Challenges of In-Flight Calibrations for the Mars Reconnaissance Orbiter Payload

NASA Technical Reports Server (NTRS)

Xaypraseuth, Peter

2007-01-01

The Mars Reconnaissance Orbiter is the most complex spacecraft that has ever been sent to investigate the Red Planet. A major part of what makes this mission so complex is the suite of instruments that were selected. The instruments on MRO vary from a simple imaging system, not much larger than a pocket knife to the largest camera ever flown to another planet. Not only does the size of the instruments vary, so do the scientific investigations associated with each instrument. In order to ensure that this payload suite would be able to satisfy all of its science objectives, a major effort was put forth by the MRO Project to ensure these instruments were well calibrated prior to the start of the Primary Science Phase. The in-flight calibration plan for MRO proved to be quite challenging, given the often conflicting requirements due to the varying capability of each of the instruments and the desire to constrain the workload on the Mission Operations personnel. The quality of data returned by MRO since the start of the Primary Science Phase is a tribute to the effort that was put forth to characterize the in-flight performance of the instruments. This paper will describe the challenges associated with the planning and implementation of the various calibration events on MRO, and will exhibit some of the results from those calibrations.

Time-variable and static gravity field of Mars from MGS, Mars Odyssey, and MRO

NASA Astrophysics Data System (ADS)

Genova, Antonio; Goossens, Sander; Lemoine, Frank G.; Mazarico, Erwan; Neumann, Gregory A.; Smith, David E.; Zuber, Maria T.

2016-04-01

The Mars Global Surveyor (MGS), Mars Odyssey (ODY), and Mars Reconnaissance Orbiter (MRO) missions have significantly contributed to the determination of global high-resolution global gravity fields of Mars for the last 16 years. All three spacecraft were located in sun-synchronous, near-circular polar mapping orbits for their primary mission phases at different altitudes and Local Solar Time (LST). X-Band tracking data have been acquired from the NASA Deep Space Network (DSN) providing information on the time-variable and static gravity field of Mars. MGS operated between 1999 and 2006 at 390 km altitude. ODY and MRO are still orbiting Mars with periapsis altitudes of 400 km and 255 km, respectively. Before entering these mapping phases, all three spacecraft collected radio tracking data at lower altitudes (˜170-200 km) that help improve the resolution of the gravity field of Mars in specific regions. We analyzed the entire MGS radio tracking data set, and ODY and MRO radio data until 2015. These observations were processed using a batch least-squares filter through the NASA GSFC GEODYN II software. We combined all 2- and 3-way range rate data to estimate the global gravity field of Mars to degree and order 120, the seasonal variations of gravity harmonic coefficients C20, C30, C40 and C50 and the Love number k2. The gravity contribution of Mars atmospheric pressures on the surface of the planet has been discerned from the time-varying and static gravity harmonic coefficients. Surface pressure grids computed using the Mars-GRAM 2010 atmospheric model, with 2.5° x2.5° spatial and 2-h resolution, are converted into gravity spherical harmonic coefficients. Consequently, the estimated gravity and tides provide direct information on the solid planet. We will present the new Goddard Mars Model (GMM-3) of Mars gravity field in spherical harmonics to degree and order 120. The solution includes the Love number k2 and the 3-frequencies (annual, semi-annual, and tri-annual) time-variable coefficients of the gravity zonal harmonics C20, C30, C40 and C50. The seasonal gravity coefficients led us to determine the inter-annual mass exchange between the polar caps over ˜11 years from October 2002 to November 2014.

Relay Sequence Generation Software

NASA Technical Reports Server (NTRS)

Gladden, Roy E.; Khanampompan, Teerapat

2009-01-01

Due to thermal and electromagnetic interactivity between the UHF (ultrahigh frequency) radio onboard the Mars Reconnaissance Orbiter (MRO), which performs relay sessions with the Martian landers, and the remainder of the MRO payloads, it is required to integrate and de-conflict relay sessions with the MRO science plan. The MRO relay SASF/PTF (spacecraft activity sequence file/ payload target file) generation software facilitates this process by generating a PTF that is needed to integrate the periods of time during which MRO supports relay activities with the rest of the MRO science plans. The software also generates the needed command products that initiate the relay sessions, some features of which are provided by the lander team, some are managed by MRO internally, and some being derived.

Effect of sub-Tg annealing on CuZr and AlSm glasses: A molecular dynamics study

NASA Astrophysics Data System (ADS)

Sun, Yang; Zhang, Feng; Zhang, Yue; Ye, Zhuo; Mendelev, Mikhail; Wang, Cai-Zhuang; Ho, Kai-Ming

Cu65Zr35 and Al90Sm10 glasses, which represent strong and marginal binary metallic glass formers, respectively, were developed with a sub-Tg annealing method using Molecular Dynamics simulations. The short-range order (SRO) in both systems was characterized based on the concept of ``crystal gene'' that we established recently. Furthermore, we found that while the local clusters representing the dominant short-range order form an ever-more pronounced interpenetrating network with slower cooling rates in Cu65Zr35 glasses, the interpenetration of SRO in Al90Sm10 glasses only shows a weak dependence on the cooling rate. This clear difference in the connectivity of the SRO, which can characterize the medium-range order (MRO), could contribute to the different glass forming abilities of both systems. Work at Ames Laboratory was supported by the U.S. Department of Energy, Basic Energy Sciences, Materials Science and Engineering Division, under Contract No. DE-AC02-07CH11358.

Operation of MRO's High Resolution Imaging Science Experiment (HiRISE): Maximizing Science Participation

NASA Technical Reports Server (NTRS)

Eliason, E.; Hansen, C. J.; McEwen, A.; Delamere, W. A.; Bridges, N.; Grant, J.; Gulich, V.; Herkenhoff, K.; Keszthelyi, L.; Kirk, R.

2003-01-01

Science return from the Mars Reconnaissance Orbiter (MRO) High Resolution Imaging Science Experiment (HiRISE) will be optimized by maximizing science participation in the experiment. MRO is expected to arrive at Mars in March 2006, and the primary science phase begins near the end of 2006 after aerobraking (6 months) and a transition phase. The primary science phase lasts for almost 2 Earth years, followed by a 2-year relay phase in which science observations by MRO are expected to continue. We expect to acquire approx. 10,000 images with HiRISE over the course of MRO's two earth-year mission. HiRISE can acquire images with a ground sampling dimension of as little as 30 cm (from a typical altitude of 300 km), in up to 3 colors, and many targets will be re-imaged for stereo. With such high spatial resolution, the percent coverage of Mars will be very limited in spite of the relatively high data rate of MRO (approx. 10x greater than MGS or Odyssey). We expect to cover approx. 1% of Mars at approx. 1m/pixel or better, approx. 0.1% at full resolution, and approx. 0.05% in color or in stereo. Therefore, the placement of each HiRISE image must be carefully considered in order to maximize the scientific return from MRO. We believe that every observation should be the result of a mini research project based on pre-existing datasets. During operations, we will need a large database of carefully researched 'suggested' observations to select from. The HiRISE team is dedicated to involving the broad Mars community in creating this database, to the fullest degree that is both practical and legal. The philosophy of the team and the design of the ground data system are geared to enabling community involvement. A key aspect of this is that image data will be made available to the planetary community for science analysis as quickly as possible to encourage feedback and new ideas for targets.

49 CFR 40.163 - How does the MRO report drug test results?

Code of Federal Regulations, 2012 CFR

2012-10-01

... for the test, if indicated on the CCF (e.g., random, post-accident); (4) Date of the collection; (5... 49 Transportation 1 2012-10-01 2012-10-01 false How does the MRO report drug test results? 40.163... How does the MRO report drug test results? (a) As the MRO, it is your responsibility to report all...

