloud G2 is currently being tidally disrupted by the Galactic Center super-massive black hole, Sgr A*. The region around the black hole is populated by ˜30 Wolf-Rayet stars, which produce strong outflows. Following an analytical approach, we explore the possibility that gas clumps, such as G2, originate from the collision of identical stellar winds via the Non-Linear Thin Shell Instability. We have found that the collision of relatively slow (<750 km s^{-1}) and strong (˜10^{-5} M_{⊙} yr^{-1}) stellar winds from stars at short separations (<2000 AU) is a process that indeed could produce clumps of G2's mass and above. Such short separation encounters of single stars along their orbits are not common in the Galactic Centre, however close binaries, such as IRS 16SW, are promising clump sources (see Calderón et al. 2016). We also present the first results of 2D models of colliding wind systems using the hydrodynamics adaptive mesh refinement code RAMSES, aiming to obtain a clump mass function, and the rate of clump formation and ejection to the ISM. We study the effect of parameters such as wind properties, stellar separation and orbital motion, in order to understand how likely the formation of G2 is in this context.

  9. Multi-interferogram method for measuring interseismic deformation: Denali Fault, Alaska

    USGS Publications Warehouse

    Biggs, Juliet; Wright, Tim; Lu, Zhong; Parsons, Barry

    2007-01-01

    Studies of interseismic strain accumulation are crucial to our understanding of continental deformation, the earthquake cycle and seismic hazard. By mapping small amounts of ground deformation over large spatial areas, InSAR has the potential to produce continental-scale maps of strain accumulation on active faults. However, most InSAR studies to date have focused on areas where the coherence is relatively good (e.g. California, Tibet and Turkey) and most analysis techniques (stacking, small baseline subset algorithm, permanent scatterers, etc.) only include information from pixels which are coherent throughout the time-span of the study. In some areas, such as Alaska, where the deformation rate is small and coherence very variable, it is necessary to include information from pixels which are coherent in some but not all interferograms. We use a three-stage iterative algorithm based on distributed scatterer interferometry. We validate our method using synthetic data created using realistic parameters from a test site on the Denali Fault, Alaska, and present a preliminary result of 10.5 ?? 5.0 mm yr-1 for the slip rate on the Denali Fault based on a single track of radar data from ERS1/2. ?? 2007 The Authors Journal compilation ?? 2007 RAS.

  10. Detecting leaks in gas-filled pressure vessels using acoustic resonances

    NASA Astrophysics Data System (ADS)

    Gillis, K. A.; Moldover, M. R.; Mehl, J. B.

    2016-05-01

    We demonstrate that a leak from a large, unthermostatted pressure vessel into ambient air can be detected an order of magnitude more effectively by measuring the time dependence of the ratio p/f2 than by measuring the ratio p/T. Here f is the resonance frequency of an acoustic mode of the gas inside the pressure vessel, p is the pressure of the gas, and T is the kelvin temperature measured at one point in the gas. In general, the resonance frequencies are determined by a mode-dependent, weighted average of the square of the speed-of-sound throughout the volume of the gas. However, the weighting usually has a weak dependence on likely temperature gradients in the gas inside a large pressure vessel. Using the ratio p/f2, we measured a gas leak (dM/dt)/M ≈ - 1.3 × 10-5 h-1 = - 0.11 yr-1 from a 300-liter pressure vessel filled with argon at 450 kPa that was exposed to sunshine-driven temperature and pressure fluctuations as large as (dT/dt)/T ≈ (dp/dt)/p ≈ 5 × 10-2 h-1 using a 24-hour data record. This leak could not be detected in a 72-hour record of p/T. (Here M is the mass of the gas in the vessel and t is the time.)

  11. Clump formation through colliding stellar winds in the Galactic Centre

    NASA Astrophysics Data System (ADS)

    Calderón, D.; Ballone, A.; Cuadra, J.; Schartmann, M.; Burkert, A.; Gillessen, S.

    2016-02-01

    The gas cloud G2 is currently being tidally disrupted by the Galactic Centre supermassive black hole, Sgr A*. The region around the black hole is populated by ˜30 Wolf-Rayet stars, which produce strong outflows. We explore the possibility that gas clumps, such as G2, originate from the collision of stellar winds via the non-linear thin shell instability. Following an analytical approach, we study the thermal evolution of slabs formed in the symmetric collision of winds, evaluating whether instabilities occur, and estimating possible clump masses. We find that the collision of relatively slow (≲750 km s-1) and strong (˜10-5 M⊙ yr-1) stellar winds from stars at short separations (<10 mpc) is a process that indeed could produce clumps of G2's mass and above. Such short separation encounters of single stars along their known orbits are not common in the Galactic Centre, making this process a possible but unlikely origin for G2. We also discuss clump formation in close binaries such as IRS 16SW and in asymmetric encounters as promising alternatives that deserve further numerical study.

  12. Nutrient and population dynamics in a subglacial reservoir: a simulation case study of the Blood Falls ecosystem with implications for astrobiology

    NASA Astrophysics Data System (ADS)

    Fisher, Thomson Mason; Schulze-Makuch, Dirk

    2013-10-01

    Subglacial ecosystems have recently become of interest within the astrobiological community, as they represent a potentially habitable location in otherwise uninhabitable environments. We used data from Blood Falls, particularly the periodic discharge from the subglacial reservoir beneath Taylor Glacier, Antarctica, to construct an ecosystem model of the putative subglacial microbial community residing there using system dynamics modelling. The model results were, for the most part, within an order of magnitude of the geochemical field data. Productivity was quite low, at 6.4×10-5 g carbon l-1 yr-1. Based on the results, we draw the following conjectures for the search for life on Mars: A similar ecosystem would require a continual supply of oxidized iron for energy and generate significant amounts of reduced iron as a waste product, be relatively resilient to temporary disturbances, and, thermodynamically, would require at least 0.003 kJ mol l-1 of energy to survive at that level of productivity. These results may help to better identify the constraints and boundaries of ecosystems in extreme environments, on Earth and other planetary bodies.

  13. Can Direct Collapse Black Holes Launch Gamma-Ray Bursts and Grow to Supermassive Black Holes?

    NASA Astrophysics Data System (ADS)

    Matsumoto, Tatsuya; Nakauchi, Daisuke; Ioka, Kunihito; Heger, Alexander; Nakamura, Takashi

    2015-09-01

    The existence of black holes (BHs) of mass ˜ {10}9 {M}⊙ at z≳ 6 is a big puzzle in astrophysics because even optimistic estimates of the accretion time are insufficient for stellar-mass BHs of ˜ 10 {M}⊙ to grow into such supermassive BHs. A resolution of this puzzle might be the direct collapse of supermassive stars with mass M˜ {10}5 {M}⊙ into massive seed BHs. We find that if a jet is launched from the accretion disk around the central BH, the jet can break out of the star because of the structure of the radiation-pressure-dominated envelope. Such ultralong gamma-ray bursts with duration of ˜ {10}4-106 s and flux of 10-11-10-8 erg s-1 cm-2 could be detectable by Swift. We estimate an event rate of ≲ 1 {{yr}}-1. The total explosion energy is ≳1055-{10}56 {erg}. The resulting negative feedback delays the growth of the remnant BH by about 70 {Myr} or evacuates the host galaxy completely.

  14. He-accreting white dwarfs: accretion regimes and final outcomes

    NASA Astrophysics Data System (ADS)

    Piersanti, L.; Tornambé, A.; Yungelson, L. R.

    2014-12-01

    The behaviour of carbon-oxygen (CO) white dwarfs (WDs) subject to direct helium accretion is extensively studied. We aim to analyse the thermal response of an accreting WD to mass deposition at different timescales. The analysis has been performed for initial WD masses and accretion rates in the range 0.60-1.02 M⊙ and 10-9-10-5 M⊙ yr-1, respectively. Thermal regimes in the parameter space MWD-dot{M}_He leading to formation of red-giant-like structures, steady burning of He, and mild, strong and dynamical flashes have been identified and the transition between these regimes has been studied in detail. In particular, the physical properties of WDs experiencing the He-flash accretion regime have been investigated to determine the mass retention efficiency as a function of the accretor total mass and accretion rate. We also discuss to what extent the building up of a He-rich layer via H burning could be described according to the behaviour of models accreting He-rich matter directly. Polynomial fits to the obtained results are provided for use in binary population synthesis computations. Several applications for close binary systems with He-rich donors and CO WD accretors are considered and the relevance of the results for interpreting He novae is discussed.

  15. Multiwavelength modeling the SED of supersoft X-ray sources. II. RS Ophiuchi: From the explosion to the SSS phase

    NASA Astrophysics Data System (ADS)

    Skopal, A.

    2015-04-01

    RS Oph is a recurrent symbiotic nova that undergoes nova-like outbursts on a time scale of 20 yr. Its two last eruptions (1985 and 2006) were subject of intensive multiwavelengths observational campaign from the X-rays to the radio. This contribution aims to determine physical parameters and the ionization structure of the nova from its explosion to the first emergence of the supersoft X-rays (day 26) by using the method of multiwavelength modeling the SED. From the very beginning of the eruption, the model SED revealed the presence of both a strong stellar and nebular component of radiation in the spectrum. During the first 4 days, the nova evinced a biconical ionization structure. The ∼8200 K warm and 160-200 R⊙ extended pseudophotosphere encompassed the white dwarf (WD) around its equator to the latitude > 40 ° . The remaining space around the WD's poles was ionized, producing a strong nebular continuum with the emission measure EM ∼ 2.3 ×1062 cm-3 via the fast wind from the WD. The luminosity of the burning WD was highly super-Eddington for the whole investigated period. The wind mass loss at rates of 10-4-10-5M⊙yr-1 and the presence of jets suggest an accretion throughout a disk at a high rate, which can help to sustain the super-Eddington luminosity of the accretor for a long time.

  16. MHD Solutions for Proto-Planetary Nebulae

    NASA Astrophysics Data System (ADS)

    García-Segura, G.; López, J. A.; Franco, J.

    2003-09-01

    This paper provides solutions for the origin of post-AGB winds, their acceleration up to high speed, and the subsequent formation of extremely collimated proto-planetary nebulae. Several wind models with terminal velocities from a few tens of voidb @xkms-1 up to 10^3 voidb @xkms-1 are calculated, which produce proto-planetary nebulae with linear momentum in the range 10^36 - 10^40 voidb @xgcms-1 and with kinetic energies in the range 10^42 - 10^47 erg. These results match available observations of proto-planetary nebulae. In the present simplistic scheme, the driver of the wind is just the magnetic pressure at the stellar surface. Other forces are not taken into account in this study, except gravity. We conclude that mass-loss rates of post-AGB stars and transition times from late AGB up to planetary nebula central stars could be directly linked with the production of magnetic field at the stellar core. As an example, mass-loss rates as large as 8×10^-5 M[ scriptstyle sun ]yr-1 and transition times as short as 5,000 years are predicted.

  17. The Signature of the Central Engine in the Weakest Relativistic Explosions: GRB 100316D

    NASA Astrophysics Data System (ADS)

    Margutti, R.; Soderberg, A. M.; Wieringa, M. H.; Edwards, P. G.; Chevalier, R. A.; Morsony, B. J.; Barniol Duran, R.; Sironi, L.; Zauderer, B. A.; Milisavljevic, D.; Kamble, A.; Pian, E.

    2013-11-01

    We present late-time radio and X-ray observations of the nearby sub-energetic gamma-ray burst (GRB)100316D associated with supernova (SN) 2010bh. Our broad-band analysis constrains the explosion properties of GRB 100316D to be intermediate between highly relativistic, collimated GRBs and the spherical, ordinary hydrogen-stripped SNe. We find that ~1049 erg is coupled to mildly relativistic (Γ = 1.5-2), quasi-spherical ejecta, expanding into a medium previously shaped by the progenitor mass-loss with a rate of \\dot{M}\\, {\\sim }\\, 10^{-5}\\,M_{\\odot }\\,yr^{-1} (for an assumed wind density profile and wind velocity vw = 1000 km s-1). The kinetic energy profile of the ejecta argues for the presence of a central engine and identifies GRB 100316D as one of the weakest central-engine-driven explosions detected to date. Emission from the central engine is responsible for an excess of soft X-ray radiation that dominates over the standard afterglow at late times (t > 10 days). We connect this phenomenology with the birth of the most rapidly rotating magnetars. Alternatively, accretion onto a newly formed black hole might explain the excess of radiation. However, significant departure from the standard fall-back scenario is required.

  18. Experimental burial inhibits methanogenesis and anaerobic decomposition in water-saturated peats.

    PubMed

    Blodau, Christian; Siems, Melanie; Beer, Julia

    2011-12-01

    A mechanistic understanding of carbon (C) sequestration and methane (CH(4)) production is of great interest due to the importance of these processes for the global C budget. Here we demonstrate experimentally, by means of column experiments, that burial of water saturated, anoxic bog peat leads to inactivation of anaerobic respiration and methanogenesis. This effect can be related to the slowness of diffusive transport of solutes and evolving energetic constraints on anaerobic respiration. Burial lowered decomposition constants in homogenized peat sand mixtures from about 10(-5) to 10(-7) yr(-1), which is considerably slower than previously assumed, and methanogenesis slowed down in a similar manner. The latter effect could be related to acetoclastic methanogenesis approaching a minimum energy quantum of -25 kJ mol(-1) (CH(4)). Given the robustness of hydraulic properties that locate the oxic-anoxic boundary near the peatland surface and constrain solute transport deeper into the peat, this effect has likely been critical for building the peatland C store and will continue supporting long-term C sequestration in northern peatlands even under moderately changing climatic conditions. PMID:21958021

  19. Spectroscopic Evidence for Gas Infall in GF 9-2

    NASA Astrophysics Data System (ADS)

    Furuya, Ray S.; Kitamura, Yoshimi; Shinnaga, Hiroko

    2009-02-01

    We present spectroscopic evidence for the infall motion of gas in the natal cloud core harboring an extremely young low-mass protostar GF 9-2. We previously discussed that the ongoing collapse of the GF 9-2 core has agreement with the Larson-Penston-Hunter (LPH) theoretical solution for the gravitational collapse of a core. To discuss the gas infall on firmer ground, we have carried out on-the-fly mapping observations of the HCO+ (1-0) line using the Nobeyama 45 m telescope equipped with the 25 Beam Array Receiver System. Furthermore, we observed the HCN (1-0) line with the 45 m telescope, and the HCO+ (3-2) line with the Caltech Submillimeter Observatory 10.4 m telescope. The optically thick HCO+ and HCN lines show blueskewed profiles whose deepest absorptions are seen at the peak velocity of optically thin lines, i.e., the systemic velocity of the cloud, indicating the presence of gas infall toward the central protostar. We compared the observed HCO+ line profiles with model ones by solving the radiative transfer in the core under LTE assumption. We found that the core gas has a constant infall velocity of ~0.5 km s-1 in the central region, leading to a mass accretion rate of 2.5 × 10-5 M sun yr-1. Consequently, we confirm that the gas infall in the GF 9-2 core is consistent with the LPH solution.

  20. Implications of PSR J0737-3039B for the Galactic NS-NS binary merger rate

    NASA Astrophysics Data System (ADS)

    Kim, Chunglee; Perera, Benetge Bhakthi Pranama; McLaughlin, Maura A.

    2015-03-01

    The Double Pulsar (PSR J0737-3039) is the only neutron star-neutron star (NS-NS) binary in which both NSs have been detectable as radio pulsars. The Double Pulsar has been assumed to dominate the Galactic NS-NS binary merger rate R_g among all known systems, solely based on the properties of the first-born, recycled pulsar (PSR J0737-3039A, or A) with an assumption for the beaming correction factor of 6. In this work, we carefully correct observational biases for the second-born, non-recycled pulsar (PSR J0737-0737B, or B) and estimate the contribution from the Double Pulsar on R_g using constraints available from both A and B. Observational constraints from the B pulsar favour a small beaming correction factor for A (˜2), which is consistent with a bipolar model. Considering known NS-NS binaries with the best observational constraints, including both A and B, we obtain R_g=21_{-14}^{+28} Myr-1 at 95 per cent confidence from our reference model. We expect the detection rate of gravitational waves from NS-NS inspirals for the advanced ground-based gravitational-wave detectors is to be 8^{+10}_{-5} yr-1 at 95 per cent confidence. Within several years, gravitational-wave detections relevant to NS-NS inspirals will provide us useful information to improve pulsar population models.

  1. Detecting leaks in gas-filled pressure vessels using acoustic resonances.

    PubMed

    Gillis, K A; Moldover, M R; Mehl, J B

    2016-05-01

    We demonstrate that a leak from a large, unthermostatted pressure vessel into ambient air can be detected an order of magnitude more effectively by measuring the time dependence of the ratio p/f(2) than by measuring the ratio p/T. Here f is the resonance frequency of an acoustic mode of the gas inside the pressure vessel, p is the pressure of the gas, and T is the kelvin temperature measured at one point in the gas. In general, the resonance frequencies are determined by a mode-dependent, weighted average of the square of the speed-of-sound throughout the volume of the gas. However, the weighting usually has a weak dependence on likely temperature gradients in the gas inside a large pressure vessel. Using the ratio p/f(2), we measured a gas leak (dM/dt)/M ≈ - 1.3 × 10(-5) h(-1) = - 0.11 yr(-1) from a 300-liter pressure vessel filled with argon at 450 kPa that was exposed to sunshine-driven temperature and pressure fluctuations as large as (dT/dt)/T ≈ (dp/dt)/p ≈ 5 × 10(-2) h(-1) using a 24-hour data record. This leak could not be detected in a 72-hour record of p/T. (Here M is the mass of the gas in the vessel and t is the time.). PMID:27250456

  2. A recalibration of strong-line oxygen abundance diagnostics via the direct method and implications for the high-redshift universe

    NASA Astrophysics Data System (ADS)

    Brown, Jonathan S.; Martini, Paul; Andrews, Brett H.

    2016-05-01

    We use direct method oxygen abundances in combination with strong optical emission lines, stellar masses (M⋆), and star formation rates (SFRs) to recalibrate the N2, O3N2, and N2O2 oxygen abundance diagnostics. We stack spectra of ˜200 000 star-forming galaxies from the Sloan Digital Sky Survey in bins of M⋆ and SFR offset from the star-forming main sequence ( {Δ log (SSFR)}) to measure the weak emission lines needed to apply the direct method. All three new calibrations are reliable to within ±0.10 dex from log (M⋆/M⊙) ˜ 7.5-10.5 and up to at least 200 M⊙ yr-1 in SFR. The N2O2 diagnostic is the least subject to systematic biases. We apply the diagnostics to galaxies in the local Universe and investigate the M⋆-Z-SFR relation. The N2 and O3N2 diagnostics suggest the SFR dependence of the M⋆-Z-SFR relation varies with both M⋆ and {Δ log (SSFR)}, whereas the N2O2 diagnostic suggests a nearly constant dependence on SFR. We apply our calibrations to a sample of high-redshift galaxies from the literature, and find them to be metal-poor relative to local galaxies with similar M⋆ and SFR. The calibrations do reproduce direct method abundances of the local analogues. We conclude that the M⋆-Z-SFR relation evolves with redshift.

  3. The modelled surface mass balance of the Antarctic Peninsula at 5.5 km horizontal resolution

    NASA Astrophysics Data System (ADS)

    van Wessem, J. M.; Ligtenberg, S. R. M.; Reijmer, C. H.; van de Berg, W. J.; van den Broeke, M. R.; Barrand, N. E.; Thomas, E. R.; Turner, J.; Wuite, J.; Scambos, T. A.; van Meijgaard, E.

    2016-02-01

    This study presents a high-resolution (˜ 5.5 km) estimate of surface mass balance (SMB) over the period 1979-2014 for the Antarctic Peninsula (AP), generated by the regional atmospheric climate model RACMO2.3 and a firn densification model (FDM). RACMO2.3 is used to force the FDM, which calculates processes in the snowpack, such as meltwater percolation, refreezing and runoff. We evaluate model output with 132 in situ SMB observations and discharge rates from six glacier drainage basins, and find that the model realistically simulates the strong spatial variability in precipitation, but that significant biases remain as a result of the highly complex topography of the AP. It is also clear that the observations significantly underrepresent the high-accumulation regimes, complicating a full model evaluation. The SMB map reveals large accumulation gradients, with precipitation values above 3000 mm we yr-1 in the western AP (WAP) and below 500 mm we yr-1 in the eastern AP (EAP), not resolved by coarser data sets such as ERA-Interim. The average AP ice-sheet-integrated SMB, including ice shelves (an area of 4.1 × 105 km2), is estimated at 351 Gt yr-1 with an interannual variability of 58 Gt yr-1, which is dominated by precipitation (PR) (365 ± 57 Gt yr-1). The WAP (2.4 × 105 km2) SMB (276 ± 47 Gt yr-1), where PR is large (276 ± 47 Gt yr-1), dominates over the EAP (1.7 × 105 km2) SMB (75 ± 11 Gt yr-1) and PR (84 ± 11 Gt yr-1). Total sublimation is 11 ± 2 Gt yr-1 and meltwater runoff into the ocean is 4 ± 4 Gt yr-1. There are no significant trends in any of the modelled AP SMB components, except for snowmelt that shows a significant decrease over the last 36 years (-0.36 Gt yr-2).

  4. An estimate of the terrestrial carbon budget of Russia using inventory based, eddy covariance and inversion methods

    NASA Astrophysics Data System (ADS)

    Dolman, A. J.; Shvidenko, A.; Schepaschenko, D.; Ciais, P.; Tchebakova, N.; Chen, T.; van der Molen, M. K.; Belelli Marchesini, L.; Maximov, T. C.; Maksyutov, S.; Schulze, E.-D.

    2012-06-01

    We determine the carbon balance of Russia, including Ukraine, Belarus and Kazakhstan using inventory based, eddy covariance, Dynamic Global Vegetation Models (DGVM), and inversion methods. Our current best estimate of the net biosphere to atmosphere flux is -0.66 Pg C yr-1. This sink is primarily caused by forests that using two independent methods are estimated to take up -0.69 Pg C yr-1. Using inverse models yields an average net biopshere to atmosphere flux of the same value with a interannual variability of 35 % (1σ). The total estimated biosphere to atmosphere flux from eddy covariance observations over a limited number of sites amounts to -1 Pg C yr-1. Fires emit 137 to 121 Tg C yr-1 using two different methods. The interannual variability of fire emissions is large, up to a factor 0.5 to 3. Smaller fluxes to the ocean and inland lakes, trade are also accounted for. Our best estimate for the Russian net biosphere to atmosphere flux then amounts to -659 Tg C yr-1 as the average of the inverse models of -653 Tg C yr-1, bottom up -563 Tg C yr-1 and the independent landscape approach of -761 Tg C yr-1. These three methods agree well within their error bounds, so there is good consistency between bottom up and top down methods. The best estimate of the net land to atmosphere flux, including the fossil fuel emissions is -145 to -73 Tg C yr-1. Estimated methane emissions vary considerably with one inventory-based estimate providing a net land to atmosphere flux of 12.6 Tg C-CH4yr -1 and an independent model estimate for the boreal and Arctic zones of Eurasia of 27.6 Tg C-CH4 yr-1.

  5. Responses of streams in central Appalachian Mountain region to reduced acidic deposition--comparisons with other regions in North America and Europe.

    PubMed

    Chen, Yushun; Lin, Lian-Shin

    2009-03-15

    Data from 5 wet deposition stations and 21 streams during 1980-2006 were analyzed to investigate chemical responses of streams to reduced acidic deposition in the central Appalachian Mountain region of West Virginia, USA. Wet deposition of acidic anions (i.e., sulfate, nitrate, and chloride) and hydrogen ions decreased significantly during the studied time period. Stream sulfate showed a delayed response to the reduced acidic deposition, and showed a decrease in the 2000s (-5.54 microeq L(-1) yr(-1)) and the whole period (-0.49 microeq L(-1) yr(-1)). No significant trend of stream nitrate+nitrite and chloride was observed. Stream alkalinity increased in the 1990s (+23.33 microeq L(-1) yr(-1)) and the whole period (+7.26 microeq L(-1) yr(-1)). Stream hydrogen ions decreased in the 1990s (-0.002 microeq L(-1) yr(-1)), 2000s (-0.001 microeq L(-1) yr(-1)), and the whole period (-0.001 microeq L(-1) yr(-1)). Compared with most acidic streams and lakes in the United States and Europe, a lower decreasing rate of hydrogen ions and higher increasing rate of alkalinity were observed in the alkaline West Virginian streams in the 1990s. However, due to their initial negative or zero alkalinity values, those acidic streams showed a higher percent increase in alkalinity than that in the alkaline West Virginian streams (from 800 microeq L(-1) yr(-1) to 1200 microeq L(-1) yr(-1)). Total aluminum in the West Virginian streams decreased in the 1990s (-0.67 micromol L(-1) yr(-1)) and the whole period (-0.22 micromol L(-1) yr(-1)). The current study advanced our understanding of streams' responses to the reduced acidic deposition in the Mid-Appalachians since the passage of the 1970 and 1990 Amendments to the United States Clean Air Act (US CAAA). PMID:19073337

  6. Nitrogen and phosphorus budget of a polyculture system of sea cucumber ( Apostichopus japonicus), jellyfish ( Rhopilema esculenta) and shrimp ( Fenneropenaeus chinensis)

    NASA Astrophysics Data System (ADS)

    Li, Junwei; Dong, Shuanglin; Gao, Qinfeng; Zhu, Changbo

    2014-06-01

    The nitrogen (N) and phosphorus (P) budget and the ecological efficiency of a polyculture system of sea cucumber ( Apostichopus japonicus), jellyfish ( Rhopilema esculenta) and shrimp ( Fenneropenaeus chinensis) were studied in a cofferdam, 120.2 ha in size. The nutrients were supplied by spring tide inflow. In total, 139600 kg N yr-1 and 9730 kg P yr-1 input to the system; while 118900 kg N yr-1 and 2840 kg P yr-1 outflowed from the system concurrently, thus the outflow was 85.7% (N) and 29.2% (P) of inflow. The production of N and P was 889.5 kg yr-1 and 49.28 kg yr-1 (sea cucumber) and 204 kg yr-1 and 18.03 kg yr-1 (jellyfish and shrimp), respectively. The utilization rate of N and P by polycultured animals was 7.8‰ and 6.9‰, respectively, 21.9% and 38% higher than that of monocultured sea cucumber. Our results indicated that the polyculture system was an efficient culture system of animals and a remediation system of coastal environment as well; it scavenged 14.3% and 70.8% of N and P, respectively. Such an ecological efficiency may be improved further by increasing either the stocking density or the size of sea cucumber or both.

  7. IDENTIFYING DISCHARGE ZONES OF ARSENIC IN THE GOOSE RIVER BASIN, MAINE

    EPA Science Inventory

    Groundwater discharge areas are simulated from water balance modeling and kriging of oxygen isotopes in groundwater within the Goose River basin. Groundwater fluxes of discharge range from -10 cm yr-1 to < -25 cm yr-1 and are associated with areas of elevated arsenic in wells. De...

  8. Rates and causes of recent global sea-level rise inferred from long tide gauge data records

    NASA Astrophysics Data System (ADS)

    Nakada, Masao; Inoue, Hiroshi

    2005-05-01

    Tide gauge data at seven sites of the Permanent Service for Mean Sea Level (PSMSL), with information for relative sea-level during the past 140-200 yr, were analyzed to examine the rates and causes of the global sea-level rise (GSLR) during the twentieth century. By subtracting linear trends for relative sea-level rise during the past 100 yr from the observed data, we get the apparent GSLRs of ˜1 mm yr -1 for five sites around the Baltic Sea and Brest. The rate for San Francisco is significantly larger than this, with an optimum value ˜2 mm yr -1. The spatial difference of ˜1 mm yr -1 between these sites is reasonably explained by the recent melting of the Greenland ice sheet with an equivalent sea-level rise of ˜1 mm yr -1. The predicted relative sea-level change for this melting scenario is 0.5 mm yr -1 at sites around the Baltic Sea and Brest, and 1.5 mm yr -1 for San Francisco. The residuals between observations and predictions, ˜0.5 mm yr -1 at all sites, may be contributed by thermal expansion of seawater and/or other melting sources. These results suggest the rate of twentieth-century GSLR to be 1.5 mm yr -1.

  9. A Quantitative Food Web Model for the Macroinvertebrate Community of a Northern German Lowland Stream

    NASA Astrophysics Data System (ADS)

    Poepperl, Rainer

    2003-09-01

    Trophic interactions and cycling of organic carbon within the macroinvertebrate community of a Northern German lowland stream were analyzed based on a compartment model. The network model describes the structure of the food web quantifying biomass, production, and consumption of their elements, of the entire system and between trophic levels. System primary production is 153.7 g C m-2 yr-1 and invertebrate production 53.3 g C m-2 yr-1. Invertebrate consumption amounts to 702.6 g C m-2 yr-1. Main flows are identified between trophic level 1 and 2 and are connected with highly productive compartments. Anodonta and Pseudanodonta and Dreissena polymorpha show the highest consumption of all groups with 269.9 g C m-2 yr-1 and 114.1 g C m-2 yr-1, respectively. System consumption is highest on the import from the upstream lake with 532.5 g C m-2 yr-1, sediment detritus with 135.5 g C m-2 yr-1, and primary producers with 25.7 g C m-2 yr-1. The lowest predation pressure is observed for Bivalvia with an ecotrophic efficiency of <10% and highest for Chironomidae with 91%. Approximately 20% of organic matter entering the detritus pool are recycled to the living groups of the system. Transfer efficiencies between discrete trophic levels are generally low except for transfer of detrital material between level I and II.

  10. Radium-thorium disequilibrium and zeolite-water ion exchange in a Yellowstone hydrothermal environment

    NASA Astrophysics Data System (ADS)

    Sturchio, N. C.; Bohlke, J. K.; Binz, C. M.

    1989-05-01

    Whole rock samples of hydrothermally altered Biscuit Basin rhyolite from Yellowstone drill cores Y-7 and Y-8 were analyzed for 226Ra and 230Th to determine the extent of radioactive disequilibrium and its relation to the rates and mechanisms of element transport in the shallow portion of an active hydrothermal system. The ( 226Ra/230Th) activity ratios range from 0.73 to 1.46 and are generally correlated with Th-normalized Ba concentrations (Ba N). Values of ( 226Ra/230Th) and Ba N > 1 were found in samples containing large modal fractions of clinoptilolite; whereas values of ( 226Ra/230Th) and Ba N < 1 were found in samples containing large modal fractions of mordenite. Composition clinoptilolite and mordenite in these samples are consistent with ion exchange equilibrium between zeolites and coexisting thermal waters. Average K d mineral-waterBa values are 1.0·10 5 mL/g for clinoptilolite and 1.4·10 4 mL/g for mordenite. Apparent diffustvities through matrix porosity estimated for Ra and Ba range from ˜10 -12 to ˜10 -10 cm 2s -1 in thoroughly zeolitic rhyolite; these rates of diffusion are too low to account for the observed distance scale of ( 226Ra/230Th) disequilibrium. The correlated values of ( 226Ra /230Th) disequilibrium and Ba N represent zeolite-water ion exchange equilibrium that is caused by porous flow of water through the rock matrix and by the relatively rapid diffusion of cations within the zeolite lattices. A water flux of at least ˜2.5 ( cm water3/cm rock3) yr -1 is required to produce measurable ( 226Ra/230Th) disequilibrium, whereas at least ˜23 ( cm water3/cm rock3) yr -1 is r for the sample exhibiting the most extreme ( 226Ra/230Th) disequilibrium; these fluxes are much higher than those that can be inferred from net mass transfers of stable species. The zeolite-water ion exchange process appears to have been operating for at least 8000 yr in the environment of the Y-7 and Y-8 drill holes.

  11. Atmospheric methyl halides and dimethyl sulfide from cattle

    NASA Astrophysics Data System (ADS)

    Williams, Jody; Wang, Nun-Yii; Cicerone, Ralph J.; Yagi, Kazuyuki; Kurihara, Mitsunori; Terada, Fuminori

    1999-06-01

    We have measured emissions of CH3Cl, CH3Br, and (CH3)2S (DMS) from Holstein cows. In one experiment, two cows were studied in separate metabolic research chambers for a 24-hour period while on a normal diet and were studied for an additional 24-hour period 1 week later after being placed on a diet enhanced in chloride and bromide. Methyl chloride emissions ranged between 0.4 × 10-3 and 1.5 × 10-3 g cow-1 d-1, while methyl bromide emissions were much smaller, 3 × 10-6-2 × 10-5 g cow-1 d-1. Daily emissions of methane from these cows were 134-180 g cow-1 d-1, quite similar to values found in many previous studies. A second 24-hour study of two different cows on normal diets yielded daily emissions of 0.6 × 10-3 and 0.9 × 10-3 g CH3Cl, 0-1.0 × 10-6 g CH3Br, and 191 and 176 g CH4. If these emissions of CH3Cl and CH3Br are representative of the 1.3 billion head of cattle worldwide, then the global source of atmospheric CH3Cl and CH3Br from cattle would be 0.23-0.70 Gg yr-1 and (1-10) × 10-3 Gg yr-1, respectively. These emissions of CH3Cl and CH3Br represent <0.02% and <0.005%, respectively, of the total annual global atmospheric sources of these compounds; therefore, emissions of CH3Cl and CH3Br from cattle are insignificant contributors to their total sources. Discovered serendipitously, DMS emissions were between 0.17 and 0.24 g cow-1 d-1, and chloroform emissions were 2 × 10-4-3 × 10-3 g cow-1 d-1. DMS from cattle is not a major source over hemispheric or global scales but could be important in certain geographical regions. Chloroform (CHCl3) emissions were similarly detected and quantified, as were those of C2H5X (X = Cl or Br).

  12. Abiotic methane flux from the Chimaera seep and Tekirova ophiolites (Turkey): Understanding gas exhalation from low temperature serpentinization and implications for Mars

    NASA Astrophysics Data System (ADS)

    Etiope, Giuseppe; Schoell, Martin; Hosgörmez, Hakan

    2011-10-01

    The emission of abiotic methane (CH 4) into the atmosphere from low temperature serpentinization in ophiolitic rocks is documented to date only in four countries, the Philippines, Oman, New Zealand, and Turkey. Serpentinization produces large amounts of hydrogen (H 2) which in theory may react with CO 2 or CO to form hydrocarbons (Fischer-Tropsch Type synthesis, FTT). Similar mechanisms have been invoked to explain the CH 4 detected on Mars, so that understanding flux and exhalation modality of ophiolitic gas on Earth may contribute to decipher the potential degassing on Mars. This work reports the first direct measurements of gas (CH 4, CO 2) flux ever done on onshore ophiolites with present-day serpentinization. We investigated the Tekirova ophiolites at Çirali, in Turkey, hosting the Chimaera seep, a system of gas vents issuing from fractures in a 5000 m 2 wide ophiolite outcrop. At this site at least 150-190 t of CH 4 is annually released into the atmosphere. The molecular and isotopic compositions of C 1-C 5 alkanes, CO 2, and N 2 combined with source rock maturity data and thermogenic gas formation modelling suggested a dominant abiotic component (~ 80-90%) mixed with thermogenic gas. Abiotic H 2-rich gas is likely formed at temperatures below 50 °C, suggested by the low deuterium/hydrogen isotopic ratio of H 2 (δD H2: - 720‰), consistent with the low geothermal gradient of the area. Abiotic gas synthesis must be very fast and effective in continuously producing an amount of gas equivalent to the long-lasting (> 2 millennia) emission of > 100 t CH 4 yr - 1 , otherwise pressurised gas accumulation must exist. Over the same ophiolitic formation, 3 km away from Chimaera, we detected an invisible microseepage of abiotic CH 4 with fluxes from 0.07 to 1 g m - 2 d - 1 . On Mars similar fluxes could be able to sustain the CH 4 plume apparently recognised in the Northern Summer 2003 (10 4 or 10 5 t yr - 1 ) over the wide olivine bedrock and outcrops of hydrated

  13. Drought effects on soil CO

    NASA Astrophysics Data System (ADS)

    van Straaten, O.; Veldkamp, E.; Köhler, M.; Anas, I.

    2009-12-01

    Climate change induced droughts pose a serious threat to ecosystems across the tropics and sub-tropics, particularly to those areas not adapted to natural dry periods. In order to study the vulnerability of cacao (Theobroma cacao) - Gliricidia sepium agroforestry plantations to droughts a large scale throughfall displacement roof was built in Central Sulawesi, Indonesia. In this 19-month replicated experiment, we measured soil surface CO2 efflux (soil respiration) in three simulated drought plots compared with three adjacent control plots. Soil respiration rates peaked at intermediate soil moisture and decreased under increasingly dry conditions (drought induced), but also decreased when soils became water saturated, as evidenced in control plots. The simulated drought plots exhibited a slight decrease in soil respiration compared to the control plots (average 13% decrease). The strength of the drought effect was spatially variable - while some measurement chamber sites reacted strongly ("responsive") to the decrease in soil water content (up to R2=0.70) (n=11), others did not react at all ("non-responsive") (n=7). The degree of soil CO2 respiration drought response was highest around cacao tree stems and decreased with distance from the stem (R2=0.22). A significant correlation was measured between "responsive" soil respiration chamber sites and sap flux density ratios of cacao (R=0.61) and Gliricidia (R=0.65). Leaf litter CO2 respiration decreased as conditions became drier. During dry periods the litter layer contributed approximately 3-4% of the total CO2 efflux and up to 40% during wet periods. A CO2 flush was recorded during the rewetting phase that lasted for approximately two weeks, during which time accumulated labile carbon stocks mineralized. The net effect on soil CO2 emissions over the duration of the experiment was neutral, control plots respired 11.1±0.5 Mg C ha-1 yr-1, while roof plots respired 10.5±0.5 Mg C ha-1 yr-1.

  14. Coccolithophore export production in response to monsoonal upwelling off Somalia (northwestern Indian Ocean)

    NASA Astrophysics Data System (ADS)

    Broerse, A. T. C.; Brummer, G.-J. A.; Hinte, J. E. Van

    Coccolithophores, collected in a sediment trap at 1032 m depth off Somalia from June 1992 to February 1993, responded rapidly to the SW and NE Monsoons with changes in productivity, species composition, coccolith:coccosphere ratio, and CaCO 3 production. Statistically identified species clusters and sample clusters consistently matched hydrographic periods distinguished by sea-surface temperature, wind velocities and nutrient concentrations, as well as δ15N values in the sediment-trap samples. The deep-photic zone species Florisphaera profunda and Gladiolithus flabellatus were dominant in the early SW Monsoon when coastally upwelled water carried by a large gyre, passed over the station. The opportunistic species Emiliania huxleyi and Gephyrocapsa oceanica dominated during the height of the SW Monsoon and exhibited maximum fluxes during the beginning of upwelling relaxation in September. Most other coccolithophore species showed maximum relative abundances in a later stage of the upwelling relaxation when coccolithophore fluxes started to decrease. In the inter-Monsoon period stratified, nutrient-depleted, surface waters coincided with low coccolithophore fluxes. Several less abundant, oligotrophic species exhibited maximum percentages in this period. During the NE Monsoon both deep and shallow living species displayed a rapid increase in fluxes in response to a moderate wind-induced entrainment of nutrients. During this period maximum fluxes were recorded, with 1.1×10 9 coccolithsm-2 d-1 and 4.8×10 6 coccospheresm-2 d-1. Average, time-weighted, total fluxes were 4.7×10 8coccolithsm-2 d-1 and 12.2×10 5coccospheresm-2 d-1, corresponding to a (computed) coccolithophore-CaCO 3 flux of 8.1 mgm-2 d-1 (=2.9 gm-2 yr-1) , which is 13.2% (13.5% including Thoracosphaera spp.) of the yearly total CaCO 3 flux. The average CaCO 3 flux in the fine fraction (<32 μm) was 21.4 mg/ m-2/ day -1 (=7.8 gm-2 yr-1) , contributing 34.3% to the total CaCO 3 flux on a yearly basis.

  15. Systematics of Dynamical Mass Ejection, Nucleosynthesis, and Radioactively Powered Electromagnetic Signals from Neutron-star Mergers

    NASA Astrophysics Data System (ADS)

    Bauswein, A.; Goriely, S.; Janka, H.-T.