49 CFR 40.163 - How does the MRO report drug test results?

Code of Federal Regulations, 2011 CFR

2011-10-01

... for the test, if indicated on the CCF (e.g., random, post-accident); (4) Date of the collection; (5... 49 Transportation 1 2011-10-01 2011-10-01 false How does the MRO report drug test results? 40.163... How does the MRO report drug test results? (a) As the MRO, it is your responsibility to report all...

49 CFR 40.163 - How does the MRO report drug test results?

Code of Federal Regulations, 2013 CFR

2013-10-01

... for the test, if indicated on the CCF (e.g., random, post-accident); (4) Date of the collection; (5... 49 Transportation 1 2013-10-01 2013-10-01 false How does the MRO report drug test results? 40.163... How does the MRO report drug test results? (a) As the MRO, it is your responsibility to report all...

49 CFR 40.149 - May the MRO change a verified drug test result?

Code of Federal Regulations, 2010 CFR

2010-10-01

... 49 Transportation 1 2010-10-01 2010-10-01 false May the MRO change a verified drug test result? 40... § 40.149 May the MRO change a verified drug test result? (a) As the MRO, you may change a verified test... positive. You would change X's test result from positive to negative and contact Y to conduct a...

Child Temperament Moderates Effects of Parent-Child Mutuality on Self-Regulation: A Relationship-Based Path for Emotionally Negative Infants

PubMed Central

Kim, Sanghag; Kochanska, Grazyna

2012-01-01

This study examined infants’ negative emotionality as moderating the effect of parent-child Mutually Responsive Orientation (MRO) on children’s self-regulation (N=102). Negative emotionality was observed in anger-eliciting episodes and in interactions with parents at 7 months. MRO was coded in naturalistic interactions at 15 months. Self-regulation was measured at 25 months in effortful control battery and as self-regulated compliance to parental requests and prohibitions. Negative emotionality moderated the effects of mother-child MRO. Highly negative infants were less self-regulated when they were in unresponsive relationships (low MRO), but more self-regulated when in responsive relationships (high MRO). For infants not prone to negative emotionality, there was no link between MRO and self-regulation. The “regions-of-significance” analysis supported the differential susceptibility model not the diathesis-stress model. PMID:22670684

Structural and chemical orders in N i 64.5 Z r 35.5 metallic glass by molecular dynamics simulation

DOE PAGES

Tang, L.; Wen, T. Q.; Wang, N.; ...

2018-03-06

The atomic structure of Ni 64.5Zr 35.5 metallic glass has been investigated by molecular dynamics (MD) simulations. The calculated structure factors from the MD glassy sample at room temperature agree well with the X-ray diffraction (XRD) and neutron diffraction (ND) experimental data. Using the pairwise cluster alignment and clique analysis methods, we show that there are three types dominant short-range order (SRO) motifs around Ni atoms in the glass sample of Ni 64.5Zr 35.5, i.e., Mixed- Icosahedron(ICO)-Cube, Twined-Cube and icosahedron-like clusters. Furthermore, chemical order and medium-range order (MRO) analysis show that the Mixed-ICOCube and Twined-Cube clusters exhibit the characteristics ofmore » the crystalline B2 phase. In conclusion, our simulation results suggest that the weak glass-forming ability (GFA) of Ni 64.5Zr 35.5 can be attributed to the competition between the glass forming ICO SRO and the crystalline Mixed-ICO-Cube and Twined-Cube motifs.« less

Structural and chemical orders in N i 64.5 Z r 35.5 metallic glass by molecular dynamics simulation

DOE Office of Scientific and Technical Information (OSTI.GOV)

Tang, L.; Wen, T. Q.; Wang, N.

The atomic structure of Ni 64.5Zr 35.5 metallic glass has been investigated by molecular dynamics (MD) simulations. The calculated structure factors from the MD glassy sample at room temperature agree well with the X-ray diffraction (XRD) and neutron diffraction (ND) experimental data. Using the pairwise cluster alignment and clique analysis methods, we show that there are three types dominant short-range order (SRO) motifs around Ni atoms in the glass sample of Ni 64.5Zr 35.5, i.e., Mixed- Icosahedron(ICO)-Cube, Twined-Cube and icosahedron-like clusters. Furthermore, chemical order and medium-range order (MRO) analysis show that the Mixed-ICOCube and Twined-Cube clusters exhibit the characteristics ofmore » the crystalline B2 phase. In conclusion, our simulation results suggest that the weak glass-forming ability (GFA) of Ni 64.5Zr 35.5 can be attributed to the competition between the glass forming ICO SRO and the crystalline Mixed-ICO-Cube and Twined-Cube motifs.« less

Structural and chemical orders in N i64.5Z r35.5 metallic glass by molecular dynamics simulation

NASA Astrophysics Data System (ADS)

Tang, L.; Wen, T. Q.; Wang, N.; Sun, Y.; Zhang, F.; Yang, Z. J.; Ho, K. M.; Wang, C. Z.

2018-03-01

The atomic structure of N i64.5Z r35.5 metallic glass has been investigated by molecular dynamics (MD) simulations. The calculated structure factors from the MD glassy sample at room temperature agree well with the x-ray diffraction (XRD) and neutron diffraction (ND) experimental data. Using the pairwise cluster alignment and clique analysis methods, we show that there are three types of dominant short-range order (SRO) motifs around Ni atoms in the glass sample of N i64.5Z r35.5 , i.e., mixed-icosahedron(ICO)-cube, intertwined-cube, and icosahedronlike clusters. Furthermore, chemical order and medium-range order (MRO) analysis show that the mixed-ICO-cube and intertwined-cube clusters exhibit the characteristics of the crystalline B2 phase. Our simulation results suggest that the weak glass-forming ability (GFA) of N i64.5Z r35.5 can be attributed to the competition between the glass forming ICO SRO and the crystalline mixed-ICO-cube and intertwined-cube motifs.

Long-Term Periodicity of the Mars Exospheric Density from MRO and Mars Odyssey Radio Tracking Data

NASA Astrophysics Data System (ADS)

Genova, A.; Goossens, S. J.; Lemoine, F. G.; Mazarico, E.; Smith, D. E.; Zuber, M. T.

2014-12-01

The Mars Odyssey and Mars Reconnaissance Orbiter (MRO) missions have collected more than 11 years of continuous tracking data of spacecraft in orbit around Mars. The radio science data are generally used to determine the static and seasonal gravity field of the central body. However, these two spacecraft are in different sun-synchronous orbits that cover a wide range of altitudes (250-410 km) where investigation of the atmosphere and climate of Mars so far have not been supported by in situ and remote sensing measurements. The drag perturbation acting on the probes provides indirect measurements of the Martian atmospheric density. Therefore, we focused our work on the determination of the long-term periodicity of the atmospheric constituents in the Mars exosphere with Mars Odyssey and MRO radio tracking data. We implemented the Drag Temperature Model (DTM) -Mars model into our Precise Orbit Determination (POD) program GEODYN-II to adequately reproduce variations in temperature and (partial) density along ODY and MRO trajectories. The recovery of Mars' atmospheric dynamics using Doppler tracking data requires the accurate modeling of all forces acting on the spacecraft. The main non-conservative force, apart from drag, is solar radiation pressure. Spacecraft panel reflectivities and the radiation pressure-scaling factor are not estimated, but we adjusted empirical once-per-revolution along-track periodic accelerations (cosine and sine) over each orbital arc to mitigate solar radiation pressure mismodeling. After converging the orbital data arcs, and editing out all the data during superior conjunctions, we combined the MRO and Mars Odyssey arcs in a global solution where we estimated spacecraft initial states, time-correlated drag scale factors, and annual and semi-annual variability of the major constituents in the Mars upper atmosphere. We will show that the updated DTM-Mars model provides a better prediction of the long-term variability of the dominant species, which are CO2, O, and He at the MRO and ODY orbit altitudes. The indirect measurements of atmospheric density profiles at those altitudes provide additional information to improve general circulation models, which already suitably represent lower altitudes in the atmosphere.

Mars Reconnaissance Orbiter Navigation Strategy for Dual Support of Insight and ExoMars Entry, Descent and Landing Demonstrator Module in 2016

NASA Technical Reports Server (NTRS)

Wagner, Sean V.; Menon, Premkumar R.; Chung, Min-Kun J.; Williams, Jessica L.

2015-01-01

Mars Reconnaissance Orbiter (MRO) will support NASA's InSight Mission and ESA's ExoMars Entry, Descent and Landing Demonstrator Module (EDM) in the fall of 2016 when both landers arrive at Mars. MRO provided relay support during the Entry, Descent and Landing (EDL) sequences of Mars Phoenix Lander in 2008 and the Mars Science Laboratory in 2012. Unlike these missions, MRO will coordinate between two EDL events separated by only three weeks: InSight on September 28, 2016 and EDM on October 19, 2016. This paper describes MRO Navigation's maneuver strategy to move MRO's ascending node to meet the In- Sight EDL phasing requirement and support EDM.

Raman scattering boson peak and differential scanning calorimetry studies of the glass transition in tellurium-zinc oxide glasses.

PubMed

Stavrou, E; Tsiantos, C; Tsopouridou, R D; Kripotou, S; Kontos, A G; Raptis, C; Capoen, B; Bouazaoui, M; Turrell, S; Khatir, S

2010-05-19

Raman scattering and differential scanning calorimetry (DSC) measurements have been carried out on four mixed tellurium-zinc oxide (TeO(2))(1 - x)(ZnO)(x) (x = 0.1, 0.2, 0.3, 0.4) glasses under variable temperature, with particular attention being given to the respective glass transition region. From the DSC measurements, the glass transition temperature T(g) has been determined for each glass, showing a monotonous decrease of T(g) with increasing ZnO content. The Raman study is focused on the low-frequency band of the glasses, the so-called boson peak (BP), whose frequency undergoes an abrupt decrease at a temperature T(d) very close to the respective T(g) values obtained by DSC. These results show that the BP is highly sensitive to dynamical effects over the glass transition and provides a means for an equally reliable (to DSC) determination of T(g) in tellurite glasses and other network glasses. The discontinuous temperature dependence of the BP frequency at the glass transition, along with the absence of such a behaviour by the high-frequency Raman bands (due to local atomic vibrations), indicates that marked changes of the medium range order (MRO) occur at T(g) and confirms the correlation between the BP and the MRO of glasses.

49 CFR 40.123 - What are the MRO's responsibilities in the DOT drug testing program?

Code of Federal Regulations, 2014 CFR

2014-10-01

... drug testing program? 40.123 Section 40.123 Transportation Office of the Secretary of Transportation PROCEDURES FOR TRANSPORTATION WORKPLACE DRUG AND ALCOHOL TESTING PROGRAMS Medical Review Officers and the Verification Process § 40.123 What are the MRO's responsibilities in the DOT drug testing program? As an MRO...

49 CFR 40.123 - What are the MRO's responsibilities in the DOT drug testing program?

Code of Federal Regulations, 2012 CFR

2012-10-01

... drug testing program? 40.123 Section 40.123 Transportation Office of the Secretary of Transportation PROCEDURES FOR TRANSPORTATION WORKPLACE DRUG AND ALCOHOL TESTING PROGRAMS Medical Review Officers and the Verification Process § 40.123 What are the MRO's responsibilities in the DOT drug testing program? As an MRO...

49 CFR 40.123 - What are the MRO's responsibilities in the DOT drug testing program?

Code of Federal Regulations, 2013 CFR

2013-10-01

... drug testing program? 40.123 Section 40.123 Transportation Office of the Secretary of Transportation PROCEDURES FOR TRANSPORTATION WORKPLACE DRUG AND ALCOHOL TESTING PROGRAMS Medical Review Officers and the Verification Process § 40.123 What are the MRO's responsibilities in the DOT drug testing program? As an MRO...

49 CFR 40.123 - What are the MRO's responsibilities in the DOT drug testing program?

Code of Federal Regulations, 2010 CFR

2010-10-01

... drug testing program? 40.123 Section 40.123 Transportation Office of the Secretary of Transportation PROCEDURES FOR TRANSPORTATION WORKPLACE DRUG AND ALCOHOL TESTING PROGRAMS Medical Review Officers and the Verification Process § 40.123 What are the MRO's responsibilities in the DOT drug testing program? As an MRO...

49 CFR 40.123 - What are the MRO's responsibilities in the DOT drug testing program?

Code of Federal Regulations, 2011 CFR

2011-10-01

... drug testing program? 40.123 Section 40.123 Transportation Office of the Secretary of Transportation PROCEDURES FOR TRANSPORTATION WORKPLACE DRUG AND ALCOHOL TESTING PROGRAMS Medical Review Officers and the Verification Process § 40.123 What are the MRO's responsibilities in the DOT drug testing program? As an MRO...

14 CFR 120.113 - Medical Review Officer, Substance Abuse Professional, and Employer Responsibilities.

Code of Federal Regulations, 2012 CFR

2012-01-01

...: CERTIFICATION AND OPERATIONS DRUG AND ALCOHOL TESTING PROGRAM Drug Testing Program Requirements § 120.113... provision of MRO services as part of its drug testing program. (b) Medical Review Officer (MRO). The MRO... working days after verifying a positive drug test result or refusal to submit to a test. (2) During the...

14 CFR 120.113 - Medical Review Officer, Substance Abuse Professional, and Employer Responsibilities.

Code of Federal Regulations, 2014 CFR

2014-01-01

...: CERTIFICATION AND OPERATIONS DRUG AND ALCOHOL TESTING PROGRAM Drug Testing Program Requirements § 120.113... provision of MRO services as part of its drug testing program. (b) Medical Review Officer (MRO). The MRO... working days after verifying a positive drug test result or refusal to submit to a test. (2) During the...

14 CFR 120.113 - Medical Review Officer, Substance Abuse Professional, and Employer Responsibilities.

Code of Federal Regulations, 2013 CFR

2013-01-01

...: CERTIFICATION AND OPERATIONS DRUG AND ALCOHOL TESTING PROGRAM Drug Testing Program Requirements § 120.113... provision of MRO services as part of its drug testing program. (b) Medical Review Officer (MRO). The MRO... working days after verifying a positive drug test result or refusal to submit to a test. (2) During the...