    2013-08-01

    We investigate systematically the dynamical mass ejection, r-process nucleosynthesis, and properties of electromagnetic counterparts of neutron-star (NS) mergers in dependence on the uncertain properties of the nuclear equation of state (EOS) by employing 40 representative, microphysical high-density EOSs in relativistic, hydrodynamical simulations. The crucial parameter determining the ejecta mass is the radius R 1.35 of a 1.35 M ⊙ NS. NSs with smaller R 1.35 ("soft" EOS) eject systematically higher masses. These range from ~10-3 M ⊙ to ~10-2 M ⊙ for 1.35-1.35 M ⊙ binaries and from ~5 × 10-3 M ⊙ to ~2 × 10-2 M ⊙ for 1.2-1.5 M ⊙ systems (with kinetic energies between ~5 × 1049 erg and 1051 erg). Correspondingly, the bolometric peak luminosities of the optical transients of symmetric (asymmetric) mergers vary between 3 × 1041 erg s-1 and 14 × 1041 erg s-1 (9 × 1041 erg s-1 and 14.5 × 1041 erg s-1) on timescales between ~2 hr and ~12 hr. If these signals with absolute bolometric magnitudes from -15.0 to -16.7 are measured, the tight correlation of their properties with those of the merging NSs might provide valuable constraints on the high-density EOS. The r-process nucleosynthesis exhibits a remarkable robustness independent of the EOS, producing a nearly solar abundance pattern above mass number 130. By the r-process content of the Galaxy and the average production per event the Galactic merger rate is limited to 4 × 10-5 yr-1 (4 × 10-4 yr-1) for a soft (stiff) NS EOS, if NS mergers are the main source of heavy r-nuclei. The production ratio of radioactive 232Th to 238U attains a stable value of 1.64-1.67, which does not exclude NS mergers as potential sources of heavy r-material in the most metal-poor stars.

  16. The modelled surface mass balance of the Antarctic Peninsula at 5.5 km horizontal resolution

    NASA Astrophysics Data System (ADS)

    van Wessem, J. M.; Ligtenberg, S. R. M.; Reijmer, C. H.; van de Berg, W. J.; van den Broeke, M. R.; Barrand, N. E.; Thomas, E. R.; Turner, J.; Wuite, J.; Scambos, T. A.; van Meijgaard, E.

    2015-09-01

    This study presents a high-resolution (~ 5.5 km) estimate of Surface Mass Balance (SMB) over the period 1979-2014 for the Antarctic Peninsula (AP), generated by the regional atmospheric climate model RACMO2.3 and a Firn Densification Model (FDM). RACMO2.3 is used to force the FDM, which calculates processes in the snowpack, such as meltwater percolation, refreezing and runoff. We evaluate model output with 132 in-situ SMB observations and discharge rates from 6 glacier drainage basins, and find that the model realistically simulates the strong spatial variability in precipitation, but that significant biases remain as a result of the highly complex topography of the AP. It is also clear that the observations significantly underrepresent the high-accumulation regimes. The SMB map reveals large accumulation gradients, with precipitation values above 3000 mm we yr-1 over the western AP (WAP) and below 500 mm we yr-1 on the eastern AP (EAP), not resolved by coarser data-sets such as ERA-Interim. The other SMB components are one order of magnitude smaller, with drifting snow sublimation the largest ablation term removing up to 100 mm we yr-1 of mass. Snowmelt is widespread over the AP, reaching 500 mm we yr-1 towards the northern ice shelves, but the meltwater mostly refreezes. As a result runoff fluxes are low, but still considerable (200 mm we yr-1) over the Larsen (B/C), Wilkins and George VI ice shelves. The average AP ice sheet integrated SMB, including ice shelves (an area of 4.1 × 105 km2), is estimated at 351 Gt yr-1 with an interannual variability of 58 Gt yr-1, which is dominated by precipitation (PR) (365 ± 57 Gt yr-1). The WAP (2.4 × 105 km2) SMB (276 ± 47 Gt yr-1), where PR is large (276 ± 47 Gt yr-1), dominates over the EAP (1.7 × 105 km2) SMB (75 ± 11 Gt yr-1) and PR (84 ± 11 Gt yr-1). Total sublimation is 11 ± 2 Gt yr-1 and meltwater runoff into the ocean is 4 ± 4 Gt yr-1. There are no significant trends in any of the AP SMB components, except

  17. Changes in ground-level PM mass concentration and column aerosol optical depth over East Asia during 2004-2014

    NASA Astrophysics Data System (ADS)

    Nam, J.; Kim, S. W.; Park, R.; Yoon, S. C.; Sugimoto, N.; Park, J. S.; Hong, J.

    2015-12-01

    Multi-year records of moderate resolution imaging spectroradiometer (MODIS), ground-level particulate matter (PM) mass concentration, cloud-aerosol lidar with orthogonal polarization (CALIOP), and ground-level lidar were analyzed to investigate seasonal and annual changes of aerosol optical depth (AOD) and PM mass concentration over East Asia. Least mean square fit method is applied to detect the trends and their magnitudes for each selected regions and stations. Eleven-year MODIS measurements show generally increasing trends in both AOD (1.18 % yr-1) and Ångström exponent (0.98 % yr-1), especially over the east coastal industrialized region in China. Monthly variation of AOD show maximum value at April-July, which were related to the progress of summer monsoon rain band and stationary continental air mass on the northeast of Asia. Increasing trends of AOD were found for eight cites in China (0.80 % yr-1) and Seoul site, Korea (0.40 % yr-1), whereas no significant change were shown in Gosan background site (0.04 % yr-1) and decreasing trend at five background sites in Japan (-0.42 % yr-1). Contrasting to AOD trend, all fifteen sites in China (-1.28 % yr-1), Korea (-2.77 % yr-1), and Japan (-2.03 % yr-1) showed decreasing trend of PM10 mass concentration. Also, PM2.5 mass concentration at Beijing, Seoul, Rishiri, and Oki show significant decreasing trend of -1.16 % yr-1. To further discuss the opposite trend of surface PM mass concentration and column AOD, we investigate vertical aerosol profile from lidar measurements. AOD estimated for planetary boundary layer (surface~1.5 km altitude; AODPBL) from CALIOP measurements over East China show decreasing trend of -1.71 % yr-1 over the period of 2007-2014, wherever AOD estimated for free troposphere (1.5 km~5 km altitude; AODFT) show increasing trend of 2.92 % yr-1. In addition, ground-level lidar measurements in Seoul show decreasing AODPBL trend of -2.57 % yr-1, whereas, AODFT show no significant change (-0.44 % yr

  18. Radiocesium wash-off associated with soil erosion from various land uses after the Fukushima Dai-ichi NPP accident

    NASA Astrophysics Data System (ADS)

    Wakiyama, Yoshifumi; Onda, Yuichi; Yoshimura, Kazuya; Kato, Hiroaki; Konoplev, Alexei; Zheleznyak, Mark

    2014-05-01

    Soil erosion is the initial process which drives radiocesium into the aquatic systems and therefore the quantification of radiocesium wash-off associated with soil erosion is indispensable for mitigating the risks. This study presents two year's observation of soil erosion and radiocesium wash-off to quantify differences in radiocesium behavior in various land uses. Seven runoff plots were established in four landscapes; uncultivated farmland (Farmland A1, Farmland B1), cultivated farmland (Farmland A2, Farmland B2), grassland (Grassland A, Grassland B) and Japanese cedar forest (Forest) in Kawamata town, an area affected by the Fukushima Dai-ichi Nuclear Power Plant accident. The discharged sediments were collected approximately every two weeks. In laboratories, collected sediments were dried and weighed for calculating soil erosion rates (kg m-2) and served for measurements of radiocesium concentration (Bq kg-1) with HPGe detectors. The erosivity factor of the Universal Soil Loss Equation (R-factor: MJ mm ha-1 hr-1 yr-1) was calculated based on the data of precipitation. Standardized soil erosion rates (kg m-2 MJ-1 mm-1 ha hr yr), observed soil erosion rates divided by R-factor, was 1.8 × 10-4 in Farmland A1, 6.0 × 10-4 in Farmland A2, 1.5 × 10-3 in Farmland B1, 8.3 × 10-4 in Farmland B2, 9.6 × 10-6 in Grassland A, 5.9 × 10-6 in Grassland B and 2.3 × 10-6 in Forest. These erosion rates were basically proportional to their vegetation cover of soil surfaces except for cultivated farmlands. Concentrations of Cs-137 in eroded sediments basically depended on the local deposition of Cs-137 and varied enormously with ranging several orders of magnitude in all the landscapes. For the observation period of time decreasing trends in concentrations of Cs-137 in eroded sediments were not obvious. To compare these results with those of Chernobyl, we calculated normalized 'solid' wash-off coefficient (m2 g-1) with dividing the mean total concentration of Cs-137 in

  19. A large and persistent carbon sink in the World s forests

    SciTech Connect

    Pan, Yude; Birdsey, Richard A.; Fang, Jingyun; Houghton, Richard; Kauppi, Pekka; Kurz, Werner; Phillips, Oliver; Shvidenko, Anatoly; Lewis, Simon; Canadell, Josep; Ciais, Philippe; Jackson, Robert B; Pacala, Stephen; Mcguire, David; Piao, Shilong; Rautiainen, Aapo; Sitch, Stephen; Hayes, Daniel J

    2011-01-01

    The terrestrial carbon (C) sink has been large in recent decades, but its size and location remain uncertain. Using forest inventory data and long-term ecosystem C studies, we estimated a total forest sink of 2.4 0.4 Pg C yr 1 globally for 1990-2007. We also estimated a source of 1.3 0.7 Pg C yr 1 from tropical land-use change, consisting of a gross tropical deforestation emission of 2.9 0.5 Pg C yr 1 partially compensated by a C sink in tropical forest regrowth of 1.6 0.5 Pg C yr 1. Together, the fluxes comprise a net global forest sink of 1.1 0.8 Pg C yr 1, with tropical estimates having the largest uncertainties. This forest sink is equivalent in magnitude to the terrestrial sink deduced from fossil fuel emissions and constraints of ocean and atmospheric sinks.

  20. Global tropospheric ozone variations from 2003 to 2011 as seen by SCIAMACHY

    NASA Astrophysics Data System (ADS)

    Ebojie, F.; Burrows, J. P.; Gebhardt, C.; Ladstätter-Weißenmayer, A.; von Savigny, C.; Rozanov, A.; Weber, M.; Bovensmann, H.

    2016-01-01

    An analysis of the tropospheric ozone (O3) columns (TOCs) derived from SCIAMACHY limb-nadir-matching (LNM) observations during the period 2003-2011, focusing on global variations in TOC, is described. The changes are derived using a multivariate linear regression model. TOC shows changes of -0.2 ± 0.4, 0.3 ± 0.4, 0.1 ± 0.5 and 0.1 ± 0.2 % yr-1, which are not statistically significant at the 2σ level in the latitude bands 30-50° N, 20° S-0, 0-20° N and 50-30° S, respectively. Tropospheric O3 shows statistically significant increases over some regions of South Asia (1-3 % yr-1), the South American continent (up to 2 % yr-1), Alaska (up to 2 % yr-1) and around Congo in Africa (up to 2 % yr-1). Significant increase in TOC is determined off the continents including Australia (up to 2 % yr-1), Eurasia (1-3 % yr-1) and South America (up to 3 % yr-1). Significant decrease in TOC (up to -3 % yr-1) is observed over some regions of the continents of North America, Europe and South America. Over the oceanic regions including the Pacific, North Atlantic and Indian oceans, significant decreases in TOC (-1 to -3 % yr-1) were observed. In addition, the response of the El Niño-Southern Oscillation (ENSO) and quasi-biennial oscillation (QBO) to changes in TOC for the period 2003-2011 was investigated. The result shows extensive regions, mostly in the tropics and Northern Hemisphere extratropics, of significant ENSO responses to changes in TOC and a significant QBO response to TOC changes over some regions.

  1. Physical and biological characteristics of the pelagic system across Fram Strait to Kongsfjorden

    NASA Astrophysics Data System (ADS)

    Hop, Haakon; Falk-Petersen, Stig; Svendsen, Harald; Kwasniewski, Slawek; Pavlov, Vladimir; Pavlova, Olga; Søreide, Janne E.

    2006-10-01

    handful of amphipod species and the polar cod. The ice-associated biomass transport of ice-amphipods was calculated, based on the ice area transport, at about 3.55 × 10 6 ton wet weight per year or about 4.2 × 10 5 t C yr -1. This represents a large energy input to the Greenland Sea, but also a drain on the core population residing in the multi-year pack ice (MYI) in the Arctic Ocean. A continuous habitat loss of MYI due to climate warming will likely reduce dramatically the sympagic food source. The pelagic and sympagic food web structures were revealed by stable isotopes. The carbon sources of particulate organic matter (POM), being Ice-POM and Pelagic-POM, revealed different isotopic signals in the organisms of the food web, and also provided information about the sympagic-pelagic and pelagic-benthic couplings. The marine food web and energy pathways were further determined by fatty acid trophic markers, which to a large extent supported the stable isotope picture of the marine food web, although some discrepancies were noted, particularly with regard to predator-prey relationships of ctenophores and pteropods.

  2. Decadal variability in the oxygen inventory of North Atlantic subtropical underwater captured by sustained, long-term oceanographic time series observations

    NASA Astrophysics Data System (ADS)

    Montes, Enrique; Muller-Karger, Frank E.; Cianca, Andrés.; Lomas, Michael W.; Lorenzoni, Laura; Habtes, Sennai

    2016-03-01

    Historical observations of potential temperature (θ), salinity (S), and dissolved oxygen concentrations (O2) in the tropical and subtropical North Atlantic (0-500 m; 0-40°N, 10-90°W) were examined to understand decadal-scale changes in O2 in subtropical underwater (STUW). STUW is observed at four of the longest, sustained ocean biogeochemical and ecological time series stations, namely, the CArbon Retention In A Colored Ocean (CARIACO) Ocean Time Series Program (10.5°N, 64.7°W), the Bermuda Atlantic Time-series Study (BATS; 31.7°N, 64.2°W), Hydrostation "S" (32.1°N, 64.4°W), and the European Station for Time-series in the Ocean, Canary Islands (ESTOC; 29.2°N, 15.5°W). Observations over similar time periods at CARIACO (1996-2013), BATS (1988-2011), and Hydrostation S (1980-2013) show that STUW O2 has decreased approximately 0.71, 0.28, and 0.37 µmol kg-1 yr-1, respectively. No apparent change in STUW O2 was observed at ESTOC over the course of the time series (1994-2013). Ship observation data for the tropical and subtropical North Atlantic archived at NOAA National Oceanographic Data Center show that between 1980 and 2013, STUW O2 (upper ~300 m) declined 0.58 µmol kg-1 yr-1 in the southeastern Caribbean Sea (10-15°N, 60-70°W) and 0.68 µmol kg-1 yr-1 in the western subtropical North Atlantic (30-35°N, 60-65°W). A declining O2 trend was not observed in the eastern subtropical North Atlantic (25-30°N, 15-20°W) over the same period. Most of the observed O2 loss seems to result from shifts in ventilation associated with decreased wind-driven mixing and a slowing down of STUW formation rates, rather than changes in diffusive air-sea O2 gas exchange or changes in the biological oceanography of the North Atlantic. Variability of STUW O2 showed a significant relationship with the wintertime (January-March) Atlantic Multidecadal Oscillation index (AMO, R2 = 0.32). During negative wintertime AMO years trade winds are typically stronger between 10°N and 30

  3. Quantitative analysis of the FUV, UV and optical spectrum of the O3 star HD 93129A.

    NASA Astrophysics Data System (ADS)

    Taresch, G.; Kudritzki, R. P.; Hurwitz, M.; Bowyer, S.; Pauldrach, A. W. A.; Puls, J.; Butler, K.; Lennon, D. J.; Haser, S. M.

    1997-05-01

    A quantitative analysis of the extremely hot and massive galactic O3If^*^ supergiant HD 93129A is carried out using stellar wind and pseudo photospheric lines observed in the FUV, UV and optical spectrum together with hydrodynamical NLTE model atmospheres. The analysis in the FUV is combined with spectrum synthesis of the molecular and atomic/ionic interstellar spectrum to disentangle stellar and interstellar blends. It is demonstrated that the combined stellar/interstellar spectrum synthesis technique is crucial for the determination of both interstellar column densities and stellar properties. The fraction of hydrogen atoms in molecular form in the Carina interstellar clouds is found to be 0.1, smaller than one would expect for its E(B-V) value of 0.54. We attribute this to dissociation by the strong FUV radiation field of HD 93129A. The excitation temperature of ortho-hydrogen (J=1) is about 80K, whereas the excitation to higher levels requires temperatures up to 230K in accordance with NLTE effects for interstellar H_2_ as discussed in the literature. The abundance of HD relative to H_2_ is of the order of 10^-5^. For CO we obtain an upper limit of 2.6x10^-5^. Abundances for the interstellar atomic and ionic species are also derived. The terminal velocity of the stellar wind of HD 93129A is 3200+/-200km/s and the rate of mass-loss is 18x10^-6^Msun_/yr. The ionization equilibrium of the optical emission and P-Cygni lines of NIII, NIV and NV is used to determine the effective temperature as T_eff_=52000+/-1000K in reasonable agreement with previous values obtained from the helium ionization equilibrium. This high temperature is confirmed independently by an analysis of the ArVI/ArVII ionization equilibrium in the FUV. The luminosity of HD 93129A is log L/Lsun_=6.4+/-0.1 corresponding to a zero age main sequence mass of slightly in excess of 120Msun_. This very high mass is consistent with the mass determined from the stellar gravity and with the mass derived from

  4. The early gaseous and stellar mass assembly of Milky Way-type galaxy haloes

    NASA Astrophysics Data System (ADS)

    Hensler, Gerhard

    2015-08-01

    In cosmological simulations of Cold Dark Matter (CDM) structure formation a vast number of subhalos is expected around massive galaxies like the Milky Way (MW). These DM subhalos are filled with baryons, gas that forms stars very early as observed from the stellar populations in the MW satellite galaxies. Satellite galaxies evolve in the tidal field of their mature galaxy and suffer accretion to the major galaxy and their partly disruption. By this, their mass loss is expected to feed the galaxy halo with stars and gas.From the Via Lactea II simulations we select a massive DM halo with its satellite system which evolves in the simulations to a present-day MW-type galaxy. We follow its evolution from redshift 4.5 to 2.5, i.e. over almost 2 billion years of the most interesting epoch of mass assembly. A high mass resolution allows for even low-mass satellites down to 10^5 Msun, but limits their distance range to the innermost 240 satellites of the system only. The applied chemo-dynamical method includes star formation, stellar energetic and chemical feedback, and gas physical processes.After the onset of the simulation our models demonstrate the action of tidal effects and satellite merging on the star-formation rate of the satellites, their gas loss by means of hot-gas expansion, of ram-pressure and tidal stripping, and the tidal extraction of stars, leading to the formation of the stellar and gaseous galactic halo. We also analyze the evolution of the satellites’ mass function, their baryonic and DM mass distributions, chemical abundances, their compactness, their present-day appearance, etc. with respect to observations and present-day correlations.

  5. Formation of Jupiter-like Planets around Solar-type Stars

    NASA Astrophysics Data System (ADS)

    Boss, A. P.

    1995-12-01

    The gas giant planets of our solar system are believed to have formed through a two step process. First, collisional accumulation of a swarm of planetesimals produces a ~ 10 M_oplus core of ice and rock. Second, this core accretes an envelope of hydrogen and helium gas through the hydrodynamic collapse of disk gas onto the growing protoplanet. A necessary condition for the formation of gas giant planets is thus the presence of icy planetesimals, which cannot form inside the ice condensation radius of the disk at the time when planetary accumulation is occurring. The ice condensation radius in protoplanetary disk models thus sets a lower limit on the radius at which Jupiter-like planets could form. Radiative hydrodynamical models have been computed of the thermal structure of low mass protoplanetary disks orbiting a solar-mass protostar, with the disk being heated by mass accretion from the parent dense cloud core. These models predict that the midplane temperature falls below the ice condensation point ( ~ 160 K) only for radii of several AU or more, for a wide variety of disk masses (0.01 to 0.13 M_sun) and for a range of disk mass accretion rates ( ~ 10(-7) to ~ 10(-5) M_sun/yr). Variations in other parameters such as the radial density profile and the dust grain opacity have even less effect on temperatures. The location of the ice condensation radius is restricted to the range of ~ 3 AU to ~ 7 AU in these models. If the companion to 51 Peg (a solar-type star) is a gas giant planet, then the companion could not have formed at its present radius of ~ 0.05 AU, but must have suffered significant orbital evolution after its formation. A likely cause of such orbital decay is gravitational interaction between the companion and a protoplanetary disk that evidently survived longer than the solar nebula did.

  6. OT2_jkauff01_3: Maddalena's Cloud: A unique Laboratory for Early Evolutionary Stages of massive GMCs?

    NASA Astrophysics Data System (ADS)

    Kauffmann, J.

    2011-09-01

    We propose to establish the evolutionary state of Maddalena's Cloud. This region is regularly discussed as a prototype for a giant molecular cloud (GMC) in an early phase of its life. This suggestion is based on the fact that this region of about 3x10^5 M_sun is entirely devoid of embedded massive stars. Thus, this region potentially presents an ideal site to study the initial conditions for the evolution towards clouds like Orion A. This is not entirely clear, though: it has also been argued that this cloud might be at the end of its life, and is now dispersing after being "stirred up" by previous star formation. We therefore propose to execute two complementary experiments to establish the cloud's evolutionary status. Both will use wide-field parallel mode SPIRE/PACS dust emission maps. First, we will obtain the first reliable estimates for the mass of the cloud and its clumps to revise the --- presently very uncertain --- virial analysis on which suggestions for cloud dispersal are based. Second, we will search for deeply embedded young stellar objects (YSOs): if these very young (class 0-I) YSOs exist throughout the cloud, it would be hard to argue that this is a cloud in which star formation is ending. Depending on these experiments, our data will then be used to constrain the physical conditions in the early life of massive GMCs. Certainly, the properties of this cloud are unique: we only expect to find about 6 such massive clouds without O stars within 2.2kpc from sun. This is the only cloud of this sort we presently know, and so our observations will have a significant legacy value for studies of star formation.

  7. A neutral hydrogen cavity in M101: expanding supershell evacuated by multiple supernovae

    NASA Astrophysics Data System (ADS)

    Ray, Alak; Chakraborti, Sayan

    2015-08-01

    A subset of neutral hydrogen (H I) cavities detected in our Milkyway galaxy and other nearby star forming galaxies may represent expanding supershells driven by the combined mechanical feedback from multiple supernovae occurring in OB associations. However, most extragalactic H I cavities do not have a demonstrated expansion velocity nor an identified OB association inside them. In the nearby, face-on spiral galaxy M101, an unbroken expanding H I supershell was found with a UV-emitting young stellar association inside it. From The HI Nearby Galaxy Survey (THINGS) datacubes (undertaken at the NRAO Very Large Array, VLA) to study the H I emission from nearby galaxies, we measured its size to be about 500 pc and expansion velocity of 20 km/s by identifying its approaching and receding components in the position velocity space, using 21 cm emission spectroscopy. This H I cavity provides us with an ideal system to test the theory of supershells driven by the mechanical feedback from multiple Supernovae, advanced by McCray and Kafatos. We compared the UV emission of the cluster inside the supershell with simulated spectral energy distribution of synthetic clusters of the appropriate age (~15 Myr) and found that the observed UV flux is consistent with an association of mass (~10^5 MSun) required by the energy budget of the supershell. Supershell characteristics of this galaxy can be used to infer the neutral hydrogen scale height and mean neutral hydrogen density in the disk of M101. Another UV-emitting stellar association in the overdense swept-up gas in the supershell is found and this will be discussed in the context of propagating star formation. Spatially resolved integral field spectroscopy may determine the metallicity enrichment of the gas and the true age of the stellar population and has the potential to reveal the role of multiple stellar populations within the cavity.

  8. Moments of inertia for neutron and strange stars: Limits derived for the Crab pulsar

    NASA Astrophysics Data System (ADS)

    Bejger, M.; Haensel, P.

    2002-12-01

    Recent estimates of the properties of the Crab nebula are used to derive constraints on the moment of inertia, mass and radius of the pulsar. To this purpose, we employ an approximate formula combining these three parameters. Our ``empirical formula'' I =~ a(x) M R2, where x=(M/Msun) (km/R), is based on numerical results obtained for thirty theoretical equations of state of dense matter. The functions a(x) for neutron stars and strange stars are qualitatively different. For neutron stars aNS(x)=x/(0.1+2x) for x<=0.1 (valid for M>0.2 Msun) and aNS(x)={2/ 9}(1+5x) for x>0.1. For strange stars aSS(x)={2/ 5}(1+x) (not valid for strange stars with crust and M<0.1 Msun). We obtain also an approximate expression for the maximum moment of inertia Imax,45 =~ (-0.37 + 7.12* xmax) (Mmax/Msun)(RM_max/ {10 km})2, where I45 = I/1045 g* cm2, valid for both neutron stars and strange stars. Applying our formulae to the evaluated values of ICrab, we derive constraints on the mass and radius of the pulsar. { A very conservative evaluation of the expanding nebula mass, Mneb=2 Msun, yields MCrab>1.2 Msun and RCrab= 10-14 km. Setting the most recent evaluation (``central value'') Mneb=4.6 Msun rules out most of the existing equations of state, leaving only the stiffest ones: MCrab>1.9 Msun, RCrab= 14-15 km.

  9. Separated Fringe Packet Binary Star Astrometry at the CHARA Array - An Update

    NASA Astrophysics Data System (ADS)

    Ten Brummelaar, Theo; Farrington, C. D.; Mason, B. D.; Roberts, L. C.; Turner, N. H.

    2014-01-01

    When observed with optical long-baseline interferometers (OLBI), components of a binary star which are sufficiently separated such that their interferometric fringe packets do not overlap are referred to as Separated Fringe Packet (SFP) binaries. At the CHARA Array these `wide' binaries are in the range of a few tens of milliarcseconds and extend out into the regime of systems resolved by speckle interferometry at single, large-aperture telescopes. These SFP measurements can provide additional data for orbits lacking good phase coverage, help constrain elements of already established orbits, and locate new binaries in the under-sampled regime between the bounds of spectroscopic surveys and speckle interferometry. Unlike binary stars whose fringes overlap, a visibility calibration star is not needed, and the separation of the fringe packets can provide an accurate vector separation. We apply the SFP approach to Omega Andromeda, HD 178911, and Xi Cephei. For these systems we determine masses for the two components of 0.963+/-0.049 M_{sun}; and 0.860+/-0.051 M_{sun}; and an orbital parallax of 39.54+/-1.85 mas for Omega Andromeda, for HD 178911 masses of 0.802+/-0.055 M_{sun}; and 0.622+/-0.053 M_{sun}; with orbital parallax of 28.26+/-1.70 mas, and masses of 1.045+/-0.031 M_{sun}; and 0.408+/-0.066 M_{sun}; orbital parallax of 38.10+/-2.81 mas for Xi Cephei.

  10. An estimate of the terrestrial carbon budget of Russia using inventory-based, eddy covariance and inversion methods

    NASA Astrophysics Data System (ADS)

    Dolman, A. J.; Shvidenko, A.; Schepaschenko, D.; Ciais, P.; Tchebakova, N.; Chen, T.; van der Molen, M. K.; Belelli Marchesini, L.; Maximov, T. C.; Maksyutov, S.; Schulze, E.-D.

    2012-12-01

    We determine the net land to atmosphere flux of carbon in Russia, including Ukraine, Belarus and Kazakhstan, using inventory-based, eddy covariance, and inversion methods. Our high boundary estimate is -342 Tg C yr-1 from the eddy covariance method, and this is close to the upper bounds of the inventory-based Land Ecosystem Assessment and inverse models estimates. A lower boundary estimate is provided at -1350 Tg C yr-1 from the inversion models. The average of the three methods is -613.5 Tg C yr-1. The methane emission is estimated separately at 41.4 Tg C yr-1. These three methods agree well within their respective error bounds. There is thus good consistency between bottom-up and top-down methods. The forests of Russia primarily cause the net atmosphere to land flux (-692 Tg C yr-1 from the LEA. It remains however remarkable that the three methods provide such close estimates (-615, -662, -554 Tg C yr-1) for net biome production (NBP), given the inherent uncertainties in all of the approaches. The lack of recent forest inventories, the few eddy covariance sites and associated uncertainty with upscaling and undersampling of concentrations for the inversions are among the prime causes of the uncertainty. The dynamic global vegetation models (DGVMs) suggest a much lower uptake at -91 Tg C yr-1, and we argue that this is caused by a high estimate of heterotrophic respiration compared to other methods.

  11. Reactive nitrogen emissions from crop and livestock farming in India

    NASA Astrophysics Data System (ADS)

    Aneja, Viney P.; Schlesinger, William H.; Erisman, Jan Willem; Behera, Sailesh N.; Sharma, Mukesh; Battye, William

    2012-02-01

    The rapid increase in anthropogenic nitrogen emissions to the atmosphere is matter of concern for the environment, as these may lead to photochemical air pollution, reduced visibility, eutrophication of surface waters, changes in biodiversity, acid rain, stratospheric ozone depletion, and global warming. In this study, ambient emissions of reactive nitrogen (ammonia and nitrous oxide) from animal and crop farming are analyzed for the base year 2003. This objective was achieved by the systematic development of a spatially resolved emissions inventory on a Geographic Information System (GIS) platform. Emissions of ammonia (NH 3) and nitrous oxide (N 2O) were estimated: (i) from livestock; 1705 Gg/yr and 214 Gg yr -1 and (ii) fertilizer applications; 2697 Gg yr -1 and 326 Gg yr -1. These estimated emissions were compared and contrasted with global, U.S., and European emissions of reactive nitrogen; emissions from India were second only to China. From the spatially resolved emission inventory, it was observed that the state of Uttar Pradesh has the highest NH 3 emission (522 Gg yr -1) followed by the state of Maharashtra (425 Gg yr -1) both from animal and crop farming. Similarly the State of Uttar Pradesh has the highest N 2O emission (70 Gg yr -1) followed by the state of Maharashtra (47 Gg yr -1).

  12. Mid-IR and radio images of IC 418: dust in a young planetary nebula.

    NASA Astrophysics Data System (ADS)

    Meixner, M.; Skinner, C. J.; Keto, E.; Zijlstra, A.; Hoare, M. G.; Arens, J. F.; Jernigan, J. G.

    1996-09-01

    " radius. This structure may suggest a mass loss history for IC 418 in which its progenitor AGB star experienced a superwind (˙(M)~4x10^-5^Msun_/yr, v~11km/s) just before departing the AGB.

  13. Exchanges of sediment between the flood plain and channel of the Amazon River in Brazil

    USGS Publications Warehouse

    Dunne, T.; Mertes, L.A.K.; Meade, R.H.; Richey, J.E.; Forsberg, B.R.

    1998-01-01

    Sediment transport through the Brazilian sector of the Amazon River valley, a distance of 2010 km, involves exchanges between the channel and the flood plain that in each direction exceed the annual flux of sediment out of the river at O??bidos (???1200 Mt yr-1). The exchanges occur through bank erosion, bar deposition, settling from diffuse overbank flow, and sedimentation in flood-plain channels. We estimated the magnitude of these exchanges for each of 10 reaches of the valley, and combined them with calculations of sediment transport into and out of the reaches based on sediment sampling and flow records to define a sediment budget for each reach. Residuals in the sediment budget of a reach include errors of estimation and erosion or deposition within the channel. The annual supply of sediment entering the channel from bank erosion was estimated to average 1570 Mt yr-1 (1.3 ?? the O??bidos flux) and the amount transferred from channel transport to the bars (380 Mt yr-1) and the flood plain (460 Mt yr-1 in channelized flow; 1230 Mt yr-1 in diffuse overbank flow) totaled 2070 Mt yr-1 (1.7 ?? the O??bidos flux). Thus, deposition on the bars and flood plain exceeded bank erosion by 500 Mt yr-1 over a 10-16 yr period. Sampling and calculation of sediment loads in the channel indicate a net accumulation in the valley floor of approximately 200 Mt yr-1 over 16 yr, crudely validating the process-based calculations of the sediment budget, which in turn illuminate the physical controls on each exchange process. Another 300-400 Mt yr-1 are deposited in a delta plain downstream of O??bidos. The components of the sediment budget reflect hydrologie characteristics of the valley floor and geomorphic characteristics of the channel and flood plain, which in turn are influenced by tectonic features of the Amazon structural trough.

  14. Biogenic carbon fluxes from global agricultural production and consumption

    SciTech Connect

    Wolf, Julie; West, Tristram O.; Le Page, Yannick LB; Kyle, G. Page; Zhang, Xuesong; Collatz, George; Imhoff, Marc L.

    2015-10-01

    Quantification of biogenic carbon fluxes from agricultural lands is needed to generate comprehensive bottom-up estimates of net carbon exchange for global and regional carbon monitoring. We estimated global agricultural carbon fluxes associated with annual crop net primary production (NPP), harvested biomass, and consumption of biomass by humans and livestock. These estimates were combined for a single estimate of net carbon exchange (NCE) and spatially distributed to 0.05 degree resolution using MODIS satellite land cover data. Global crop NPP in 2011 was estimated at 5.25 ± 0.46 Pg C yr-1, of which 2.05 ± 0.05 Pg C yr-1 was harvested and 0.54 Pg C yr-1 was collected from crop residues for livestock fodder. Total livestock feed intake in 2011 was 2.42 ± 0.21 Pg C yr-1, of which 2.31 ± 0.21 Pg C yr-1 was emitted as CO2, 0.07 ± 0.01 Pg C yr-1 was emitted as CH4, and 0.04 Pg C yr-1 was contained within milk and egg production. Livestock grazed an estimated 1.27 Pg C yr-1 in 2011, which constituted 52.4% of total feed intake. Global human food intake was 0.57 ± 0.03 Pg C yr-1 in 2011, the majority of which is respired as CO2. Completed global cropland carbon budgets accounted for the ultimate use of ca. 80% of harvested biomass. The spatial distribution of these fluxes may be used for global carbon monitoring, estimation of regional uncertainty, and for use as input to Earth system models.

  15. Biogenic carbon fluxes from global agricultural production and consumption

    NASA Astrophysics Data System (ADS)

    Wolf, Julie; West, Tristram O.; Le Page, Yannick; Kyle, G. Page; Zhang, Xuesong; Collatz, G. James; Imhoff, Marc L.

    2015-10-01

    Quantification of biogenic carbon fluxes from agricultural lands is needed to generate comprehensive bottom-up estimates of net carbon exchange for global and regional carbon monitoring. We estimated global agricultural carbon fluxes associated with annual crop net primary production (NPP), harvested biomass, and consumption of biomass by humans and livestock. These estimates were combined for a single estimate of net carbon exchange and spatially distributed to 0.05° resolution using Moderate Resolution Imaging Spectroradiometer satellite land cover data. Global crop NPP in 2011 was estimated at 5.25 ± 0.46 Pg C yr-1, of which 2.05 ± 0.05 Pg C yr-1 was harvested and 0.54 Pg C yr-1 was collected from crop residues for livestock fodder. Total livestock feed intake in 2011 was 2.42 ± 0.21 Pg C yr-1, of which 2.31 ± 0.21 Pg C yr-1 was emitted as CO2, 0.07 ± 0.01 Pg C yr-1 was emitted as CH4, and 0.04 Pg C yr-1 was contained within milk and egg production. Livestock grazed an estimated 1.27 Pg C yr-1 in 2011, which constituted 52.4% of total feed intake. Global human food intake was 0.57 ± 0.03 Pg C yr-1 in 2011, the majority of which was respired as CO2. Completed global cropland carbon budgets accounted for the ultimate use of approximately 80% of harvested biomass. The spatial distribution of these fluxes may be used for global carbon monitoring, estimation of regional uncertainty, and for use as input to Earth system models.

  16. Offshore influence of coastal upwelling off Mauritania, NW Africa, as recorded by diatoms in sediment traps at 2195 m water depth

    NASA Astrophysics Data System (ADS)

    Lange, Carina B.; Romero, Oscar E.; Wefer, Gerold; Gabric, Albert J.

    1998-06-01

    Downward flux and taxonomic composition of diatom and silicoflagellate assemblages were determined from sediment trap samples off Cap Blanc (CB1, NW Africa) over a 1-year period (March 1988-March 1989) and compared to the assemblages in the underlying surface sedi ment. Trap content was composed of biogenic and lithogenic material. The dominant constituents of the biogenic fraction were calcium carbonate, biogenic opal, and organic matter. Coccolithophorids, planktonic foraminifera and pteropods contributed to the CaCO 3 flux; opal derived mainly from diatoms. During the sampling year prominent total flux maxima occurred in spring and summer. Highest diatom flux values were reached in March-April (20.1×10 5 valves m -2 d -1) and July-August (22.9×10 5 valves m -2 d -1) in coincidence with the total flux pattern. Radiolaria showed three distinct peaks: in autumn (16×10 4 shells m -2 d -1), spring (˜11×10 4 shells m -2 d -1) and summer (10×10 4 shells m -2 d -1). The flux pattern of silicoflagellates differed greatly from those of the other groups and from the total particle flux, with highest values between October 1988 and March 1989. For all microorganisms surveyed, September was the month of lowest production. We identified a total of 166 diatom taxa and 3 silicoflagellate species. Off Cap Blanc, upwelling occurs year-round, and "giant filaments" of relatively high pigment concentration develop and persist throughout the year with substantial seasonal and interannual variations. We show that the shifts in siliceous phytoplankton do reflect both the seaward displacement of the coastal upwelling center and the periods of relaxation when oligotrophic waters prevail. Accumulation rates in the surface sediment were calculated to be 1.36×10 8 valves m -2 yr -1 for diatoms and 1.05×10 6 skeletons m -2 yr -1 for silicoflagellates. Most of the diatoms found in the water column at 2195 m also occurred in the sediment surface, with a slight enrichement of robust

  17. A detailed view of the gas shell around R Sculptoris with ALMA

    NASA Astrophysics Data System (ADS)

    Maercker, M.; Vlemmings, W. H. T.; Brunner, M.; De Beck, E.; Humphreys, E. M.; Kerschbaum, F.; Lindqvist, M.; Olofsson, H.; Ramstedt, S.

    2016-02-01

    Context. During the asymptotic giant branch (AGB) phase, stars undergo thermal pulses - short-lived phases of explosive helium burning in a shell around the stellar core. Thermal pulses lead to the formation and mixing-up of new elements to the stellar surface. They are hence fundamental to the chemical evolution of the star and its circumstellar envelope. A further consequence of thermal pulses is the formation of detached shells of gas and dust around the star, several of which have been observed around carbon-rich AGB stars. Aims: We aim to determine the physical properties of the detached gas shell around R Sculptoris, in particular the shell mass and temperature, and to constrain the evolution of the mass-loss rate during and after a thermal pulse. Methods: We analyse 12CO(1-0), 12CO(2-1), and 12CO(3-2) emission, observed with the Atacama Large Millimeter/submillimeter Array (ALMA) during Cycle 0 and complemented by single-dish observations. The spatial resolution of the ALMA data allows us to separate the detached shell emission from the extended emission inside the shell. We perform radiative transfer modelling of both components to determine the shell properties and the post-pulse mass-loss properties. Results: The ALMA data show a gas shell with a radius of 19.̋5 expanding at 14.3 km s-1. The different scales probed by the ALMA Cycle 0 array show that the shell must be entirely filled with gas, contrary to the idea of a detached shell. The comparison to single-dish spectra and radiative transfer modelling confirms this. We derive a shell mass of 4.5 × 10-3 M⊙ with a temperature of 50 K. Typical timescales for thermal pulses imply a pulse mass-loss rate of 2.3 × 10-5 M⊙ yr-1. For the post-pulse mass-loss rate, we find evidence for a gradual decline of the mass-loss rate, with an average value of 1.6 × 10-5 M⊙ yr-1. The total amount of mass lost since the last thermal pulse is 0.03 M⊙, a factor four higher compared to classical models, with a

  18. First combined flux chamber survey of mercury and CO2 emissions from soil diffuse degassing at Solfatara of Pozzuoli crater, Campi Flegrei (Italy): Mapping and quantification of gas release

    NASA Astrophysics Data System (ADS)

    Bagnato, E.; Barra, M.; Cardellini, C.; Chiodini, G.; Parello, F.; Sprovieri, M.

    2014-12-01

    There have been limited studies to date targeting gaseous elemental mercury (GEM) flux from soil emission in enriched volcanic substrates and its relation with CO2 release and tectonic structures. In order to evaluate and understand the processes of soil-air exchanges involved at Solfatara of Pozzuoli volcano, the most active zone of Campi Flegrei caldera (Italy), an intensive field measurement survey has been achieved in September 2013 by using high-time resolution techniques. Soil-air exchange fluxes of GEM and CO2 have been measured simultaneously at 116 points, widely distributed within the crater. Quantification of gas flux has been assessed by using field accumulation chamber method in conjunction with a Lumex®-RA 915 + portable mercury vapor analyzer and a LICOR for CO2 determination, respectively. The spatial distribution of GEM and CO2 emissions correlated quite closely with the hydrothermal and geological features of the studied area. The highest GEM fluxes (from 4.04 to 5.9 × 10- 5 g m- 2 d- 1) were encountered close to the southern part of the crater interested by an intense fumarolic activity and along the SE-SW tectonic fracture (1.26 × 10- 6-6.91 × 10- 5 g GEM m- 2 d- 1). Conversely, the lowest values have been detected all along the western rim of the crater, characterized by a weak gas flux and a lush vegetation on a very sealed clay soil, which likely inhibited mercury emission (range: 1.5 × 10- 7-7.18 × 10- 6 g GEM m- 2 d- 1). Results indicate that the GEM exchange between soil and air inside the Solfatara crater is about 2-3 orders of magnitude stronger than that in the background areas (10- 8-10- 7 g m- 2 d- 1). CO2 soil diffuse degassing exhibited an analogous spatial pattern to the GEM fluxes, with emission rates ranging from about 15 to ~ 20,000 g CO2 m- 2 d- 1, from the outermost western zones to the south-eastern sector of the crater. The observed significant correlation between GEM and CO2 suggested that in volcanic system GEM

  19. On the Nature of the Prototype Luminous Blue Variable Ag Carinae. I. Fundamental Parameters During Visual Minimum Phases and Changes in the Bolometric Luminosity During the S-Dor Cycle

    NASA Astrophysics Data System (ADS)

    Groh, J. H.; Hillier, D. J.; Damineli, A.; Whitelock, P. A.; Marang, F.; Rossi, C.

    2009-06-01

    We present a detailed spectroscopic analysis of the luminous blue variable (LBV) AG Carinae (AG Car) during the last two visual minimum phases of its S-Dor cycle (1985-1990 and 2000-2003). The analysis reveals an overabundance of He, N, and Na, and a depletion of H, C, and O, on the surface of the AG Car, indicating the presence of a CNO-processed material. Furthermore, the ratio N/O is higher on the stellar surface than in the nebula. We found that the minimum phases of AG Car are not equal to each other, since we derived a noticeable difference between the maximum effective temperature achieved during 1985-1990 (22, 800 K) and 2000-2001 (17,000 K). Significant differences between the wind parameters in these two epochs were also noticed. While the wind terminal velocity was 300 km s-1 in 1985-1990, it was as low as 105 km s-1 in 2001. The mass-loss rate, however, was lower from 1985-1990 (1.5 × 10-5 M sun yr-1) than from 2000-2001 (3.7 × 10-5 M sun yr-1). We found that the wind of AG Car is significantly clumped (f sime 0.10-0.25) and that clumps must be formed deep in the wind. We derived a bolometric luminosity of 1.5 × 106 L sun during both minimum phases which, contrary to the common assumption, decreases to 1.0 × 106 L sun as the star moves toward the maximum flux in the V band. Assuming that the decrease in the bolometric luminosity of AG Car is due to the energy used to expand the outer layers of the star, we found that the expanding layers contain roughly 0.6-2 M sun. Such an amount of mass is an order of magnitude lower than the nebular mass around AG Car, but is comparable to the nebular mass found around lower-luminosity LBVs and to that of the Little Homunculus of Eta Car. If such a large amount of mass is indeed involved in the S Dor-type variability, we speculate that such instability could be a failed Giant Eruption, with several solar masses never becoming unbound from the star. Based on observations made with the 1.6 m telescope at the

  20. Atmospheric CO2 source and sink patterns over the Indian region

    NASA Astrophysics Data System (ADS)

    Fadnavis, Suvarna; Kumar, K. Ravi; Tiwari, Yogesh K.; Pozzoli, Luca

    2016-02-01

    In this paper we examine CO2 emission hot spots and sink regions over India as identified from global model simulations during the period 2000-2009. CO2 emission hot spots overlap with locations of densely clustered thermal power plants, coal mines and other industrial and urban centres; CO2 sink regions coincide with the locations of dense forest. Fossil fuel CO2 emissions are compared with two bottom-up inventories: the Regional Emission inventories in ASia (REAS v1.11; 2000-2009) and the Emission Database for Global Atmospheric Research (EDGAR v4.2) (2000-2009). Estimated fossil fuel emissions over the hot spot region are ˜ 500-950 gC m-2 yr-1 as obtained from the global model simulation, EDGAR v4.2 and REAS v1.11 emission inventory. Simulated total fluxes show increasing trends, from 1.39 ± 1.01 % yr-1 (19.8 ± 1.9 TgC yr-1) to 6.7 ± 0.54 % yr-1 (97 ± 12 TgC yr-1) over the hot spot regions and decreasing trends of -0.95 ± 1.51 % yr-1 (-1 ± 2 TgC yr-1) to -5.7 ± 2.89 % yr-1 (-2.3 ± 2 TgC yr-1) over the sink regions. Model-simulated terrestrial ecosystem fluxes show decreasing trends (increasing CO2 uptake) over the sink regions. Decreasing trends in terrestrial ecosystem fluxes imply that forest cover is increasing, which is consistent with India State of Forest Report (2009). Fossil fuel emissions show statistically significant increasing trends in all the data sets considered in this study. Estimated trend in simulated total fluxes over the Indian region is ˜ 4.72 ± 2.25 % yr-1 (25.6 TgC yr-1) which is slightly higher than global growth rate ˜ 3.1 % yr-1 during 2000-2010.

  1. Nitrous oxide fluxes from three forest types of the tropical mountain rainforests on Hainan Island, China

    NASA Astrophysics Data System (ADS)

    Bai, Zhenzhi; Yang, Gang; Chen, Huai; Zhu, Qiuan; Chen, Dexiang; Li, Yide; Wang, Xu; Wu, Zhongmin; Zhou, Guangyi; Peng, Changhui

    2014-08-01

    Tropical rainforest soil is an important source of atmospheric nitrous oxide (N2O). However, there is still considerable uncertainty about the spatial and temporal variability of N2O fluxes. To understand these fluxes, we quantified the annual N2O emissions from three tropical mountain rainforests (primary mountain rainforest, PMR; secondary mountain rainforest, SMR; and Podocarpus imbricatus plantation, PIP) in the Jianfengling National Natural Reserve on Hainan Island, China. The average of N2O emissions in this area was 2.52 ± 0.33 kg N-N2O ha-1 yr-1 (3.52 kg N-N2O ha-1 yr-1 in the wet season and 1.62 kg N-N2O ha-1 yr-1 in the dry season) during our study period, with highly seasonal variations. The mean N2O emission rates were significantly higher during the wet season (68% of the total average) than the dry season (32% of the total average) (P < 0.05). PIP had the highest N2O emission rate at 3.49 ± 0.61 kg N-N2O ha-1 yr-1 (4.74 kg N-N2O ha-1 yr-1 in the wet season and 2.32 kg N-N2O ha-1 yr-1 in the dry season), followed by SMR at 3.03 ± 0.64 kg N-N2O ha-1 yr-1 (4.16 kg N-N2O ha-1 yr-1 in the wet season and 1.97 kg N-N2O ha-1 yr-1 in the dry season), and then PMR at 1.53 ± 0.49 kg N-N2O ha-1 yr-1 (2.21 kg N-N2O ha-1 yr-1 in the wet season and 0.94 kg N-N2O ha-1 yr-1 in the dry season). We observed a significant Gaussian relationship between the N2O fluxes and soil temperature for SMR and PIP but no significant relationship in PMR. There was a significant exponential relationship between the N2O fluxes and water filled pore space (WFPS) in SMR and PIP but not in PMR.

  2. The central parsecs of M87: jet emission and an elusive accretion disc

    NASA Astrophysics Data System (ADS)

    Prieto, M. A.; Fernández-Ontiveros, J. A.; Markoff, S.; Espada, D.; González-Martín, O.

    2016-04-01

    We present the first simultaneous spectral energy distribution (SED) of M87 core at a scale of 0.4 arcsec ( ˜ 32 pc) across the electromagnetic spectrum. Two separate, quiescent, and active states are sampled that are characterized by a similar featureless SED of power-law form, and that are thus remarkably different from that of a canonical active galactic nuclei or a radiatively inefficient accretion source. We show that the emission from a jet gives an excellent representation of the core of M87 core covering ten orders of magnitude in frequency for both the active and the quiescent phases. The inferred total jet power is, however, one to two orders of magnitude lower than the jet mechanical power reported in the literature. The maximum luminosity of a thin accretion disc allowed by the data yields an accretion rate of < 6 × 10- 5 M⊙ yr- 1, assuming 10 per cent efficiency. This power suffices to explain M87 radiative luminosity at the jet frame, it is however two to three order of magnitude below that required to account for the jet's kinetic power. The simplest explanation is variability, which requires the core power of M87 to have been two to three orders of magnitude higher in the last 200 yr. Alternatively, an extra source of power may derive from black hole spin. Based on the strict upper limit on the accretion rate, such spin power extraction requires an efficiency an order of magnitude higher than predicted from magnetohydrodynamic simulations, currently in the few hundred per cent range.

  3. Accreting pre-main-sequence models and abundance anomalies in globular clusters

    NASA Astrophysics Data System (ADS)

    Tognelli, E.; Prada Moroni, P. G.; Degl'Innocenti, S.

    2015-12-01

    We investigated the possibility of producing helium-enhanced stars in globular clusters by accreting polluted matter during the pre-main-sequence phase. We followed the evolution of two different classes of pre-main-sequence accreting models, one which neglects and the other that takes into account the protostellar evolution. We analysed the dependence of the final central helium abundance, of the tracks position in the HR diagram and of the surface lithium abundance evolution on the age at which the accretion of polluted material begins and on the main physical parameters that govern the protostellar evolution. The later is the beginning of the late accretion and the lower are both the central helium and the surface lithium abundances at the end of the accretion phase and in Zero Age Main Sequence (ZAMS). In order to produce a relevant increase of the central helium content the accretion of polluted matter should start at ages lower than 1 Myr. The inclusion of the protostellar evolution has a strong impact on the ZAMS models too. The adoption of a very low seed mass (i.e. 0.001 M⊙) results in models with the lowest central helium and surface lithium abundances. The higher is the accretion rate and the lower is the final helium content in the core and the residual surface lithium. In the worst case - i.e. seed mass 0.001 M⊙ and accretion rate ≥10-5 M⊙ yr-1 - the central helium is not increased at all and the surface lithium is fully depleted in the first few million years.

  4. Hydrogen consumption by methanogens on the early Earth.

    PubMed

    Kral, T A; Brink, K M; Miller, S L; McKay, C P

    1998-06-01

    It is possible that the first autotroph used chemical energy rather than light. This could have been the main source of primary production after the initial inventory of abiotic organic material had been depleted. The electron acceptor most readily available for use by this first chemoautotroph would have been CO2. The most abundant electron donor may have been H2 that would have been outgassing from volcanoes at a rate estimated to be as large as 10(12) moles yr-1, as well as from photo-oxidation of Fe+2. We report here that certain methanogens will consume H2 down to partial pressures as low as 4 Pa (4 x 10(-5) atm) with CO2 as the sole carbon source at a rate of 0.7 ng H2 min-1 microgram-1 cell protein. The lower limit of pH2 for growth of methanogens can be understood on the basis that the pH2 needs to be high enough for one ATP to be synthesized per CO2 reduced. The pH2 values needed for growth measured here are consistent with those measured by Stevens and McKinley for growth of methanogens in deep basalt aquifers. H2-consuming autotrophs are likely to have had a profound effect on the chemistry of the early atmosphere and to have been a dominant sink for H2 on the early Earth after life began rather than escape from the Earth's atmosphere to space. PMID:9611769

  5. The X-ray light curve of the massive colliding wind Wolf-Rayet + O binary WR 21a

    NASA Astrophysics Data System (ADS)

    Gosset, Eric; Nazé, Yaël

    2016-05-01

    Our dedicated XMM-Newton monitoring, as well as archival Chandra and Swift datasets, were used to examine the behaviour of the WN5h+O3V binary WR 21a at high energies. For most of the orbit, the X-ray emission exhibits few variations. However, an increase in strength of the emission is seen before periastron, following a 1 /D relative trend, where D is the separation between both components. This increase is rapidly followed by a decline due to strong absorption as the Wolf-Rayet (WR) comes in front. The fitted local absorption value appears to be coherent with a mass-loss rate of about 1 × 10-5 M⊙ yr-1 for the WR component. However, absorption is not the only parameter affecting the X-ray emission at periastron as even the hard X-ray emission decreases, suggesting a possible collapse of the colliding wind region near to or onto the photosphere of the companion just before or at periastron. An eclipse may appear as another potential scenario, but it would be in apparent contradiction with several lines of evidence, notably the width of the dip in the X-ray light curve and the absence of variations in the UV light curve. Afterwards, the emission slowly recovers, with a strong hysteresis effect. The observed behaviour is compatible with predictions from general wind-wind collision models although the absorption increase is too shallow. Based on observations collected at ESO as well as with Swift, Chandra, and the ESA science mission XMM-Newton, an ESA Science Mission with instruments and contributions directly funded by ESA Member States and the USA (NASA).

  6. Fire-induced Carbon Emissions and Regrowth Uptake in Western U.S. Forests: Documenting Variation Across Forest Types, Fire Severity, and Climate Regions

    NASA Technical Reports Server (NTRS)

    Ghimire, Bardan; Williams, Christopher A.; Collatz, George James; Vanderhoof, Melanie

    2012-01-01

    The forest area in the western United States that burns annually is increasing with warmer temperatures, more frequent droughts, and higher fuel densities. Studies that examine fire effects for regional carbon balances have tended to either focus on individual fires as examples or adopt generalizations without considering how forest type, fire severity, and regional climate influence carbon legacies. This study provides a more detailed characterization of fire effects and quantifies the full carbon impacts in relation to direct emissions, slow release of fire-killed biomass, and net carbon uptake from forest regrowth. We find important variations in fire-induced mortality and combustion across carbon pools (leaf, live wood, dead wood, litter, and duff) and across low- to high-severity classes. This corresponds to fire-induced direct emissions from 1984 to 2008 averaging 4 TgC/yr and biomass killed averaging 10.5 TgC/yr, with average burn area of 2723 sq km/yr across the western United States. These direct emission and biomass killed rates were 1.4 and 3.7 times higher, respectively, for high-severity fires than those for low-severity fires. The results show that forest regrowth varies greatly by forest type and with severity and that these factors impose a sustained carbon uptake legacy. The western U.S. fires between 1984 and 2008 imposed a net source of 12.3 TgC/yr in 2008, accounting for both direct fire emissions (9.5 TgC/yr) and heterotrophic decomposition of fire-killed biomass (6.1 TgC yr1) as well as contemporary regrowth sinks (3.3 TgC/yr). A sizeable trend exists toward increasing emissions as a larger area burns annually.

  7. A new dust budget in the Large Magellanic Cloud

    NASA Astrophysics Data System (ADS)

    Zhu, Chunhua; Lü, Guoliang; Wang, Zhaojun

    2015-08-01

    The origin of dust in a galaxy is poorly understood. Recently, surveys of the Large Magellanic Cloud (LMC) have provided astrophysical laboratories for dust studies. Using a method of population synthesis, we investigate the contributions of dust produced by asymptotic giant branch (AGB) stars, common envelope (CE) ejecta and Type II supernovae (SNe II) to the total dust budget in the LMC. Based on our models, the dust production rates (DPRs) of AGB stars in the LMC are between about 2.5 × 10-5 and 4.0 × 10-6 M⊙ yr-1. The uncertainty mainly results from different models for the dust yields of AGB stars. The DPRs of CE ejecta are about 6.3 × 10-6 (the initial binary fraction is 50 per cent). These results are within the large scatter of several observational estimates. AGB stars mainly produce carbon grains, which is consistent with observations. Most of the dust grains manufactured by CE ejecta are silicate and iron grains. The contributions of SNe II are very uncertain. Compared with SNe II without reverse shock, the DPRs of AGB stars and CE ejecta are negligible. However, if only 2 per cent of dust grains produced by SNe II can survive after reverse shock, the contributions of SNe II are very small. The total dust masses produced by AGB stars in the LMC are between 2.8 × 104 and 3.2 × 105 M⊙, and those produced by CE ejecta are about 6.3 × 104. They are much lower than the values estimated by observations. Therefore, there should be other dust sources in the LMC.

  8. Super-Eddington wind scenario for the progenitors of type Ia supernovae: Accreting He-rich matter onto white dwarfs

    NASA Astrophysics Data System (ADS)

    Wang, B.; Li, Y.; Ma, X.; Liu, D.-D.; Cui, X.; Han, Z.

    2015-12-01

    Context. Supernovae of type Ia (SNe Ia) are believed to be thermonuclear explosions of carbon-oxygen white dwarfs (CO WDs). However, the mass accretion process onto CO WDs is still not completely understood. Aims: In this paper, we study the accretion of He-rich matter onto CO WDs and explore a scenario in which a strong wind forms on the surface of the WD if the total luminosity exceeds the Eddington limit. Methods: Using a stellar evolution code called modules for experiments in stellar astrophysics (MESA), we simulated the He accretion process onto CO WDs for WDs with masses of 0.6-1.35 M⊙ and various accretion rates of 10-8-10-5 M⊙ yr-1. Results: If the contribution of the total luminosity is included when determining the Eddington accretion rate, then a super-Eddington wind could be triggered at relatively lower accretion rates than those of previous studies based on steady-state models. The super-Eddington wind can prevent the WDs with high accretion rates from evolving into red-giant-like He stars. We found that the contributions from thermal energy of the WD are non-negligible, judging by our simulations, even though the nuclear burning energy is the dominating source of luminosity. We also provide the limits of the steady He-burning regime in which the WDs do not lose any accreted matter and increase their mass steadily, and calculated the mass retention efficiency during He layer flashes for various WD masses and accretion rates. These obtained results can be used in future binary population synthesis computations.

  9. Methane bubbling from northern lakes: present and future contributions to the global methane budget.

    PubMed

    Walter, Katey M; Smith, Laurence C; Chapin, F Stuart

    2007-07-15

    Large uncertainties in the budget of atmospheric methane (CH4) limit the accuracy of climate change projections. Here we describe and quantify an important source of CH4 -- point-source ebullition (bubbling) from northern lakes -- that has not been incorporated in previous regional or global methane budgets. Employing a method recently introduced to measure ebullition more accurately by taking into account its spatial patchiness in lakes, we estimate point-source ebullition for 16 lakes in Alaska and Siberia that represent several common northern lake types: glacial, alluvial floodplain, peatland and thermokarst (thaw) lakes. Extrapolation of measured fluxes from these 16 sites to all lakes north of 45 degrees N using circumpolar databases of lake and permafrost distributions suggests that northern lakes are a globally significant source of atmospheric CH4, emitting approximately 24.2+/-10.5Tg CH4yr(-1). Thermokarst lakes have particularly high emissions because they release CH4 produced from organic matter previously sequestered in permafrost. A carbon mass balance calculation of CH4 release from thermokarst lakes on the Siberian yedoma ice complex suggests that these lakes alone would emit as much as approximately 49000Tg CH4 if this ice complex was to thaw completely. Using a space-for-time substitution based on the current lake distributions in permafrost-dominated and permafrost-free terrains, we estimate that lake emissions would be reduced by approximately 12% in a more probable transitional permafrost scenario and by approximately 53% in a 'permafrost-free' Northern Hemisphere. Long-term decline in CH4 ebullition from lakes due to lake area loss and permafrost thaw would occur only after the large release of CH4 associated thermokarst lake development in the zone of continuous permafrost. PMID:17513268

  10. Gross Nitrogen Mineralization in Surface Sediments of the Yangtze Estuary.

    PubMed

    Lin, Xianbiao; Hou, Lijun; Liu, Min; Li, Xiaofei; Yin, Guoyu; Zheng, Yanling; Deng, Fengyu

    2016-01-01

    Nitrogen mineralization is a key biogeochemical process transforming organic nitrogen to inorganic nitrogen in estuarine and coastal sediments. Although sedimentary nitrogen mineralization is an important internal driver for aquatic eutrophication, few studies have investigated sedimentary nitrogen mineralization in these environments. Sediment-slurry incubation experiments combined with 15N isotope dilution technique were conducted to quantify the potential rates of nitrogen mineralization in surface sediments of the Yangtze Estuary. The gross nitrogen mineralization (GNM) rates ranged from 0.02 to 5.13 mg N kg(-1) d(-1) in surface sediments of the study area. The GNM rates were generally higher in summer than in winter, and the relative high rates were detected mainly at sites near the north branch and frontal edge of this estuary. The spatial and temporal distributions of GNM rates were observed to depend largely on temperature, salinity, sedimentary organic carbon and nitrogen contents, and extracellular enzyme (urease and L-glutaminase) activities. The total mineralized nitrogen in the sediments of the Yangtze Estuary was estimated to be about 6.17 × 10(5) t N yr(-1), and approximately 37% of it was retained in the estuary. Assuming the retained mineralized nitrogen is totally released from the sediments into the water column, which contributed 12-15% of total dissolved inorganic nitrogen (DIN) sources in this study area. This result indicated that the mineralization process is a significant internal nitrogen source for the overlying water of the Yangtze Estuary, and thus may contribute to the estuarine and coastal eutrophication. PMID:26991904

  11. Progenitors of Type IIB Supernovae in the Light of Radio and X-Rays from SN 2013DF

    NASA Astrophysics Data System (ADS)

    Kamble, Atish; Margutti, Raffaella; Soderberg, Alicia M.; Chakraborti, Sayan; Fransson, Claes; Chevalier, Roger; Powell, Diana; Milisavljevic, Dan; Parrent, Jerod; Bietenholz, Michael

    2016-02-01

    We present radio and X-ray observations of the nearby SN IIb 2013df in NGC 4414 from 10 to 250 days after the explosion. The radio emission showed a peculiar steep-to-shallow spectral evolution. We present a model in which inverse Compton cooling of synchrotron emitting electrons can account for the observed spectral and light curve evolution. A significant mass-loss rate, \\dot{M}≈ 8× {10}-5 {M}⊙ yr-1 for a wind velocity of 10 km s-1, is estimated from the detailed modeling of radio and X-ray emission, which are primarily due to synchrotron and bremsstrahlung, respectively. We show that SN 2013df is similar to SN 1993J in various ways. The shock wave speed of SN 2013df was found to be average among the radio supernovae; {v}{sh}/c˜ 0.07. We did not find any significant deviation from smooth decline in the light curve of SN 2013df. One of the main results of our self-consistent multiband modeling is the significant deviation from energy equipartition between magnetic fields and relativistic electrons behind the shock. We estimate {ɛ }e=200{ɛ }B. In general for SNe IIb, we find that the presence of bright optical cooling envelope emission is linked with free-free radio absorption and bright thermal X-ray emission. This finding suggests that more extended progenitors, similar to that of SN 2013df, suffer from substantial mass loss in the years before the supernova.

  12. Stellar and Gas Dynamical Model for Tidal Disruption Events in a Quiescent Galaxy

    NASA Astrophysics Data System (ADS)

    Mageshwaran, T.; Mangalam, A.

    2015-12-01

    A detailed model of the tidal disruption events (TDEs) has been constructed using stellar dynamical and gas dynamical inputs that include black hole (BH) mass M•, specific orbital energy E and angular momentum J, star mass M⋆ and radius R⋆, and the pericenter of the star orbit rp(E, J, M•). We solved the steady state Fokker-Planck equation using the standard loss cone theory for the galactic density profile ρ (r) ∝ r-γ and stellar mass function ξ(m) where m = M⋆/M⊙ and obtained the feeding rate of stars to the BH integrated over the phase space as {\\dot{N}}t\\propto {M}\\bullet {\\boldsymbol{β }}, where {\\boldsymbol{β }}=-0.3+/- 0.01 for M• > 107M⊙ and ˜6.8 × 10-5 Yr-1 for γ = 0.7. We use this to model the in-fall rate of the disrupted debris, \\dot{M}(E,J,m,t), and discuss the conditions for the disk formation, finding that the accretion disk is almost always formed for the fiduciary range of the physical parameters. We also find the conditions under which the disk formed from the tidal debris of a given star with a super Eddington accretion phase. We have simulated the light curve profiles in the relevant optical g band and soft X-rays for both super and sub-Eddington accretion disks as a function of \\dot{M}(E,J,t). Using this, standard cosmological parameters, and mission instrument details, we predict the detectable TDE rates for various forthcoming surveys as a function of γ.

  13. Forming Super-Massive Black Hole Seeds under the Influence of a Nearby Anisotropic Multi-Frequency Source

    NASA Astrophysics Data System (ADS)

    Regan, John A.; Johansson, Peter H.; Wise, John H.

    2016-04-01

    The photo-dissociation of {H_2} by a nearby anisotropic source of radiation is seen as a critical component in creating an environment in which a direct collapse black hole may form. Employing radiative transfer we model the effect of multi-frequency (0.76 eV - 60 eV) radiation on a collapsing halo at high redshift. We vary both the shape of the spectrum which emits the radiation and the distance to the emitting galaxy. We use blackbody spectra with temperatures of {T = 10^4 K} and {T = 10^5 K} and a realistic stellar spectrum. We find that an optimal zone exists between 1 kpc and 4 kpc from the emitting galaxy. If the halo resides too close to the emitting galaxy the photo-ionising radiation creates a large HII region which effectively disrupts the collapsing halo, too far from the source and the radiation flux drops below the level of the expected background and the {H_2} fraction remains too high. When the emitting galaxy is initially placed between 1 kpc and 2 kpc from the collapsing halo, with a spectral shape consistent with a star-forming high redshift galaxy, then a large central core forms. The mass of the central core is between 5000 and 10000 M_{⊙}at a temperature of approximately 1000 K. This core is however surrounded by a reservoir of hotter gas at approximately 8000 K which leads to mass inflow rates of the order of ˜0.1 M_{⊙} yr-1.

  14. Massive stars on the verge of exploding: the properties of oxygen sequence Wolf-Rayet stars

    NASA Astrophysics Data System (ADS)

    Tramper, F.; Straal, S. M.; Sanyal, D.; Sana, H.; de Koter, A.; Gräfener, G.; Langer, N.; Vink, J. S.; de Mink, S. E.; Kaper, L.

    2015-09-01

    Context. Oxygen sequence Wolf-Rayet (WO) stars are a very rare stage in the evolution of massive stars. Their spectra show strong emission lines of helium-burning products, in particular highly ionized carbon and oxygen. The properties of WO stars can be used to provide unique constraints on the (post-)helium burning evolution of massive stars, and their remaining lifetimes and the expected properties of their supernovae. Aims: We aim to homogeneously analyze the currently known presumed-single WO stars to obtain the key stellar and outflow properties and to constrain their evolutionary state. Methods: We use the line-blanketed non-local thermal equilibrium atmosphere code cmfgen to model the X-Shooter spectra of the WO stars and to deduce the atmospheric parameters. We calculate dedicated evolutionary models to determine the evolutionary state of the stars. Results: The WO stars have extremely high temperatures that range from 150 kK to 210 kK, and very low surface helium mass fractions that range from 44% down to 14%. Their properties can be reproduced by evolutionary models with helium zero-age main sequence masses of MHe,ini = 15-25 M⊙ that exhibit a fairly strong (a few times 10-5M⊙ yr-1), homogeneous (fc> 0.3) stellar wind. Conclusions: WO stars represent the final evolutionary stage of stars with estimated initial masses of Mini = 40-60 M⊙. They are post core-helium burning and predicted to explode as type Ic supernovae within a few thousand years. Based on observations obtained at the European Southern Observatory under program IDs 091.C-0934 and 093.D-0591.Appendices are available in electronic form at http://www.aanda.org

  15. Atmospheric deposition of SO 4-S and (NH 4+NO 3)-N at two rural sites in the Western Maracaibo Lake Basin, Venezuela

    NASA Astrophysics Data System (ADS)

    Morales, Jose Agustin; Bifano, Claudio; Escalona, Andres

    Rain samples were collected by events from November 1988 to November 1989 at La Esperanza and Catatumbo sites. Dry deposition was collected only at La Esperanza. Volume weighted average pH values of the rainfall samples were between 4.23 and 4.64, individual samples reaching as low as pH 3.0. An excess of sulfate greater than 96% was obtained at both sites. The wet deposition of hydronium and sulfate showed the same seasonal cycle. The highest inputs were obtained in April during the early rainy season, and November which is the second peak rainfall period. The amounts of (NH 4+NO 3)-N ha -1 yr -1 added by wet deposition ranged from 5.2 kg at La Esperanza to 11.4 kg at Catatumbo (ammonium accounts for about 67% of these amounts), and the corresponding amounts of SO 4-S deposited ranged from 10.5 to 12.5 kg, respectively. These amounts of S and N annually deposited by precipitation are substantially higher than those found in eastern Venezuelan sites, and slightly lower than the values reported for rural areas of Europe and North America. In La Esperanza it was estimated that wet deposition accounts for about 93% of the inorganic-N and for about 80% of the SO 4-S annually added by dry and wet deposition. It is envisaged that in Lake Maracaibo Basin large argricultural and uncultivated land areas downwind of the El Tablazo Petrochemical Complex, Cardon-Amuay and, probably, the Aruba-Curacao refineries and urban Maracaibo might already be affected by anthropogenic air pollution as evidenced by the higher level of H +, SO -24, NO -3 and NH +4 wet deposition found at the La Esperanza and Catatumbo sites in comparison with other rural sites in Venezuela.

  16. The Relation between Galaxy Structure and Spectral Type: Implications for the Buildup of the Quiescent Galaxy Population at 0.5 < z < 2.0

    NASA Astrophysics Data System (ADS)

    Yano, Michael; Kriek, Mariska; van der Wel, Arjen; Whitaker, Katherine E.

    2016-02-01

    We present the relation between galaxy structure and spectral type, using a K-selected galaxy sample at 0.5 < z < 2.0. Based on similarities between the UV-to-NIR spectral energy distributions (SEDs), we classify galaxies into 32 spectral types. The different types span a wide range in evolutionary phases, and thus—in combination with available CANDELS/F160W imaging—are ideal to study the structural evolution of galaxies. Effective radii (Re) and Sérsic parameters (n) have been measured for 572 individual galaxies, and for each type, we determine Re at fixed stellar mass by correcting for the mass-size relation. We use the rest-frame U - V versus V - J diagram to investigate evolutionary trends. When moving into the direction perpendicular to the star-forming sequence, in which we see the Hα equivalent width and the specific star formation rate (sSFR) decrease, we find a decrease in Re and an increase in n. On the quiescent sequence we find an opposite trend, with older redder galaxies being larger. When splitting the sample into redshift bins, we find that young post-starburst galaxies are most prevalent at z > 1.5 and significantly smaller than all other galaxy types at the same redshift. This result suggests that the suppression of star formation may be associated with significant structural evolution at z > 1.5. At z < 1, galaxy types with intermediate sSFRs (10-11.5-10-10.5 yr-1) do not have post-starburst SED shapes. These galaxies have similar sizes as older quiescent galaxies, implying that they can passively evolve onto the quiescent sequence, without increasing the average size of the quiescent galaxy population.

  17. Type IIb Supernova 2013df Entering into an Interaction Phase: A Link between the Progenitor and the Mass Loss

    NASA Astrophysics Data System (ADS)

    Maeda, K.; Hattori, T.; Milisavljevic, D.; Folatelli, G.; Drout, M. R.; Kuncarayakti, H.; Margutti, R.; Kamble, A.; Soderberg, A.; Tanaka, M.; Kawabata, M.; Kawabata, K. S.; Yamanaka, M.; Nomoto, K.; Kim, J. H.; Simon, J. D.; Phillips, M. M.; Parrent, J.; Nakaoka, T.; Moriya, T. J.; Suzuki, A.; Takaki, K.; Ishigaki, M.; Sakon, I.; Tajitsu, A.; Iye, M.

    2015-07-01

    We report the late-time evolution of Type IIb supernova (SN IIb) 2013df. SN 2013df showed a dramatic change in its spectral features at ˜1 yr after the explosion. Early on it showed typical characteristics shared by SNe IIb/Ib/Ic dominated by metal emission lines, while later on it was dominated by broad and flat-topped Hα and He i emissions. The late-time spectra are strikingly similar to SN IIb 1993J, which is the only previous example clearly showing the same transition. This late-time evolution is fully explained by a change in the energy input from the 56Co decay to the interaction between the SN ejecta and dense circumstellar matter (CSM). The mass-loss rate is derived to be ˜ (5.4+/- 3.2)× {10}-5 {M}⊙ yr-1 (for the wind velocity of ˜20 km s-1), similar to SN 1993J but larger than SN IIb 2011dh by an order of magnitude. The striking similarity between SNe IIb 2013df and 1993J in the (candidate) progenitors and the CSM environments and the contrast in these natures to SN 2011dh infer that there is a link between the natures of the progenitor and the mass loss: SNe IIb with a more extended progenitor have experienced a much stronger mass loss in the final centuries toward the explosion. It might indicate that SNe IIb from a more extended progenitor are the explosions during a strong binary interaction phase, while those from a less extended progenitor have a delay between the strong binary interaction and the explosion. Based on data collected at the Subaru Telescope, operated by the National Astronomical Observatory of Japan, and also at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona.

  18. Asymptotic giant branch stars in the Large Magellanic Cloud: evolution of dust in circumstellar envelopes

    NASA Astrophysics Data System (ADS)

    Dell'Agli, F.; Ventura, P.; Schneider, R.; Di Criscienzo, M.; García-Hernández, D. A.; Rossi, C.; Brocato, E.

    2015-03-01

    We calculated theoretical evolutionary sequences of asymptotic giant branch (AGB) stars, including the formation and evolution of dust grains in their circumstellar envelopes. By considering stellar populations of the Large Magellanic Cloud (LMC), we calculate synthetic colour-colour and colour-magnitude diagrams, which are compared with those obtained by the Spitzer Space Telescope. The comparison between observations and theoretical predictions outlines that extremely obscured carbon stars and oxygen-rich sources experiencing hot bottom burning (HBB) occupy well-defined, distinct regions in the colour-colour ([3.6] - [4.5], [5.8] - [8.0]) diagram. The C-rich stars are distributed along a diagonal strip that we interpret as an evolutionary sequence, becoming progressively more obscured as the stellar surface layers enrich in carbon. Their circumstellar envelopes host solid carbon dust grains with size in the range 0.05 < a < 0.2 μm. The presence of silicon carbide (SiC) particles is expected only in the more metal-rich stars. The reddest sources, with [3.6] - [4.5] > 2, are the descendants of stars with initial mass Min ˜ 2.5-3 M⊙ in the very latest phases of AGB life. The oxygen-rich stars with the reddest colours ([5.8] - [8.0] > 0.6) are those experiencing HBB, the descendants of ˜5 M⊙ objects formed 108 yr ago; alumina and silicate dust starts forming at different distances from the central star. The overall dust production rate in the LMC is ˜4.5 × 10-5 M⊙ yr-1, the relative percentages due to C and M stars being 85 and 15 per cent, respectively.

  19. Colliding Winds in Symbiotic Binary Systems. II. Colliding Winds Geometries and Orbital Motion in the Symbiotic Nova AG Pegasi

    NASA Astrophysics Data System (ADS)

    Kenny, H. T.; Taylor, A. R.

    2007-06-01

    AG Pegasi has been observed at high angular resolution and sensitivity at the Very Large Array (VLA) at 5 GHz in four epochs between 1984 and 1991. Analysis of the radio visibilities indicate that a mass of 4.0+/-0.5×10-5 Msolar is concentrated in the inner nebula and is moving outward at a velocity of 53+/-4 km s-1 (D=600 pc assumed). In order to explain the observed morphology of the inner nebula, a new colliding winds model is derived, which includes the effects of orbital motion (CWo model). Orbital effects cannot be ignored in AG Pegasi since the orbital timescale (2.25 yr; Meinunger 1981) is short compared to the likely timescale of wind collision (symbiotic nova eruption beginning ~1850 Merrill 1959). When these effects are considered, the interaction front between binary stellar winds is wrapped into spiral walls whose density decreases outward with 1/r2. Distinctive geometries are found to arise depending on which wind dominates the interaction, the late-type wind from the symbiotic ``cool component,'' or the high-velocity wind from the ``hot component.'' Application of the CWo model to AG Peg suggests that the observed transient lobe enhancements of the inner nebula arise due to changes in the mass-loss rate from the hot component. Hot component mass-loss rates ranging between 2.1 and 6.0×10-8 Msolar yr-1 are derived. The model is also successful in reproducing the radio spectrum of the central unresolved object of the system. A position angle of -15deg+/-10deg is inferred for the orbital pole as projected on the plane of the sky.

  20. Shock Breakout and Early Light Curves of Type II-P Supernovae Observed with Kepler

    NASA Astrophysics Data System (ADS)

    Garnavich, Peter M.; Tucker, Bradley E.; Rest, Armin; Shaya, Edward J.; Olling, Robert; Kasen, Daniel; Villar, Victoria; KEGS

    2016-01-01

    We discovered two transient events in the Kepler field with light curves that strongly suggest they are type II-P supernovae. Using the fast cadence of the Kepler observations we precisely estimate the rise time to maximum for KSN2011a and KSN2011d as 10.5±0.4 and 13.3±0.4 rest-frame days respectively. We find the progenitor radius of KSN2011a (280±20 R⊙) to be significantly smaller than that for KSN2011d (490±20 R⊙) but both have similar explosion energies of 2.0±0.3 ×1051 erg.The rising light curve of KSN2011d is an excellent match to that predicted by simple models of exploding red supergiants (RSG). However, the early rise of KSN2011a is faster than the models predict possibly due to the supernova shockwave moving into pre-existing wind or mass-loss from the RSG. A mass loss rate of 10-4 M⊙ yr-1 from the RSG can explain the fast rise without impacting the optical flux at maximum light or the shape of the post-maximum light curve.No shock breakout emission is seen in KSN2011a, but this is likely due to the circumstellar interaction suspected in the fast rising light curve. The early light curve of KSN2011d does show excess emission consistent with model predictions of a shock breakout. This is the first optical detection of a shock breakout from a type II-P supernova.

  1. Shock Breakout and Early Light Curves of Type II-P Supernovae Observed with Kepler

    NASA Astrophysics Data System (ADS)

    Garnavich, P. M.; Tucker, B. E.; Rest, A.; Shaya, E. J.; Olling, R. P.; Kasen, D.; Villar, A.

    2016-03-01

    We discovered two transient events in the Kepler field with light curves that strongly suggest they are type II-P supernovae (SNe II-P). Using the fast cadence of the Kepler observations we precisely estimate the rise time to maximum for KSN2011a and KSN2011d as 10.5 ± 0.4 and 13.3 ± 0.4 rest-frame days, respectively. Based on fits to idealized analytic models, we find the progenitor radius of KSN2011a (280 ± 20 R⊙) to be significantly smaller than that for KSN2011d (490 ± 20 R⊙), but both have similar explosion energies of 2.0 ± 0.3 × 1051 erg. The rising light curve of KSN2011d is an excellent match to that predicted by simple models of exploding red supergiants (RSG). However, the early rise of KSN2011a is faster than the models predict, possibly due to the supernova shock wave moving into pre-existing wind or mass-loss from the RSG. A mass-loss rate of 10-4M⊙ yr-1 from the RSG can explain the fast rise without impacting the optical flux at maximum light or the shape of the post-maximum light curve. No shock breakout emission is seen in KSN2011a, but this is likely due to the circumstellar interaction suspected in the fast rising light curve. The early light curve of KSN2011d does show excess emission consistent with model predictions of a shock breakout. This is the first optical detection of a shock breakout from a SNe II-P.

  2. Unbeamed tidal disruption events at hard X-rays

    NASA Astrophysics Data System (ADS)

    Hryniewicz, K.; Walter, R.

    2016-02-01

    Context. Owing to their thermal emission, tidal disruption events (TDEs) were regularly detected in the soft X-rays and sometimes in the optical. Only a few TDEs have been detected at hard X-rays: two are high redshift beamed events, one of which occurred at the core of a nearby galaxy, and the most recent one is of a different nature, involving a compact object in the Milky Way. Aims: The aims of this work are to obtain a first sample of hard X-ray-selected unbeamed TDEs, to determine their frequency and to probe whether TDEs usually or exceptionally emit at hard X-ray energies. Methods: We performed extensive searches for hard X-ray flares at positions in over 53 000 galaxies, up to a distance of 100 Mpc in the Swift/BAT archive. Light curves were extracted and parametrized. The quiescent hard X-ray emission was used to exclude persistently active galactic nuclei. Significant flares from non-active galaxies were derived and checked for possible contamination. Results: We found a sample of nine TDE candidates, which translates into a rate of 2 × 10-5 galaxy-1 yr-1 above the BAT detection limit. This rate is consistent with those observed by XMM-Newton at soft X-rays and in the optical from SDSS observations, and is as expected from simulations. We conclude that hard X-ray emission should be ubiquitous in un-beamed TDEs and that electrons should be accelerated in their accretion flow.

  3. Stellar Winds and Embedded Star Formation in the Galactic Center Quintuplet and Arches Clusters: Multifrequency Radio Observations

    NASA Astrophysics Data System (ADS)

    Lang, Cornelia C.; Johnson, Kelsey E.; Goss, W. M.; Rodríguez, Luis F.

    2005-11-01

    A multifrequency, multiconfiguration study has been made of the compact radio sources in the Galactic center Quintuplet and Arches stellar clusters using the Very Large Array. Ten radio sources have been detected in the Quintuplet cluster. The majority of these radio sources have rising spectral indices and are positionally coincident with young massive stars that are known to have powerful stellar winds. We conclude that the three most compact of these sources are produced by stellar wind emission; thus, mass-loss rates can be derived and have an average value of 3×10-5 Msolar yr-1. The remainder of the sources are likely to be a combination of stellar wind emission and free-free emission from surrounding ionized gas. In three cases, the radio sources have no stellar counterpart, and the radio emission is thought to arise from compact or ultracompact H II regions. If so, these sources would be the first detections of embedded massive stars to be discovered in the Galactic center clusters. The radio nebula associated with the Pistol star resembles the nebula surrounding the luminous blue variable star η Car and may be related to the stellar wind of the Pistol star. Ten compact radio sources are also detected in the Arches cluster and are interpreted to be stellar wind sources, consistent with previous findings. Several of the sources show moderate variability (10%-30%) in their flux density, possibly related to a nonthermal component in the wind emission. A number of radio sources in both clusters have X-ray counterparts, which have been interpreted to be the shocked, colliding winds of massive binary systems.