Assessing the Relationship between Airlines' Maintenance Outsourcing and Aviation Professionals' Job Satisfaction

NASA Astrophysics Data System (ADS)

McCamey, Rotorua

The current economic and security challenges placed an additional burden on U.S. airlines to provide optimum service at reasonable costs to the flying public. In efforts to stay competitive, U.S. airlines increased foreign-based outsourcing of aircraft major repair and overhaul (MRO) mainly to reduce labor costs and conserve capital. This concentrated focus on outsourcing and restructuring, ignored job dissatisfaction among remaining employees which could reduce and or eliminate an airline's competitiveness. The purpose of this quantitative study was (a) to assess the relationship between increased levels of foreign-based MRO outsourcing and aviation professionals' job satisfaction (Y1); (b) to assess the influence of increased levels of foreign-based outsourcing on MRO control (Y2), MRO error rate (Y3), and MRO technical punctuality (Y4) as perceived by aviation professionals; and (c) to assess the influence of increased levels of foreign-based MRO outsourcing on technical skills (Y5) and morale ( Y6) as perceived by aviation professionals. The survey instrument was utilized based on Paul Spector's Job Satisfaction Questionnaire and MRO specific questions. A random sample of 300 U.S. airline participants was requested via MarketTools to meet required sample size of 110 as determined through a priori power analysis. Study data rendered 198 useable surveys of 213 total responses, and correlation, multiple regression, and ANOVA methods were used to test study hypotheses. The Spearman's rho for (Y 1) was statistically significant, p = .010 and multiple regression was statistically significant, p < .001. A one-way ANOVA indicated participants differed in their opinions of (Y2) through (Y6), Recommendations for future research include contrasting domestic and global MRO providers, and examining global aircraft parts suppliers and aviation technical training.

49 CFR 40.127 - What are the MRO's functions in reviewing negative test results?

Code of Federal Regulations, 2013 CFR

2013-10-01

... 49 Transportation 1 2013-10-01 2013-10-01 false What are the MRO's functions in reviewing negative test results? 40.127 Section 40.127 Transportation Office of the Secretary of Transportation PROCEDURES FOR TRANSPORTATION WORKPLACE DRUG AND ALCOHOL TESTING PROGRAMS Medical Review Officers and the Verification Process § 40.127 What are the MRO's...

49 CFR 40.167 - How are MRO reports of drug results transmitted to the employer?

Code of Federal Regulations, 2011 CFR

2011-10-01

... 49 Transportation 1 2011-10-01 2011-10-01 false How are MRO reports of drug results transmitted to the employer? 40.167 Section 40.167 Transportation Office of the Secretary of Transportation PROCEDURES FOR TRANSPORTATION WORKPLACE DRUG AND ALCOHOL TESTING PROGRAMS Medical Review Officers and the Verification Process § 40.167 How are MRO reports...

49 CFR 40.165 - To whom does the MRO transmit reports of drug test results?

Code of Federal Regulations, 2013 CFR

2013-10-01

... 49 Transportation 1 2013-10-01 2013-10-01 false To whom does the MRO transmit reports of drug test results? 40.165 Section 40.165 Transportation Office of the Secretary of Transportation PROCEDURES FOR TRANSPORTATION WORKPLACE DRUG AND ALCOHOL TESTING PROGRAMS Medical Review Officers and the Verification Process § 40.165 To whom does the MRO...

49 CFR 40.165 - To whom does the MRO transmit reports of drug test results?

Code of Federal Regulations, 2011 CFR

2011-10-01

... 49 Transportation 1 2011-10-01 2011-10-01 false To whom does the MRO transmit reports of drug test results? 40.165 Section 40.165 Transportation Office of the Secretary of Transportation PROCEDURES FOR TRANSPORTATION WORKPLACE DRUG AND ALCOHOL TESTING PROGRAMS Medical Review Officers and the Verification Process § 40.165 To whom does the MRO...

A Complex Interplay among the Parent-Child Relationship, Effortful Control, and Internalized, Rule-Compatible Conduct in Young Children: Evidence from Two Studies

ERIC Educational Resources Information Center

Kochanska, Grazyna; Kim, Sanghag

2014-01-01

We propose a model linking the early parent-child mutually responsive orientation (MRO), children's temperament trait of effortful control, and their internalization of conduct rules. In a developmental chain, effortful control was posited as a mediator of the links between MRO and children's internalization. MRO was further posited as a moderator…

NESC Independent Review of the Mars Reconnaissance Orbiter (MRO) Contamination Thermal/Vacuum (T/V) Anomaly Technical Consultation Report

NASA Technical Reports Server (NTRS)

Sutter, James K.; Leidecker, Henning W.; Panda, Binayak; Piascik, Robert S.; Muirhead, Brian K.; Peeler, Debra

2009-01-01

The NESC eras requested by the NASA Jet Propulsion Laboratory (JPL) to conduct an independent review of the Mars Reconnaissance Orbiter (MRO) Thermal/Vacuum (T/V) Anomaly Assessment. Because the anomaly resulted in the surface contamination of the MRO, selected members of the Materials Super Problem Resolution Team (SPRT) and the NASA technical community having technical expertise relative to contamination issues were chosen for the independent review. The consultation consisted of a review of the MRO Project's reported response to the assessment findings, a detailed review of JPL technical assessment final report, and detailed discussions with the JPL assessment team relative to their findings.

49 CFR 40.159 - What does the MRO do when a drug test result is invalid?

Code of Federal Regulations, 2013 CFR

2013-10-01

... 49 Transportation 1 2013-10-01 2013-10-01 false What does the MRO do when a drug test result is invalid? 40.159 Section 40.159 Transportation Office of the Secretary of Transportation PROCEDURES FOR TRANSPORTATION WORKPLACE DRUG AND ALCOHOL TESTING PROGRAMS Medical Review Officers and the Verification Process § 40.159 What does the MRO do when a...

Seasonal and Static Gravity Field of Mars from MGS, Mars Odyssey and MRO Radio Science

NASA Technical Reports Server (NTRS)

Genova, Antonio; Goossens, Sander; Lemoine, Frank G.; Mazarico, Erwan; Neumann, Gregory A.; Smith, David E.; Zuber, Maria T.

2016-01-01

We present a spherical harmonic solution of the static gravity field of Mars to degree and order 120, GMM-3, that has been calculated using the Deep Space Network tracking data of the NASA Mars missions, Mars Global Surveyor (MGS), Mars Odyssey (ODY), and the Mars Reconnaissance Orbiter (MRO). We have also jointly determined spherical harmonic solutions for the static and time-variable gravity field of Mars, and the Mars k 2 Love numbers, exclusive of the gravity contribution of the atmosphere. Consequently, the retrieved time-varying gravity coefficients and the Love number k 2 solely yield seasonal variations in the mass of the polar caps and the solid tides of Mars, respectively. We obtain a Mars Love number k 2 of 0.1697 +/-0.0027 (3- sigma). The inclusion of MRO tracking data results in improved seasonal gravity field coefficients C 30 and, for the first time, C 50 . Refinements of the atmospheric model in our orbit determination program have allowed us to monitor the odd zonal harmonic C 30 for approx.1.5 solar cycles (16 years). This gravity model shows improved correlations with MOLA topography up to 15% larger at higher harmonics ( l = 60–80) than previous solutions.

Seasonal and static Gravity Field of Mars from MGS, Mars Odyssey and MRO Radio Science

NASA Technical Reports Server (NTRS)

Genova, Antonio; Goossens, Sander; Lemoine, Frank G.; Mazarico, Erwan; Neumann, Gregory A.; Smith, David E.; Zuber, Maria T.

2016-01-01

We present a spherical harmonic solution of the static gravity field of Mars to degree and order 120, GMM-3, that has been calculated using the Deep Space Network tracking data of the NASA Mars missions, Mars Global Surveyor (MGS), Mars Odyssey (ODY), and the Mars Reconnaissance Orbiter (MRO). We have also jointly determined spherical harmonic solutions for the static and time-variable gravity field of Mars, and the Mars k(sub 2) Love numbers, exclusive of the gravity contribution of the atmosphere. Consequently, the retrieved time-varying gravity coefficients and the Love number k(sub 2) solely yield seasonal variations in the mass of the polar caps and the solid tides of Mars, respectively. We obtain a Mars Love number k(sub 2) of 0.1697 +/- 0.0027 (3- sigma). The inclusion of MRO tracking data results in improved seasonal gravity field coefficients C(sub 30) and, for the first time, C 50. Refinements of the atmospheric model in our orbit determination program have allowed us to monitor the odd zonal harmonic C(sub 30) for approximately 1.5 solar cycles (16 years). This gravity model shows improved correlations with MOLA topography up to 15% larger at higher harmonics ( l = 60-80) than previous solutions.