  4. Signatures of Young Star Formation Activity within Two Parsecs of Sgr A*

    NASA Astrophysics Data System (ADS)

    Yusef-Zadeh, F.; Wardle, M.; Sewilo, M.; Roberts, D. A.; Smith, I.; Arendt, R.; Cotton, W.; Lacy, J.; Martin, S.; Pound, M. W.; Rickert, M.; Royster, M.

    2015-07-01

    We present radio and infrared observations indicating ongoing star formation activity inside the ˜2-5 pc circumnuclear ring at the Galactic center. Collectively these measurements suggest a continued disk-based mode of ongoing star formation has taken place near Sgr A* over the last few million years. First, Very Large Array observations with spatial resolution 2.″17 × 0.″81 reveal 13 water masers, several of which have multiple velocity components. The presence of interstellar water masers suggests gas densities that are sufficient for self-gravity to overcome the tidal shear of the 4× {10}6 {M}⊙ black hole. Second, spectral energy distribution modeling of stellar sources indicates massive young stellar object (YSO) candidates interior to the molecular ring, supporting in situ star formation near Sgr A* and appear to show a distribution similar to that of the counter-rotating disks of ˜100 OB stars orbiting Sgr A*. Some YSO candidates (e.g., IRS 5) have bow shock structures, suggesting that they have gaseous disks that are phototoevaporated and photoionized by the strong radiation field. Third, we detect clumps of SiO (2-1) and (5-4) line emission in the ring based on Combined Array for Research in Millimeter-wave Astronomy and Sub-Millimeter Array observations. The FWHM and luminosity of the SiO emission is consistent with shocked protostellar outflows. Fourth, two linear ionized features with an extent of ˜0.8 pc show blue and redshifted velocities between +50 and -40 km s-1, suggesting protostellar jet driven outflows with mass-loss rates of ˜ 5× {10}-5 {M}⊙ yr-1. Finally, we present the imprint of radio dark clouds at 44 GHz, representing a reservoir of molecular gas that feeds star formation activity close to Sgr A*.

  5. OISTER optical and near-infrared observations of the super-Chandrasekhar supernova candidate SN 2012dn: Dust emission from the circumstellar shell

    NASA Astrophysics Data System (ADS)

    Yamanaka, Masayuki; Maeda, Keiichi; Tanaka, Masaomi; Tominaga, Nozomu; Kawabata, Koji S.; Takaki, Katsutoshi; Kawabata, Miho; Nakaoka, Tatsuya; Ueno, Issei; Akitaya, Hiroshi; Nagayama, Takahiro; Takahashi, Jun; Honda, Satoshi; Omodaka, Toshihiro; Miyanoshita, Ryo; Nagao, Takashi; Watanabe, Makoto; Isogai, Mizuki; Arai, Akira; Itoh, Ryosuke; Ui, Takahiro; Uemura, Makoto; Yoshida, Michitoshi; Hanayama, Hidekazu; Kuroda, Daisuke; Ukita, Nobuharu; Yanagisawa, Kenshi; Izumiura, Hideyuki; Saito, Yoshihiko; Masumoto, Kazunari; Ono, Rikako; Noguchi, Ryo; Matsumoto, Katsura; Nogami, Daisaku; Morokuma, Tomoki; Oasa, Yumiko; Sekiguchi, Kazuhiro

    2016-05-01

    We present extensively dense observations of the super-Chandrasekhar supernova (SC SN) candidate SN 2012dn from -11 to +140 d after the date of its B-band maximum in the optical and near-infrared (NIR) wavelengths conducted through the OISTER ToO (Optical and Infrared Synergetic Telescopes for Education and Research Target of Opportunity) program. The NIR light curves and color evolutions up to 35 days after the B-band maximum provided an excellent match with those of another SC SN 2009dc, providing further support to the nature of SN 2012dn as an SC SN. We found that SN 2012dn exhibited strong excesses in the NIR wavelengths from 30 d after the B-band maximum. The H- and Ks-band light curves exhibited much later maximum dates at 40 and 70 d after the B-band maximum, respectively, compared with those of normal SNe Ia. The H- and Ks-band light curves subtracted by those of SN 2009dc displayed plateaued evolutions, indicating an NIR echo from the surrounding dust. The distance to the inner boundary of the dust shell is limited to 4.8-6.4 × 10-2 pc. No emission lines were found in its early phase spectra, suggesting that the ejecta-circumstellar material interaction could not occur. On the other hand, we found no signature that strongly supports the scenario of dust formation. The mass-loss rate of the pre-explosion system is estimated to be 10-6-10-5 M⊙ yr-1, assuming that the wind velocity of the system is 10-100 km s-1, which suggests that the progenitor of SN 2012dn could be a recurrent nova system. We conclude that the progenitor of this SC SN could be explained by the single-degenerate scenario.

  6. Washout/rainout contribution in wet deposition estimated by 0.5 mm precipitation sampling/analysis

    NASA Astrophysics Data System (ADS)

    Aikawa, Masahide; Hiraki, Takatoshi

    A precipitation dataset collected on a 0.5 mm precipitation basis was studied. The parameters analyzed in this study were the pH (i.e., H + concentration), electric conductivity (EC), and SO42- and NO3- concentrations. The NO3- concentration clearly decayed with an increase of the precipitation amount, while a larger variation was observed in the SO42- concentration even when the precipitation amount increased. Assuming that the decaying NO3- concentration (0.70 μg ml -1) was the result of the rainout process, the estimates were: annual total deposition, 3252 mg m -2 yr -1; rainout process, 1092 mg m -2 yr -1; and rainout/total, 34%. The estimates for SO42- were: annual total deposition, 4687 mg m -2 yr -1; rainout process, 2096 mg m -2 yr -1; and rainout/total, 45%.

  7. Reviews and syntheses: Greenhouse gas emissions in natural and agricultural lands in sub-Saharan Africa: synthesis of available data and suggestions for further studies

    NASA Astrophysics Data System (ADS)

    Kim, D.-G.; Thomas, A. D.; Pelster, D.; Rosenstock, T. S.; Sanz-Cobena, A.

    2015-10-01

    This paper summarizes currently available data on greenhouse gas (GHG) emissions from African natural and agricultural lands, outlines the knowledge gaps and suggests future directions and strategies for GHG emission studies. GHG emission data were collected from 73 studies conducted in 22 countries in sub-Saharan Africa (SSA). Soil GHG emissions from African natural terrestrial systems ranged from 3.3 to 57.0 Mg carbon dioxide (CO2) ha-1 yr-1, -4.8 to 3.5 kg methane (CH4) ha-1 yr-1 and -0.1 to 13.7 kg nitrous oxide (N2O) ha-1 yr-1. Soil physical and chemical properties, rewetting, vegetation type, forest management and land-use changes were all found to be important factors affecting soil GHG emissions. Greenhouse gas emissions from African aquatic systems ranged from 5.7 to 232.0 Mg CO2 ha-1 yr-1, -26.3 to 2741.9 kg CH4 ha-1 yr-1 and 0.2 to 3.5 kg N2O ha-1 yr-1 and were strongly affected by discharge. Soil GHG emissions from African croplands ranged from 1.7 to 141.2 Mg CO2 ha-1 yr-1, -1.3 to 66.7 kg CH4 ha-1 yr-1and 0.05 to 112.0 kg N2O ha-1 yr-1 and the N2O emission factor (EF) ranged from 0.01 to 4.1 %. Incorporation of crop residues or manure with inorganic fertilizers resulted in significant changes in GHG emissions but these were different for CO2 and N2O. Soil GHG emissions in vegetable gardens ranged from 73.3 to 132.0 Mg CO2 ha-1 yr-1 and 53.4 to 177.6 kg N2O ha-1 yr-1 and N2O EFs ranged from 3 to 4 %. Soil CO2 and N2O emissions from agroforestry were 38.6 Mg CO2 ha-1 yr-1 and 0.2 to 26.7 kg N2O ha-1 yr-1, respectively. Improving fallow with nitrogen (N)-fixing trees increased CO2 and N2O emissions compared to conventional croplands and type and quality of plant residue is likely to be an important control factor affecting N2O emissions. Throughout agricultural lands, N2O emissions slowly increased with N inputs below 150 kg N ha-1 yr-1 and increased exponentially with N application rates up to 300 kg N ha-1 yr-1. The lowest yield-scaled N2O emissions

  8. Benthic macrofauna productivity enhancement by an artificial reef in Delaware Bay, USA

    SciTech Connect

    Steimle, F; Foster, Karen L.; Kropp, Roy K.; Conlin, B

    2002-10-15

    To understand the potential enhancement value of a habitat-loss mitigation reef in Delaware Bay, especially as a source of food for fishery resources, the secondary productivity of the reef epifauna and nearby sand infauna was estimated and compared. The mean production of natural sand infauna was estimated at between 215 and 249 kcal m(2) yr(-1), while that of the epifauna on the reef surfaces was between 3990 and 9555 kcal m(2) yr(-1). With the 36 m(2) footprint of a reef unit as a basis for comparison, the 407 m(2) of reef unit surface covering that footprint produced 1.62-3.89 X 10(6) kcal yr(-1) of epifauna compared with 7.74-8.96 X 10(3) kcal yr(-1) per footprint area for the adjacent sand infauna. There was, however, substantial annual variability in the productivity of the epifauna, based on the recruitment success of Mytilus edulis.

  9. Carbon accumulation and allocation in a primary Bornean tropical rainforest

    NASA Astrophysics Data System (ADS)

    Katayama, A.; Komatsu, H.; Kume, T.; Ohashi, M.; Nakagawa, M.; Otsuki, K.; Kumagai, T.

    2010-12-01

    To develop our knowledge of global carbon cycling, it is important to know all components of allocated carbon in tropical rainforests because of their enormous accumulation and elimination. Our goals in this study are to estimate carbon allocation (i.e. carbon flux to aboveground biomass increment, litterfall, aboveground plant respiration and belowground) and compare GPP based on biometric and flux measurement in a primary Bornean tropical rainforest. GPP estimated by biometric method (35.39 tCha-2yr-1) was similar to that measured by flux measurement (31.56 tCha-2yr-1). Mean annual aboveground biomass increment (2.77 tCha-2yr-1) was reasonable compared to former literatures in spite of larger aboveground biomass (272 tCha-2yr-1). Ratio of TBCF to GPP (0.55) was extremely high. These results suggested that considerable carbon is allocated to belowground, causing low productivity of aboveground biomass.

  10. Diapycnal diffusivity in the core and oxycline of the tropical North Atlantic oxygen minimum zone

    NASA Astrophysics Data System (ADS)

    Köllner, Manuela; Visbeck, Martin; Tanhua, Toste; Fischer, Tim

    2016-08-01

    Diapycnal diffusivity estimates from two Tracer Release Experiments (TREs) and microstructure measurements in the oxycline and core of the oxygen minimum zone (OMZ) in the Eastern Tropical North Atlantic (ETNA) are compared. For the first time, two TREs within the same area at different depths were realized: the Guinea Upwelling Tracer Release Experiment (GUTRE) initiated in 2008 in the oxycline at approximately 320 m depth, and the Oxygen Supply Tracer Release Experiment (OSTRE) initiated in 2012 in the core of the OMZ at approximately 410 m depth. The mean diapycnal diffusivity Dz was found to be insignificantly smaller in the OMZ core with (1.06 ± 0.24) × 10- 5 m2 s- 1 compared to (1.11 ± 0.22) × 10- 5 m2 s- 1 90 m shallower in the oxycline. Unexpectedly, GUTRE tracer was detected during two of the OSTRE surveys which showed that the estimated diapycnal diffusivity from GUTRE over a time period of seven years was within the uncertainty of the previous estimates over a time period of three years. The results are consistent with the Dz estimates from microstructure measurements and demonstrate that Dz does not vary significantly vertically in the OMZ within the depth range of 200-600 m and does not change with time. The presence of a seamount chain in the vicinity of the GUTRE injection region did not cause enhanced Dz compared to the smoother bottom topography of the OSTRE injection region, although the analysis of vertical shear spectra from ship ADCP data showed elevated internal wave energy level in the seamount vicinity. However, the two tracer patches covered increasingly overlapping areas with time and thus spatially integrated increasingly similar fields of local diffusivity, as well as the difference in local stratification counteracted the influence of roughness on Dz. For both experiments no significant vertical displacements of the tracer were observed, thus diapycnal upwelling within the ETNA OMZ is below the uncertainty level of 5 m yr- 1.

  11. Estimating Asian terrestrial carbon fluxes from CONTRAIL aircraft and surface CO2 observations for the period 2006 to 2010

    NASA Astrophysics Data System (ADS)

    Zhang, H. F.; Chen, B. Z.; van der Laan-Luijkx, I. T.; Machida, T.; Matsueda, H.; Sawa, Y.; Fukuyama, Y.; Labuschagne, C.; Langenfelds, R.; van der Schoot, M.; Xu, G.; Yan, J. W.; Zhou, L. X.; Tans, P. P.; Peters, W.

    2013-10-01

    Current estimates of the terrestrial carbon fluxes in Asia ("Asia" refers to lands as far west as the Urals and is divided into Boreal Eurasia, Temperate Eurasia and tropical Asia based on TransCom regions) show large uncertainties particularly in the boreal and mid-latitudes and in China. In this paper, we present an updated carbon flux estimate for Asia by introducing aircraft CO2 measurements from the CONTRAIL (Comprehensive Observation Network for Trace gases by Airline) program into an inversion modeling system based on the CarbonTracker framework. We estimated the averaged annual total Asian terrestrial land CO2 sink was about -1.56 Pg C yr-1 over the period 2006-2010, which offsets about one-third of the fossil fuel emission from Asia (+4.15 Pg C yr-1). The uncertainty of the terrestrial uptake estimate was derived from a set of sensitivity tests and ranged from -1.07 to -1.80 Pg C yr-1, comparable to the formal Gaussian error of ±1.18 Pg C yr-1 (1-sigma). The largest sink was found in forests, predominantly in coniferous forests (-0.64 Pg C yr-1) and mixed forests (-0.14 Pg C yr-1); and the second and third large carbon sinks were found in grass/shrub lands and crop lands, accounting for -0.44 Pg C yr-1 and -0.20 Pg C yr-1, respectively. The peak-to-peak amplitude of inter-annual variability (IAV) was 0.57 Pg C yr-1 ranging from -1.71 Pg C yr-1 to -2.28 Pg C yr-1. The IAV analysis reveals that the Asian CO2 sink was sensitive to climate variations, with the lowest uptake in 2010 concurrent with summer flood/autumn drought and the largest CO2 sink in 2009 owing to favorable temperature and plentiful precipitation conditions. We also found the inclusion of the CONTRAIL data in the inversion modeling system reduced the uncertainty by 11% over the whole Asian region, with a large reduction in the southeast of Boreal Eurasia, southeast of Temperate Eurasia and most Tropical Asian areas.

  12. Estimating Asian terrestrial carbon fluxes from CONTRAIL aircraft and surface CO2 observations for the period 2006-2010

    NASA Astrophysics Data System (ADS)

    Zhang, H. F.; Chen, B. Z.; Machida, T.; Matsueda, H.; Sawa, Y.; Fukuyama, Y.; Langenfelds, R.; van der Schoot, M.; Xu, G.; Yan, J. W.; Cheng, M. L.; Zhou, L. X.; Tans, P. P.; Peters, W.

    2014-06-01

    Current estimates of the terrestrial carbon fluxes in Asia show large uncertainties particularly in the boreal and mid-latitudes and in China. In this paper, we present an updated carbon flux estimate for Asia ("Asia" refers to lands as far west as the Urals and is divided into boreal Eurasia, temperate Eurasia and tropical Asia based on TransCom regions) by introducing aircraft CO2 measurements from the CONTRAIL (Comprehensive Observation Network for Trace gases by Airline) program into an inversion modeling system based on the CarbonTracker framework. We estimated the averaged annual total Asian terrestrial land CO2 sink was about -1.56 Pg C yr-1 over the period 2006-2010, which offsets about one-third of the fossil fuel emission from Asia (+4.15 Pg C yr-1). The uncertainty of the terrestrial uptake estimate was derived from a set of sensitivity tests and ranged from -1.07 to -1.80 Pg C yr-1, comparable to the formal Gaussian error of ±1.18 Pg C yr-1 (1-sigma). The largest sink was found in forests, predominantly in coniferous forests (-0.64 ± 0.70 Pg C yr-1) and mixed forests (-0.14 ± 0.27 Pg C yr-1); and the second and third large carbon sinks were found in grass/shrub lands and croplands, accounting for -0.44 ± 0.48 Pg C yr-1 and -0.20 ± 0.48 Pg C yr-1, respectively. The carbon fluxes per ecosystem type have large a priori Gaussian uncertainties, and the reduction of uncertainty based on assimilation of sparse observations over Asia is modest (8.7-25.5%) for most individual ecosystems. The ecosystem flux adjustments follow the detailed a priori spatial patterns by design, which further increases the reliance on the a priori biosphere exchange model. The peak-to-peak amplitude of inter-annual variability (IAV) was 0.57 Pg C yr-1 ranging from -1.71 Pg C yr-1 to -2.28 Pg C yr-1. The IAV analysis reveals that the Asian CO2 sink was sensitive to climate variations, with the lowest uptake in 2010 concurrent with a summer flood and autumn drought and the largest

  13. Global ocean carbon uptake: magnitude, variability and trends

    NASA Astrophysics Data System (ADS)

    Wanninkhof, R.; Park, G.-H.; Takahashi, T.; Sweeney, C.; Feely, R.; Nojiri, Y.; Gruber, N.; Doney, S. C.; McKinley, G. A.; Lenton, A.; Le Quéré, C.; Heinze, C.; Schwinger, J.; Graven, H.; Khatiwala, S.

    2012-08-01

    Estimates of the anthropogenic global-integrated sea-air carbon dioxide (CO2) flux from 1990 to 2009, based on different models and measurements, range from -1.4 to -2.6 Pg C yr-1. The median values of anthropogenic CO2 for each method show better agreement and are: -1.9 for Pg C yr-1 for numerical ocean general circulation hind cast models (OGCMs) with parameterized biogeochemistry; -2.1 Pg C yr-1 for atmospheric inverse models; -1.9 Pg C yr-1 for global atmospheric constraints based on O2 / N2 ratios for 1990-2000; and -2.4 Pg C yr-1 for oceanic inverse models. An updated estimate of this anthropogenic CO2 flux based on a climatology of sea-air partial pressure of CO2 differences (ΔpCO2) (Takahashi et al., 2009) and a bulk formulation of gas transfer with wind speed for year 2000 is -2.0 Pg C yr-1. Using this ΔpCO2 climatology and empirical relationships of pCO2 with sea-surface temperature (SST) anomalies (Park et al., 2010a), the interannual variability of the contemporary CO2 flux is estimated to be 0.20 Pg C yr-1 (1σ) from 1990 through 2009. This is similar to the variability estimated by the OGCMs of 0.16 Pg C yr-1 but smaller than the interannual variability from atmospheric inverse estimates of 0.40 Pg C yr-1. The variability is largely driven by large-scale climate re-organizations. The decadal trends for different methods range from -0.13 (Pg C yr-1) decade-1 to -0.50 (Pg C yr-1) decade-1. The OGCMs and the data based sea-air CO2 flux estimates show smaller uptakes and appreciably smaller decadal trends than estimates based on changes in carbon inventory suggesting that methods capable of resolving shorter timescales are showing a slowing of the rate of ocean CO2 uptake. It is not clear if this large difference in trend is a methodological issue or a real natural feedback.

  14. Analysis of crustal deformation in Luzon, Philippines using geodetic observations and earthquake focal mechanisms

    NASA Astrophysics Data System (ADS)

    Galgana, Gerald; Hamburger, Michael; McCaffrey, Robert; Corpuz, Ernesto; Chen, Qizhi

    2007-03-01

    We utilize regional GPS velocities from Luzon, Philippines, with focal mechanism data from the Harvard Centroid Moment Tensor (CMT) Catalog, to constrain tectonic deformation in the complex plate boundary zone between the Philippine Sea Plate and Eurasia (the Sundaland block). Processed satellite imagery and digital elevation models are used with existing gravity anomaly, seismicity, and geologic maps to define a suite of six elastic blocks. Geodetic and focal mechanism data are inverted simultaneously to estimate plate rotations and fault-locking parameters for each of the tectonic blocks and faults comprising Luzon. Major tectonic structures that were found to absorb the plate convergence include the Manila Trench (20-100 mm yr - 1 ) and East Luzon Trough (˜ 9-15 mm yr - 1 )/Philippine Trench (˜ 29-34 mm yr - 1 ), which accommodate eastward and westward subduction beneath Luzon, respectively; the left-lateral strike-slip Philippine Fault (˜ 20-40 mm yr - 1 ), and its northward extensions, the Northern Cordillera Fault (˜ 17-37 mm yr - 1 transtension), and the Digdig Fault (˜ 17-27 mm yr - 1 transpression). The Macolod Corridor, a zone of active volcanism, crustal thinning, extension, and extensive normal and strike-slip faulting in southwestern Luzon, is associated with left-lateral, transtensional slip of ˜ 5-10 mm yr - 1 . The Marikina Fault, which separates the Central Luzon block from the Southwestern Luzon block, reveals ˜ 10-12 mm yr - 1 of left-lateral transpression. Our analysis suggests that much of the Philippine Fault and associated splays are locked to partly coupled, while the Manila and Philippine trenches appear to be poorly coupled. Luzon is best characterized as a tectonically active plate boundary zone, comprising six mobile elastic tectonic blocks between two active subduction zones. The Philippine Fault and associated intra-arc faults accommodate much of the trench-parallel component of relative plate motion.

  15. Reconciling estimates of the contemporary North American carbon balance among terrestrial biosphere models, atmospheric inversions, and a new approach for estimating net ecosystem exchange from inventory-based data

    USGS Publications Warehouse

    Hayes, Daniel J.; Turner, David P.; Stinson, Graham; McGuire, A. David; Wei, Yaxing; West, Tristram O.; Heath, Linda S.; de Jong, Bernardus; McConkey, Brian G.; Birdsey, Richard A.; Kurz, Werner A.; Jacobson, Andrew R.; Huntzinger, Deborah N.; Pan, Yude; Post, W. Mac; Cook, Robert B.

    2012-01-01

    We develop an approach for estimating net ecosystem exchange (NEE) using inventory-based information over North America (NA) for a recent 7-year period (ca. 2000–2006). The approach notably retains information on the spatial distribution of NEE, or the vertical exchange between land and atmosphere of all non-fossil fuel sources and sinks of CO2, while accounting for lateral transfers of forest and crop products as well as their eventual emissions. The total NEE estimate of a -327 ± 252 TgC yr-1 sink for NA was driven primarily by CO2 uptake in the Forest Lands sector (-248 TgC yr-1), largely in the Northwest and Southeast regions of the US, and in the Crop Lands sector (-297 TgC yr-1), predominantly in the Midwest US states. These sinks are counteracted by the carbon source estimated for the Other Lands sector (+218 TgC yr-1), where much of the forest and crop products are assumed to be returned to the atmosphere (through livestock and human consumption). The ecosystems of Mexico are estimated to be a small net source (+18 TgC yr-1) due to land use change between 1993 and 2002. We compare these inventory-based estimates with results from a suite of terrestrial biosphere and atmospheric inversion models, where the mean continental-scale NEE estimate for each ensemble is -511 TgC yr-1 and -931 TgC yr-1, respectively. In the modeling approaches, all sectors, including Other Lands, were generally estimated to be a carbon sink, driven in part by assumed CO2 fertilization and/or lack of consideration of carbon sources from disturbances and product emissions. Additional fluxes not measured by the inventories, although highly uncertain, could add an additional -239 TgC yr-1 to the inventory-based NA sink estimate, thus suggesting some convergence with the modeling approaches.

  16. Calculation of Manure Production and Excretion of Nitrogen, Phosphorous and Potassium by Dairy Cattle in the Comarca Lagunera

    Technology Transfer Automated Retrieval System (TEKTRAN)

    The objective of this study is to show how to calculate dairy manure production and the manure content of N, P and K. At the regional level, 7.5 x 106 ton yr-1 of fresh manure is produced, with 12.3% of dry matter (DM) content, for a total of 925,000 ton yr-1 (DM). Total N excreted is 46,200 ton yr-...

  17. Atmospheric flux, transport and mass balance of (210)Pb and (137)Cs radiotracers in different regions of Romania.

    PubMed

    Begy, R Cs; Kovacs, T; Veres, D; Simon, H

    2016-05-01

    This study focuses on the determination of (210)Pb and (137)Cs fluxes from different areas in Transylvania, Romania and on the determination of transport and mass balance within the lacustrine system of Red Lake. In order to achieve this, samples were taken from six different locations (Bihor County area, Ighiel area, Red Lake area, Mluha Peatbog, Mohos Peatbog and Zanoaga Rosie Peat bog in the Semenic Mountains) throughout Romania, these being compared to the values of the Danube Delta area. The activity concentrations of the soil samples were measured by gamma spectrometry (HPGe detector) for both (210)Pbtotal, (210)Pbsup ((226)Ra) and (137)Cs, while peat samples were measured by both alpha ((210)Po) spectrometry (PIPS detectors) as well. The mean value for the (210)Pb flux was measured in the Danube Delta region (42±8Bqm(-2) yr(-1)), while the highest was measured in the Semenic Peatbog (227±54Bqm(-2) yr(-1)); the average being 132±8Bqm(-2) yr(-1). In case of (137)Cs the mean was 298±3Bqm(-2) yr(-1), maximum being 1683±15Bqm(-2) yr(-1) in case of Ighiel area and minimum being 32±1Bqm(-2) yr(-1) in the Danube Delta region. In case of the Red Lake, from the total inventory of 410±23Bqm(-2) yr(-1) in the sediments, the loss by outflows is 100±12Bqm(-2) yr(-1), the catchment to lake transfer factor being 0.84%. PMID:26922393

  18. Assessing the integrated sediment trapping role of man-made and natural sediment sinks, Minizr catchment, Ethiopia

    NASA Astrophysics Data System (ADS)

    Mekonnen, Mulatie; Keesstra, Saskia; Stroosnijder, Leo; Baartman, Jantiene

    2016-04-01

    To enhance sedimentation within a catchment, man-made sediment trapping (ST) measures and natural sediment sinks are playing a vital role. To evaluate the ST role of such measures, this study was conducted at Minizr catchment, northwest Ethiopian highlands. Man-made soil and water conservation (SWC) structures constructed within the catchment and natural sediment sinks (floodplain and wetland) were digitized and quantified from Google earth imagery. Sediment pins, vertical cut measurements through the deposit (after the rainy season) and SWC structures dimension measurements (before and after the rainy seasons) were used to estimate the trapped sediment depth. Inflow and outflow suspended sediment measurements were done to calculate sediment trapping efficacies (STEs). On average, SWC structures trapped ~7922 t yr-1 (56 kg m-1 yr-1) and micro-trenches trapped ~13260 kg yr-1 (a micro-trench trapped 23 kg yr-1). A floodplain located near the centre of the catchment trapped ~ 9971 t yr-1 (59 kg m-2 yr-1) and a wetland located near the outlet of the catchment trapped ~ 8715 t yr-1 (36 kg m-2 yr-1). The STEs of the wetland and the floodplain were found to be 85 % and 77 %, respectively. Substantial difference was observed between the STE of grassed and un-grassed waterways, 75 % and 21 %, respectively. About ~40 % of the transported sediment was trapped by major sediment traps (both man-made and natural) and ~60 % is still leaving the catchment and entering into Koga reservoir. Although man-made structures and natural sediment sinks trapped large amount of sediment, the rate of sediment red-deposition is lower than the rate of sediment export at the outlet of the catchment, which is because of lack of an integrated ST approach.

  19. Reduction in NO(x) emission trends over China: regional and seasonal variations.

    PubMed

    Gu, Dasa; Wang, Yuhang; Smeltzer, Charles; Liu, Zhen

    2013-11-19

    We analyzed satellite observations of nitrogen dioxide (NO2) columns by the Ozone Monitoring Instrument (OMI) over China from 2005 to 2010 in order to estimate the top-down anthropogenic nitrogen oxides (NOx) emission trends. Since NOx emissions were affected by the economic slowdown in 2009, we removed one year of abnormal data in the analysis. The estimated average emission trend is 4.01 ± 1.39% yr(-1), which is slower than the trend of 5.8-10.8% yr(-1) reported for previous years. We find large regional, seasonal, and urban-rural variations in emission trends. The average NOx emission trend of 3.47 ± 1.07% yr(-1) in warm season (June-September) is less than the trend of 5.03 ± 1.92% yr(-1) in cool season (October-May). The regional annual emission trends decrease from 4.76 ± 1.61% yr(-1) in North China Plain to 3.11 ± 0.98% yr(-1) in Yangtze River Delta and further down to -4.39 ± 1.81% yr(-1) in Pearl River Delta. The annual emission trends of the four largest megacities, Shanghai, Beijing, Guangzhou, and Shenzhen are -0.76 ± 0.29%, 0.69 ± 0.27%, -4.46 ± 1.22%, and -7.18 ± 2.88% yr(-1), considerably lower than the regional averages or surrounding rural regions. These results appear to suggest that a number of factors, including emission control measures of thermal power plants, increased hydro-power usage, vehicle emission regulations, and closure or migration of high-emission industries, have significantly reduced or even reversed the increasing trend of NOx emissions in more economically developed megacities and southern coastal regions, but their effects are not as significant in other major cities or less economically developed regions. PMID:24152067

  20. Revisiting the Earth's sea-level and energy budgets from 1961 to 2008

    NASA Astrophysics Data System (ADS)

    Church, John A.; White, Neil J.; Konikow, Leonard F.; Domingues, Catia M.; Cogley, J. Graham; Rignot, Eric; Gregory, Jonathan M.; van den Broeke, Michiel R.; Monaghan, Andrew J.; Velicogna, Isabella

    2011-09-01

    We review the sea-level and energy budgets together from 1961, using recent and updated estimates of all terms. From 1972 to 2008, the observed sea-level rise (1.8 ± 0.2 mm yr-1 from tide gauges alone and 2.1 ± 0.2 mm yr-1 from a combination of tide gauges and altimeter observations) agrees well with the sum of contributions (1.8 ± 0.4 mm yr-1) in magnitude and with both having similar increases in the rate of rise during the period. The largest contributions come from ocean thermal expansion (0.8 mm yr-1) and the melting of glaciers and ice caps (0.7 mm yr-1), with Greenland and Antarctica contributing about 0.4 mm yr-1. The cryospheric contributions increase through the period (particularly in the 1990s) but the thermosteric contribution increases less rapidly. We include an improved estimate of aquifer depletion (0.3 mm yr-1), partially offsetting the retention of water in dams and giving a total terrestrial storage contribution of -0.1 mm yr-1. Ocean warming (90% of the total of the Earth's energy increase) continues through to the end of the record, in agreement with continued greenhouse gas forcing. The aerosol forcing, inferred as a residual in the atmospheric energy balance, is estimated as -0.8 ± 0.4 W m-2 for the 1980s and early 1990s. It increases in the late 1990s, as is required for consistency with little surface warming over the last decade. This increase is likely at least partially related to substantial increases in aerosol emissions from developing nations and moderate volcanic activity.

  1. Reconciling estimates of the contemporary North American carbon balance among terrestrial biosphere models, atmospheric inversions and a new approach for estimating net ecosystem exchange from inventory-based data

    SciTech Connect

    Hayes, Daniel J; Turner, David P; Stinson, Graham; Mcguire, David; Wei, Yaxing; West, Tristram O.; Heath, Linda S.; De Jong, Bernardus; McConkey, Brian G.; Birdsey, Richard A.; Kurz, Werner; Jacobson, Andrew; Huntzinger, Deborah; Pan, Yude; Post, Wilfred M; Cook, Robert B

    2012-01-01

    We develop an approach for estimating net ecosystem exchange (NEE) using inventory-based information over North America (NA) for a recent 7-year period (ca. 2000 2006). The approach notably retains information on the spatial distribution of NEE, or the vertical exchange between land and atmosphere of all non-fossil fuel sources and sinks of CO2, while accounting for lateral transfers of forest and crop products as well as their eventual emissions. The total NEE estimate of a 327 252 TgC yr1 sink for NA was driven primarily by CO2 uptake in the Forest Lands sector (248 TgC yr1), largely in the Northwest and Southeast regions of the US, and in the Crop Lands sector (297 TgC yr1), predominantly in the Midwest US states. These sinks are counteracted by the carbon source estimated for the Other Lands sector (+218 TgC yr1), where much of the forest and crop products are assumed to be returned to the atmosphere (through livestock and human consumption). The ecosystems of Mexico are estimated tobe a small net source (+18 TgC yr1) due to land use change between 1993 and 2002. We compare these inventorybased estimates with results from a suite of terrestrial biosphere and atmospheric inversion models, where the mean continental-scale NEE estimate for each ensemble is 511 TgC yr1 and 931 TgC yr1, respectively. In the modeling approaches, all sectors, including Other Lands, were generally estimated to be a carbon sink, driven in part by assumed CO2 fertilization and/or lack of consideration of carbon sources from disturbances and product emissions. Additional fluxes not measured by the inventories, although highly uncertain, could add an additional 239 TgC yr1 to the inventory-based NA sink estimate, thus suggesting some convergence with the modeling approaches.

  2. H2O vapor excitation in dusty AGB envelopes. A PACS view of OH 127.8+0.0

    NASA Astrophysics Data System (ADS)

    Lombaert, R.; Decin, L.; de Koter, A.; Blommaert, J. A. D. L.; Royer, P.; De Beck, E.; de Vries, B. L.; Khouri, T.; Min, M.

    2013-06-01

    Context. AGB stars lose a large percentage of their mass in a dust-driven wind. This creates a circumstellar envelope, which can be studied through thermal dust emission and molecular emission lines. In the case of high mass-loss rates, this study is complicated by the high optical depths and the intricate coupling between gas and dust radiative transfer characteristics. An important aspect of the physics of gas-dust interactions is the strong influence of dust on the excitation of several molecules, including H2O. Aims: The dust and gas content of the envelope surrounding the high mass-loss rate OH/IR star OH 127.8+0.0, as traced by Herschel observations, is studied, with a focus on the H2O content and the dust-to-gas ratio. We report detecting a large number of H2O vapor emission lines up to J = 9 in the Herschel data, for which we present the measured line strengths. Methods: The treatments of both gas and dust species are combined using two numerical radiative transfer codes. The method is illustrated for both low and high mass-loss-rate sources. Specifically, we discuss different ways of assessing the dust-to-gas ratio: 1) from the dust thermal emission spectrum and the CO molecular gas line strengths; 2) from the momentum transfer from dust to gas and the measured gas terminal velocity; and 3) from the determination of the required amount of dust to reproduce H2O lines for a given H2O vapor abundance. These three diagnostics probe different zones of the outflow, for the first time allowing an investigation of a possible radial dependence of the dust-to-gas ratio. Results: We modeled the infrared continuum and the CO and H2O emission lines in OH 127.8+0.0 simultaneously. We find a dust-mass-loss rate of (0.5 ± 0.1) × 10-6 M⊙ yr-1 and an H2O ice fraction of 16% ± 2% with a crystalline-to-amorphous ratio of 0.8 ± 0.2. The gas temperature structure is modeled with a power law, leading to a constant gas-mass-loss rate between 2 × 10-5 M⊙ yr-1 and 1 × 10

  3. Global mercury emissions to the atmosphere from anthropogenic and natural sources

    NASA Astrophysics Data System (ADS)

    Pirrone, N.; Cinnirella, S.; Feng, X.; Finkelman, R. B.; Friedli, H. R.; Leaner, J.; Mason, R.; Mukherjee, A. B.; Stracher, G. B.; Streets, D. G.; Telmer, K.

    2010-02-01

    This paper provides an up-to-date assessment of global mercury emissions from anthropogenic and natural sources. On an annual basis, natural sources account for 5207 Mg of mercury released to the global atmosphere, including the contribution from re-emission processes, which are emissions of previously deposited mercury originating from anthropogenic and natural sources, and primary emissions from natural reservoirs. Anthropogenic sources, which include a large number of industrial point sources, are estimated to account for 2320 Mg of mercury emitted annually. The major contributions are from fossil-fuel fired power plants (810 Mg yr-1), artisanal small scale gold mining (400 Mg yr-1), non-ferrous metals manufacturing (310 Mg yr-1), cement production (236 Mg yr-1), waste disposal (187 Mg yr-1) and caustic soda production (163 Mg yr-1). Therefore, our current estimate of global mercury emissions suggests that the overall contribution from natural sources (primary emissions+re-emissions) and anthropogenic sources is nearly 7527 Mg per year, the uncertainty associated with these estimates are related to the typology of emission sources and source regions.

  4. Global mercury emissions to the atmosphere from anthropogenic and natural sources

    NASA Astrophysics Data System (ADS)

    Pirrone, N.; Cinnirella, S.; Feng, X.; Finkelman, R. B.; Friedli, H. R.; Leaner, J.; Mason, R.; Mukherjee, A. B.; Stracher, G. B.; Streets, D. G.; Telmer, K.

    2010-07-01

    This paper provides an up-to-date assessment of global mercury emissions from anthropogenic and natural sources. On an annual basis, natural sources account for 5207 Mg of mercury released to the global atmosphere, including the contribution from re-emission processes, which are emissions of previously deposited mercury originating from anthropogenic and natural sources, and primary emissions from natural reservoirs. Anthropogenic sources, which include a large number of industrial point sources, are estimated to account for 2320 Mg of mercury emitted annually. The major contributions are from fossil-fuel fired power plants (810 Mg yr-1), artisanal small scale gold mining (400 Mg yr-1), non-ferrous metals manufacturing (310 Mg yr-1), cement production (236 Mg yr-1), waste disposal (187 Mg yr-1) and caustic soda production (163 Mg yr-1). Therefore, our current estimate of global mercury emissions suggests that the overall contribution from natural sources (primary emissions + re-emissions) and anthropogenic sources is nearly 7527 Mg per year, the uncertainty associated with these estimates are related to the typology of emission sources and source regions.

  5. Relationship between C:N/C:O Stoichiometry and Ecosystem Services in Managed Production Systems

    PubMed Central

    Ghaley, Bhim B.; Sandhu, Harpinder S.; Porter, John R.

    2015-01-01

    Land use and management intensity can influence provision of ecosystem services (ES). We argue that forest/agroforestry production systems are characterized by relatively higher C:O/C:N and ES value compared to arable production systems. Field investigations on C:N/C:O and 15 ES were determined in three diverse production systems: wheat monoculture (Cwheat), a combined food and energy system (CFE) and a beech forest in Denmark. The C:N/C:O ratios were 194.1/1.68, 94.1/1.57 and 59.5/1.45 for beech forest, CFE and Cwheat, respectively. The economic value of the non-marketed ES was also highest in beech forest (US$ 1089 ha-1 yr-1) followed by CFE (US$ 800 ha-1 yr-1) and Cwheat (US$ 339 ha-1 yr-1). The combined economic value was highest in the CFE (US$ 3143 ha-1 yr-1) as compared to the Cwheat (US$ 2767 ha-1 yr-1) and beech forest (US$ 2365 ha-1 yr-1). We argue that C:N/C:O can be used as a proxy of ES, particularly for the non-marketed ES, such as regulating, supporting and cultural services. These ES play a vital role in the sustainable production of food and energy. Therefore, they should be considered in decision making and developing appropriate policy responses for land use management. PMID:25894553

  6. Water for food and nature in drought-prone tropics: vapour shift in rain-fed agriculture.

    PubMed Central

    Rockström, Johan

    2003-01-01

    This paper quantifies the eco-hydrological challenge up until 2050 of producing food in balance with goods and services generated by water-dependent ecosystems in nature. Particular focus is given to the savannah zone, covering 40% of the land area in the world, where water scarcity constitutes a serious constraint to sustainable development. The analysis indicates an urgent need for a new green revolution, which focuses on upgrading rain-fed agriculture. Water requirements to produce adequate diets for humans are shown to be relatively generic irrespective of hydro-climate, amounting to a global average of 1,300 m(3) cap(-1) yr(-1). Present food production requires an estimated 6,800 km(3) yr(-1) of consumptive green water (5,000 km(3) yr(-1) in rain-fed agriculture and 1,800 km(3) yr(-1) from irrigated crops). Without considering water productivity gains, an additional 5,800 km(3) yr(-1) of water is needed to feed a growing population in 2,050 and eradicate malnutrition. It is shown that the bulk of this water will be used in rain-fed agriculture. A dynamic analysis of water productivity and management options indicates that large 'crop per drop' improvements can be achieved at the farm level. Vapour shift in favour of productive green water flow as crop transpiration could result in relative water savings of 500 km(3) yr(-1) in semi-arid rain-fed agriculture. PMID:14728794

  7. Gull contributions of phosphorus and nitrogen to a Cape Cod kettle pond

    USGS Publications Warehouse

    Portnoy, J.W.; Soukup, M.A.

    1990-01-01

    Nutrient excretion rates and the annual contribution of P from the feces of the gulls Larus argentatus and L. marinus (and of N from L. argentatus) to the nutrient budget of Gull Pond (Wellfleet), a soft water seepage lake, have been estimated. Intensive year-round gull counts by species were combined with determinations of defecation rate and the nutrient content of feces to quantitatively assess the P loading rates associated with regular gull use of this coastal pond on a seasonal and annual basis. Total P loading from gulls was estimated to be 52 kg yr?1, with 17 kg from L. argentatus and 35 kg from L. marinus, resulting from about 5.0 ? 106 h yr?1 and 1.7 ? 106 h yr?1 of pond use. This compares with P loading estimates of 67 kg yr?1 from upgradient septic systems, 2 kg yr?1 from precipitation and 3 kg yr?1 from unpolluted ground water. Fifty-six percent of annual gull P loading was associated with migratory activity in late fall. Estimated annual N loading by L. argentatus was 14 kg TKN, 206 g NO3-N, and 1.85 g g NH3-N.

  8. Global riverine N and P transport to ocean increased during the twentieth century despite increased retention along the aquatic continuum

    NASA Astrophysics Data System (ADS)

    Beusen, A. H. W.; Bouwman, A. F.; Van Beek, L. P. H.; Mogollón, J. M.; Middelburg, J. J.

    2015-12-01

    Various human activities, including agriculture, water consumption, river damming, and aquaculture, have intensified over the last century. This has had a major impact on nitrogen (N) and phosphorus (P) cycling in global continental waters. In this study, we use a coupled nutrient-input, hydrology, in-stream nutrient retention model to quantitatively track the changes in the global freshwater N and P cycles over the 20th century. Our results suggest that, during this period, the global nutrient delivery to streams increased from 34 to 64 Tg N yr-1 and from 5 to 9 Tg N yr-1. Furthermore, in-stream retention and removal grew from 14 to 27 Tg N yr-1 and 3 to 5 Tg N yr-1. One of the major cause of increased retention is the growing number of reservoirs which now account for 24 and 22 % of global N and P retention/removal in freshwater systems, respectively. This increase in nutrient retention could not balance the increase in nutrient delivery to rivers with the consequence that river nutrient transport to the ocean increased from 19 to 37 Tg N yr-1 and from 2 to 4 Tg N yr-1. Human activities have also led to a global increase in the molar N : P ratio in freshwater bodies.

  9. The carbon balance of Russia

    NASA Astrophysics Data System (ADS)

    Dolman, Han; Shvidenko, Anatoly; Recapp Russia Synthesis Team

    2013-04-01

    We determine the net land to atmosphere flux of carbon in Russia, including Ukraine, Belarus and Kazakhstan using inventory based, eddy covariance, and inversion methods. Our high boundary estimate is -342 Tg C yr-1 from the eddy covariance method, and this is close to the upper bounds of the inventory based Land Ecosystem Assessment and inverse models estimate. A lower boundary estimate is provided at -1350 Tg C yr-1 from from the inversion models. The average of the three methods is -613.5 Tg C yr-1. The methane emission is estimated separately at 41.4 TgC yr-1. These three methods agree well within their respective error bounds. There is thus good consistency between bottom up and top down methods. The forests of Russia primarily cause the net atmosphere to land flux ( -692 Tg C yr-1 from the LEA) with remarkable little interannual variability. It remains however remarkable that the three methods provide such close estimates (-615, -662, -554 TgCyr-1) for NBP, given the inherent uncertainties in all of the approaches. The lack of recent forest inventories, the few eddy covariance sites and associated uncertainty with upscaling and under sampling of concentrations for the inversions are among the prime causes of the uncertainty. The DGVMs suggest a much lower uptake at -91Tg C yr-1 and we argue that this is caused by a high estimate of heterotrophic respiration compared to other methods.

  10. Relationship between C:N/C:O stoichiometry and ecosystem services in managed production systems.

    PubMed

    Ghaley, Bhim B; Sandhu, Harpinder S; Porter, John R

    2015-01-01

    Land use and management intensity can influence provision of ecosystem services (ES). We argue that forest/agroforestry production systems are characterized by relatively higher C:O/C:N and ES value compared to arable production systems. Field investigations on C:N/C:O and 15 ES were determined in three diverse production systems: wheat monoculture (Cwheat), a combined food and energy system (CFE) and a beech forest in Denmark. The C:N/C:O ratios were 194.1/1.68, 94.1/1.57 and 59.5/1.45 for beech forest, CFE and Cwheat, respectively. The economic value of the non-marketed ES was also highest in beech forest (US$ 1089 ha(-1) yr(-1)) followed by CFE (US$ 800 ha(-1) yr(-1)) and Cwheat (US$ 339 ha(-1) yr(-1)). The combined economic value was highest in the CFE (US$ 3143 ha(-1) yr(-1)) as compared to the Cwheat (US$ 2767 ha(-1) yr(-1)) and beech forest (US$ 2365 ha(-1) yr(-1)). We argue that C:N/C:O can be used as a proxy of ES, particularly for the non-marketed ES, such as regulating, supporting and cultural services. These ES play a vital role in the sustainable production of food and energy. Therefore, they should be considered in decision making and developing appropriate policy responses for land use management. PMID:25894553

  11. Global riverine N and P transport to ocean increased during the 20th century despite increased retention along the aquatic continuum

    NASA Astrophysics Data System (ADS)

    Beusen, Arthur H. W.; Bouwman, Alexander F.; Van Beek, Ludovicus P. H.; Mogollón, José M.; Middelburg, Jack J.

    2016-04-01

    Various human activities - including agriculture, water consumption, river damming, and aquaculture - have intensified over the last century. This has had a major impact on nitrogen (N) and phosphorus (P) cycling in global continental waters. In this study, we use a coupled nutrient-input-hydrology-in-stream nutrient retention model to quantitatively track the changes in the global freshwater N and P cycles over the 20th century. Our results suggest that, during this period, the global nutrient delivery to streams increased from 34 to 64 Tg N yr-1 and from 5 to 9 Tg P yr-1. Furthermore, in-stream retention and removal grew from 14 to 27 Tg N yr-1 and 3 to 5 Tg P yr-1. One of the major causes of increased retention is the growing number of reservoirs, which now account for 24 and 22 % of global N and P retention/removal in freshwater systems, respectively. This increase in nutrient retention could not balance the increase in nutrient delivery to rivers with the consequence that river nutrient transport to the ocean increased from 19 to 37 Tg N yr-1 and from 2 to 4 Tg P yr-1. Human activities have also led to a global increase in the molar N : P ratio in freshwater bodies.

  12. Comprehensive multiyear carbon budget of a temperate headwater stream

    NASA Astrophysics Data System (ADS)

    Argerich, Alba; Haggerty, Roy; Johnson, Sherri L.; Wondzell, Steven M.; Dosch, Nicholas; Corson-Rikert, Hayley; Ashkenas, Linda R.; Pennington, Robert; Thomas, Christoph K.

    2016-05-01

    Headwater streams comprise nearly 90% of the total length of perennial channels in global catchments. They mineralize organic carbon entering from terrestrial systems, evade terrestrial carbon dioxide (CO2), and generate and remove carbon through in-stream primary production and respiration. Despite their importance, headwater streams are often neglected in global carbon budgets primarily because of a lack of available data. We measured these processes, in detail, over a 10 year period in a stream draining a 96 ha forested watershed in western Oregon, USA. This stream, which represents only 0.4% of the watershed area, exported 159 kg C ha-1 yr-1, similar to the global exports for large rivers. Stream export was dominated by downstream transport of dissolved inorganic carbon (63 kg C ha-1 yr-1) and by evasion of CO2 to the atmosphere (42 kg C ha-1 yr-1), leaving the remainder of 51 kg C ha-1 yr-1 for downstream transport of organic carbon (17 kg C ha-1 yr-1 and 34 kg C ha-1 yr-1 in dissolved and particulate form, respectively).

  13. Fifteen-Year Global Time Series of Satellite-Derived Fine Particulate Matter

    SciTech Connect

    Boys, B. L.; Martin, R. V.; van Donkelaar, A.; MacDonell, R. J.; Hsu, N. C.; Cooper, M. J.; Yantosca, R. M.; Lu, Z.; Streets, D. G.; Zhang, Q.; Wang, S. W.

    2014-10-07

    Ambient fine particulate matter (PM2.5) is a leading environmental risk factor for premature mortality. We use aerosol optical depth (AOD) retrieved from two satellite instruments, MISR and SeaWiFS, to produce a unified 15-year global time series (1998-2012) of ground-level PM2.5 concentration at a resolution of 1 degrees x 1 degrees. The GEOS-Chem chemical transport model (CTM) is used to relate each individual AOD retrieval to ground-level PM2.5. Four broad areas showing significant, spatially coherent, annual trends are examined in detail: the Eastern U.S. (-0.39 +/- 0.10 mu g m(-3) yr(-1)), the Arabian Peninsula (0.81 +/- 0.21 mu g m(-3) yr(-1)), South Asia (0.93 +/- 0.22 mu g m(-3) yr(-1)) and East Asia (0.79 +/- 0.27 mu g m(-3) yr(-1)). Over the period of dense in situ observation (1999-2012), the linear tendency for the Eastern U.S. (-0.37 +/- 0.13 mu g m(-3) yr(-1)) agrees well with that from in situ measurements (-0.38 +/- 0.06 mu g m(-3) yr(-1)). A GEOS-Chem simulation reveals that secondary inorganic aerosols largely explain the observed PM2.5 trend over the Eastern U.S., South Asia, and East Asia, while mineral dust largely explains the observed trend over the Arabian Peninsula.

  14. Nitrogen in crop production: An account of global flows

    NASA Astrophysics Data System (ADS)

    Smil, Vaclav

    1999-06-01

    Human activities have roughly doubled the amount of reactive N that enters the element's biospheric cycle. Crop production is by far the single largest cause of this anthropogenic alteration. Inorganic fertilizers now provide 80 Tg N yr-1 (Tg = 1012 g), managed (symbiotic) biofixation adds about 20 Tg N yr-1, and between 28 and 36 Tg N yr-1 are recycled in organic wastes. Anthropogenic inputs (including N in seeds and irrigation water) now supply about 85% of 170 (151-186) Tg N reaching the world's cropland every year. About half of this input, 85 Tg N yr-1, is taken up by harvested crops and their residues. Quantification of N losses from crop fields is beset by major uncertainties. Losses to the atmosphere (denitrification and volatilization) amount to 26-60 Tg N yr-1, while waters receive (from leaching and erosion) 32-45 Tg N yr-1. These N losses are the major reason behind the growing concerns about the enrichment of the biosphere with reactive N. The best evidence suggests that in spite of some significant local and regional losses, the world's agricultural land accumulates N. The addition of 3-4 billion people before the year 2050 will require further substantial increases of N input in cropping, but a large share of this demand can come from improved efficiency of N fertilizer use.

  15. Population dynamics and secondary production of the cockle Cerastoderma edule: A comparison between Merja Zerga (Moroccan Atlantic Coast) and Arcachon Bay (French Atlantic Coast)

    NASA Astrophysics Data System (ADS)

    Gam, Mériame; de Montaudouin, Xavier; Bazairi, Hocein

    2010-04-01

    Cockle ( Cerastoderma edule) population dynamics were studied at the southern limit of the distribution of this marine bivalve in Merja Zerga, Morocco. Parameters such as growth, mortality, and production were compared with those of a population at Arcachon Bay (France) a site in the center of the cockle's range. At each sampling period between two and three cohorts were simultaneously observed at each site and the average total abundance was usually higher at Merja Zerga. Recruitment occurred at both sites in spring when temperature rose above 19 °C, independently of the month. In Merja Zerga, winter recruitment was also observed at one occasion, following high sediment disturbance. The first year (2005-06) at Merja Zerga, the mortality rate was close to nil for juveniles and was Z = 1.5 yr - 1 for adults, providing a high production (64 g dry weight m - 2 yr - 1 ). At Arcachon during the same period, the juvenile mortality rate was Z = 10.9 yr - 1 , the adult mortality rate was 3.4 yr - 1 and production was 26 gDW m -2 yr - 1 . The second year (2006-07), mortality after recruitment was much higher ( Z = 8.6 yr - 1 , for juveniles) and similar to what was observed at Arcachon ( Z = 8.4 yr - 1 ). Mortality rate of adults was higher at Merja Zerga ( Z = 3.0 yr - 1 ) than at Arcachon ( Z = 1.5 yr - 1 ). Production was lower at Arcachon than at Merja Zerga although growth performances were higher at Arcachon. The higher growth performance at Arcachon ( Φ' = 3.3) was mainly due to high asymptotic length ( L∞ = 38 mm) and was related to low intraspecific competition compared to Merja Zerga where cockle abundance was higher ( Φ' = 3.1, L∞ = 31 mm). P/B was low in both sites and slightly higher at Arcachon (1.1-1.5 against 1.0-1.1 yr - 1 ). At Arcachon, recruitment was correlated with temperature, a peak occurring when temperature rose above 19 °C (June-July). At Merja Zerga, recruitment was already 2-3 months earlier but was not significantly correlated to

  16. Environmental footprints show China and Europe’s evolving resource appropriation for soybean production in Mato Grosso, Brazil

    NASA Astrophysics Data System (ADS)

    Lathuillière, Michael J.; Johnson, Mark S.; Galford, Gillian L.; Couto, Eduardo G.

    2014-07-01

    Mato Grosso has become the center of Brazil’s soybean industry, with production located across an agricultural frontier expanding into savanna and rainforest biomes. We present environmental footprints of soybean production in Mato Grosso and resource flows accompanying exports to China and Europe for the 2000s using five indicators: deforestation, land footprint (LF), carbon footprint (CF), water footprint (WF), and nutrient footprints. Soybean production was associated with 65% of the state’s deforestation, and 14-17% of total Brazilian land use change carbon emissions. The decade showed two distinct production systems illustrated by resources used in the first and second half of the decade. Deforestation and carbon footprint declined 70% while land, water, and nutrient footprints increased almost 30% between the two periods. These differences coincided with a shift in Mato Grosso’s export destination. Between 2006 and 2010, China surpassed Europe in soybean imports when production was associated with 97 m2 deforestation yr-1 ton-1 of soybean, a LF of 0.34 ha yr-1 ton-1, a carbon footprint of 4.6 ton CO2-eq yr-1 ton-1, a WF of 1908 m3 yr-1 ton-1, and virtual phosphorous and potassium of 5.0 kg P yr-1 ton-1 and 0.0042 g K yr-1 ton-1. Mato Grosso constructs soil fertility via phosphorous and potassium fertilizer sourced from third party countries and imported into the region. Through the soybean produced, Mato Grosso then exports both water derived from its abundant, seasonal precipitation and nutrients obtained from fertilizer. In 2010, virtual water flows were 10.3 km3 yr-1 to China and 4.1 km3 yr-1 to Europe. The total embedded nutrient flows to China were 2.12 Mtons yr-1 and 2.85 Mtons yr-1 to Europe. As soybean production grows with global demand, the role of Mato Grosso’s resource use and production vulnerabilities highlight the challenges with meeting future international food security needs.

  17. Interactions between nitrogen deposition, land cover conversion, and climate change determine the contemporary carbon balance of Europe

    NASA Astrophysics Data System (ADS)

    Churkina, G.; Zaehle, S.; Hughes, J.; Viovy, N.; Chen, Y.; Jung, M.; Heumann, B. W.; Ramankutty, N.; Heimann, M.; Jones, C.

    2010-09-01

    European ecosystems are thought to take up large amounts of carbon, but neither the rate nor the contributions of the underlying processes are well known. In the second half of the 20th century, carbon dioxide concentrations have risen by more that 100 ppm, atmospheric nitrogen deposition has more than doubled, and European mean temperatures were increasing by 0.02 °C yr-1. The extents of forest and grasslands have increased with the respective rates of 5800 km2 yr-1 and 1100 km2 yr-1 as agricultural land has been abandoned at a rate of 7000 km2 yr-1. In this study, we analyze the responses of European land ecosystems to the aforementioned environmental changes using results from four process-based ecosystem models: BIOME-BGC, JULES, ORCHIDEE, and O-CN. The models suggest that European ecosystems sequester carbon at a rate of 56 TgC yr-1 (mean of four models for 1951-2000) with strong interannual variability (±88 TgC yr-1, average across models) and substantial inter-model uncertainty (±39 TgC yr-1). Decadal budgets suggest that there has been a continuous increase in the mean net carbon storage of ecosystems from 85 TgC yr-1 in 1980s to 108 TgC yr-1 in 1990s, and to 114 TgC yr-1 in 2000-2007. The physiological effect of rising CO2 in combination with nitrogen deposition and forest re-growth have been identified as the important explanatory factors for this net carbon storage. Changes in the growth of woody vegetation are suggested as an important contributor to the European carbon sink. Simulated ecosystem responses were more consistent for the two models accounting for terrestrial carbon-nitrogen dynamics than for the two models which only accounted for carbon cycling and the effects of land cover change. Studies of the interactions of carbon-nitrogen dynamics with land use changes are needed to further improve the quantitative understanding of the driving forces of the European land carbon balance.

  18. Comparison of Forest Carbon Changes in China and the Continental U.S.

    NASA Astrophysics Data System (ADS)

    Ju, W.

    2015-12-01

    Weimin Ju1, Chunhua Zhang1, Jing M. Chen2, Fangmin Zhang3, Xiqun Wang4, 1International Institute for Earth System Science, Nanjing University, Nanjing, 210023, China 2 Department of Geography, University of Toronto, Toronto, Ontario, Canada 3Jiangsu Key Laboratory of Agricultural Meteorology, College of Applied Meteorology, Nanjing University of Information Science and Technology, Nanjing, Jiangsu, China 4Planning and Design Institute of Forest Products Industry, State Forestry Administration of China, Beijing, 100010, China Carbon changes of forests in China and the continental U.S. were investigated using national forest inventory datasets and the InTEC model, which integrates the effects of forest age, atmospheric CO2concentration, nitrogen deposition, and climate. Pervious to simulations, the changes of net primary productivity (NPP) in the InTEC model was calibrated using field measured NPP and ages of forests. Both forest inventory and model simulations indicated that carbon sequestration by forests in China increased significantly in recent decades. The forest inventory based estimates indicated that biomass carbon sinks of forest stands were 86.0 Tg C yr-1 and 174.0 Tg C yr-1 in China and 132.5 Tg C yr-1and 147.0 Tg C yr-1 in the continental U.S. during the periods from 1989 to 2008 and from 1999 to 2008, respectively. The InTEC model simulations indicated that the total carbon sinks of forests were 170.4 Tg C yr-1, 200.2 Tg C yr-1, 217.7 Tg C yr-1 in China and 225.9 Tg C yr-1, 222.7 Tg C yr-1, and 230.5 Tg C yr-1 in the continental U.S. during the periods from 1981 to 2010, from 1991 to 2010, and from 2001 to 2010, respectively. Forest carbon sink density was higher in China than that in the continental U.S., mainly due to a larger fraction of young forests in China. Total carbon sequestration by forests in China was close to that in the continental U.S. during the recent decade.

  19. A probabilistic estimate of global marine N-fixation and denitrification

    NASA Astrophysics Data System (ADS)

    Eugster, Olivier; Gruber, Nicolas

    2012-12-01

    We determine the global rates of marine N-fixation and denitrification and their associated uncertainties by combining marine geochemical and physical data with a new two-dimensional box model that separates the Atlantic from the IndoPacific basins. The uncertainties are estimated using a probabilistic approach on the basis of a suite of 2500 circulation configurations of this box model. N-fixation and denitrification are diagnosed in an inverse manner for each of these configurations using N*, P*, and the stable nitrogen isotope composition of nitrate as data constraints. Our approach yields a median water column denitrification rate of 52 TgN yr-1 (39 to 66 TgN yr-1, 5th to 95th percentile) and a median benthic denitrification rate of 93 TgN yr-1 (68 to 122 TgN yr-1). The resulting benthic-to-water column denitrification ratio of 1.8 confirms that the isotopic signature of water column denitrification has a limited influence on the global mean stable isotopic value of nitrate due to the dilution of the waters with a denitrification signal with the remainder of the ocean's nitrate pool. On the basis of two different approaches, we diagnose a global N-fixation rate of between 94 TgN yr-1 and 175 TgN yr-1, with a best estimate of 131 TgN yr-1 and 134 TgN yr-1, respectively. Most of the N-fixation occurs in the IndoPacific suggesting a relative close spatial coupling between sources and sinks in the ocean. Our N-fixation and denitrification estimates plus updated estimates of atmospheric deposition and riverine input yield a pre-industrial marine N cycle that is balanced to within 3 TgN yr-1 (-38 to 40 TgN yr-1). Our budget implies a median residence time for fixed N of 4,200 yr (3,500 to 5,000 yr).

  20. Strain accumulation and rotation in western Nevada, 1993-2000

    USGS Publications Warehouse

    Svarc, J.L.; Savage, J.C.; Prescott, W.H.; Ramelli, A.R.

    2002-01-01

    The positions of 44 GPS monuments in an array extending from the Sierra Nevada at the latitude of Reno to near Austin, Nevada, have been measured several times in the 1993-2000 interval. The western half of the array spans the Walker Lane belt, whereas the eastern half spans the central Nevada seismic zone (CNSZ). The principal strain rates in the Walker Lane belt are 29.6 ?? 5.3 nstrain yr-1 N88.4??E ?? 5.4?? and -12.8 ?? 6.0 nanostrain yr-1 N01.6??W ?? 5.4??, extension reckoned positive, and the clockwise (as seen from above the Earth) rotation rate about a vertical axis is 13.6 ?? 4.0 nrad yr-1. The quoted uncertainties are standard deviations. The motion in the Walker Lane belt can then be represented by a zone striking N35??W subject to 16.8 ?? 4.9 nstrain yr-1 extension perpendicular to it and 19.5 ?? 4.0 nstrain yr-1 right-lateral, simple shear across it. The N35??W strike of the zone is the same as the direction of the local tangent to the small circle drawn about the Pacific-North America pole of rotation. The principal strain rates for the CNSZ are 46.2 ?? 11.0 nstrain yr-1 N49.9??W ?? 6.0?? and -13.6 ?? 6.1 nstrain yr-1 N40.1??E ?? 6.0??, and the clockwise rotation rate about a vertical axis is 20.3 ?? 6.3 nrad yr-1. The motion across the CNSZ can then be represented by a zone striking N12??E subject to 32.6 ?? 11.0 nstrain yr-1 extension perpendicular to it and 25.1 ?? 6.3 nstrain yr-1 right-lateral, simple shear across it. The N12??E strike of the zone is similar to the strikes of the faults (Rainbow Mountain, Fairview Peak, and Dixie Valley) within it.

  1. Estimate of changes in agricultural terrestrial nitrogen pathways and ammonia emissions from 1850 to present in the Community Earth System Model

    NASA Astrophysics Data System (ADS)

    Riddick, Stuart; Ward, Daniel; Hess, Peter; Mahowald, Natalie; Massad, Raia; Holland, Elisabeth

    2016-06-01

    Nitrogen applied to the surface of the land for agricultural purposes represents a significant source of reactive nitrogen (Nr) that can be emitted as a gaseous Nr species, be denitrified to atmospheric nitrogen (N2), run off during rain events or form plant-useable nitrogen in the soil. To investigate the magnitude, temporal variability and spatial heterogeneity of nitrogen pathways on a global scale from sources of animal manure and synthetic fertilizer, we developed a mechanistic parameterization of these pathways within a global terrestrial land model, the Community Land Model (CLM). In this first model version the parameterization emphasizes an explicit climate-dependent approach while using highly simplified representations of agricultural practices, including manure management and fertilizer application. The climate-dependent approach explicitly simulates the relationship between meteorological variables and biogeochemical processes to calculate the volatilization of ammonia (NH3), nitrification and runoff of Nr following manure or synthetic fertilizer application. For the year 2000, approximately 125 Tg N yr-1 is applied as manure and 62 Tg N yr-1 is applied as synthetic fertilizer. We estimate the resulting global NH3 emissions are 21 Tg N yr-1 from manure (17 % of manure production) and 12 Tg N yr-1 from fertilizer (19 % of fertilizer application); reactive nitrogen runoff during rain events is calculated as 11 Tg N yr-1 from manure and 5 Tg N yr-1 from fertilizer. The remaining nitrogen from manure (93 Tg N yr-1) and synthetic fertilizer (45 Tg N yr-1) is captured by the canopy or transferred to the soil nitrogen pools. The parameterization was implemented in the CLM from 1850 to 2000 using a transient simulation which predicted that, even though absolute values of all nitrogen pathways are increasing with increased manure and synthetic fertilizer application, partitioning of nitrogen to NH3 emissions from manure is increasing on a percentage basis, from

  2. Recent decadal trends in global phytoplankton composition

    NASA Astrophysics Data System (ADS)

    Rousseaux, Cecile S.; Gregg, Watson W.

    2015-10-01

    Identifying major trends in biogeochemical composition of the oceans is essential to improve our understanding of biological responses to climate forcing. Using the NASA Ocean Biogeochemical Model combined with ocean color remote sensing data assimilation, we assessed the trends in phytoplankton composition (diatoms, cyanobacteria, coccolithophores, and chlorophytes) at a global scale for the period 1998-2012. We related these trends in phytoplankton to physical conditions (surface temperature, surface photosynthetically available radiation (PAR), and mixed layer depth (MLD)) and nutrients (iron, silicate, and nitrate). We found a significant global decline in diatoms (-1.22% yr-1, p < 0.05). This trend was associated with a significant (p < 0.05) shallowing of the MLD (-0.20% yr-1), a significant increase in PAR (0.09% yr-1), and a significant decline in nitrate (-0.38% yr-1). The global decline in diatoms was mostly attributed to their decline in the North Pacific (-1.00% yr-1, p < 0.05), where the MLD shallowed significantly and resulted in a decline in all three nutrients (p < 0.05). None of the other phytoplankton groups exhibited a significant change globally, but regionally there were considerable significant trends. A decline in nutrients in the northernmost latitudes coincided with a significant decline in diatoms (North Pacific, -1.00% yr-1) and chlorophytes (North Atlantic, -9.70% yr-1). In the northern midlatitudes (North Central Pacific and Atlantic) where nutrients were more scarce, a decline in nutrients was associated with a decline in smaller phytoplankton: cyanobacteria declined significantly in the North Central Pacific (-0.72% yr-1) and Atlantic (-1.56% yr-1), and coccolithophores declined significantly in the North Central Atlantic (-2.06% yr-1). These trends represent the diversity and complexity of mechanisms that drives phytoplankton communities to adapt to variable conditions of nutrients, light, and mixed layer depth. These results provide

  3. Decadal trends in global CO emissions as seen by MOPITT

    NASA Astrophysics Data System (ADS)

    Yin, Y.; Chevallier, F.; Ciais, P.; Broquet, G.; Fortems-Cheiney, A.; Pison, I.; Saunois, M.

    2015-12-01

    Negative trends of carbon monoxide (CO) concentrations are observed in the recent decade by both surface measurements and satellite retrievals over many regions of the globe, but they are not well explained by current emission inventories. Here, we analyse the observed CO concentration decline with an atmospheric inversion that simultaneously optimizes the two main CO sources (surface emissions and atmospheric hydrocarbon oxidations) and the main CO sink (atmospheric hydroxyl radical OH oxidation). Satellite CO column retrievals from Measurements of Pollution in the Troposphere (MOPITT), version 6, and surface observations of methane and methyl chloroform mole fractions are assimilated jointly for the period covering 2002-2011. Compared to the model simulation prescribed with prior emission inventories, trends in the optimized CO concentrations show better agreement with that of independent surface in situ measurements. At the global scale, the atmospheric inversion primarily interprets the CO concentration decline as a decrease in the CO emissions (-2.3 % yr-1), more than twice the negative trend estimated by the prior emission inventories (-1.0 % yr-1). The spatial distribution of the inferred decrease in CO emissions indicates contributions from western Europe (-4.0 % yr-1), the United States (-4.6 % yr-1) and East Asia (-1.2 % yr-1), where anthropogenic fuel combustion generally dominates the overall CO emissions, and also from Australia (-5.3 % yr-1), the Indo-China Peninsula (-5.6 % yr-1), Indonesia (-6.7 % y-1), and South America (-3 % yr-1), where CO emissions are mostly due to biomass burning. In contradiction with the bottom-up inventories that report an increase of 2 % yr-1 over China during the study period, a significant emission decrease of 1.1 % yr-1 is inferred by the inversion. A large decrease in CO emission factors due to technology improvements would outweigh the increase in carbon fuel combustions and may explain this decrease. Independent

  4. Hubble Space Telescope WFPC2 Study of the Trapezium Cluster: The Influence of Circumstellar Disks on the Initial Mass Function

    NASA Astrophysics Data System (ADS)

    Robberto, M.; Song, J.; Mora Carrillo, G.; Beckwith, S. V. W.; Makidon, R. B.; Panagia, N.

    2004-05-01

    We have performed the first measures of mass accretion rates in the core of the Orion Nebula Cluster. Four adjacent fields centered on the Trapezium stars have been imaged in the U and B bands using the Wide Field Planetary Camera 2 (WFPC2) on board the Hubble Space Telescope. We obtained photometry for 91 stars in the U band (F336W) and 71 stars in the B band (F439W). The WFPC2 archive was also searched to obtain complementary V-band (F547M) and I-band (F791W) photometry. In this paper we focus our attention on a group of 40 stars with known spectral types and complete UBVI WFPC2 photometry. We locate each star on the H-R diagram, considering both the standard ISM reddening law with RV=3.1 and the ``anomalous'' reddening law with RV=5.5 more appropriate for the Orion Nebula. Then we derive the stellar masses and ages by comparing with the evolutionary tracks and isochrones calculated by D'Antona & Mazzitelli and Palla & Stahler. Approximately three-quarters of the sources show excess luminosity in the U band, which we attribute to mass accretion. The known correlation between the U-band excess and the total accretion luminosity, recalibrated for our photometric system, allows us to estimate the accretion rates, which are all found to be in the range 10-8 to 10-12 Msolar yr-1. For stars older than 1 Myr, there is some evidence of a relation between mass accretion rates and stellar age. Overall, mass accretion rates appear lower than those measured by other authors in the Orion flanking fields or in Taurus-Auriga. Mass accretion rates remain low even in the vicinity of the 10-5 Msolar yr-1 birth line of Palla & Stahler, suggesting that in the core of the Trapezium cluster, disk accretion has been recently depressed by an external mechanism. We suggest that the UV radiation generated by the Trapezium OB stars, responsible for the disk evaporation, may also cause the drop of the mass accretion rate. In this scenario, low-mass stars may terminate their pre

  5. Using (137)Cs and (210)Pbex and other sediment source fingerprints to document suspended sediment sources in small forested catchments in south-central Chile.

    PubMed

    Schuller, P; Walling, D E; Iroumé, A; Quilodrán, C; Castillo, A; Navas, A

    2013-10-01

    A study of the impact of forest harvesting operations on sediment mobilization from forested catchments has been undertaken in south-central Chile. The study focused on two sets of small paired catchments (treatment and control), with similar soil type, but contrasting mean annual rainfall, located about 400 km apart at Nacimiento (1200 mm yr(-1)) and Los Ulmos (2500 mm yr(-1)). The objective was to study the changes in the relative contribution of the primary sources of fine sediment caused by forestry operations. Attention focused on the pre-harvest and post-harvest periods and the post-replanting period was included for the Nacimiento treatment catchment. The sediment source fingerprinting technique was used to document the contributions of the potential sources. Emphasis was placed on discriminating between the forest slopes, forest roads and channel erosion as potential sources of fine sediment and on assessing the relative contributions of these three sources to the sediment yield from the catchments. The fallout radionuclides (FRNs) (137)Cs and excess lead-210, the environmental radionuclides (226)Ra and (40)K and soil organic matter (SOM) were tested as possible fingerprints for discriminating between potential sediment sources. The Kruskal-Wallis test and discriminant function analysis were used to guide the selection of the optimum fingerprint set for each catchment and observation period. Either one or both of the FRNs were selected for inclusion in the optimum fingerprint for all datasets. The relative contribution of each sediment source to the target sediment load was estimated using the selected fingerprint properties, and a mixing model coupled with a Monte Carlo simulation technique that takes account of uncertainty in characterizing sediment source properties. The goodness of fit of the mixing model was tested by comparing the measured and simulated fingerprint properties for the target sediment samples. In the Nacimiento treatment catchment

  6. On the discovery of CO nighttime emissions on Titan by Cassini/VIMS: Derived stratospheric abundances and geological implications

    NASA Astrophysics Data System (ADS)

    Baines, Kevin H.; Drossart, Pierre; Lopez-Valverde, Miguel A.; Atreya, Sushil K.; Sotin, Christophe; Momary, Thomas W.; Brown, Robert H.; Buratti, Bonnie J.; Clark, Roger N.; Nicholson, Philip D.

    2006-12-01

    We present a quantitative analysis of CO thermal emissions discovered on the nightside of Titan by Baines et al. [2005. The atmospheres of Saturn and Titan in the near-infrared: First results of Cassini/VIMS. Earth, Moon, and Planets, 96, 119-147]. in Cassini/VIMS spectral imagery. We identify these emission features as the P and R branches of the 1-0 vibrational band of carbon monoxide (CO) near 4.65 μm. For CH 3D, the prominent Q branch of the ν 2 fundamental band of CH 3D near 4.55 μm is apparent. CO 2 emissions from the strong v3 vibrational band are virtually absent, indicating a CO 2 abundance several orders of magnitude less than CO, in agreement with previous investigations. Analysis of CO emission spectra obtained over a variety of altitudes on Titan's nightside limb indicates that the stratospheric abundance of CO is 32±15 ppm, and together with other recent determinations, suggests a vertical distribution of CO nearly constant at this value from the surface throughout the troposphere to at least the stratopause near 300 km altitude. The corresponding total atmospheric content of CO in Titan is ˜2.9±1.5×10 14 kg. Given the long lifetime of CO in the oxygen-poor Titan atmosphere (˜0.5-1.0 Gyr), we find a mean CO atmospheric production rate of 6±3×10 5 kg yr -1. Given the lack of primordial heavy noble gases observed by Huygens [Niemann et al., 2005. The abundances of constituents of Titan's atmosphere from the GCMS on the Huygens probe. Nature, 438, 779-784], the primary source of atmospheric CO is likely surface emissions. The implied CO/CH 4 mixing ratio of near-surface material is 1.8±0.9×10 -4, based on an average methane surface emission rate over the past 0.5 Gyr of 1.3×10 -13 gm cm -2 s -1 as required to balance hydrocarbon haze production via methane photolysis [Wilson and Atreya, 2004. Current state of modeling the photochemistry of Titan's mutually dependent atmosphere and ionosphere. J. Geophys. Res. 109, E06002 Doi:10.1029/2003JE

  7. A low pre-infall mass for the Carina dwarf galaxy from disequilibrium modelling

    PubMed Central

    Ural, Uğur; Wilkinson, Mark I.; Read, Justin I.; Walker, Matthew G.

    2015-01-01

    Dark matter-only simulations of galaxy formation predict many more subhalos around a Milky Way-like galaxy than the number of observed satellites. Proposed solutions require the satellites to inhabit dark matter halos with masses 109–1010 Msun at the time they fell into the Milky Way. Here we use a modelling approach, independent of cosmological simulations, to obtain a pre-infall mass of Msun for one of the Milky Way's satellites: Carina. This determination of a low halo mass for Carina can be accommodated within the standard model only if galaxy formation becomes stochastic in halos below ∼1010 Msun. Otherwise Carina, the eighth most luminous Milky Way dwarf, would be expected to inhabit a significantly more massive halo. The implication of this is that a population of ‘dark dwarfs' should orbit the Milky Way: halos devoid of stars and yet more massive than many of their visible counterparts. PMID:26133650

  8. Formation of the first galaxies under Population III stellar feedback

    NASA Astrophysics Data System (ADS)

    Jeon, Myoungwon

    2015-01-01

    The first galaxies, which formed a few hundred million years after the big bang, are related to important cosmological questions. Given thatthey are thought to be the basic building blocks of large galaxies seen today, understanding their formation and properties is essentialto studying galaxy formation as a whole. In this dissertation talk, I will present the results of our highly-resolved cosmological ab-initio simulations to understand the assembly process of first galaxies under the feedback from the preceding generations of first stars, the so-called Population III (Pop III). The first stars formed at z≲30 in dark matter (DM) minihalos with M_{vir}=10^5-10^6Msun, predominately via molecular hydrogen (H_2) cooling. Radiation from Pop III stars dramatically altered the gas within their host minihalos, through photoionization, photoheating, and photoevaporation. Once a Pop III star explodes as a supernova (SN), heavy elements are dispersed, enriching the interstellar (ISM) and intergalactic medium (IGM), thus initiating the process of chemical evolution. I will begin by presenting how the SN explosion of the first stars influences early cosmic history, specifically assessing the time delay in further star formation and tracing the evolution of metal-enriched gas until the second episode star formation happens. These results will show the role of Pop III supernovae on the star formation transition from Pop III to Population II. Additionally, the more distant, diffuse IGM was heated by X-rays emitted by accreting black holes (BHs), or high-mass X-ray binaries (HMXBs), both remnants of Pop III stars. I will present results of a series of simulations where we study the impact of X-ray feedback from BHs and HMXBs on the star formation history in the early universe, and discuss the resulting implications on reionization. I will also present the role of X-rays on the early BH growth, providing constraints on models for supermassive black hole formation. Finally, I

  9. Massive star-forming regions across the galaxy

    NASA Astrophysics Data System (ADS)

    Rygl, Kazi Lucie Jessica

    2010-04-01

    Star-forming regions trace the spiral structure of the Galaxy. They are regions of increased column density and therefore traced well by the extinction in the mid-infrared based on the Spitzer/GLIMPSE 3.6-4.5 micron color excess maps. A sample of 25 high extinction clouds (HECs) was studied in the 1.2 mm dust continuum emission, and followed up by observations of ammonia plus several other molecules using the Effelsberg 100m, IRAM 30m and APEX telescopes. With these data we want to investigate the most early stages of massive star formation, which are currently still largely unknown. Three cloud classes were defined from their morphology in the 1.2 mm continuum maps: the early diffuse HECs, with a low contrast between the clump and cloud emission; the peaked HECs, with an increased contrast; the late multiply peaked HECs, with more than one clump and a high contrast between the clump and the cloud emission. The clouds are cold (T 16 K) and massive (M 800 M_sun) and contain dense clumps (n 10^5 cm^{-3}) of 0.3 pc in size. These clumps were investigated for evidence of gravitational collapse or expansion, for high velocity outflows, and for the presence of young stellar objects. Based on these results we interpret the three cloud classes as an evolutionary sequence of star-forming clouds. Accurate distances are a crucial parameter for establishing the mass, size, and luminosity of an object. Also, for understanding the spiral structure of the Galaxy trustworthy distances are necessary. The most accurate method to measure these is the trigonometric parallax. Using the European Very Large Baseline Interferometry Network of radio antennas we measured, for the first time, parallaxes of 6.7 GHz methanol masers. This transition belongs to the strongest maser species in the Galaxy, it is stable and observed toward numerous massive star-forming regions. We measured distances and proper motions toward L 1287, L 1206, NGC 281-W, ON 1 and S 255, and obtained their 3-dimensional

  10. The evolution of the equivalent width of the Hα emission line and specific star formation rate in star-forming galaxies at 1 < z < 5

    NASA Astrophysics Data System (ADS)

    Mármol-Queraltó, E.; McLure, R. J.; Cullen, F.; Dunlop, J. S.; Fontana, A.; McLeod, D. J.

    2016-08-01

    We present the results of a study which uses spectral energy distribution (SED) fitting to investigate the evolution of the equivalent width (EW) of the Hα emission line in star-forming galaxies over the redshift interval 1 < z < 5. After first demonstrating the ability of our SED-fitting technique to recover EW(Hα) using a sample of galaxies at z ≃ 1.3 with EW(Hα) measurements from 3D-HST grism spectroscopy, we proceed to apply our technique to samples of spectroscopically confirmed and photometric-redshift selected star-forming galaxies at z ≥ 1 in the CANDELS (Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey) UDS and GOODS-S fields. Confining our analysis to a constant stellar mass range (9.5 < log (M⋆/M⊙) < 10.5), we find that the median EW(Hα) evolves only modestly with redshift, reaching a rest-frame value of EW(Hα) =301 ± 30 Å by redshift z ≃ 4.5. Furthermore, using estimates of star formation rate (SFR) based on both UV luminosity and Hα line flux, we use our galaxy samples to compare the evolution of EW(Hα) and specific star formation rate (sSFR). Our results indicate that over the redshift range 1 < z < 5, the evolution displayed by EW(Hα) and sSFR is consistent, and can be adequately parametrized as ∝ (1 + z)1.0 ± 0.2. As a consequence, over this redshift range, we find that the sSFR and rest-frame EW(Hα) of star-forming galaxies with stellar masses M⋆ ≃ 10^{10}{ M_{sun;} are related by EW(Hα)/Å = (63 ± 7) × sSFR/Gyr-1. Given the current uncertainties in measuring the SFRs of high-redshift galaxies, we conclude that EW(Hα) provides a useful independent tracer of sSFR for star-forming galaxies out to redshifts of z = 5.