49 CFR 40.161 - What does the MRO do when a drug test specimen is rejected for testing?

Code of Federal Regulations, 2011 CFR

2011-10-01

... negative test is required (e.g., in the case of a pre-employment, return-to-duty, or follow-up test). (c... 49 Transportation 1 2011-10-01 2011-10-01 false What does the MRO do when a drug test specimen is... Verification Process § 40.161 What does the MRO do when a drug test specimen is rejected for testing? As the...

49 CFR 40.161 - What does the MRO do when a drug test specimen is rejected for testing?

Code of Federal Regulations, 2010 CFR

2010-10-01

... negative test is required (e.g., in the case of a pre-employment, return-to-duty, or follow-up test). (c... 49 Transportation 1 2010-10-01 2010-10-01 false What does the MRO do when a drug test specimen is... Verification Process § 40.161 What does the MRO do when a drug test specimen is rejected for testing? As the...

49 CFR 40.161 - What does the MRO do when a drug test specimen is rejected for testing?

Code of Federal Regulations, 2012 CFR

2012-10-01

... negative test is required (e.g., in the case of a pre-employment, return-to-duty, or follow-up test). (c... 49 Transportation 1 2012-10-01 2012-10-01 false What does the MRO do when a drug test specimen is... Verification Process § 40.161 What does the MRO do when a drug test specimen is rejected for testing? As the...

49 CFR 40.161 - What does the MRO do when a drug test specimen is rejected for testing?

Code of Federal Regulations, 2014 CFR

2014-10-01

... negative test is required (e.g., in the case of a pre-employment, return-to-duty, or follow-up test). (c... 49 Transportation 1 2014-10-01 2014-10-01 false What does the MRO do when a drug test specimen is... Verification Process § 40.161 What does the MRO do when a drug test specimen is rejected for testing? As the...

49 CFR 40.161 - What does the MRO do when a drug test specimen is rejected for testing?

Code of Federal Regulations, 2013 CFR

2013-10-01

... negative test is required (e.g., in the case of a pre-employment, return-to-duty, or follow-up test). (c... 49 Transportation 1 2013-10-01 2013-10-01 false What does the MRO do when a drug test specimen is... Verification Process § 40.161 What does the MRO do when a drug test specimen is rejected for testing? As the...

KSC-05PD-1605

NASA Technical Reports Server (NTRS)

2005-01-01

KENNEDY SPACE CENTER, FLA. At the Atlas V Spaceflight Operations Center, the launch team goes through a wet dress rehearsal for launch of the Mars Reconnaissance Orbiter (MRO), scheduled for Aug. 10. Launch of the MRO aboard an Atlas V rocket will be from Launch Complex 41 at Cape Canaveral Air Force Station in Florida. A wet rehearsal includes pre-liftoff operations and a fueling of the rockets engine. The MRO was built by Lockheed Martin for NASA Jet Propulsion Laboratory in California. It is the next major step in Mars exploration and scheduled for launch from Cape Canaveral Air Force Station. The MRO is an important next step in fulfilling NASAs vision of space exploration and ultimately sending human explorers to Mars and beyond.

KSC-05PD-1606

NASA Technical Reports Server (NTRS)

2005-01-01

KENNEDY SPACE CENTER, FLA. At the Atlas V Spaceflight Operations Center, the launch team goes through a wet dress rehearsal for launch of the Mars Reconnaissance Orbiter (MRO), scheduled for Aug. 10. Launch of the MRO aboard an Atlas V rocket will be from Launch Complex 41 at Cape Canaveral Air Force Station in Florida. A wet rehearsal includes pre-liftoff operations and a fueling of the rockets engine. The MRO was built by Lockheed Martin for NASA Jet Propulsion Laboratory in California. It is the next major step in Mars exploration and scheduled for launch from Cape Canaveral Air Force Station. The MRO is an important next step in fulfilling NASAs vision of space exploration and ultimately sending human explorers to Mars and beyond.

KSC-05PD-1607

NASA Technical Reports Server (NTRS)

2005-01-01

KENNEDY SPACE CENTER, FLA. At the Atlas V Spaceflight Operations Center, the launch team goes through a wet dress rehearsal for launch of the Mars Reconnaissance Orbiter (MRO), scheduled for Aug. 10. At right, in the foreground, is NASAs Public Information Officer George Diller, who is commentator for launches of NASA payloads on expendable launch vehicles. Launch of the MRO aboard an Atlas V rocket will be from Launch Complex 41 at Cape Canaveral Air Force Station in Florida. A wet rehearsal includes pre-liftoff operations and fueling the rockets engine. The MRO was built by Lockheed Martin for NASA Jet Propulsion Laboratory in California. It is the next major step in Mars exploration and scheduled for launch from Cape Canaveral Air Force Station. The MRO is an important next step in fulfilling NASAs vision of space exploration and ultimately sending human explorers to Mars and beyond.

Relay Support for the Mars Science Laboratory Mission

NASA Technical Reports Server (NTRS)

Edwards, Charles D. Jr,; Bell, David J.; Gladden, Roy E.; Ilott, Peter A.; Jedrey, Thomas C.; Johnston, M. Daniel; Maxwell, Jennifer L.; Mendoza, Ricardo; McSmith, Gaylon W.; Potts, Christopher L.;

KSC-05PD-0820

NASA Technical Reports Server (NTRS)

2005-01-01

KENNEDY SPACE CENTER, FLA. At Kennedy Space Centers Shuttle Landing Facility, the second of two containers with the Mars Reconnaissance Orbiter (MRO) equipment is lifted onto a flatbed truck for transport to the Payload Hazardous Servicing Facility. The MRO was built by Lockheed-Martin for NASAs Jet Propulsion Laboratory in California. It is the next major step in Mars exploration and scheduled for launch from Cape Canaveral Air Force Station in a window opening Aug. 10. The MRO carries six primary instruments: the High Resolution Imaging Science Experiment, Context Camera, Mars Color Imager, Compact Reconnaissance Imaging Spectrometer for Mars, Mars Climate Sounder and Shallow Radar. By 2007, the MRO will begin a series of global mapping, regional survey and targeted observations from a near-polar, low-altitude Mars orbit. It will observe the atmosphere and surface of Mars while probing its shallow subsurface as part of a follow the water strategy.

KSC-05PD-1001

NASA Technical Reports Server (NTRS)

2005-01-01

KENNEDY SPACE CENTER, FLA. In the Payload Hazardous Servicing Facility at NASAs Kennedy Space Center, engineers move the gimbal closer to the Mars Reconnaissance Orbiter (MRO) in the background. The gimbal will be installed on the MRO solar panel. A gimbal is an appliance that allows an object to remain horizontal even as its support tips. In the PHSF, the spacecraft will undergo multiple mechanical assembly operations and electrical tests to verify its readiness for launch. A major deployment test will check out the spacecrafts large solar arrays. The MRO was built by Lockheed Martin for NASAs Jet Propulsion Laboratory in California. It is the next major step in Mars exploration and scheduled for launch from Cape Canaveral Air Force Station in a window opening Aug. 10. The MRO is an important next step in fulfilling NASAs vision of space exploration and ultimately sending human explorers to Mars and beyond.

KSC-05PD-1000

NASA Technical Reports Server (NTRS)

2005-01-01

KENNEDY SPACE CENTER, FLA. In the Payload Hazardous Servicing Facility at NASAs Kennedy Space Center, a worker guides the gimbal across the floor to the Mars Reconnaissance Orbiter (MRO) in the background. The gimbal will be installed on the MRO solar panel. A gimbal is an appliance that allows an object to remain horizontal even as its support tips. In the PHSF, the spacecraft will undergo multiple mechanical assembly operations and electrical tests to verify its readiness for launch. A major deployment test will check out the spacecrafts large solar arrays. The MRO was built by Lockheed Martin for NASAs Jet Propulsion Laboratory in California. It is the next major step in Mars exploration and scheduled for launch from Cape Canaveral Air Force Station in a window opening Aug. 10. The MRO is an important next step in fulfilling NASAs vision of space exploration and ultimately sending human explorers to Mars and beyond.

The impact of new and emerging technologies in the commercial aviation maintenance, repair, and overhaul industry a Delphi study

NASA Astrophysics Data System (ADS)

Gray, Janet

Purpose. The purpose of this study was to identify new or emerging technological trends and events that are likely to occur between now and 2017 that will have an impact on the commercial aviation maintenance, repair, and overhaul (MRO) industry. Further, it was the purpose of this study to examine those technological trends and events believed to provide the greatest impact and, given the experts' analysis, identify the feasibility of implementation. Methodology. This descriptive study utilized the Delphi method with a panel of twenty-four experts comprised of practitioners, theorists, and futurists. A priority matrix was utilized to determine the impact and feasibility of trend and events. Findings. The experts identified fifty-three trends and events that will impact the commercial aviation maintenance, repair, and overhaul (MRO) industry. Analysis of the priority matrix revealed eighteen trends and events were of high priority and high feasibility. Conclusions. The responses from the expert panel were examined and the findings analyzed. The following are the conclusions constructed from the data provided by the Delphi panel of experts: (1) the need to respond to the demands of the maintenance, repair, and overhaul (MRO) industry such as down time, efficiency, cost, and environmental concerns by implementing new technology, (2) the demand to integrate and implement new technology as indicative of the priority matrix scoring high importance/high feasibility, (3) to proactively address the inadequate professional development in new technologies, and (4) the consensus reached by the panel of experts of importance and feasibility of implementation of new technologies encompass eighteen trends and events. Implications and recommendations for action. The implementation of new and emerging technological advances in the commercial aviation maintenance, repair, and overhaul (MRO) industry between now and 2017 will be dependent on the technologies' capacity to reduce downtime and increase efficiency. In order to maintain America's global leadership in aviation, integration of innovated technology is key.

Magnificent Mars 10 Years of Mars Reconnaissance Orbiter

NASA Image and Video Library

2016-03-09

NASA's Mars Reconnaissance Orbiter has clocked more than a decade of service at the Red Planet and has yielded scientific discoveries and magnificent views of a distant world. Video uses spacecraft animation and stills set to music. These images taken by MRO's HiRISE camera are not in true color because they include infrared information in order to be optimized for geological science.

Mining the wealth of Phobos multispectral data contained in MEX-OMEGA and MRO-CRISM datasets

NASA Astrophysics Data System (ADS)

Pajola, Maurizio; Roush, Ted

2016-04-01

The origin of Phobos is still strongly debated between in situ versus asteroid capture formation scenarios. Growing interest in Phobos as a scientific destination is demonstrated by the multiple NASA-Discovery missions presented in 2015, the proposed ESA-M class mission PhoDEx, and JAXA's Mars Moon's sample return mission (MMX, Mars Moons eXploration). This large number of Phobos dedicated missions and JAXA's planned mission clearly illustrate the scientific interest in Phobos as a destination. We believe that there is still a wealth of data that can be mined in order to constrain Phobos' surface properties and possibly its origin. There are several multispectral Phobos datasets available on the NASA-Planetary Data System. In this work we focus on the first steps aimed to perform a new spectral analysis on the Mars satellite Phobos. We made use of the available Mars Express (MEX) OMEGA spectral cubes, obtained throughout the MEX mission, and Mars Reconnaissance Orbiter (MRO) CRISM hyperspectral data obtained during early MRO orbits around Mars. Previous analyses (Fraeman et al. 2012, 2014) mainly focus on three specific Regions of Interest, ROIs, located inside the so-called blue and red regions of Phobos, i.e. inside or close to Stickney crater (the biggest crater on Phobos, 8-km in diameter) and its eastern ejecta blanket. We extended this analysis by considering multiple ROIs located both in the leading and the trailing hemispheres of the satellite, taking advantage of the broader coverage of the OMEGA and CRISM data. This provides the possibility to detect spectral properties of intermediate areas located in the transition region between the blue and the red spectral unit. The analyses can enable i) documentation of how the spectral slope changes between these two units, ii) their boundaries and surface extent, and iii) identify additional surface materials, if present. This work paves the way to a more thorough analysis, foreseen in the near future, where the widest spectral wavelength range available (from near UV to far-IR) will be mined, returning a desirable complete picture of surface properties to enable planning for, and validation/confirmation by, future Phobos spacecraft. Acknowledgements: We make use of the public NASA-Planetary Data System MEX-OMEGA and MRO-CRISM spectral data of Phobos. M.P. was supported for this research by an appointment to the NASA Postdoctoral Program at the Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. References: Fraeman et al. 2012, J. Geophy. Res, E00J15, 10.1029/2012JE004137; Fraeman et al., 2014, Icarus, 229, 196-205, 10.1016/icarus.2013.11.021

A Vision for the MRO/HiRISE Operations Center: Getting the Data to the People

NASA Technical Reports Server (NTRS)

Eliason, E. M.; McEwen, A. S.; Delamere, W. A.; Grant, J. A.; Gulick, V. C.; Hansen, C. J.; Herkenhoff, K. E.; Keszthelyi, L.; Kirk, R. L.; Mellon, M. T.

2002-01-01

The MRO/HiRISE Operations Center provides a mechanism for Mars investigators to particaipate in selection of targets and access to the aquired images. Additional information is contained in the original extended abstract.

Quantitative real-time optical imaging of the tissue metabolic rate of oxygen consumption

NASA Astrophysics Data System (ADS)

Ghijsen, Michael; Lentsch, Griffin R.; Gioux, Sylvain; Brenner, Matthew; Durkin, Anthony J.; Choi, Bernard; Tromberg, Bruce J.

2018-03-01

The tissue metabolic rate of oxygen consumption (tMRO2) is a clinically relevant marker for a number of pathologies including cancer and arterial occlusive disease. We present and validate a noncontact method for quantitatively mapping tMRO2 over a wide, scalable field of view at 16 frames / s. We achieve this by developing a dual-wavelength, near-infrared coherent spatial frequency-domain imaging (cSFDI) system to calculate tissue optical properties (i.e., absorption, μa, and reduced scattering, μs‧, parameters) as well as the speckle flow index (SFI) at every pixel. Images of tissue oxy- and deoxyhemoglobin concentration ( [ HbO2 ] and [HHb]) are calculated from optical properties and combined with SFI to calculate tMRO2. We validate the system using a series of yeast-hemoglobin tissue-simulating phantoms and conduct in vivo tests in humans using arterial occlusions that demonstrate sensitivity to tissue metabolic oxygen debt and its repayment. Finally, we image the impact of cyanide exposure and toxicity reversal in an in vivo rabbit model showing clear instances of mitochondrial uncoupling and significantly diminished tMRO2. We conclude that dual-wavelength cSFDI provides rapid, quantitative, wide-field mapping of tMRO2 that can reveal unique spatial and temporal dynamics relevant to tissue pathology and viability.