  11. The Accretion Rates and White Dwarf Components of Nova-Like Cataclysmic Variables

    NASA Astrophysics Data System (ADS)

    Mizusawa, Trisha; Merritt, J.; Bonaro, M.; Foran, S.; Plumberg, C.; Stewart, H.; Wiley, T.; Ballouz, R.; Sion, E.

    2009-01-01

    We present the results of a multi-component synthetic spectral analysis of the archival far ultraviolet spectra of several key nova-like variables including members of the SW Sex, RW Tri, UX UMa and VY Scl subclasses: KR Aur, V795 Her, BP Lyn, V825 Her, HL Aqr, RW Tri and V425 Cas. Accretion rates as well as the flux contribution of the accreting white dwarf are included in our analysis. Except for RW Tri which has a reliable trigonometric parallax, we computed the distances to the nova-like systems using the method of Knigge(2006, MNRAS, 373, 484). For KR Aur, we find that the white dwarf has T_eff = 29,000 +/- 2000K, log g = 8.4 and contributes 18% of the FUV flux while an accretion disk with accretion rate Mdot = 3 x 10-10 Msun/yr at an inclination of 41 degrees, contributes the remainder. Our analysis of seven archival IUE spectra of RW Tri at its parallax distance consistently yields a low mass (0.4 Msun) white dwarf and an average accretion rate, Mdot = 6.3 x 10-9 Msun/yr. We find that an accreting white dwarf rather than accretion disk dominates the far UV spectrum of V425 Cas while HL Aqr's and V825 Her's FUV spectra are dominated by an accretion disk with Mdot = 1 x 10-9 Msun/yr and 3 x 10-9 Msun/yr, respectively. For BP Lyn we find Mdot = 1 x 10-8 Msun/yr and we explore the possiblity that V795 Her is an intermediate polar. We discuss the implications of our results for the evolutionary status of nova-like variables. This work is supported by NSF grant AST-0807892 to Villanova University and by the Delaware Space Grant Consortium

  12. Throughfall deposition of sulfur to a mixed oak and pine forest in

    NASA Astrophysics Data System (ADS)

    Singer, A.; Ganor, E.; Fried, M.; Shamay, Y.

    The deposition of sulfur in a forest site on Mt. Carmel was monitored during the years 1989-1992. Wet deposition, bulk deposition and dry deposition were monitored on an open site. Through-fall and stemflow were sampled in a natural, mixed pine ( Pinus halepensis) and oak ( Quercus calliprinos) forest. In more than 65% of the rain events, the pH of wet deposition was acidic (⩽ 5.6) and in nearly 40% of the events it was strongly acidic. The average wet deposition was 12.5 kg ha -1 yr -1 SO 4S. This suggested that the wet deposition of SO 4S on the Carmel was in the upper range of unpolluted areas. Bulk deposition contributed 14.3 kg ha -1 yr -1 SO4S. Coarse-grained dry deposition averaged to 58 kg ha -1 yr -1 and the average deposition rate of gypsum was4.9 kg ha -1 yr -1containing 0.92 kg ha -1 yr -1 sulfur. Pine throughfall contained 38 kg ha -1 yr -1 S and oak throughfall contained 18 kg ha -1 yr -1. Pine throughfall thus contained approximately twice as much S than oak throughfall, probably as a result of the much larger specific surface area of pine. Stemflow was negligible. The total S deposition on Mt. Carmel was considerably larger than in unpolluted forests of U.S. and Canada, but smaller than in polluted forests of Germany. The pine forests on the western slopes of the central mountain range seemed to have the important function of "filtering" the air masses that come from the western coastal area, thus preventing S pollution advancing inland.

  13. Historical atmospheric mercury emissions and depositions in North America compared to mercury accumulations in sedimentary records

    NASA Astrophysics Data System (ADS)

    Pirrone, Nicola; Allegrini, Ivo; Keeler, Gerald J.; Nriagu, Jerome O.; Rossmann, Ronald; Robbins, John A.

    Gold and silver production in North America (included United States, Canada and Mexico) released a large amount of mercury to the atmosphere until well into this century when mercury (Hg) amalgamation was replaced by cyanide concentration. Since then, emissions from industries have been the dominant anthropogenic sources of atmospheric Hg in North America as a whole. Past Hg emissions from gold and silver extractions in North America during the 1800s do not show a clear evidence of atmospheric deposition occurred at the coring sites considered in this study. Estimated atmospheric emissions of Hg in North America peaked in 1879 (at about 1708 t yr -1) and 1920 (at about 940 t yr -1), primarily due to Hg emissions from gold and silver mining. After the Great Economic Depression (1929) Hg emissions peaked again in the 1947 (274 t yr -1), in 1970 (325 t yr -1) and in 1989 (330 t yr -1) as result of increased Hg emissions from industrial sources, though improvements in the emissions control technology in United States and Canada have been substantial. Estimates of total atmospheric deposition fluxes of Hg to water and terrestrial receptors were in the range of 14.3-19.8 μg m -2 yr -1 in North America as a whole, and averaged 135 μg m -2 yr -1 (global background + local emissions) in the Great Lakes. These values were in good agreement with recent estimates reported in literature. The comparison of atmospheric Hg deposition fluxes with Hg accumulation rates in sediment cores suggests that atmospheric deposition was the major source of Hg entering the lakes system at coring sites, however, important contributions to Lake Ontario sediment cores sites from 1940 to 1970 were likely originated from local point sources (i.e. direct discharges).

  14. Evaluation Of Elastic Strain Accumulation In The Southern Indian Peninsula By GPS-Geodesy

    NASA Astrophysics Data System (ADS)

    Narayanababu, R.; Ec, M.; Tummala, C.

    2004-12-01

    The computed elastic strain accumulation in the southern Indian peninsula from the GPS derived velocity fields of the global network of GPS stations, in and around the Indian plate which includes Maitri, Indian Antarctic Station, show a significant departure from rigid plate behaviour in a manner consistent with the mapped intra plate stress field, observations of deformations and seismicity in the region. Our results of intraplate strain accumulation within Antarctica Plate covering three sites MAIT, CAS1 and DAV1 are 1.8x10-9yr-1, 1.6x10-9yr-1 and 1.1x10-9yr-1, respectively. Similarly, the estimates of interplate strain accumulation between Antarctica and other plates Somalia (SEY1), Africa (HARO), Australia (YAR1), and diffuse plate boundary between India and Australia (COCO) are found to be 1.1x10-9yr-1, 1.0x10-10yr-1, 1.27x10-8yr-1 and 1.18x10-8yr-1, respectively. These estimates are in good agreement with the earlier studies on estimation of global strain rate. The combined GPS and seismic analysis confirm the emergence of diffuse plate boundary between India and Australia and relates to the late Miocene Himalayan uplift. The calculated stress field in the West of the Indian Peninsula has a roughly N-S directed tensional and E-W oriented compressional character and the velocity vectors of all other sites throw a significant insight into the plausible causes of the strain accumulation processes in the Indian Ocean and the northward movement of Indian plate.

  15. O 2 reduction and denitrification rates in shallow aquifers

    USGS Publications Warehouse

    Tesoriero, A.J.; Puckett, L.J.

    2011-01-01

    O 2 reduction and denitrification rates were determined in shallow aquifers of 12 study areas representing a wide range in sedimentary environments and climatic conditions. Zero-and first-order rates were determined by relating reactant or product concentrations to apparent groundwater age. O 2 reduction rates varied widely within and between sites, with zero-order rates ranging from <3 ??mol L -1 yr -1 to more than 140 ??mol L -1 yr -1 and first-order rates ranging from 0.02 to 0.27 yr -1. Moderate denitrification rates (10-100 ??mol N L -1 yr -1; 0.06-0.30 yr -1) were observed in most areas with O 2 concentrations below 60 mol L -1, while higher rates (>100 mol N L -1 yr -1; >0.36 yr -1) occur when changes in lithology result in a sharp increase in the supply of electron donors. Denitrification lag times (i.e., groundwater travel times prior to the onset of denitrification) ranged from <20 yr to >80 yr. The availability of electron donors is indicated as the primary factor affecting O 2 reduction rates. Concentrations of dissolved organic carbon (DOC) and/or sulfate (an indicator of sulfide oxidation) were positively correlated with groundwater age at sites with high O 2 reduction rates and negatively correlated at sites with lower rates. Furthermore, electron donors from recharging DOC are not sufficient to account for appreciable O 2 and nitrate reduction. These relations suggest that lithologic sources of DOC and sulfides are important sources of electrons at these sites but surface-derived sources of DOC are not. A review of published rates suggests that denitrification tends to occur more quickly when linked with sulfide oxidation than with carbon oxidation. copyright 2011 by the American Geophysical Union.

  16. The Carbon Budget of Coastal Waters of Eastern North America

    NASA Astrophysics Data System (ADS)

    Najjar, R.; Boyer, E. W.; Burdige, D.; Butman, D. E.; Cai, W. J.; Canuel, E. A.; Chen, R. F.; Friedrichs, M. A.; Griffith, P. C.; Herrmann, M.; Kemp, W. M.; Kroeger, K. D.; Mannino, A.; McCallister, S. L.; McGillis, W. R.; Mulholland, M. R.; Salisbury, J.; Signorini, S. R.; Tian, H.; Tzortziou, M.; Vlahos, P.; Wang, A. Z.; Zimmerman, R. C.; Pilskaln, C. H.

    2015-12-01

    Observations and the output of numerical and statistical models are synthesized to construct a carbon budget of the coastal waters of eastern North America. The domain extends from the head of tide to (roughly) the continental shelf break and from southern Florida to southern Nova Scotia. The domain area is 2% tidal wetlands, 19% estuarine open water, and 78% shelf water. Separate budgets are constructed for inorganic and organic carbon; for tidal wetlands, estuaries, and shelf waters; and for three main subregions: the Gulf of Maine, the Mid-Atlantic Bight, and the South Atlantic Bight. Net primary production for the study region is about 150 Tg C yr-1, with 12% occurring in tidal wetlands and 7% in estuaries. Though respiration and photosynthesis are nearly balanced in most systems and regions, tidal wetlands and shelf waters are each found to be net autotrophic whereas estuaries are net heterotrophic. The domain as a whole is a sink of 5 Tg C yr-1 of atmospheric CO2, with tidal wetlands and shelf waters taking up 10 Tg C yr-1 (split roughly equally) and estuaries releasing 5 Tg C yr-1 to the atmosphere. Carbon burial is about 3 Tg C yr-1, split roughly equally among tidal wetlands, estuaries, and shelf waters. Rivers supply 6-7 Tg C yr-1 to estuaries, about 2/3 of which is organic. Tidal wetlands supply an additional 4 Tg C yr-1 to estuaries, about half of which is organic. Carbon in organic and inorganic forms is exported from estuaries to shelf waters and from shelf waters to the open ocean. In summary, tidal wetlands and estuaries, though small in area, contribute substantially to the overall carbon budget of the region.

  17. O2 reduction and denitrification rates in shallow aquifers

    NASA Astrophysics Data System (ADS)

    Tesoriero, Anthony J.; Puckett, Larry J.

    2011-12-01

    O2 reduction and denitrification rates were determined in shallow aquifers of 12 study areas representing a wide range in sedimentary environments and climatic conditions. Zero- and first-order rates were determined by relating reactant or product concentrations to apparent groundwater age. O2 reduction rates varied widely within and between sites, with zero-order rates ranging from <3 μmol L-1 yr-1 to more than 140 μmol L-1 yr-1 and first-order rates ranging from 0.02 to 0.27 yr-1. Moderate denitrification rates (10-100 μmol N L-1 yr-1; 0.06-0.30 yr-1) were observed in most areas with O2 concentrations below 60 μmol L-1, while higher rates (>100 μmol N L-1 yr-1; >0.36 yr-1) occur when changes in lithology result in a sharp increase in the supply of electron donors. Denitrification lag times (i.e., groundwater travel times prior to the onset of denitrification) ranged from <20 yr to >80 yr. The availability of electron donors is indicated as the primary factor affecting O2 reduction rates. Concentrations of dissolved organic carbon (DOC) and/or sulfate (an indicator of sulfide oxidation) were positively correlated with groundwater age at sites with high O2 reduction rates and negatively correlated at sites with lower rates. Furthermore, electron donors from recharging DOC are not sufficient to account for appreciable O2 and nitrate reduction. These relations suggest that lithologic sources of DOC and sulfides are important sources of electrons at these sites but surface-derived sources of DOC are not. A review of published rates suggests that denitrification tends to occur more quickly when linked with sulfide oxidation than with carbon oxidation.

  18. The VMC survey - XV. The Small Magellanic Cloud-Bridge connection history as traced by their star cluster populations

    NASA Astrophysics Data System (ADS)

    Piatti, Andrés E.; de Grijs, Richard; Rubele, Stefano; Cioni, Maria-Rosa L.; Ripepi, Vincenzo; Kerber, Leandro

    2015-06-01

    We present results based on YJKs photometry of star clusters located in the outermost, eastern region of the Small Magellanic Cloud (SMC). We analysed a total of 51 catalogued clusters whose colour-magnitude diagrams (CMDs), having been cleaned from field-star contamination, were used to assess the clusters' reality and estimate ages of the genuine systems. Based on CMD analysis, 15 catalogued clusters were found to be possible non-genuine aggregates. We investigated the properties of 80 per cent of the catalogued clusters in this part of the SMC by enlarging our sample with previously obtained cluster ages, adopting a homogeneous scale for all. Their spatial distribution suggests that the oldest clusters, log(t yr-1) ≥ 9.6, are in general located at greater distances to the galaxy's centre than their younger counterparts - 9.0 ≤ log(t yr-1) ≤ 9.4 - while two excesses of clusters are seen at log(t yr-1) ˜ 9.2 and log(t yr-1) ˜ 9.7. We found a trail of younger clusters which follow the wing/bridge components. This long spatial sequence does not only harbour very young clusters, log(t yr-1) ˜ 7.3, but it also hosts some of intermediate ages, log(t yr-1) ˜ 9.1. The derived cluster and field-star formation frequencies as a function of age are different. The most surprising feature is an observed excess of clusters with ages of log(t yr-1) < 9.0, which could have been induced by interactions with the LMC.

  19. Net greenhouse gas balance in China's Croplands over the last three decades and its mitigation potential.

    PubMed

    Zhang, Wen; Yu, Yongqiang; Li, Tingting; Sun, Wenjuan; Huang, Yao

    2014-01-01

    Cropland soils have been shown to emit nitrous oxide (N2O) and methane (CH4) into the atmosphere and to sequester carbon when field management is improved, yet the spatiotemporal changes in the N2O and CH4 emissions and the soil organic carbon (SOC) in China's croplands are unclear with regard to an integrated global warming potential (GWP). This limits our overall evaluation of anthropogenic greenhouse gas (GHG) emissions and impairs effective decision making. On the basis of model simulations primarily from 1980 to 2009, we estimated a 69% increase in the gross GWP of CH4 and N2O emissions, from 244 Tg CO2-equiv yr(-1) in the early 1980s to 413 Tg CO2-equiv yr(-1) in the late 2000s. The SOC was estimated to have increased from 54 Tg CO2-equiv yr(-1) to 117 Tg CO2-equiv yr(-1) during the same period. A reduction in the carbon input during the rice season, along with an improvement of synthetic nitrogen use efficiency in crops to 40%, would mitigate GHG emissions by 111 Tg CO2-equiv yr(-1) and keep SOC sequestration at 82 Tg CO2 yr(-1). Together, this would amount to a reduction of 193 Tg CO2-equiv yr(-1), representing ∼47% of the gross GWP in the late 2000s. The mitigation of GHG emissions in Henan, Shandong, Hunan, Jiangsu, Hubei, Sichuan, Anhui, Jiangxi, Guangdong and Hebei Provinces could lead to a ∼66% national improvement and should be given priority. PMID:24512240

  20. Multiyear precipitation reduction strongly decreases carbon uptake over northern China

    NASA Astrophysics Data System (ADS)

    Yuan, Wenping; Liu, Dan; Dong, Wenjie; Liu, Shuguang; Zhou, Guangsheng; Yu, Guirui; Zhao, Tianbao; Feng, Jinming; Ma, Zhuguo; Chen, Jiquan; Chen, Yang; Chen, Shiping; Han, Shijie; Huang, Jianping; Li, Linghao; Liu, Huizhi; Liu, Shaoming; Ma, Mingguo; Wang, Yanfeng; Xia, Jiangzhou; Xu, Wenfang; Zhang, Qiang; Zhao, Xinquang; Zhao, Liang

    2014-05-01

    Drought has been a concern in global and regional water, carbon, and energy cycles. From 1999 to 2011, northern China experienced a multiyear precipitation reduction that significantly decreased water availability as indicated by the Palmer Drought Severity Index and soil moisture measurements. In this study, a light use efficiency model (EC-LUE) and an ecosystem physiological model (IBIS) were used to characterize the impacts of long-term drought on terrestrial carbon fluxes in northern China. EC-LUE and IBIS models showed the reduction of averaged GPP of 0.09 and 0.05 Pg C yr-1 during 1999-2011 compared with 1982-1998. Based on the IBIS model, simulated ecosystem respiration experienced an insignificant decrease from 1999 to 2011. The multiyear precipitation reduction changed the regional carbon uptake of 0.011 Pg C yr-1 from 1982 to 1998 to a net source of 0.018 Pg C yr-1 from 1999 to 2011. Moreover, a pronounced decrease in maize yield in almost all provinces in the study region was found from 1999 to 2011 versus the average of yield from1978 to 2011. The largest maize yield reduction occurred in Beijing (2499 kg ha-1 yr-1), Jilin (2180 kg ha-1 yr-1), Tianjing (1923 kg ha-1 yr-1), and Heilongjiang (1791 kg ha-1 yr-1), and the maize yield anomaly was significantly correlated with the annual precipitation over the entire study area. Our results revealed that recent climate change, especially drought-induced water stress, is the dominant cause of the reduction in the terrestrial carbon sink over northern China.

  1. Atmospheric histories and growth trends of C4F10, C5F12, C6F14, C7F16 and C8F18

    NASA Astrophysics Data System (ADS)

    Ivy, D. J.; Arnold, T.; Harth, C. M.; Steele, L. P.; Mühle, J.; Rigby, M.; Salameh, P. K.; Leist, M.; Krummel, P. B.; Fraser, P. J.; Weiss, R. F.; Prinn, R. G.

    2012-05-01

    Atmospheric observations and trends are presented for the high molecular weight perfluorocarbons (PFCs): decafluorobutane (C4F10), dodecafluoropentane (C5F12), tetradecafluorohexane (C6F14), hexadecafluoroheptane (C7F16) and octadecafluorooctane (C8F18). Their atmospheric histories are based on measurements of 36 Northern Hemisphere and 46 Southern Hemisphere archived air samples collected between 1973 to 2011 using the Advanced Global Atmospheric Gases Experiment (AGAGE) "Medusa" preconcentration gas chromatography-mass spectrometry systems. A new calibration scale was prepared for each PFC, with estimated accuracies of 6.8% for C4F10, 7.8% for C5F12, 4.0% for C6F14, 6.6% for C7F16 and 7.9% for C8F18. Based on our observations the 2011 globally averaged dry air mole fractions of these heavy PFCs are: 0.17 parts-per-trillion (ppt, i.e., parts per 1012) for C4F10, 0.12 ppt for C5F12, 0.27 ppt for C6F14, 0.12 ppt for C7F16 and 0.09 ppt for C8F18. These atmospheric mole fractions combine to contribute to a global average radiative forcing of 0.35 mW m-2, which is 6% of the total anthropogenic PFC radiative forcing (Montzka and Reimann, 2011; Oram et al., 2012). The growth rates of the heavy perfluorocarbons were largest in the late 1990s peaking at 6.2 parts per quadrillion (ppq, i.e., parts per 1015) per year (yr) for C4F10, at 5.0 ppq yr-1 for C5F12 and 16.6 ppq yr-1 for C6F14 and in the early 1990s for C7F16 at 4.7 ppq yr-1 and in the mid 1990s for C8F18 at 4.8 ppq yr-1. The 2011 globally averaged mean atmospheric growth rates of these PFCs are subsequently lower at 2.2 ppq yr-1 for C4F10, 1.4 ppq yr-1 for C5F12, 5.0 ppq yr-1 for C6F14, 3.4 ppq yr-1 for C7F16 and 0.9 ppq yr-1 for C8F18. The more recent slowdown in the growth rates suggests that emissions are declining as compared to the 1980s and 1990s.

  2. Disturbance-induced reduction of biomass carbon sinks of China’s forests in recent years

    NASA Astrophysics Data System (ADS)

    Zhang, Chunhua; Ju, Weimin; Chen, Jing M.; Wang, Xiqun; Yang, Lin; Zheng, Guang

    2015-11-01

    Forests play a critical role in mitigating climate change because of their high carbon storage and productivity. China has experienced a pronounced increase in forest area resulting from afforestation and reforestation activities since the 1970s. However, few comprehensive analyses have been made to assess the recent dynamics of biomass carbon sinks in China’s forests. This study refined biomass carbon sinks of China’s forests based on eight forest inventories from 1973 to 2013. These sinks increased from 25.0 to 166.5 Tg C yr-1 between 1973 and 2008, and then decreased to 130.9 Tg C yr-1 for the period of 2009-2013 because the increases in forest area and biomass carbon density became slower. About 7% and 93% of this sink reduction occurred in planted and natural forests. The carbon sinks for young, middle-aged and premature forests decreased by 27.3, 27.0, and 7.6 Tg C yr-1, respectively. 42% of this decrease was offset by mature and overmature forests. During 2009-2013, forest biomass carbon sinks decreased in all regions but the north and northwest regions. The drivers for changes of forest biomass sinks differ spatially. More intensive harvest of young and middle-aged forests and snow damage were the major drivers for the decreases of biomass carbon sinks in the east (8.0 Tg C yr-1) and south (19.8 Tg C yr-1) regions. The carbon sink reduction in the southwest region (16.7 Tg C yr-1) was mainly caused by increased timber harvesting and natural disturbances, such as droughts in Yunnan province, snow damage in Guizhou province and forest fires in Sichuan province. In the northeast region, the sink reduction occurred mainly in Heilongjiang province (7.9 Tg C yr-1) and was caused dominantly by the combined effects of diseases, windthrow and droughts. The carbon sink increase was primarily attributed to forest growth and decreased deforestation in the north (10.0 Tg C yr-1) and northwest (2.3 Tg C yr-1) regions.

  3. Complex forest dynamics indicate potential for slowing carbon accumulation in the southeastern United States

    NASA Astrophysics Data System (ADS)

    Coulston, John W.; Wear, David N.; Vose, James M.

    2015-01-01

    Over the past century forest regrowth in Europe and North America expanded forest carbon (C) sinks and offset C emissions but future C accumulation is uncertain. Policy makers need insights into forest C dynamics as they anticipate emissions futures and goals. We used land use and forest inventory data to estimate how forest C dynamics have changed in the southeastern United States and attribute changes to land use, management, and disturbance causes. From 2007-2012, forests yielded a net sink of C because of net land use change (+6.48 Tg C yr-1) and net biomass accumulation (+75.4 Tg C yr-1). Forests disturbed by weather, insect/disease, and fire show dampened yet positive forest C changes (+1.56, +1.4, +5.48 Tg C yr-1, respectively). Forest cutting caused net decreases in C (-76.7 Tg C yr-1) but was offset by forest growth (+143.77 Tg C yr-1). Forest growth rates depend on age or stage of development and projected C stock changes indicate a gradual slowing of carbon accumulation with anticipated forest aging (a reduction of 9.5% over the next five years). Additionally, small shifts in land use transitions consistent with economic futures resulted in a 40.6% decrease in C accumulation.

  4. A method for the correction of proper motions of stars around an extragalactic object in photographic astrometry

    NASA Astrophysics Data System (ADS)

    Ducourant, C.; Rapaport, M.

    1991-01-01

    A method is described to correct the proper motions of catalogue stars present on overlapping plates around a quasar. The local reference system defined by the adjusted catalogue appears closer to an inertial system than the original catalogue. First we present the method we developed: an overlap technique is applied to reduce simultaneously the measurements of the plates while using the presence of the quasar as a fixed point. The overlap treatment allows to take account of the a priori errors of the catalogue and to determine an estimation of these errors. We apply this method to a set of two old plates and one new plate containing AGK 3 stars and the quasar 3C 273. The resulting mini-catalogue of 26 AGK 3 stars has an accuracy of around 0".08 on positions and 0.005 arcsec yr-1 on proper motions. Our method achieved an improvement of a factor 1.7 of the precision of the catalogue data. The estimates of the quasar's proper motion components obtained by separate reduction of each exposure using the AGK 3 data were μα = -0.007 arcsec yr-1 and μδ = -0.010 arcsec yr-1. The estimates become μα = -0.0002 arcsec yr-1 and μδ = -0.0002 arcsec yr-1 if the adjusted mini-catalogue is used.

  5. The Greenland Ice Sheet as a hot spot of phosphorus weathering and export in the Arctic

    NASA Astrophysics Data System (ADS)

    Hawkings, Jon; Wadham, Jemma; Tranter, Martyn; Telling, Jon; Bagshaw, Elizabeth; Beaton, Alexander; Simmons, Sarah-Louise; Chandler, David; Tedstone, Andrew; Nienow, Peter

    2016-02-01

    The contribution of ice sheets to the global biogeochemical cycle of phosphorus is largely unknown, due to the lack of field data. Here we present the first comprehensive study of phosphorus export from two Greenland Ice Sheet glaciers. Our results indicate that the ice sheet is a hot spot of phosphorus export in the Arctic. Soluble reactive phosphorus (SRP) concentrations, up to 0.35 µM, are similar to those observed in Arctic rivers. Yields of SRP are among the highest in the literature, with denudation rates of 17-27 kg P km-2 yr-1. Particulate phases, as with nonglaciated catchments, dominate phosphorus export (>97% of total phosphorus flux). The labile particulate fraction differs between the two glaciers studied, with significantly higher yields found at the larger glacier (57.3 versus 8.3 kg P km-2 yr-1). Total phosphorus yields are an order of magnitude higher than riverine values reported in the literature. We estimate that the ice sheet contributes ~15% of total bioavailable phosphorus input to the Arctic oceans (~11 Gg yr-1) and dominates total phosphorus input (408 Gg yr-1), which is more than 3 times that estimated from Arctic rivers (126 Gg yr-1). We predict that these fluxes will rise with increasing ice sheet freshwater discharge in the future.

  6. BARGEN continuous GPS data across the eastern Basin and Range province, and implications for fault system dynamics

    NASA Astrophysics Data System (ADS)

    Niemi, Nathan A.; Wernicke, Brian P.; Friedrich, Anke M.; Simons, Mark; Bennett, Richard A.; Davis, James L.

    2004-12-01

    We collected data from a transect of continuous Global Positioning System (GPS) sites across the eastern Basin and Range province at latitude 39°N from 1997-2000. Intersite velocities define a region ~350 km wide of broadly distributed strain accumulation at ~10 nstr yr-1. On the western margin of the region, site EGAN, ~10 km north of Ely, Nevada, moved at a rate of 3.9 +/- 0.2 mm yr-1 to the west relative to site CAST, which is on the Colorado Plateau. Velocities of most sites to the west of Ely moved at an average rate of ~3 mm yr-1 relative to CAST, defining an area across central Nevada that does not appear to be extending significantly. The late Quaternary geological velocity field, derived using seismic reflection and neotectonic data, indicates a maximum velocity of EGAN with respect to the Colorado Plateau of ~4 mm yr-1, also distributed relatively evenly across the region. The geodetic and late Quaternary geological velocity fields, therefore, are consistent, but strain release on the Sevier Desert detachment and the Wasatch fault appears to have been anomalously high in the Holocene. Previous models suggesting horizontal displacement rates in the eastern Basin and Range near 3 mm yr-1, which focused mainly along the Wasatch zone and Intermountain seismic belt, may overestimate the Holocene Wasatch rate by at least 50 per cent and the Quaternary rate by nearly an order of magnitude, while ignoring potentially major seismogenic faults further to the west.

  7. Assessment of the magnitude of ammonia emissions in the United Kingdom

    NASA Astrophysics Data System (ADS)

    Sutton, M. A.; Place, C. J.; Eager, M.; Fowler, D.; Smith, R. I.

    Estimates of ammonia emission in the U.K. have been critically reviewed with the aim of establishing the magnitude and uncertainty of each of the sources. European studies are also reviewed, with the U.K. providing a useful case study to highlight the uncertainties common to all ammonia emission inventories. This analysis of the emission factors and their application to U.K. sources supports an emission of 450 (231-715) Gg NH 3 yr -1. Agricultural activities are confirmed as the major source, providing 406 (215-630) Gg NH 3yr -1 (90% of the total), and therefore dominate uncertainties. Non-agricultural sources include sewage, pets, horses, humans, combustion and wild animals, though these contribute only 44 (16-85) Gg yr -1. Cattle represent the largest single uncertainty, accounting for 245 (119-389) Gg yr -1. The major uncertainties for cattle derive from estimation of the amount of nitrogen (N) excreted, the % N volatilized from land spreading of wastes, and the % N volatilized from stored farm-yard manure. Similar relative uncertainties apply to each of sheep, pigs and poultry, as well as fertilized crops, though these are quantitatively less important. Accounting; for regional differences in livestock demography, emission of 347, 63 and 40 Gg yr -1 are estimated for England & Wales, Scotland, and Northern Ireland, respectively. Though very uncertain, the total is in good agreement with estimates required to balance the U.K. atmospheric NH. budget.

  8. Relevance of estuaries adjacent to megalopolis as modifiers of internal shelf areas

    NASA Astrophysics Data System (ADS)

    Wagener, Angela; Lazzzari, Leticia; Carreira, Renato; Farias, Cassia; Mauad, Cristiane

    2014-05-01

    Guanabara Bay located in the humid tropical region is a eutrophic estuarine system bordered by the second largest metropolitan area of Brazil. Human intervention resulted in water conditions ranging from complete anoxia in the polluted inner bay area to the adjacent, relatively pristine, open coastal area. In the present work the goals were to estimate nutrients and carbon fluxes between the bay and the adjacent coastal waters and to characterize by using stable isotopes, hydrocarbons and sterols the provenance of the exported/imported organic matter. Water samples were collected from three different depths over 25 hours cycles in the wet and dry seasons at a single station strategically positioned in the bay. Measurements included CTD, nutrients, chlorophylls, DOC, POC, PN, δ13C and δ15N, hydrocarbons and sterols in SPM. Most substances showed higher concentrations in ebb tide events and through statistical tools a significant difference between the campaigns was proved. The fluxes estimated on annual basis revealed the expressive exportation to the inner continental shelf of 1.27x104 Kmol DIN yr-1, 9.52x102 Kmol DIP yr-1, 2.65x104 tons DOC yr-1, 1.96x104 tons COP yr-1, 2.96x104 tons NP yr-1.

  9. Quantification of carbon dioxide, methane, nitrous oxide, and chloroform emissions from atmospheric observations at Mace Head and Radon efflux measurement over Ireland

    NASA Astrophysics Data System (ADS)

    BIRAUD, S.; IELSCH, G.

    2001-12-01

    Flux estimates of CO2, CH4, N2O, and CHCl3 over Ireland are inferred from continuous atmospheric records of these species. We use radon-222 (222Rn) as a reference compound to estimate unknown sources of other species. In order to better quantify 222Rn exhalation from the soil and its seasonal variability, two field campaigns have been conducted during wintertime (October 2000) and summertime (July 2001). The correlation between each species and 222Rn is calculated for a suite of diurnal events that have been selected in the Mace Head record over the period 1995-1997 to represent air masses exposed to sources over Ireland. We established data selection based on criteria using 222Rn and 212Pb thresholds. We estimated flux densities of 12-15 103 kg CH4 km-2 yr-1, 680-830 kg N2O km-2 yr-1, and 20-30 kg CHCl3 km-2 yr-1 for CH4, N2O, and CHCl3, respectively. We also inferred flux densities of 250-310 103 kg C km-2 yr-1 for CO2 during wintertime, of 760-950 103 kg C km-2 yr-1 for CO2 during summer nighttime.

  10. Long-term particle measurements in Finnish Arctic: Part II - Trend analysis and source location identification

    NASA Astrophysics Data System (ADS)

    Laing, James R.; Hopke, Philip K.; Hopke, Eleanor F.; Husain, Liaquat; Dutkiewicz, Vincent A.; Paatero, Jussi; Viisanen, Yrjö.

    2014-05-01

    Forty-seven years (1964-2010) of weekly trace metal and major ion concentrations in total suspended particle samples from Kevo, Finland were analyzed for long-term trends and by source identification methods. Significant long-term decreasing trends were detected for most species. The largest decreases over the 47 years were Sb (-3.90% yr-1), Pb (-3.87% yr-1), Mn (-3.45% yr-1), Cd (-3.42% yr-1), and Ca (-3.13% yr-1). As, Pb, and Cd concentrations at Kevo were consistent with the reported time-trends of European emissions inventories. Pb concentrations at Kevo have dramatically decreased (92%) in the past 47 years due to the reduced use of leaded gasoline in automobiles. Back-trajectory analysis suggests that the main source areas of anthropogenic species (V, Cd, Mn, Mo, Sb, Tl, W) were predominantly in Eastern Europe, European Russia, and the Baltics. Markers of stationary fuel combustion (V, Mn, Mo, Sb, Se, and Tl) pointed towards source regions in the Pechora Basin and Ural industrial areas in Russia, and near gas and oil fields in western Kazakhstan.

  11. X-Ray Measured Dynamics of Tycho's Supernova Remnant

    NASA Technical Reports Server (NTRS)

    Katsuda, Satoru; Petre, Robert; Hughes, John; Hwang, Una; Yamaguchi, Hiroya; Hayato, Asami; Mori, Koji; Tsunemi, Hiroshi

    2010-01-01

    We present X-ray proper-motion measurements of the forward shock and reverse-shocked ejecta in Tycho's supernova remnant, based on three sets of archival Chandra data taken in 2000, 2003, and 2007. We find that the proper motion of the edge of the remnant (i.e., the forward shock and protruding ejecta knots) varies from 0.''20 yr-1 (expansion index m = 0.33, where R = tm ) to 0.''40 yr-1 (m = 0.65) with azimuthal angle in 2000-2007 measurements, and 0.''14 yr-1 (m = 0.26) to 0.''40 yr-1 (m = 0.65) in 2003-2007 measurements. The azimuthal variation of the proper motion and the average expansion index of [approx]0.5 are consistent with those derived from radio observations. We also find proper motion and expansion index of the reverse-shocked ejecta to be 0.''21-0.''31 yr-1 and 0.43-0.64, respectively. From a comparison of the measured m-value with Type Ia supernova evolutionary models, we find a pre-shock ambient density around the remnant of [less, similar]0.2 cm-3.

  12. Complex forest dynamics indicate potential for slowing carbon accumulation in the southeastern United States.

    PubMed

    Coulston, John W; Wear, David N; Vose, James M

    2015-01-01

    Over the past century forest regrowth in Europe and North America expanded forest carbon (C) sinks and offset C emissions but future C accumulation is uncertain. Policy makers need insights into forest C dynamics as they anticipate emissions futures and goals. We used land use and forest inventory data to estimate how forest C dynamics have changed in the southeastern United States and attribute changes to land use, management, and disturbance causes. From 2007-2012, forests yielded a net sink of C because of net land use change (+6.48 Tg C yr(-1)) and net biomass accumulation (+75.4 Tg C yr(-1)). Forests disturbed by weather, insect/disease, and fire show dampened yet positive forest C changes (+1.56, +1.4, +5.48 Tg C yr(-1), respectively). Forest cutting caused net decreases in C (-76.7 Tg C yr(-1)) but was offset by forest growth (+143.77 Tg C yr(-1)). Forest growth rates depend on age or stage of development and projected C stock changes indicate a gradual slowing of carbon accumulation with anticipated forest aging (a reduction of 9.5% over the next five years). Additionally, small shifts in land use transitions consistent with economic futures resulted in a 40.6% decrease in C accumulation. PMID:25614123

  13. Rising critical emission of air pollutants from renewable biomass based cogeneration from the sugar industry in India

    NASA Astrophysics Data System (ADS)

    Sahu, S. K.; Ohara, T.; Beig, G.; Kurokawa, J.; Nagashima, T.

    2015-09-01

    In the recent past, the emerging India economy is highly dependent on conventional as well as renewable energy to deal with energy security. Keeping the potential of biomass and its plentiful availability, the Indian government has been encouraging various industrial sectors to generate their own energy from it. The Indian sugar industry has adopted and made impressive growth in bagasse (a renewable biomass, i.e. left after sugercane is crushed) based cogeneration power to fulfil their energy need, as well as to export a big chunk of energy to grid power. Like fossil fuel, bagasse combustion also generates various critical pollutants. This article provides the first ever estimation, current status and overview of magnitude of air pollutant emissions from rapidly growing bagasse based cogeneration technology in Indian sugar mills. The estimated emission from the world’s second largest sugar industry in India for particulate matter, NOX, SO2, CO and CO2 is estimated to be 444 ± 225 Gg yr-1, 188 ± 95 Gg yr-1, 43 ± 22 Gg yr-1, 463 ± 240 Gg yr-1 and 47.4 ± 9 Tg yr-1, respectively in 2014. The studies also analyze and identify potential hot spot regions across the country and explore the possible further potential growth for this sector. This first ever estimation not only improves the existing national emission inventory, but is also useful in chemical transport modeling studies, as well as for policy makers.

  14. Spatial and temporal Antarctic Ice Sheet mass trends, glacio-isostatic adjustment, and surface processes from a joint inversion of satellite altimeter, gravity, and GPS data

    NASA Astrophysics Data System (ADS)

    Martín-Español, Alba; Zammit-Mangion, Andrew; Clarke, Peter J.; Flament, Thomas; Helm, Veit; King, Matt A.; Luthcke, Scott B.; Petrie, Elizabeth; Rémy, Frederique; Schön, Nana; Wouters, Bert; Bamber, Jonathan L.

    2016-02-01

    We present spatiotemporal mass balance trends for the Antarctic Ice Sheet from a statistical inversion of satellite altimetry, gravimetry, and elastic-corrected GPS data for the period 2003-2013. Our method simultaneously determines annual trends in ice dynamics, surface mass balance anomalies, and a time-invariant solution for glacio-isostatic adjustment while remaining largely independent of forward models. We establish that over the period 2003-2013, Antarctica has been losing mass at a rate of -84 ± 22 Gt yr-1, with a sustained negative mean trend of dynamic imbalance of -111 ± 13 Gt yr-1. West Antarctica is the largest contributor with -112 ± 10 Gt yr-1, mainly triggered by high thinning rates of glaciers draining into the Amundsen Sea Embayment. The Antarctic Peninsula has experienced a dramatic increase in mass loss in the last decade, with a mean rate of -28 ± 7 Gt yr-1 and significantly higher values for the most recent years following the destabilization of the Southern Antarctic Peninsula around 2010. The total mass loss is partly compensated by a significant mass gain of 56 ± 18 Gt yr-1 in East Antarctica due to a positive trend of surface mass balance anomalies.

  15. Modeling sustainable reuse of nitrogen-laden wastewater by poplar.

    PubMed

    Wang, Yusong; Licht, Louis; Just, Craig

    2016-06-01

    Numerical modeling was used to simulate the leaching of nitrogen (N) to groundwater as a consequence of irrigating food processing wastewater onto grass and poplar under various management scenarios. Under current management practices for a large food processor, a simulated annual N loading of 540 kg ha(-1) yielded 93 kg ha(-1) of N leaching for grass and no N leaching for poplar during the growing season. Increasing the annual growing season N loading to approximately 1,550 kg ha(-1) for poplar only, using "weekly", "daily" and "calculated" irrigation scenarios, yielded N leaching of 17 kg ha(-1), 6 kg ha(-1), and 4 kg ha(-1), respectively. Constraining the simulated irrigation schedule by the current onsite wastewater storage capacity of approximately 757 megaliters (Ml) yielded N leaching of 146 kg ha(-1) yr(-1) while storage capacity scenarios of 3,024 and 4,536 Ml yielded N leaching of 65 and 13 kg ha(-1) yr(-1), respectively, for a loading of 1,550 kg ha(-1) yr(-1). Further constraining the model by the current wastewater storage volume and the available land area (approximately 1,000 hectares) required a "diverse" irrigation schedule that was predicted to leach a weighted average of 13 kg-N ha(-1) yr(-1) when dosed with 1,063 kg-N ha(-1) yr(-1). PMID:26375195

  16. An analysis of the carbon balance of the Arctic Basin

    SciTech Connect

    Mcguire, David; Hayes, Daniel J; Kicklighter, David W.; Manizza, Manfredi; Zhuang, Qianlai; Chen, Min; Follows, Michael J; Gurney, Kevin; Mcclelland, James W; Melillo, Jerry; Peterson, Bruce; Prinn, Ronald

    2010-01-01

    This study used several model-based tools to analyse the dynamics of the Arctic Basin between 1997 and 2006 as a linked system of land-ocean-atmosphere C exchange. The analysis estimates that terrestrial areas of the Arctic Basin lost 62.9 Tg C yr 1 and that the Arctic Ocean gained 94.1 Tg C yr 1. Arctic lands and oceans were a net CO2 sink of 108.9 Tg C yr 1, which is within the range of uncertainty in estimates from atmospheric inversions. Although both lands and oceans of the Arctic were estimated to be CO2 sinks, the land sink diminished in strength because of increased fire disturbance compared to previous decades, while the ocean sink increased in strength because of increased biological pump activity associated with reduced sea ice cover. Terrestrial areas of the Arctic were a net source of 41.5 Tg CH4 yr 1 that increased by 0.6 Tg CH4 yr 1 during the decade of analysis, a magnitude that is comparable with an atmospheric inversion of CH4. Because the radiative forcing of the estimated CH4 emissions is much greater than the CO2 sink, the analysis suggests that the Arctic Basin is a substantial net source of green house gas forcing to the climate system.