Medium-range structure and glass forming ability in Zr–Cu–Al bulk metallic glasses

DOE PAGES

Zhang, Pei; Maldonis, Jason J.; Besser, M. F.; ...

2016-03-05

Fluctuation electron microscopy experiments combined with hybrid reverse Monte Carlo modeling show a correlation between medium-range structure at the nanometer scale and glass forming ability in two Zr–Cu–Al bulk metallic glass (BMG) alloys. Both Zr 50Cu 35Al 15 and Zr 50Cu 45Al 5 exhibit two nanoscale structure types, one icosahedral and the other more crystal-like. In Zr 50Cu 35Al 15, the poorer glass former, the crystal-like structure is more stable under annealing below the glass transition temperature, T g, than in Zr 50Cu 45Al 5. Variable resolution fluctuation microscopy of the MRO clusters show that in Zr 50Cu 35Al 15more » on sub-Tg annealing, the crystal-like clusters shrink even as they grow more ordered, while icosahedral-like clusters grow. Furthermore, the results suggest that achieving better glass forming ability in this alloy system may depend more on destabilizing crystal-like structures than enhancing non-crystalline structures.« less

Validation and Inter-Comparison of Limb Sounding Profiles from MRO/MCS and MGS/TES

NASA Astrophysics Data System (ADS)

Shirley, J. H.; McConnochie, T. M.; Kass, D. M.; Kleinböhl, A.; Schofield, J. T.; Heavens, N. G.; McCleese, D. J.; Benson, J.; Hinson, D. P.; Bandfield, J. L.

2014-07-01

Nighttime atmospheric temperatures in northern middle latitudes during Mars' aphelion season obtained by MGS/TES and MRO/MCS are compared with MGS radio science results. Profile mean Δ Ts of <= 2 K demonstrate consistency of retrieved temperatures.

The Gravity Field of Mars From MGS, Mars Odyssey, and MRO Radio Science

NASA Technical Reports Server (NTRS)

Genova, Antonio; Goossens, Sander; Lemoine, Frank G.; Mazarico, Erwan; Smith, David E.; Zuber, Maria T.

2015-01-01

The Mars Global Surveyor (MGS), Mars Odyssey (ODY), and Mars Reconnaissance Orbiter (MRO) missions have enabled NASA to conduct reconnaissance and exploration of Mars from orbit for sixteen consecutive years. These radio systems on these spacecraft enabled radio science in orbit around Mars to improve the knowledge of the static structure of the Martian gravitational field. The continuity of the radio tracking data, which cover more than a solar cycle, also provides useful information to characterize the temporal variability of the gravity field, relevant to the planet's internal dynamics and the structure and dynamics of the atmosphere [1]. MGS operated for more than 7 years, between 1999 and 2006, in a frozen sun-synchronous, near-circular, polar orbit with the periapsis at approximately 370 km altitude. ODY and MRO have been orbiting Mars in two separate sun-synchronous orbits at different local times and altitudes. ODY began its mapping phase in 2002 with the periapis at approximately 390 km altitude and 4-5pm Local Solar Time (LST), whereas the MRO science mission started in November 2006 with the periapis at approximately 255 km altitude and 3pm LST. The 16 years of radio tracking data provide useful information on the atmospheric density in the Martian upper atmosphere. We used ODY and MRO radio data to recover the long-term periodicity of the major atmospheric constituents -- CO2, O, and He -- at the orbit altitudes of these two spacecraft [2]. The improved atmospheric model provides a better prediction of the annual and semi-annual variability of the dominant species. Therefore, the inclusion of the recovered model leads to improved orbit determination and an improved gravity field model of Mars with MGS, ODY, and MRO radio tracking data.

Investigating the Department of Defense’s Implementation of Passive Radio Frequency Identification (RFID)

DTIC Science & Technology

2005-12-01

Logistics Support Activity MIT Massachusetts Institution of Technology MRE Meals -Ready-to-Eat MRO Material Release Order MSC Military Sealift... increase once item tagging becomes mandated. Reader, middleware, specialized hardware, and physical infrastructure costs can add up too. Reader’s...that system integration revenues could surpass hardware by 2007 (Asif & Mandviwalla, 2005, p. 26). (4) Training. Training is another challenge

MRO Context Camera (CTX) Investigation Primary Mission Results

NASA Astrophysics Data System (ADS)

Edgett, K. S.; Malin, M. C.; Science; Operations Teams, M.

2008-12-01

The Mars Reconnaissance Orbiter (MRO) Context Camera (CTX) acquires panchromatic images of Mars at ~6 m/pixel; the majority cover areas 30 km wide by 43 to 313 km long. As of 31 August 2008, 36% of Mars was imaged at 6 m/pixel and 10.8% was covered more than once. Areas imaged multiple times include stereopairs and locations covered repeatedly to monitor dust-raising events, seasonal frost patterns, or landforms and albedo features known or anticipated to change. CTX provides context for data acquired by other MRO science instruments, as well. Using our knowledge of imaging performance as a function of seasonal atmospheric, frost, and insolation conditions from the 4 Mars-year Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) investigation, we undertook several time-dependent campaigns to create 6 m/pixel mosaics of regions such as Hellas Planitia, the south polar residual cap (covered in spring and in summer), and the north polar region. In addition, we obtained 6 m/pixel mosaics of the Valles Marineris, Sinus Meridiani, Marte Valles, Athabasca Valles, portions of the northern plains, fretted terrain and chaotic terrain, large volcanoes, yardang-forming materials in Amazonis and Aeolis, the small volcanoes and platy flows south of Cerberus, and many other regions. We monitored thousands of mid-latitude gullies, and we used our MOC experience to target dust-raising events that repeat every year at the same locations. Retreat of cliffs formed in layers of CO2 ice in the south polar cap was observed for the 5th southern summer since 1999. Dozens of new impact craters and crater clusters were observed; all formed since 1999 and some formed during the MRO Primary Mission. We routinely re-targeted the new impact sites to see how they change and alert other MRO instrument teams so they could observe them. CTX images of the cratered highlands emphasize the view that the upper crust of Mars is layered with interbedded filled and buried valleys, fluvial channels, and impact craters ranging in diameter from meters to hundreds of kilometers. CTX observations reiterate a critical MOC result regarding small, sub-kilometer diameter craters: the substrates most resistant to erosion retain the most small craters (and the boulders produced by the impacts). CTX images provide many examples in which a younger, harder substrate (e.g., a lava flow) is more heavily cratered (with < 1 km diameter craters) than subjacent, older rock units. One example occurs in the form of lava flows located immediately west of Meridiani Planum; similar flows underlie the hematite-bearing, plains- forming rock in nearby Miyamoto Crater. Northern Meridiani also exhibits exhumed, low-order streams (of the scale of hillslope rills and creeks); these were filled, buried, lithified, and later returned to the surface by erosion-some of them in inverted form. Terrain immediately west of Juventae Chasma exhibits similar inverted streams and rills that were first documented by MOC and provide key evidence for rainfall and hillslope runoff. CTX data show that there are many hundreds of inverted fluvial channels, of a variety of sizes, all over the planet, especially in Arabia Terra, Solis Planum, and Thaumasia. We also used CTX to map a small, unnamed outflow channel system west of Bond Crater, and we have been documenting all of the small Martian volcanoes, typically < 30 km across, including those occurring in the Labyrinthus Noctis. CTX data are widely available, as they are archived with the NASA Planetary Data System on a rolling basis every 6 months.

Mars Reconnaissance Orbiter Navigation Strategy for the Comet Siding Spring Encounter

NASA Technical Reports Server (NTRS)

Menon, Premkumar R.; Wagner, Sean V.; Martin-Mur, Tomas J.; Jefferson, David C.; Ardalan, Shadan M.; Chung, Min-Kun J.; Lee, Kyong J.; Schulze, William B.