  17. An analysis of the carbon balance of the Arctic Basin from 1997 to 2006

    USGS Publications Warehouse

    McGuire, A.D.; Hayes, D.J.; Kicklighter, D.W.; Manizza, M.; Zhuang, Q.; Chen, M.; Follows, M.J.; Gurney, K.R.; McClelland, J.W.; Melillo, J.M.; Peterson, B.J.; Prinn, R.G.

    2010-01-01

    This study used several model-based tools to analyse the dynamics of the Arctic Basin between 1997 and 2006 as a linked system of land-ocean-atmosphere C exchange. The analysis estimates that terrestrial areas of the Arctic Basin lost 62.9 Tg C yr-1 and that the Arctic Ocean gained 94.1 Tg C yr-1. Arctic lands and oceans were a net CO2 sink of 108.9 Tg C yr-1, which is within the range of uncertainty in estimates from atmospheric inversions. Although both lands and oceans of the Arctic were estimated to be CO2 sinks, the land sink diminished in strength because of increased fire disturbance compared to previous decades, while the ocean sink increased in strength because of increased biological pump activity associated with reduced sea ice cover. Terrestrial areas of the Arctic were a net source of 41.5 Tg CH4 yr-1 that increased by 0.6 Tg CH4 yr-1 during the decade of analysis, a magnitude that is comparable with an atmospheric inversion of CH4. Because the radiative forcing of the estimated CH4 emissions is much greater than the CO2 sink, the analysis suggests that the Arctic Basin is a substantial net source of green house gas forcing to the climate system.

  18. Deformation across the Pacific-North America plate boundary near San Francisco, California

    USGS Publications Warehouse

    Prescott, W.H.; Savage, J.C.; Svarc, J.L.; Manaker, D.

    2001-01-01

    We have detected a narrow zone of compression between the Coast Ranges and the Great Valley, and we have estimated slip rates for the San Andreas, Rodgers Creek, and Green Valley faults just north of San Francisco. These results are based on an analysis of campaign and continuous Global Positioning System (GPS) data collected between 1992 and 2000 in central California. The zone of compression between the Coast Ranges and the Great Valley is 25 km wide. The observations clearly show 3.8??1.5 mm yr-1 of shortening over this narrow zone. The strike slip components are best fit by a model with 20.8??1.9 mm yr-1 slip on the San Andreas fault, 10.3??2.6 mm yr-1 on the Rodgers Creek fault, and 8.1??2.1 mm yr-1 on the Green Valley fault. The Pacific-Sierra Nevada-Great Valley motion totals 39.2??3.8 mm yr-1 across a zone that is 120 km wide (at the latitude of San Francisco). Standard deviations are one ??. The geodetic results suggest a higher than geologic rate for the Green Valley fault. The geodetic results also suggest an inconsistency between geologic estimates of the San Andreas rate and seismologic estimates of the depth of locking on the San Andreas fault. The only convergence observed is in the narrow zone along the border between the Great Valley and the Coast Ranges.

  19. Using 137Cs technique to quantify soil erosion and deposition rates in an agricultural catchment in the black soil region, Northeast China

    NASA Astrophysics Data System (ADS)

    Fang, Haiyan; Sun, Liying; Qi, Deli; Cai, Qiangguo

    2012-10-01

    Soil erosion significantly affects the productive black soil region in Northeast China. Quantification of the soil erosion is necessary for designing efficient degradation control strategies. 137Cs measurements undertaken on 61 sampling points collected within a 28.5 ha agricultural catchment in the black soil region of Northeast China were used to establish the magnitude and spatial pattern of soil redistribution rates as well as sediment budget within the catchment. Estimated soil redistribution rates using the Mass Balance Model 2 (MBM2) ranged from - 56.8 to 171.4 t ha- 1 yr- 1 for the sampling points that were verified by means of both runoff plot data and pedological investigation. Erosion generally occurred behind the shelterbelts, especially in the ephemeral gully susceptible areas, while deposition mainly occurred along the shelterbelts and at the catchment outlet. In the study catchment, 69% of the eroded sediments came from the slopes and 31% the ephemeral gullies. Sediments deposited along the shelterbelts at a rate of ca. 78 t yr- 1 and ca. 33 t yr- 1 at the catchment outlet. The gross soil loss rate for the catchment was - 4.4 t ha- 1 yr- 1 with a sediment delivery ratio of 53%. The mean rate of - 14.5 t ha- 1 yr- 1 in the erosion areas was much higher than the tolerable value, suggesting that effective soil conservation measures are urgently required to reduce the severe black soil loss for sustainable management of the soil resource.

  20. The Uncertain Carbon Emissions in China (Invited)

    NASA Astrophysics Data System (ADS)

    Liu, Z.; Guan, D.

    2013-12-01

    Anthropogenic fossil fuel emissions are considered as being well understood with a low uncertainty (9.1 × 0.5Gt C yr-1). By using full transparency emission inventory which the energy consumption, fuel heating values, carbon content and oxidation rate reported separately in sectoal level, here we found new 2.1 Gt C yr-1 (23% of global total) uncertainties of carbon emission inventory, which mainly contributed by the mass energy use and consumption coal quality in China and by misunderstanding of fuel quality in international fossil fuel trade. Increment of coal's carbon emission in China and India are equivalent to 130 % of global total coal's emission growth during 2008-2010, by using macro energy statistics and bottom up coal mine datasets, the difference carbon emission estimates from China and India can up to 1.32 C yr-1. Emissions from international trade of coal could produce another 0.08 Gt C yr-1 uncertainty. These new emerging 1.4 Gt C yr-1 uncertainties implies a significant mis-estimation of human induced carbon emissions and a new dominating factor in contributing the global carbon budget residual.

  1. On VI Observations of Galaxy Clusters: Evidence for Modest Cooling Flows

    NASA Astrophysics Data System (ADS)

    Bregman, Joel N.; Fabian, A. C.; Miller, Eric D.; Irwin, Jimmy A.

    2006-05-01

    A prediction of the galaxy-cluster cooling flow model is that as gas cools from the ambient cluster temperature, emission lines are produced in gas at subsequently decreasing temperatures. Gas passing through 105.5 K emits in the lines of O VI λλ1032, 1035, and here we report a FUSE study of these lines in three cooling flow clusters, Abell 426, Abell 1795, and AWM 7. No emission was detected from AWM 7, but O VI is detected from the centers of Abell 426 and Abell 1795, and possibly to the south of the center in Abell 1795, where X-ray and optical emission line filaments lie. In Abell 426 these line luminosities imply a cooling rate of 32+/-6 Msolar yr-1 within the central r=6.2 kpc region, while for Abell 1795 the central cooling rate is 26+/-7 Msolar yr-1 (within r=22 kpc), and about 42+/-9 Msolar yr-1 including the southern pointing. Including other studies, three of six clusters have O VI emission, and they also have star formation as well as emission lines from 104 K gas. These observations are generally consistent with the cooling flow model, but at a rate closer to 30 Msolar yr-1 than to the originally suggested values of 102-10 3 Msolar yr-1.

  2. Emission Lines from the Gas Disk around TW Hydra and the Origin of the Inner Hole

    NASA Astrophysics Data System (ADS)

    Gorti, U.; Hollenbach, D.; Najita, J.; Pascucci, I.

    2011-07-01

    We compare line emission calculated from theoretical disk models with optical to submillimeter wavelength observational data of the gas disk surrounding TW Hya and infer the spatial distribution of mass in the gas disk. The model disk that best matches observations has a gas mass ranging from ~10-4 to 10-5 M sun for 0.06 AU < r < 3.5 AU and ~0.06 M sun for 3.5 AU < r < 200 AU. We find that the inner dust hole (r < 3.5 AU) in the disk must be depleted of gas by ~1-2 orders of magnitude compared with the extrapolated surface density distribution of the outer disk. Grain growth alone is therefore not a viable explanation for the dust hole. CO vibrational emission arises within r ~ 0.5 AU from thermal excitation of gas. [O I] 6300 Å and 5577 Å forbidden lines and OH mid-infrared emission are mainly due to prompt emission following UV photodissociation of OH and water at r <~ 0.1 AU and at r ~ 4 AU. [Ne II] emission is consistent with an origin in X-ray heated neutral gas at r <~ 10 AU, and may not require the presence of a significant extreme-ultraviolet (hν > 13.6 eV) flux from TW Hya. H2 pure rotational line emission comes primarily from r ~ 1 to 30 AU. [O I] 63 μm, HCO+, and CO pure rotational lines all arise from the outer disk at r ~ 30-120 AU. We discuss planet formation and photoevaporation as causes for the decrease in surface density of gas and dust inside 4 AU. If a planet is present, our results suggest a planet mass ~4-7 MJ situated at ~3 AU. Using our photoevaporation models and the best surface density profile match to observations, we estimate a current photoevaporative mass loss rate of 4 × 10-9 M sun yr-1 and a remaining disk lifetime of ~5 million years.

  3. The relativistic pulsar-white dwarf binary PSR J1738+0333 - II. The most stringent test of scalar-tensor gravity

    NASA Astrophysics Data System (ADS)

    Freire, Paulo C. C.; Wex, Norbert; Esposito-Farèse, Gilles; Verbiest, Joris P. W.; Bailes, Matthew; Jacoby, Bryan A.; Kramer, Michael; Stairs, Ingrid H.; Antoniadis, John; Janssen, Gemma H.

    2012-07-01

    We report the results of a 10-year timing campaign on PSR J1738+0333, a 5.85-ms pulsar in a low-eccentricity 8.5-h orbit with a low-mass white dwarf companion. We obtained 17 376 pulse times of arrival with a stated uncertainty smaller than ?s and weighted residual rms of ?s. The large number and precision of these measurements allow highly significant estimates of the proper motion μα, δ= (+7.037 ± 0.005, +5.073 ± 0.012) mas yr-1, parallax πx = (0.68 ± 0.05) mas and a measurement of the apparent orbital decay, ? (all 1σ uncertainties). The measurements of μα, δ and πx allow for a precise subtraction of the kinematic contribution to the observed orbital decay; this results in a significant measurement of the intrinsic orbital decay: ?. This is consistent with the orbital decay from the emission of gravitational waves predicted by general relativity, ?, i.e. general relativity passes the test represented by the orbital decay of this system. This agreement introduces a tight upper limit on dipolar gravitational wave emission, a prediction of most alternative theories of gravity for asymmetric binary systems such as this. We use this limit to derive the most stringent constraints ever on a wide class of gravity theories, where gravity involves a scalar-field contribution. When considering general scalar-tensor theories of gravity, our new bounds are more stringent than the best current Solar system limits over most of the parameter space, and constrain the matter-scalar coupling constant ? to be below the 10-5 level. For the special case of the Jordan-Fierz-Brans-Dicke, we obtain the 1σ bound ?, which is within a factor of 2 of the Cassini limit. We also use our limit on dipolar gravitational wave emission to constrain a wide class of theories of gravity which are based on a generalization of Bekenstein's Tensor-Vector-Scalar gravity, a relativistic formulation of modified Newtonian dynamics.

  4. Numerical Simulation of Moisture Flux in Deep Unsaturated Zones

    NASA Astrophysics Data System (ADS)

    Cooper, C.; Young, M.; Sharpe, S.; Miller, J.

    2003-04-01

    Understanding the rate and direction of liquid water movement in the valley fill sediments in the northern Mojave Desert (USA) is important for understanding groundwater recharge and near-surface soil water budgets. In some areas, the upward hydraulic gradient in the unsaturated zone drives liquid water upward. We used the multiphase, multicomponent simulator TOUGH2 to identify hydraulic processes and their magnitudes controlling liquid and vapor flux through a 250 m, one-dimensional column of unconsolidated sediment. Ten samples of unconsolidated sediment were collected from depths ranging from land surface to 31 m below land surface. The samples were repacked to original bulk density and analyzed for unsaturated hydraulic properties using an open-flow centrifuge. In the model, evaporation was simulated by prescribing the gas phase pressure at a thin, highly permeable "atmospheric" grid block at the land surface with zero relative humidity. The rest of the column was initially prescribed a gas pressure that was the sum of the ambient dry air pressure and the saturated vapor pressure at the assumed temperature. Root water uptake was modeled using the reservoir-engineering concept of a productivity index for a well, where the root operated against a slight, constant, prescribed pressure less than the reference atmospheric pressure. A 24,000-year precipitation sequence, generated from biotic distributions (e.g. ostracodes and pack-rat middens), was prescribed at the upper boundary. For our initial and boundary conditions, the simulations show that liquid flow is upward with velocities ranging between zero and 5 x 10-5 mm yr-1, depending on depth below ground surface. The zero flux plane fluctuates in depth between 14 and 17 meters, below which liquid flow is downward. In the absence of plants, liquid flow is downward throughout the entire profile and simulation period. Our simulations show that the "memory" of the system is on the order of 10,000 years; that is, the

  5. The Tista Megafan, a ~50 kyr Record of Drainage Development, Erosion and Weathering in the Sikkim Himalayas (Eastern India)

    NASA Astrophysics Data System (ADS)

    Abrahami, R.; Huyghe, P.; Van Der Beek, P.; Lowick, S.; Garzanti, E.; Revillon, S.; Carcaillet, J.; Chakraborty, T.

    2015-12-01

    The Tista River, a major tributary of the Brahmaputra drainage system (Eastern Himalaya) has built a fluvial deposit which extents over 16500 km2. The Tista megafan stands out because of (1) its disproportionate size compared to that of the upstream Tista River catchment (8000 km2), and (2) it has been incised about 50m by the river at the topographic front of the mountain range. Neither the timing of deposition/incision of the megafan sediments, and their potential tectonic or climatic controls have yet been investigated. We use both IRSL and 10Be cosmogenic data to respectively constrain the date of deposition and abandonment of the different lobes of the megafan. We suggest that two distal lobes developed successively downstream from a common proximal lobe. Deposition took place since ~50 ka and incision began at 4.0 +0.6/-0.4 ka at an average rate of 10.5 +0.6/-1.8 mm yr-1. In addition, petrology, isotope geochemistry (ɛNd, 87Sr/86Sr) and chemical composition performed on modern river sands and late-Quaternary megafan sediments allows characterizing (1) provenance variations through time of megafan deposits and their implication for drainage development (2) the weathering history of Sikkim recorded by the megafan deposits. Results show that the Tista fan deposits are mainly sourced from the High Himalayan Crystalline domain and the Tethyan Sedimentary Series, (consistent with high erosion rates identified in north Sikkim at millennial timescale). Variations in provenance and weathering through time recorded by the Tista megafan deposits can be linked to climatic variations with strong monsoonal precipitations penetrating further northward into the southern Tibetan plateau. Tectonic processes seem to play a minor role. Otherwise, we propose as a first hypothesis that the Kosi River has recently (at ~4 ka) captured the upper part of the Tista catchment. That could explain the particular isotopic signature of the Tista megafan deposits, its recent incision, its

  6. SN 2007uy - metamorphosis of an aspheric Type Ib explosion

    NASA Astrophysics Data System (ADS)

    Roy, Rupak; Kumar, Brijesh; Maund, Justyn R.; Schady, Patricia; Olivares, E. Felipe; Malesani, Daniele; Leloudas, Giorgos; Nandi, Sumana; Tanvir, Nial; Milisavljevic, Dan; Hjorth, Jens; Misra, Kuntal; Kumar, Brajesh; Pandey, S. B.; Sagar, Ram; Chandola, H. C.

    2013-09-01

    The supernovae (SNe) of Type Ibc are rare and the detailed characteristics of these explosions have been studied only for a few events. Unlike Type II SNe, the progenitors of Type Ibc have never been detected in pre-explosion images. So, to understand the nature of their progenitors and the characteristics of the explosions, investigation of proximate events is necessary. Here we present the results of multiwavelength observations of Type Ib SN 2007uy in the nearby (˜29.5 Mpc) galaxy NGC 2770. Analysis of the photometric observations revealed this explosion as an energetic event with peak absolute R-band magnitude -18.5 ± 0.16, which is about 1 mag brighter than the mean value (-17.6 ± 0.6) derived for well observed Type Ibc events. The SN is highly extinguished, E(B - V) = 0.63 ± 0.15 mag, mainly due to foreground material present in the host galaxy. From optical light curve modelling we determine that about 0.3 M⊙ radioactive 56Ni is produced and roughly 4.4 M⊙ material is ejected during this explosion with liberated energy ˜15 × 1051 erg, indicating the event to be an energetic one. Through optical spectroscopy, we have noticed a clear aspheric evolution of several line-forming regions, but no dependency of asymmetry is seen on the distribution of 56Ni inside the ejecta. The SN shock interaction with the circumstellar material is clearly noticeable in radio follow-up, presenting a synchrotron self-absorption dominated light curve with a contribution of free-free absorption during the early phases. Assuming a Wolf-Rayet (WR) star, with wind velocity ≳ 103 km s- 1, as a progenitor, we derive a lower limit to the mass-loss rate inferred from the radio data as M˙ ⪆ 2.4 × 10-5 M⊙ yr-1, which is consistent with the results obtained for other Type Ibc SNe bright at radio frequencies.

  7. Membership, binarity and accretion among very low-mass stars and brown dwarfs of the σ Orionis cluster

    NASA Astrophysics Data System (ADS)

    Kenyon, M. J.; Jeffries, R. D.; Naylor, Tim; Oliveira, J. M.; Maxted, P. F. L.

    2005-01-01

    Intermediate-resolution (R~ 7000) spectroscopy is presented for 76 photometrically selected very low-mass (0.04 < M < 0.3 Msolar) candidate members of the young cluster around σ Orionis (σ Ori). More than two-thirds appear to be genuine cluster members on the basis that they exhibit LiI 6708-Åabsorption, weak NaI 8183/8195 Åfeatures and a radial velocity consistent with the cluster mean. Photometric selection alone therefore appears to be very effective in identifying cluster members in this mass range. Only six objects appear to be certain non-members; however, a substantial subset of 13 candidates have ambiguous or contradictory indications of membership and lack Li absorption. Together with an observed spread in the equivalent width of the Li absorption feature in the cooler stars of our sample, this indicates that there may be deficiencies in our understanding of the formation of this line in cool, low-gravity objects. Four candidate binary cluster members are identified. Consideration of sampling and radial velocity measurement precision leads us to conclude that either the fraction of very low-mass stars and brown dwarfs in small separation (a < 1 au) binary systems is larger than in field M-dwarfs, or the distribution of separations is much less skewed towards large separations. This conclusion hinges critically on the correct identification of the small number of binary candidates, although it remains significant even when only the candidate members displaying Li absorption are considered. Broadened Hα emission, indicative of circum(sub)stellar accretion discs is found in five or six of the candidate cluster members, three of which probably have substellar masses. The fraction of accretors (10 +/- 5 per cent) is similar to that found in stars of higher mass in the σ Ori cluster using Hα emission as a diagnostic, but much lower than found for very low-mass stars and brown dwarfs of younger clusters. The time-scale for accretion rates to drop to <~10

  8. The SCUBA 8-mJy survey - I. Submillimetre maps, sources and number counts

    NASA Astrophysics Data System (ADS)

    Scott, S. E.; Fox, M. J.; Dunlop, J. S.; Serjeant, S.; Peacock, J. A.; Ivison, R. J.; Oliver, S.; Mann, R. G.; Lawrence, A.; Efstathiou, A.; Rowan-Robinson, M.; Hughes, D. H.; Archibald, E. N.; Blain, A.; Longair, M.

    2002-04-01

    We present maps, source lists and derived number counts from the largest, unbiased, extragalactic submillimetre (submm) survey so far undertaken with the SCUBA camera on the James Clerk Maxwell Telescope (JCMT). Our maps are located in two regions of sky (ELAIS N2 and Lockman-Hole E) and cover 260arcmin2 , to a typical rms noise level of σ 850 ~=2.5mJybeam-1 . We have reduced the data using both the standard JCMT surf procedures, and our own IDL -based pipeline which produces zero-footprint maps and noise images. The uncorrelated noise maps produced by the latter approach have enabled us to apply a maximum likelihood method to measure the statistical significance of each peak in our maps, leading to properly quantified errors on the flux density of all potential sources. We detect 19 sources with signal-to-noise ratios (S/N)>4, and 38 with S/N>3.5. To assess both the completeness of this survey and the impact of source confusion as a function of flux density, we have applied our source-extraction algorithm to a series of simulated images. The result is a new estimate of the submm source counts over the flux-density range S 850 ~=5-15mJy, which we compare with estimates derived by other workers, and with the predictions of a number of models. Our best estimate of the cumulative source count at S 850 >8mJy is per square degree. Assuming that the majority of sources lie at z >1.5, this result implies that the comoving number density of high-redshift galaxies forming stars at a rate in excess of 1000Msolar yr-1 is ~=10-5 Mpc-3 , with only a weak dependence on the precise redshift distribution. This number density corresponds to the number density of massive ellipticals with L >3-4L * in the present-day Universe , and is also the same as the comoving number density of comparably massive, passively evolving objects in the redshift band 1

  9. Studies based on global subsurface radar sounding of the Moon by SELENE (Kaguya) Lunar Radar Sounder (LRS): A summary

    NASA Astrophysics Data System (ADS)

    Kumamoto, A.; Yamaguchi, Y.; Yamaji, A.; Kobayashi, T.; Oshigami, S.; Ishiyama, K.; Nakamura, N.; Goto, Y.

    2015-12-01

    The Lunar Radar Sounder (LRS) onboard the SELENE (Kaguya) spacecraft has successfully performed radar sounder observations of the lunar subsurface structures and passive observations of natural radio and plasma waves from the lunar orbit. After the transfer of the spacecraft into the final lunar orbit and antenna deployment, the operation of LRS started on October 29, 2007. Through the operation until June 10, 2009, 130 million pulses worth of radar sounder data have been obtained [Ono et al., 2010]. Based on the datasets of the first lunar global subsurface radar sounding, Ono et al. [2009] revealed that there are distinct reflectors at a depth of several hundred meters in the nearside maria, which are inferred to be buried regolith layers covered by a basalt layer with a thickness of several hundred meters. Based on the further survey, Pommerol et al. [2010] pointed out the negative correlation of clear subsurface echoes with the maps of ilmenite, and suggested that dense ilmenite attenuates the radar pulse in the basaltic mare lava, and cause the absence of the clear subsurface echoes. That also suggests there are undetected subsurface reflectors especially below the young lava flow units with high ilmenite abundance. Kobayashi et al. [2012] applied synthetic aperture radar (SAR) processing to SELENE LRS data in order to obtain distinct radargram. Taking advantage of analyzing waveform data sent via high data rate telemetry from the Moon, we can perform advanced data analyses on the ground. We started providing the both SAR processed and waveform datasets via SELENE Data Archive (http://l2db.selene.darts.isas.jaxa.jp/index.html.en) since 2015. Oshigami et al. [2014] estimated volumes of basalt units in the ages of 2.7 Ga to 3.8 Ga in the nearside maria. The volume was derived from the depth of subsurface reflectors measured by LRS. The volumes of the geologic units were 103 to 104 km3. The average eruption rates were 10-5 to 10-3 km3 yr-1. The estimated volumes

  10. Phase-resolved XMM-Newton observations of the massive WR+O binary WR 22

    NASA Astrophysics Data System (ADS)

    Gosset, E.; Nazé, Y.; Sana, H.; Rauw, G.; Vreux, J.-M.

    2009-12-01

    Aims. To better understand the phenomenon of colliding winds in massive binary stars, we study the X-ray lightcurve of a WR+O system of the Carina region, a system well known for the high mass of its primary. Methods: Phase-resolved X-ray observations of the massive WR+O binary system WR 22 were performed with the XMM-Newton facility. We observed the object at seven different phases from near apastron to near periastron. Results: The X-ray spectrum can be represented by a two-component, optically thin, thermal plasma model with a first one at a typical temperature of 0.6 keV and a second hotter one in the range 2.0-4.5 keV. The hot component is indicative of a colliding wind phenomenon, but its flux is remarkably constant with time despite the high eccentricity of the orbit. Although surprising at first, this actually does not contradict the results of the hydrodynamical simulations of the wind collision that we performed. When the system goes from apastron to periastron, the soft part of the X-ray flux is progressively lowered by an increasing intervening absorbing column. This behaviour can be interpreted in terms of an X-ray emitting plasma located near the O star, but not fully intrinsic to it, and accompanying the star when it dives into the wind of the WR component. A model is presented that interprets most of the observational constraints. This model suggests that the mass-loss rate of dot{M}WR 1.6 × 10-5 {M}⊙ yr-1 assumed for the WR could still be slightly too high, whereas it is already lower than other published values. From the comparison of the observed and the expected absorptions at phases near periastron, we deduce that the hard X-ray emitting collision zone should at least have a typical size of 50-60 R⊙, but that the size for the soft X-ray emitting region could reach 244 R⊙ if the assumed mass-loss rate is correct. We also present an upper limit to the X-ray luminosity of the WR component that further questions the existence of intrinsic X

  11. Herschel/PACS spectroscopy of NGC 4418 and Arp 220: H2O, H218O, OH, 18OH, O I, HCN, and NH3

    NASA Astrophysics Data System (ADS)

    González-Alfonso, E.; Fischer, J.; Graciá-Carpio, J.; Sturm, E.; Hailey-Dunsheath, S.; Lutz, D.; Poglitsch, A.; Contursi, A.; Feuchtgruber, H.; Veilleux, S.; Spoon, H. W. W.; Verma, A.; Christopher, N.; Davies, R.; Sternberg, A.; Genzel, R.; Tacconi, L.

    2012-05-01

    Full range Herschel/PACS spectroscopy of the (ultra)luminous infrared galaxies NGC 4418 and Arp 220, observed as part of the SHINING key programme, reveals high excitation in H2O, OH, HCN, and NH3. In NGC 4418, absorption lines were detected with Elower > 800 K (H2O), 600 K (OH), 1075 K (HCN), and 600 K (NH3), while in Arp 220 the excitation is somewhat lower. While outflow signatures in moderate excitation lines are seen in Arp 220 as have been seen in previous studies, in NGC 4418 the lines tracing its outer regions are redshifted relative to the nucleus, suggesting an inflow with Ṁ ≲ 12 M⊙ yr-1. Both galaxies have compact and warm (Tdust ≳ 100 K) nuclear continuum components, together with a more extended and colder component that is much more prominent and massive in Arp 220. A chemical dichotomy is found in both sources: on the one hand, the nuclear regions have high H2O abundances, ~10-5, and high HCN/H2O and HCN/NH3 column density ratios of 0.1-0.4 and 2-5, respectively, indicating a chemistry typical of evolved hot cores where grain mantle evaporation has occurred. On the other hand, the high OH abundance, with OH/H2O ratios of ~0.5, indicates the effects of X-rays and/or cosmic rays. The nuclear media have high surface brightnesses (≳1013 L⊙/kpc2) and are estimated to be very thick (NH ≳ 1025 cm-2). While NGC 4418 shows weak absorption in H218O and 18OH, with a 16O-to-18O ratio of ≳250-500, the relatively strong absorption of the rare isotopologues in Arp 220 indicates 18O enhancement, with 16O-to-18O of 70-130. Further away from the nuclear regions, the H2O abundance decreases to ≲10-7 and the OH/H2O ratio is reversed relative to the nuclear region to 2.5-10. Despite the different scales and morphologies of NGC 4418, Arp 220, and Mrk 231, preliminary evidence is found for an evolutionary sequence from infall, hot-core like chemistry, and solar oxygen isotope ratio to high velocity outflow, disruption of the hot core chemistry and

  12. Timing of detachment faulting in the Bullfrog Hills and Bare Mountain area, southwest Nevada: Inferences from40Ar/39Ar, K-Ar, U-Pb, and fission track thermochronology

    USGS Publications Warehouse

    Hoisch, T.D.; Heizler, M.T.; Zartman, R.E.

    1997-01-01

    Crustal extension in the Bullfrog Hills and Bare Mountain area of southwest Nevada is associated with movement along a regional detachment fault. Normal faulting in the upper plate and rapid cooling (denudation) of the lower plate were coeval with Miocene silicic volcanism and with west-northwest transport along the detachment fault. A west-northwest progression of tilting along upper plate normal faults is indicated by ages of the volcanic rocks in relation to angular unconformities. Near the breakaway, tilting in the upper plate occurred between 12.7 and 11.6 Ma, continued less strongly past 10.7 Ma, and was over by 8.2 Ma. Ten to 20 km west of the breakaway, tilting occurred between 10.7 and 10.33 Ma, continued less strongly after 10.33 Ma, and was over by 8.1 Ma. The cooling histories of the lower plate metamorphic rocks were determined by thermochronologic dating methods: K-Ar and 40Ar/39Ar on muscovite, biotite, and hornblende, 40Ar/39Ar on K-feldspar, U-Pb on apatite, zircon, and sphene, and fission track on apatite, zircon, and sphene. Lower plate rocks 10 km west of the breakaway cooled slowly from Early Cretaceous lower-amphibolite facies conditions through 350??50?? to 300??50??C between 57 and 38 Ma, then cooled rapidly from 205??50?? to 120??50??C between 12.6??1.6 and 11.1??1.9 Ma. Lower plate rocks 20 km west of the breakaway cooled slowly from Early Cretaceous upper-amphibolite facies conditions through 500??50??C at 78-67 Ma, passed through 350??50?? to 300??50??C between 16.3??0.4 and 10.5??0.3 Ma, then cooled rapidly from 285??50?? to 120??50??C between 10.2 and 8.6 Ma. Upper plate tilting and rapid cooling (denudation) of the lower plate occurred simultaneously in the respective areas. The early slow-cooling part of the lower plate thermal histories was probably related to erosion at the Earth's surface, which stripped off about 9 km of material in 50 to 100 m.y. The results indicate an initial fault dip ???30?? and a 12 mm yr-1 west

  13. Outflow of hot and cold molecular gas from the obscured secondary nucleus of NGC 3256: closing in on feedback physics

    NASA Astrophysics Data System (ADS)

    Emonts, B. H. C.; Piqueras-López, J.; Colina, L.; Arribas, S.; Villar-Martín, M.; Pereira-Santaella, M.; Garcia-Burillo, S.; Alonso-Herrero, A.

    2014-12-01

    The nuclei of merging galaxies are often deeply buried in dense layers of gas and dust. In these regions, gas outflows driven by starburst and active galactic nuclear activity are believed to play a crucial role in the evolution of these galaxies. However, to fully understand this process it is essential to resolve the morphology and kinematics of such outflows. Using near-infrared integral-field spectroscopy obtained with SINFONI on the Very Large Telescope, we detect a kpc-scale structure of high-velocity molecular hydrogen (H2) gas associated with the deeply buried secondary nucleus of the infrared-luminous merger-galaxy NGC 3256. We show that this structure is most likely the hot component of a molecular outflow, which was recently also detected in the cold molecular gas through CO emission. This outflow, with a total molecular gas mass of MH2 ~ 2 × 107M⊙, is among the first to be spatially resolved in both the hot molecular H2 gas with VLT/SINFONI and the cold molecular CO emitting gas with ALMA. The hot and cold components share a similar morphology and kinematics, with a hot-to-cold molecular gas mass ratio of ~ 6 × 10-5. The high (~100 pc) resolution at which we map the geometry and velocity structure of the hot outflow reveals a biconical morphology with opening angle ~40° and gas spread across a FWZI ~ 1200 km s-1. Because this collimated outflow is oriented close to the plane of the sky, the molecular gas may reach maximum intrinsic outflow velocities of ~1800 km s-1, with an average mass outflow rate of at least Ṁoutfl ~ 20 M⊙ yr-1. By modeling the line-ratios of various near-infrared H2 transitions, we show that the H2-emitting gas in the outflow is heated through shocks or X-rays to a temperature of T ~ 1900 ± 300 K. The energy needed to drive the collimated outflow is most likely provided by a hidden Compton-thick AGN or by the nuclear starburst. We show that the global kinematics of the molecular outflow that we detect in NGC 3256 mimic

  14. Leo P: An Unquenched Very Low-mass Galaxy

    NASA Astrophysics Data System (ADS)

    McQuinn, Kristen B. W.; Skillman, Evan D.; Dolphin, Andrew; Cannon, John M.; Salzer, John J.; Rhode, Katherine L.; Adams, Elizabeth A. K.; Berg, Danielle; Giovanelli, Riccardo; Girardi, Léo; Haynes, Martha P.

    2015-10-01

    Leo P is a low-luminosity dwarf galaxy discovered through the blind H i Arecibo Legacy Fast ALFA survey. The H i and follow-up optical observations have shown that Leo P is a gas-rich dwarf galaxy with active star formation, an underlying older population, and an extremely low oxygen abundance. We have obtained optical imaging with the Hubble Space Telescope to two magnitudes below the red clump in order to study the evolution of Leo P. We refine the distance measurement to Leo P to be 1.62 ± 0.15 Mpc, based on the luminosity of the horizontal branch stars and 10 newly identified RR Lyrae candidates. This places the galaxy at the edge of the Local Group, ˜0.4 Mpc from Sextans B, the nearest galaxy in the NGC 3109 association of dwarf galaxies of which Leo P is clearly a member. The star responsible for ionizing the H ii region is most likely an O7V or O8V spectral type, with a stellar mass ≳25 M⊙. The presence of this star provides observational evidence that massive stars at the upper end of the initial mass function are capable of being formed at star formation rates as low as ˜10-5 M⊙ yr-1. The best-fitting star formation history (SFH) derived from the resolved stellar populations of Leo P using the latest PARSEC models shows a relatively constant star formation rate over the lifetime of the galaxy. The modeled luminosity characteristics of Leo P at early times are consistent with low-luminosity dSph Milky Way satellites, suggesting that Leo P is what a low-mass dSph would look like if it evolved in isolation and retained its gas. Despite the very low mass of Leo P, the imprint of reionization on its SFH is subtle at best, and consistent with being totally negligible. The isolation of Leo P, and the total quenching of star formation of Milky Way satellites of similar mass, implies that the local environment dominates the quenching of the Milky Way satellites. Based on observations made with the NASA/ESA Hubble Space Telescope (HST), obtained from the

  15. Early-time spectra of supernovae and their precursor winds. The luminous blue variable/yellow hypergiant progenitor of SN 2013cu

    NASA Astrophysics Data System (ADS)

    Groh, Jose H.

    2014-12-01

    We present the first quantitative spectroscopic modeling of an early-time supernova (SN) that interacts with its progenitor wind. Using the radiative transfer code CMFGEN, we investigate the recently reported 15.5 h post-explosion spectrum of the type IIb SN 2013cu. We are able to directly measure the chemical abundances of a SN progenitor and find a relatively H-rich wind, with H and He abundances (by mass) of X = 0.46 ± 0.2 and Y = 0.52 ± 0.2, respectively. The wind is enhanced in N and depleted in C relative to solar values (mass fractions of 8.2 × 10-3 and 1.0 × 10-5, respectively). We obtain that a slow, dense wind or circumstellar medium surrounds the precursor at the pre-SN stage, with a wind terminal velocity vwind ≲ 100 km s-1 and mass-loss rate of Ṁ ≃ 3 × 10-3 (vwind/ 100 km s-1) M⊙ yr-1. These values are lower than previous analytical estimates, although Ṁ/υ∞ is consistent with previous work. We also compute a CMFGEN model to constrain the progenitor spectral type; the high Ṁ and low vwind imply that the star had an effective temperature of ≃ 8000 K immediately before the SN explosion. Our models suggest that the progenitor was either an unstable luminous blue variable or a yellow hypergiant undergoing an eruptive phase, and rule out a Wolf-Rayet star. We classify the post-explosion spectra at 15.5 h as XWN5(h) and advocate for the use of the prefix "X" (eXplosion) to avoid confusion between post-explosion, non-stellar spectra, and those of massive stars. We show that the XWN spectrum results from the ionization of the progenitor wind after the SN, and that the progenitor spectral type is significantly different from the early post-explosion spectral type owing to the huge differences in the ionization structure before and after the SN event. We find the following temporal evolution: LBV/YHG → XWN5(h) → SN IIb. Future early-time spectroscopy in the UV will further constrain the properties of SN precursors, such as their

  16. Femoral lipectomy increases postprandial lipemia in women.

    PubMed

    Hernandez, Teri L; Bessesen, Daniel H; Cox-York, Kimberly A; Erickson, Christopher B; Law, Christopher K; Anderson, Molly K; Wang, Hong; Jackman, Matthew R; Van Pelt, Rachael E

    2015-07-01

    Femoral subcutaneous adipose tissue (SAT) appears to be cardioprotective compared with abdominal SAT, possibly through better triglyceride (TG) sequestration. We hypothesized that removal of femoral SAT would increase postprandial TG through a reduction in dietary fatty acid (FA) storage. Normal-weight (means ± SD; BMI 23.9 ± 2.6 kg/m(2)) women (n = 29; age 45 ± 6 yr) were randomized to femoral lipectomy (LIPO) or control (CON) and followed for 1 yr. Regional adiposity was measured by DEXA and CT. A liquid meal labeled with [(14)C]oleic acid was used to trace the appearance of dietary FA in plasma (6-h postprandial TG), breath (24-h oxidation), and SAT (24-h [(14)C]TG storage). Fasting LPL activity was measured in abdominal and femoral SAT. DEXA leg fat mass was reduced after LIPO vs. CON (Δ-1.4 ± 0.7 vs. 0.1 ± 0.5 kg, P < 0.001) and remained reduced at 1 yr (-1.1 ± 1.4 vs. -0.2 ± 0.5 kg, P < 0.05), as did CT thigh subcutaneous fat area (-39.6 ± 36.6 vs. 4.7 ± 14.6 cm(2), P < 0.05); DEXA trunk fat mass and CT visceral fat area were unchanged. Postprandial TG increased (5.9 ± 7.7 vs. -0.6 ± 5.3 × 10(3) mg/dl, P < 0.05) and femoral SAT LPL activity decreased (-21.9 ± 22.3 vs. 10.5 ± 26.5 nmol·min(-1)·g(-1), P < 0.05) 1 yr following LIPO vs. CON. There were no group differences in (14)C-labeled TG appearing in abdominal and femoral SAT or elsewhere. In conclusion, femoral fat remained reduced 1 yr following lipectomy and was accompanied by increased postprandial TG and reduced femoral SAT LPL activity. There were no changes in storage of meal-derived FA or visceral fat. Our data support a protective role for femoral adiposity on circulating TG independent of dietary FA storage and visceral adiposity. PMID:25968576

  17. The Flux of Large Meteoroids Observed with Lunar Impact Monitoring

    NASA Technical Reports Server (NTRS)

    Cooke, W. J.; Suggs, R. M.; Moser, D. E.; Suggs, R. J.

    2014-01-01

    The flux of large meteoroids is not well determined due to relatively low number statistics, due mainly to the lack of collecting area available to meteor camera systems (10(2)-10(5) km2). Larger collecting areas are needed to provide reasonable statistics for flux calculations. The Moon, with millions of square kilometers of lunar surface, can be used as a detector for observing the population of large meteoroids in the tens of grams to kilogram mass range. This is accomplished by observing the flash of light produced when a meteoroid impacts the lunar surface, converting a portion of its kinetic energy to visible light detectable from Earth. A routine monitoring program at NASA's Marshall Space Flight Center has recorded over 300 impact flashes since early 2006. The program utilizes multiple 0.35 m (14 inch) Schmidt-Cassegrain telescopes, outfitted with video cameras using the 1/2 inch Sony EXview HAD CCDTM chip, to perform simultaneous observations of the earthshine hemisphere of the Moon when the lunar phase is between 0.1 and 0.5. This optical arrangement permits monitoring of approximately 3.8x10(6) km2 of lunar surface. A selection of 126 flashes recorded in 266.88 hours of photometric skies was analyzed, creating the largest and most homogeneous dataset of lunar impact flashes to date. Standard CCD photometric techniques outlined in [1] were applied to the video to determine the luminous energy, kinetic energy, and mass for each impactor, considering a range of luminous efficiencies. The flux to a limiting energy of 2.5x10(-6) kT TNT or 1.05×10(7) J is 1.03×10(-7) km(-2) hr(-1) and the flux to a limiting mass of 30 g is 6.14×10(-10) m(-2) yr(-1). Comparisons made with measurements and models of the meteoroid population indicate that the flux of objects in this size range is slightly lower (but within the error bars) than the power law distribution determined for the near Earth object population by [2].

  18. The flux of large meteoroids observed with lunar impact monitoring

    NASA Astrophysics Data System (ADS)

    Cooke, W.; Suggs, R.; Moser, D.; Suggs, R. J.

    2014-07-01

    The flux of large meteoroids is not well determined due to relatively low number statistics, due mainly to the lack of collecting area available to meteor camera systems (10^2-10^5 km^2). Larger collecting areas are needed to provide reasonable statistics for flux calculations. The Moon, with millions of square kilometers of lunar surface, can be used as a detector for observing the population of large meteoroids in the tens of grams to kilogram mass range. This is accomplished by observing the flash of light produced when a meteoroid impacts the lunar surface, converting a portion of its kinetic energy to visible light detectable from the Earth. A routine monitoring program at NASA's Marshall Space Flight Center has recorded over 300 impact flashes since early 2006. The program utilizes multiple 0.35-m (14-inch) Schmidt-Cassegrain telescopes, outfitted with video cameras using the 1⁄2 inch Sony EXview HAD CCDTM chip, to perform simultaneous observations of the earthshine hemisphere of the Moon when the lunar phase is between 0.1 and 0.5. This optical arrangement permits monitoring of approximately 3.8×10^6 km^2 of lunar surface. A selection of 126 flashes recorded in 266.88 hours of photometric skies was analyzed, creating the largest and most homogeneous dataset of lunar impact flashes to date. Standard CCD photometric techniques outlined in [1] were applied to the video to determine the luminous energy, kinetic energy, and mass for each impactor, considering a range of luminous efficiencies. The flux to a limiting energy of 2.5×10^{-6} kT TNT or 1.05×10^7 J is 1.03×10^{-7} km^{-2} hr^{-1} and the flux to a limiting mass of 30 g is 6.14×10^{-10} m^{-2} yr^{-1}. Comparisons made with measurements and models of the meteoroid population indicate that the flux of objects in this size range is slightly lower (but within the error bars) than the power law distribution determined for the near-Earth-object population by [2].

  19. New observations and models of circumstellar CO line emission of AGB stars in the Herschel SUCCESS programme

    NASA Astrophysics Data System (ADS)

    Danilovich, T.; Teyssier, D.; Justtanont, K.; Olofsson, H.; Cerrigone, L.; Bujarrabal, V.; Alcolea, J.; Cernicharo, J.; Castro-Carrizo, A.; García-Lario, P.; Marston, A.

    2015-09-01

    Context. Asymptotic giant branch (AGB) stars are in one of the latest evolutionary stages of low to intermediate-mass stars. Their vigorous mass loss has a significant effect on the stellar evolution, and is a significant source of heavy elements and dust grains for the interstellar medium. The mass-loss rate can be well traced by carbon monoxide (CO) line emission. Aims: We present new Herschel/HIFI and IRAM 30 m telescope CO line data for a sample of 53 galactic AGB stars. The lines cover a fairly large range of excitation energy from the J = 1 → 0 line to the J = 9 → 8 line, and even the J = 14 → 13 line in a few cases. We perform radiative transfer modelling for 38 of these sources to estimate their mass-loss rates. Methods: We used a radiative transfer code based on the Monte Carlo method to model the CO line emission. We assume spherically symmetric circumstellar envelopes that are formed by a constant mass-loss rate through a smoothly accelerating wind. Results: We find models that are consistent across a broad range of CO lines for most of the stars in our sample, i.e., a large number of the circumstellar envelopes can be described with a constant mass-loss rate. We also find that an accelerating wind is required to fit, in particular, the higher-J lines and that a velocity law will have a significant effect on the model line intensities. The results cover a wide range of mass-loss rates (~10-8 to 2 × 10-5 M⊙ yr-1) and gas expansion velocities (2 to 21.5 km s-1) , and include M-, S-, and C-type AGB stars. Our results generally agree with those of earlier studies, although we tend to find slightly lower mass-loss rates by about 40%, on average. We also present "bonus" lines detected during our CO observations. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.Based on observations carried out with the IRAM 30 m Telescope. IRAM is

  20. Molecular clouds and star formation : a multiwavelength study of Perseus, Serpens, and Ophiuchus

    NASA Astrophysics Data System (ADS)

    Enoch, Melissa Lanae

    NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document.In this thesis I utilize large-scale millimeter and mid- to far-infrared surveys to address a number of outstanding questions regarding the formation of low mass stars in molecular clouds. Continuum [lambda] = 1.1 mm maps completed with Bolocam at a resolution of 31" cover the largest areas observed to date at millimeter or submillimeter wavelengths in three molecular clouds: 7.5 deg(2) in Perseus (140 pc(2) at the adopted distance of d = 250 pc), 10.8 deg(2) (50 pc(2) at d = 125 pc) in Ophiuchus, and 1.5 deg(2) (30 pc(2) at d = 125 pc) in Serpens. These surveys are sensitive to dense substructures with mean density n [...] 2 - 3 x 10(4) cm(-3). A total of 122 cores are detected in Perseus, 44 in Ophiuchus, and 35 in Serpens above mass detection limits of 0.1 - 0.2 Msun. Combining with Spitzer mid- and far-infrared maps from the c2d Legacy program provides wavelength coverage from [lambda] = 1.25-1100 micron, and enables the assembly of an unbiased, complete sample of the youngest star forming objects in three environments. This sample includes 108 prestellar cores, 43 Class 0 sources and 94 Class I sources.The approximately equal number of starless cores and embedded protostars in each cloud implies a starless core lifetime of 2 - 4 x 10(5) yr, only a few free-fall timescales. This timescale, considerably shorter than the timescale predicted by the classic scenario of magnetic field support in which core evolution is moderated by ambipolar diffusion, suggests that turbulence is the dominant process controlling the formation and evolution of dense cores. However, dense cores in all three clouds are found only at high cloud column densities, where [...] 7 mag, and the fraction of cloud mass in these cores is less than 10%, indicating that magnetic fields must play some role as well. Measured angular deconvolved sizes of the majority of starless cores are

  1. Optical and X-ray monitoring, Doppler imaging, and space motion of the young star Par 1724 in Orion

    NASA Astrophysics Data System (ADS)

    Neuhaeuser, R.; Wolk, S. J.; Torres, G.; Preibisch, Th.; Stout-Batalha, N. M.; Hatzes, A. P.; Frink, S.; Wichmann, R.; Covino, E.; Alcala, J. M.; Brandner, W.; Walter, F. M.; Sterzik, M. F.; Koehler, R.

    1998-06-01

    We present a detailed study of the young T Tauri star Par 1724, located 15 arc min north of the Trapezium cluster in Orion. Our extensive VRI photometric measurements confirm the rotational period to be 5.7 days. Repeated high-resolution spectra show variability in the radial velocity with the same period. A Doppler imaging analysis based on high-S/N high-resolution spectra yields an image showing a pronounced dark feature (spot) at relatively low latitude, which is responsible for most or all of the observed variability. Our high-resolution spectra yield a rotational velocity of v * sin i =~ 71 km s(-1) , a surface gravity of log g =~ 3, and a mean heliocentric radial velocity of ~ 23 km s(-1) , the latter being consistent with membership to the Orion association. The equivalent width of the lithium 6708 Angstroms line is variable, consistent with rotational modulation. The line is stronger when the spot is on the front side; the lithium abundance observed when the spot is on the back side is consistent with the primordial value. Many ROSAT X-ray observations show that Par 1724 is a strong and variable X-ray source. It has shown one of the most powerful X-ray flares. Our deep infrared imaging at high spatial resolution reveals no physically bound visual companions down to ~ 1 arc sec separations and a magnitude difference up to Delta R = 7 mag, and also no companion down to ~ 0.13 arc sec with Delta K = 2.5 mag. We also present the spectral energy distribution of Par 1724 and show that it does not display infrared excess. We estimate the bolometric luminosity to be ~ 49 Lsun, the spectral type to be K0, and the radius to be ~ 9 Rsun. Although Par 1724 appears to have lost all its circumstellar material, its bolometric luminosity places it very close to the stellar birth-line at an age of only ~ 2 * 10(5) years, with a mass of ~ 3 Msun. According to its present location and 3D space motion ( ~ 20 km s(-1) to the north relative to the cluster), Par 1724 may have

  2. Fundamental parameters of Wolf-Rayet stars. I. Ofpe/WN9 stars.

    NASA Astrophysics Data System (ADS)

    Crowther, P. A.; Hillier, D. J.; Smith, L. J.

    1995-01-01

    A detailed study has been carried out for 4 LMC Ofpe/WN9 (`slash') stars, and the sole Galactic WN9 star WR108 (HDE 313846), using new high S/N spectroscopy and archive UV and near-IR spectroscopy. Our observations reveal that photospheric Of features such as HeIIλ4542 are absent from the optical spectra of our sampled stars. All observed optical lines are formed in the stellar wind, and so we prefer WN9 or WN10 classifications based on the relative strengths of NIIλ3995 and NIIIλ4634-41, with BE 381 and Sk-66 40 prototype WN9 and WN10 stars, respectively. HDE 269927c and R84 are given WN9 classifications, with WR108 newly assigned WN9+abs due to the spectral appearance of the upper Balmer series. The distance to WR108 is determined from an analysis of its interstellar spectrum. Previously WR108 has been considered to be a possible member of Sgr OB1 (1.6 kpc, Lundstroem & Stenholm 1984[LS84]) which results in a uniquely low stellar luminosity for this type of object. Using the standard Galactic rotation curve of Fich et al. (1989) we derive 5+/-1 kpc, resulting in a luminosity very similar to R84. Tailored analyses using the WR standard model, including metals, result in the following stellar parameters for all stars: T_*_=29.5+/-1.0kK, L/Lsun_=10^5.65+/-0.2^, ˙(M)=3.5+/-1x10^-5^Msun_/yr and vinfinity_=400+/-100km/s (vinfinity_=1170km/s for WR108). The stellar parameters determined for R84 compare well with those determined previously by Schmutz et al. (1991)[SCH+91] indicating that the effect of CNO elements is negligible for WN stars. The metallicity of the LMC stars is around Z~0.008 while Z~0.035 results for the Galactic WN9 star. Abundances for the LMC stars (H/He=2.5+/-1, N/He~0.003, C/N~0.1) are in reasonable agreement with the results of evolutionary models at low metallicity (Schaerer et al. 1993a) although observed luminosities are significantly lower than predictions for stars entering the WR phase. The luminosity and chemistry of R84 are identical

  3. New estimates of the production of volatile gases from ablating carbonaceous micrometeoroids at Earth and Mars during an E-belt-type Late Heavy Bombardment

    NASA Astrophysics Data System (ADS)

    Court, Richard W.; Sephton, Mark A.

    2014-11-01

    Heating and ablation of micrometeoroids during atmospheric entry yields volatile gases capable of altering atmospheric chemistry, surface climate and habitability. We have subjected powdered samples of the carbonaceous chondrites Orgueil (CI1), ALH 88045 (CM1), Cold Bokkeveld (CM2), Murchison (CM2) and Mokoia (CV3) to stepped pyrolysis-Fourier transform infrared spectroscopy to simulate the atmospheric entry of micrometeoroids and to quantify the yields of water, carbon dioxide and sulphur dioxide at various temperatures, offering insights into the nature of their source phases. We have incorporated these data into the recently-developed E-Belt model of the Late Heavy Bombardment (LHB) to estimate the production of volatiles from infalling micrometeoroids at Earth and Mars around four billion years ago. At the present day, the 4 (±2) × 1010 g yr-1 of micrometeoroids arriving at Earth yield around 2.5 (±1.3) × 109 g yr-1 of indigenous water, 4.1 (±2.2) × 109 g yr-1 of total water, 1.9 (±1.0) × 109 g yr-1 of carbon dioxide and about 1.1 (±0.6) × 109 g yr-1 of sulphur dioxide, where “indigenous” water exclude water evolved at the initial pyrolysis step of 250 °C. For Mars, the infall of 6.8 × 109 g yr-1 of micrometeoroids yields 3.6 (±1.9) × 108 g yr-1 of indigenous water, 6.4 (±3.4) × 108 g yr-1 of total water, 2.4 (±1.3) × 108 g yr-1 of carbon dioxide and 1.5 (±0.8) × 108 g yr-1 of sulphur dioxide. The LHB is associated with micrometeoroidal infall masses of 1.3 (±0.8) × 1022 g at Earth and 2.3 (±1.3) × 1021 g at Mars. For Earth, this mass is estimated to have produced 8.3 (±4.9) × 1020 g of indigenous water, 1.4 (±0.8) × 1021 g of total water, 6.3 (±3.7) × 1020 g of carbon dioxide and 3.8 (±2.2) × 1020 g of sulphur dioxide, with production rates in the peak 50 Myr of the LHB estimated at 5.1 (±3.1) × 1012 g yr-1 of indigenous water, 8.6 (±5.1) × 1012 g yr-1 of total water, 3.9 (±2.3) × 1012 g yr-1 of carbon dioxide and 2

  4. Detection of highly ionized iron during a giant flare of GX 301-2

    NASA Astrophysics Data System (ADS)

    Fuerst, Felix; Kreykenbohm, Ingo; Kretschmar, Peter; Ballhausen, Ralf; Pottschmidt, Katja

    2016-03-01

    GX 301-2 is a well known accreting X-ray pulsar on an eccentric orbit (P=41.5d, e=0.47; Koh et al. 1997, ApJ 479, 933) around its extremely massive companion star (M=43 Msun), showing regular outbursts centered about 1.4d before periastron passage.

  5. Trace Metal Budgets for a Forested Watershed in the New Jersey Pine Barrens

    NASA Astrophysics Data System (ADS)

    Swanson, Karen A.; Johnson, Arthur H.

    1980-04-01

    Deposition of Pb, Cu, Ni, Fe, Mn, and Cd on the McDonalds Branch Basin in bulk precipitation was 25.4, 5.3, 6.6, 64.6, 20.7, and <2 mg m-2 yr-1 for a 1 year period in 1978-1979. Output in streamflow was 1.7, 0.7, 1.9, 148, 12.8, and <1 mg m-2 yr-1, respectively, and loss to deep groundwater was 1.4, 1.9, 2.3, 123, 20.4, and <1 mg m-2 yr-1. Pb, Cu, and Ni accumulated in the basin, while there was a net loss of Fe and Mn from the ecosystem. The major mechanism for movement of Fe and Pb out of the basin was interpreted to be complexation with and transport by mobile organic matter.

  6. Twenty years of continuous high time resolution volatile organic compound monitoring in the United Kingdom from 1993 to 2012

    NASA Astrophysics Data System (ADS)

    Derwent, R. G.; Dernie, J. I. R.; Dollard, G. J.; Dumitrean, P.; Mitchell, R. F.; Murrells, T. P.; Telling, S. P.; Field, R. A.

    2014-12-01

    Continuous, high frequency observations of C2 - C8 hydrocarbons began in the United Kingdom in 1993 and have continued through to the present day at a range of kerbside, urban background and rural locations. Most of the monitored hydrocarbons have shown dramatic declines in concentrations over the study period, with present levels close to an order of magnitude below their levels in the 1990s. The concentrations of 23 selected hydrocarbons have been aggregated up to give an estimate of the total VOC concentrations. These annual values have shown an exponential decline of -18% yr-1 at the London Marylebone Road kerbside site, -11% yr-1 at the London Eltham urban background site and -22% yr-1 at the rural Harwell site. Similar declines have been reported in UK road transport VOC emissions, demonstrating how the VOC emission inventories have apparently captured the salient features influencing real-world VOC emissions over the 1994-2012 period.

  7. The Gravity Probe B test of general relativity

    NASA Astrophysics Data System (ADS)

    Everitt, C. W. F.; Muhlfelder, B.; DeBra, D. B.; Parkinson, B. W.; Turneaure, J. P.; Silbergleit, A. S.; Acworth, E. B.; Adams, M.; Adler, R.; Bencze, W. J.; Berberian, J. E.; Bernier, R. J.; Bower, K. A.; Brumley, R. W.; Buchman, S.; Burns, K.; Clarke, B.; Conklin, J. W.; Eglington, M. L.; Green, G.; Gutt, G.; Gwo, D. H.; Hanuschak, G.; He, X.; Heifetz, M. I.; Hipkins, D. N.; Holmes, T. J.; Kahn, R. A.; Keiser, G. M.; Kozaczuk, J. A.; Langenstein, T.; Li, J.; Lipa, J. A.; Lockhart, J. M.; Luo, M.; Mandel, I.; Marcelja, F.; Mester, J. C.; Ndili, A.; Ohshima, Y.; Overduin, J.; Salomon, M.; Santiago, D. I.; Shestople, P.; Solomonik, V. G.; Stahl, K.; Taber, M.; Van Patten, R. A.; Wang, S.; Wade, J. R.; Worden, P. W., Jr.; Bartel, N.; Herman, L.; Lebach, D. E.; Ratner, M.; Ransom, R. R.; Shapiro, I. I.; Small, H.; Stroozas, B.; Geveden, R.; Goebel, J. H.; Horack, J.; Kolodziejczak, J.; Lyons, A. J.; Olivier, J.; Peters, P.; Smith, M.; Till, W.; Wooten, L.; Reeve, W.; Anderson, M.; Bennett, N. R.; Burns, K.; Dougherty, H.; Dulgov, P.; Frank, D.; Huff, L. W.; Katz, R.; Kirschenbaum, J.; Mason, G.; Murray, D.; Parmley, R.; Ratner, M. I.; Reynolds, G.; Rittmuller, P.; Schweiger, P. F.; Shehata, S.; Triebes, K.; VandenBeukel, J.; Vassar, R.; Al-Saud, T.; Al-Jadaan, A.; Al-Jibreen, H.; Al-Meshari, M.; Al-Suwaidan, B.

    2015-11-01

    The Gravity Probe B mission provided two new quantitative tests of Einstein’s theory of gravity, general relativity (GR), by cryogenic gyroscopes in Earth’s orbit. Data from four gyroscopes gave a geodetic drift-rate of -6601.8 ± 18.3 marc-s yr-1 and a frame-dragging of -37.2 ± 7.2 marc-s yr-1, to be compared with GR predictions of -6606.1 and -39.2 marc-s yr-1 (1 marc-s = 4.848 × 10-9 radians). The present paper introduces the science, engineering, data analysis, and heritage of Gravity Probe B, detailed in the accompanying 20 CQG papers.

  8. Esimating the emission of photopollutants from the city of Lagos from aircraft observations

    NASA Astrophysics Data System (ADS)

    Evans, M. J.; Hopkins, J.; Lee, J.; Lewis, A.; Marsham, J.; Parker, D.; Stewart, D.; Capes, G.; Williams, P.; Crosier, J.

    2007-12-01

    The city of Lagos, Nigeria is the second most populated city in Africa and by 2020 is likely to be the most populated. During the AMMA campaign in 2006 the UK BAe146 aircraft flew an orbit around the city observing the concentration of key photo-pollutants. This allowed the fluxes and thus emissions from the city to be calculated. We calculate CO, NOx and VOC emissions to be on the order of 1 Tg (CO) yr-1, 0.01 Tg (N) yr-1, 0.2 Tg (VOC) yr-1 respectively. Based upon a principal components analysis of the observations we split the emissions due to evaporative, low temperature combustion and high temperature combustion.

  9. Mapping critical loads of nitrogen deposition for aquatic ecosystems in the Rocky Mountains, USA

    USGS Publications Warehouse

    Nanus, Leora; Clow, David W.; Saros, Jasmine E.; Stephens, Verlin C.; Campbell, Donald H.

    2012-01-01

    Spatially explicit estimates of critical loads of nitrogen (N) deposition (CLNdep) for nutrient enrichment in aquatic ecosystems were developed for the Rocky Mountains, USA, using a geostatistical approach. The lowest CLNdep estimates (-1 yr-1) occurred in high-elevation basins with steep slopes, sparse vegetation, and abundance of exposed bedrock and talus. These areas often correspond with areas of high N deposition (>3 kg N ha-1 yr-1), resulting in CLNdep exceedances ≥1.5 ± 1 kg N ha-1 yr-1. CLNdep and CLNdep exceedances exhibit substantial spatial variability related to basin characteristics and are highly sensitive to the NO3- threshold at which ecological effects are thought to occur. Based on an NO3- threshold of 0.5 μmol L-1, N deposition exceeds CLNdep in 21 ± 8% of the study area; thus, broad areas of the Rocky Mountains may be impacted by excess N deposition, with greatest impacts at high elevations.

  10. Methane production from mixed tropical savanna and forest vegetation in Venezuela

    NASA Astrophysics Data System (ADS)

    Crutzen, P. J.; Sanhueza, E.; Brenninkmeijer, C. A. M.

    2006-04-01

    Measurements of methane concentrations in the boundary layer in the northern part of the Guayana shield, Venezuela, during the wet season (October 1988), showed the presence of substantial methane surface emissions. The measuring site is within the savanna climate region, but is affected by emissions from savanna and forest vegetation. From day versus night concentration measurements, with higher concentrations during night, a methane source strength near the site of 3-7×1011 molecules/cm2/s can be estimated, which includes emissions from small tracts of flooded soils, termites and especially tropical vegetation. Extrapolated to the entire savanna, this may imply a methane source of ~30-60 Tg yr-1 similar to the one calculated for tropical vegetation on the basis of recently published in vitro plant emission experiments by Keppler et al. (2006), which indicate emissions of ~30 Tg yr-1 for tropical savannas and grasslands and ~78 Tg yr-1 for tropical forests.

  11. Photometry and membership for low mass stars in the young open cluster NGC 2516

    NASA Astrophysics Data System (ADS)

    Jeffries, R. D.; Thurston, M. R.; Hambly, N. C.

    2001-09-01

    We present the results of a 0.86 square degree CCD photometric survey of the open cluster NGC 2516, which has an age of about 150 Myr and may have a much lower metallicity than the similarly-aged Pleiades. Our BVI_c survey of cluster members is complete to V =~ 20 and is used to select a preliminary catalogue of 1254 low mass (0.2Msun) cluster candidates, of which about 70-80 percent are expected to be genuine. After applying corrections for contamination by non-members and adding data for higher mass stars from the literature, we investigate the cluster binarity, luminosity and mass function, mass segregation and total mass. We find a binary fraction of 26+/-5 percent, for A to M-type systems with mass ratios between 0.6 and 1, which is very similar to the Pleiades. The mass function is metallicity and evolutionary-model dependent, but consistent with a Salpeter-like law (dN/dlog M~ M-alpha , alpha =+1.47+/-0.11 or alpha =+1.67+/-0.11 for the solar and half-solar metallicity models of Siess et al. \\cite{siess00}, and alpha =+1.58+/-0.10 for the solar metallicity models of D'Antona & Mazzitelli \\cite{dantona97}), for 0.7Msun. At lower masses (0.3Msun) there is a sharp fall in the mass function, with alpha =-0.75+/-0.20 or alpha =-0.49+/-0.13 (for the solar and half-solar metallicity models of Siess et al.), and alpha =-1.00+/-0.18 (for the solar metallicity models of D'Antona & Mazzitelli). The true stellar mass function might have alpha values up to 0.4 larger if account were taken of low mass stars in unresolved binary systems with mass ratios less than 0.6. The falling mass function of NGC 2516 at lower masses seems inconsistent with the much flatter mass functions derived from comparable data in the Pleiades and field populations. This deficit of lower mass, fainter stars is also seen in the observed luminosity function. We rule out incompleteness as the cause of this discrepancy, but demonstrate that mass segregation is clearly present

  12. [Ecosystem productivity process model for landscape based on remote sensing and surface data].

    PubMed

    Zhang, Na; Yu, Guirui; Zhao, Shidong; Yu, Zhenliang

    2003-05-01

    In this paper, the a ecosystem productivity process model for landscape (EPPML) reflecting carbon and water cycles of system was described and discussed. In EPPML, leaf area index (LAI) that greatly influenced vegetation productivity was received from remote sensing images, the spatial distribution and temporal dynamics of net primary productivity (NPP) and evapotranspiration were simulated. Geographical information system (GIS) was used to process, analyze, and display spatial data. Thus, the studies on physiological ecology could be extended, and converted from small scale to larger scale. Using EPPML, the vegetation productivity in Changbai Mountain Natural Reserve in 1995 was simulated. EPPML could well and truly simulate the NPP of main vegetations in the natural reserve. NPP was estimated to be 0.680 kg Cm.-2.yr.-1, mostly ranging from 0.105 to 1.241 kg C.m-2.yr.-1, accounting for 82.1%. The highest NPP (1.084 kg C.m-2.yr-1) appeared in mixed broad-leaved and Korean pine forests. The total NPP was estimated to be 1.332 x 10(6) t C.yr-1. The highest total NPP appeared in mixed broad-leaved and Korean pine forests and spruce-fir forest, which were 0.540 x 10(6) t C.yr.-1 and 0.428 x 10(6) t C.yr.-1, respectively. The seasonal variation of NPP appeared obvious single peak with peak value in July (6.13 g C.m-2.d-1). The most NPP accumulated in the summer, which was 0.465 kg C.m-2, secondly in the spring, and least in the winter. PMID:12924111

  13. Global emissions of HFC-143a (CH3CF3) and HFC-32 (CH2F2) from in situ and air archive atmospheric observations

    NASA Astrophysics Data System (ADS)

    O'Doherty, S.; Rigby, M.; Mühle, J.; Ivy, D. J.; Miller, B. R.; Young, D.; Simmonds, P. G.; Reimann, S.; Vollmer, M. K.; Krummel, P. B.; Fraser, P. J.; Steele, L. P.; Dunse, B.; Salameh, P. K.; Harth, C. M.; Arnold, T.; Weiss, R. F.; Kim, J.; Park, S.; Li, S.; Lunder, C.; Hermansen, O.; Schmidbauer, N.; Zhou, L. X.; Yao, B.; Wang, R. H. J.; Manning, A. J.; Prinn, R. G.

    2014-09-01

    High-frequency, in situ observations from the Advanced Global Atmospheric Gases Experiment (AGAGE), for the period 2003 to 2012, combined with archive flask measurements dating back to 1977, have been used to capture the rapid growth of HFC-143a (CH3CF3) and HFC-32 (CH2F2) mole fractions and emissions into the atmosphere. Here we report the first in situ global measurements of these two gases. HFC-143a and HFC-32 are the third and sixth most abundant hydrofluorocarbons (HFCs) respectively and they currently make an appreciable contribution to the HFCs in terms of atmospheric radiative forcing (1.7 ± 0.04 and 0.7 ± 0.02 mW m-2 in 2012 respectively). In 2012 the global average mole fraction of HFC-143a was 13.4 ± 0.3 ppt (1σ) in the lower troposphere and its growth rate was 1.4 ± 0.04 ppt yr-1; HFC-32 had a global mean mole fraction of 6.2 ± 0.2 ppt and a growth rate of 1.1 ± 0.04 ppt yr-1 in 2012. The extensive observations presented in this work have been combined with an atmospheric transport model to simulate global atmospheric abundances and derive global emission estimates. It is estimated that 23 ± 3 Gg yr-1 of HFC-143a and 21 ± 11 Gg yr-1 of HFC-32 were emitted globally in 2012, and the emission rates are estimated to be increasing by 7 ± 5% yr-1 for HFC-143a and 14 ± 11% yr-1 for HFC-32.

  14. Global emissions of HFC-143a (CH3CF3) and HFC-32 (CH2F2) from in situ and air archive atmospheric observations

    NASA Astrophysics Data System (ADS)

    O'Doherty, S.; Rigby, M.; Mühle, J.; Ivy, D. J.; Miller, B. R.; Young, D.; Simmonds, P. G.; Reimann, S.; Vollmer, M. K.; Krummel, P. B.; Fraser, P. J.; Steele, L. P.; Dunse, B.; Salameh, P. K.; Harth, C. M.; Arnold, T.; Weiss, R. F.; Kim, J.; Park, S.; Li, S.; Lunder, C.; Hermansen, O.; Schmidbauer, N.; Zhou, L. X.; Yao, B.; Wang, R. H. J.; Manning, A.; Prinn, R. G.

    2014-03-01

    High frequency, in situ observations from the Advanced Global Atmospheric Gases Experiment (AGAGE), for the period 2003 to 2012, combined with archive flask measurements dating back to 1977, have been used to capture the rapid growth of HFC-143a (CH3CF3) and HFC-32 (CH2F2) mole fractions and emissions into the atmosphere. Here we report the first in situ global measurements of these two gases. HFC-143a and HFC-32 are the third and sixth most abundant HFCs respectively and they currently make an appreciable contribution to the HFCs in terms of atmospheric radiative forcing (1.7 and 0.7 mW m2 in 2012, respectively). In 2012 the global average mole fraction of HFC-143a was 13.4 ± 0.3 ppt (1-sigma) in the lower troposphere and its growth rate was 1.4 ± 0.04 ppt yr-1; HFC-32 had a global mean mole fraction of 6.2 ± 0.2 ppt and a growth rate of 1.1 ± 0.04 ppt yr-1 in 2012. The extensive observations presented in this work have been combined with an atmospheric transport model to simulate global atmospheric abundances and derive global emission estimates. It is estimated that 23 ± 3 Gg yr-1 of HFC-143a and 21 ± 11 Gg yr-1 of HFC-32 were emitted globally in 2012, and the emission rates are estimated to be increasing 7 ± 5% yr-1 for HFC-143a and 14 ± 11% yr-1 for HFC-32.

  15. Growth of the Antarctic octocoral Primnoella scotiae and predation by the anemone Dactylanthus antarcticus

    NASA Astrophysics Data System (ADS)

    Peck, Lloyd S.; Brockington, Simon

    2013-08-01

    Growth rates in Antarctic marine ectotherms have been demonstrated to be slowed by two to five times compared to shallow-water temperate species, with no previous reports for octocorals. Here growth rates were estimated in the single axis, non-branching Antarctic octocoral Primnoella scotiae using repeated in situ length measures covering both summer and winter periods, for tagged colonies from three sites at Signy Island over a two year period. Mean rates of length increase at the different sites ranged from 0.96 mm yr-1 to 55.3 mm yr-1. The fastest individual colony growth rate at any site ranged from 2.55 mm yr-1 to 175.6 mm yr-1. The mean of the fastest growth rates across all sites was 33.0 mm yr-1±14.7 (s.e.). Growth was significantly different between sites, and also between seasons and years. The mean overall increase in diameter of the average sized colony in the study (222.5 mm in axis length) was 0.053 mm yr-1. This is the slowest reported growth rate of any octocoral to date, and is five times slower than growth in most cold water octocorals. During the study it was noted that colonies were being attacked and consumed by the anemone Dactylanthus antarcticus. At one of the sites studied, between 5% and 8% of colonies surveyed were attacked each month. Anemone dispersal was via whole body inflation and drifting to new prey colonies that were attached to using tentacle-like column protuberances.

  16. Anthropogenic perturbation of the carbon fluxes from land to ocean

    NASA Astrophysics Data System (ADS)

    Regnier, Pierre; Friedlingstein, Pierre; Ciais, Philippe; MacKenzie, Fred T.; Gruber, Nicolas; Janssens, Ivan A.; Laruelle, Goulven G.; Lauerwald, Ronny; Luyssaert, Sebastiaan; Andersson, Andreas J.; Arndt, Sandra; Arnosti, Carol; Borges, Alberto V.; Dale, Andrew W.; Gallego-Sala, Angela; Goddéris, Yves; Goossens, Nicolas; Hartmann, Jens; Heinze, Christoph; Ilyina, Tatiana; Joos, Fortunat; Larowe, Douglas E.; Leifeld, Jens; Meysman, Filip J. R.; Munhoven, Guy; Raymond, Peter A.; Spahni, Renato; Suntharalingam, Parvadha; Thullner, Martin

    2013-08-01

    A substantial amount of the atmospheric carbon taken up on land through photosynthesis and chemical weathering is transported laterally along the aquatic continuum from upland terrestrial ecosystems to the ocean. So far, global carbon budget estimates have implicitly assumed that the transformation and lateral transport of carbon along this aquatic continuum has remained unchanged since pre-industrial times. A synthesis of published work reveals the magnitude of present-day lateral carbon fluxes from land to ocean, and the extent to which human activities have altered these fluxes. We show that anthropogenic perturbation may have increased the flux of carbon to inland waters by as much as 1.0 Pg C yr-1 since pre-industrial times, mainly owing to enhanced carbon export from soils. Most of this additional carbon input to upstream rivers is either emitted back to the atmosphere as carbon dioxide (~0.4 Pg C yr-1) or sequestered in sediments (~0.5 Pg C yr-1) along the continuum of freshwater bodies, estuaries and coastal waters, leaving only a perturbation carbon input of ~0.1 Pg C yr-1 to the open ocean. According to our analysis, terrestrial ecosystems store ~0.9 Pg C yr-1 at present, which is in agreement with results from forest inventories but significantly differs from the figure of 1.5 Pg C yr-1 previously estimated when ignoring changes in lateral carbon fluxes. We suggest that carbon fluxes along the land-ocean aquatic continuum need to be included in global carbon dioxide budgets.

  17. Responses to simulated nitrogen deposition by the neotropical epiphytic orchid Laelia speciosa.

    PubMed

    Díaz-Álvarez, Edison A; Lindig-Cisneros, Roberto; de la Barrera, Erick

    2015-01-01

    Potential ecophysiological responses to nitrogen deposition, which is considered to be one of the leading causes for global biodiversity loss, were studied for the endangered endemic Mexican epiphytic orchid, Laelia speciosa, via a shadehouse dose-response experiment (doses were 2.5, 5, 10, 20, 40, and 80 kg N ha(-1) yr(-1)) in order to assess the potential risk facing this orchid given impending scenarios of nitrogen deposition. Lower doses of nitrogen of up to 20 kg N ha yr(-1), the dose that led to optimal plant performance, acted as fertilizer. For instance, the production of leaves and pseudobulbs were respectively 35% and 36% greater for plants receiving 20 kg N ha yr(-1) than under any other dose. Also, the chlorophyll content and quantum yield peaked at 0.66 ± 0.03 g m(-2) and 0.85 ± 0.01, respectively, for plants growing under the optimum dose. In contrast, toxic effects were observed at the higher doses of 40 and 80 kg N ha yr(-1). The δ (13)C for leaves averaged -14.7 ± 0.2‰ regardless of the nitrogen dose. In turn, δ (15)N decreased as the nitrogen dose increased from 0.9 ± 0.1‰ under 2.5 kg N ha(-1)yr(-1) to -3.1 ± 0.2‰ under 80 kg N ha(-1)yr(-1), indicating that orchids preferentially assimilate NH4 (+) rather than NO3 (-) of the solution under higher doses of nitrogen. Laelia speciosa showed a clear response to inputs of nitrogen, thus, increasing rates of atmospheric nitrogen deposition can pose an important threat for this species. PMID:26131375

  18. Far Ultraviolet Spectroscopy of Seven Nova-Like Variables

    NASA Astrophysics Data System (ADS)

    Mizusawa, Trisha; Merritt, Jason; Ballouz, Ronald-Louis; Bonaro, Michael; Foran, Sean; Plumberg, Christopher; Stewart, Heather; Wiley, Trayer; Sion, Edward M.

    2010-03-01

    We present the results of a multicomponent synthetic spectral analysis of the archival far ultraviolet spectra of several key nova-like variables including members of the SW Sex, RW Tri, UX UMa, and VY Scl subclasses: KR Aur, RW Tri, V825 Her, V795 Her, BP Lyn, V425 Cas, and HL Aqr. Accretion rates as well as the possible flux contribution of the accreting white dwarf are included in our analysis. Except for RW Tri, which has a reliable trigonometric parallax, we computed the distances to the nova-like systems using the method of Knigge. Our analysis of seven archival IUE spectra of RW Tri at its parallax distance of 341 pc consistently indicates a low mass (~0.4 Msolar) white dwarf and an average accretion rate, {\\overset{.}{M}} = 6.3 × 10-9 Msolar yr-1. For KR Aur, we estimate that the white dwarf has Teff = 29,000 ± 2000 K, log g = 8.4, and contributes 18% of the far-UV flux, while an accretion disk with accretion rate {\\overset{.}{M}} = 3 × 10-10 Msolar yr-1 at an inclination of 41° contributes the remainder. We find that an accretion disk dominates the far-UV spectrum of V425 Cas but a white dwarf contributes nonnegligibly with approximately 18% of the far-UV flux. For the two high state nova-likes, HL Aqr and V825 Her, their accretion disks totally dominate with {\\overset{.}{M}} = 1 × 10-9 Msolar yr-1 and 3 × 10-9 Msolar yr-1, respectively. For BP Lyn we find {\\overset{.}{M}} = 1 × 10-8 Msolar yr-1 while for V795 Her, we find an accretion rate of {\\overset{.}{M}} = 1 × 10-10 Msolar yr-1. We discuss the implications of our results for the evolutionary status of nova-like variables.

  19. Variability of projected terrestrial biosphere responses to elevated levels of atmospheric CO2 due to uncertainty in biological nitrogen fixation

    NASA Astrophysics Data System (ADS)

    Meyerholt, Johannes; Zaehle, Sönke; Smith, Matthew J.

    2016-03-01

    Including a terrestrial nitrogen (N) cycle in Earth system models has led to substantial attenuation of predicted biosphere-climate feedbacks. However, the magnitude of this attenuation remains uncertain. A particularly important but highly uncertain process is biological nitrogen fixation (BNF), which is the largest natural input of N to land ecosystems globally. In order to quantify this uncertainty and estimate likely effects on terrestrial biosphere dynamics, we applied six alternative formulations of BNF spanning the range of process formulations in current state-of-the-art biosphere models within a common framework, the O-CN model: a global map of static BNF rates, two empirical relationships between BNF and other ecosystem variables (net primary productivity and evapotranspiration), two process-oriented formulations based on plant N status, and an optimality-based approach. We examined the resulting differences in model predictions under ambient and elevated atmospheric [CO2] and found that the predicted global BNF rates and their spatial distribution for contemporary conditions were broadly comparable, ranging from 108 to 148 Tg N yr-1 (median: 128 Tg N yr-1), despite distinct regional patterns associated with the assumptions of each approach. Notwithstanding, model responses in BNF rates to elevated levels of atmospheric [CO2] (+200 ppm) ranged between -4 Tg N yr-1 (-3 %) and 56 Tg N yr-1 (+42 %) (median: 7 Tg N yr-1 (+8 %)). As a consequence, future projections of global ecosystem carbon (C) storage (+281 to +353 Pg C, or +13 to +16 %) as well as N2O emission (-1.6 to +0.5 Tg N yr-1, or -19 to +7 %) differed significantly across the different model formulations. Our results emphasize the importance of better understanding the nature and magnitude of BNF responses to change-induced perturbations, particularly through new empirical perturbation experiments and improved model representation.

  20. Variability of projected terrestrial biosphere responses to elevated levels of atmospheric CO2 due to uncertainty in biological nitrogen fixation

    NASA Astrophysics Data System (ADS)

    Meyerholt, J.; Zaehle, S.; Smith, M. J.

    2015-12-01

    Including a terrestrial nitrogen (N) cycle in Earth system models has led to substantial attenuation of predicted biosphere-climate feedbacks. However, the magnitude of this attenuation remains uncertain. A particularly important, but highly uncertain process is biological nitrogen fixation (BNF), which is the largest natural input of N to land ecosystems globally. In order to quantify this uncertainty, and estimate likely effects on terrestrial biosphere dynamics, we applied six alternative formulations of BNF spanning the range of process formulations in current state-of-the-art biosphere models within a common framework, the O-CN model: a global map of static BNF rates, two empirical relationships between BNF and other ecosystem variables (net primary productivity (NPP) and evapotranspiration), two process-oriented formulations based on plant N status, and an optimality-based approach. We examined the resulting differences in model predictions under ambient and elevated atmospheric [CO2] and found that the predicted global BNF rates and their spatial distribution for contemporary conditions were broadly comparable, ranging from 95 to 134 Tg N yr-1 (median 119 Tg N yr-1), despite distinct regional patterns associated with the assumptions of each approach. Notwithstanding, model responses in BNF rates to elevated levels of atmospheric [CO2] (+200 ppm) ranged between -4 Tg N yr-1 (-3 %) and 56 Tg N yr-1 (+42 %) (median 7 Tg N yr-1 (+8 %)). As a consequence, future projections of global ecosystem carbon storage (+281 to +353 Pg C, or +13 to +16 %), as well as N2O emission (-1.6 to +0.5 Tg N yr-1, or -19 to +7 %) differed significantly across the different model formulations. Our results emphasize the importance of better understanding the nature and magnitude of BNF responses to change-induced perturbations, particularly through new empirical perturbation experiments and improved model representation.