2015-01-01

Comet Siding Spring encountered Mars on October 19, 2014 at a distance of about 140,500 km - the nearest comet flyby of a planet in recorded history. Mars Reconnaissance Orbiter (MRO) was able to detect the comet, gather science data, and capture images of the comet as it approached Mars. To help protect MRO from the incoming comet particles, two propulsive maneuvers were performed to position the spacecraft behind Mars at the arrival time of the expected peak particle fluency. This paper documents the strategy that the MRO Navigation Team executed to mitigate risk from the comet particles while allowing scientific observations of the comet flyby.

46 CFR 16.203 - Employer, MRO, and SAP responsibilities.

Code of Federal Regulations, 2010 CFR

2010-10-01

... and among employers and service agents concerning the implementation of DOT drug testing requirements... DOT agency drug testing regulations. Compliance with these provisions is a material term of all such... CHEMICAL TESTING Required Chemical Testing § 16.203 Employer, MRO, and SAP responsibilities. (a) Employers...

46 CFR 16.203 - Employer, MRO, and SAP responsibilities.

Code of Federal Regulations, 2011 CFR

2011-10-01

... and among employers and service agents concerning the implementation of DOT drug testing requirements... DOT agency drug testing regulations. Compliance with these provisions is a material term of all such... CHEMICAL TESTING Required Chemical Testing § 16.203 Employer, MRO, and SAP responsibilities. (a) Employers...

46 CFR 16.203 - Employer, MRO, and SAP responsibilities.

Code of Federal Regulations, 2014 CFR

2014-10-01

... and among employers and service agents concerning the implementation of DOT drug testing requirements... DOT agency drug testing regulations. Compliance with these provisions is a material term of all such... CHEMICAL TESTING Required Chemical Testing § 16.203 Employer, MRO, and SAP responsibilities. (a) Employers...

46 CFR 16.203 - Employer, MRO, and SAP responsibilities.

Code of Federal Regulations, 2012 CFR

2012-10-01

... and among employers and service agents concerning the implementation of DOT drug testing requirements... DOT agency drug testing regulations. Compliance with these provisions is a material term of all such... CHEMICAL TESTING Required Chemical Testing § 16.203 Employer, MRO, and SAP responsibilities. (a) Employers...

46 CFR 16.203 - Employer, MRO, and SAP responsibilities.

Code of Federal Regulations, 2013 CFR

2013-10-01

... and among employers and service agents concerning the implementation of DOT drug testing requirements... DOT agency drug testing regulations. Compliance with these provisions is a material term of all such... CHEMICAL TESTING Required Chemical Testing § 16.203 Employer, MRO, and SAP responsibilities. (a) Employers...

Planetary protection implementation on Mars Reconnaissance Orbiter mission

NASA Astrophysics Data System (ADS)

Barengoltz, J.; Witte, J.

2008-09-01

In August 2005 NASA launched a large orbiting science observatory, the Mars Reconnaissance Orbiter (MRO), for what is scheduled to be a 5.4-year mission. High resolution imaging of the surface is a principal goal of the mission. One consequence of this goal however is the need for a low science orbit. Unfortunately this orbit fails the required 20-year orbit life set in NASA Planetary Protection (PP) requirements [NASA. Planetary protection provisions for robotic extraterrestrial missions, NASA procedural requirements NPR 8020.12C, NASA HQ, Washington, DC, April 2005.]. So rather than sacrifice the science goals of the mission by raising the science orbit, the MRO Project chose to be the first orbiter to pursue the bio-burden reduction approach. Cleaning alone for a large orbiter like MRO is insufficient to achieve the bio-burden threshold requirement in NASA PP requirements. The burden requirement for an orbiter includes spores encapsulated in non-metallic materials and trapped in joints, as well as located on all internal and external surfaces (the total spore burden). Total burden estimates are dominated by the mated and encapsulated burden. The encapsulated burden cannot be cleaned. The total burden of a smaller orbiter (e.g., Mars Odyssey) likely could not have met the requirement by cleaning; for the large MRO it is clearly impossible. Of course, a system-level partial sterilization, with its attendant costs and system design issues, could have been employed. In the approach taken by the MRO Project, hardware which will burn up (completely vaporize or ablate) before reaching the surface or will at least attain high temperature (500 °C for 0.5 s or more) due to entry heating was exempt from burden accounting. Thus the bio-burden estimate was reduced. Lockheed Martin engineers developed a process to perform what is called breakup and burn-up (B&B) analysis.Lockheed Martin Corporation.2 The use of the B&B analysis to comply with the spore burden requirement is the main subject of this article. However, several components aboard the orbiter were predicted to fail the minimum time at temperature requirements (or could not conservatively be shown to meet the conditions). An implementation plan was generated to address the highest contributors to the bio-burden assessment that fail to meet the requirements. The spore burden for these components was estimated by direct and proxy burden assays, NASA PP specifications, and dry heat microbial reduction, as appropriate. Items on the orbiter that required rework during assembly were also individually assessed. MRO met the spore burden requirement based on the B&B analysis, the MRO Planetary Protection Implementation Plan, and verification by the NASA Planetary Protection Officer’s (PPO) independent assays. The compliance was documented in the MRO PP Pre-Launch Report. MRO was approved for flight by the NASA PPO.

Improving Warehouse Inventory Management Through Rfid, Barcoding and Robotics Technologies

DTIC Science & Technology

2014-12-01

as a spider merge. This was designed and installed to speed up the conveyors . In their original design , conveyors traveled throughout the warehouse...lifts LCL lower confidence level xiv MRO material release order NPV net present value PMT positive material transfer POM Program Objective...depots. Active Radio Frequency Identification (aRFID ) Migration A program designed to move the active RFID enterprise from a proprietarily air interface

KSC-05PD-1782

NASA Technical Reports Server (NTRS)

2005-01-01

KENNEDY SPACE CENTER, FLA. Workers in the Payload Hazardous Servicing Facility maneuver the second half of the fairing toward the Mars Reconnaissance Orbiter (right) for installation. The fairing protects the spacecraft during launch and flight through the atmosphere. Once in space, it is jettisoned. Launch of the MRO aboard an Atlas V rocket will be from Launch Complex 41 at Cape Canaveral Air Force Station in Florida. The MRO is the next major step in Mars exploration and scheduled for launch from Cape Canaveral Air Force Station in a window opening Aug. 10. The MRO is an important next step in fulfilling NASAs vision of space exploration and ultimately sending human explorers to Mars and beyond.

KSC-05PD-1783

NASA Technical Reports Server (NTRS)

2005-01-01

KENNEDY SPACE CENTER, FLA. Workers in the Payload Hazardous Servicing Facility stand by as the first half of the fairing (left) is moved closer to the Mars Reconnaissance Orbiter (right) for installation. The fairing protects the spacecraft during launch and flight through the atmosphere. Once in space, it is jettisoned. Launch of the MRO aboard an Atlas V rocket will be from Launch Complex 41 at Cape Canaveral Air Force Station in Florida. The MRO is the next major step in Mars exploration and scheduled for launch from Cape Canaveral Air Force Station in a window opening Aug. 10. The MRO is an important next step in fulfilling NASAs vision of space exploration and ultimately sending human explorers to Mars and beyond.

49 CFR 40.163 - How does the MRO report drug test results?

Code of Federal Regulations, 2010 CFR

2010-10-01

..., the MRO may report negative results using an electronic data file. (1) If you report negatives using an electronic data file, the report must contain, as a minimum, the information specified in... contain your name, address, and phone number, the name of any person other than you reporting the results...

49 CFR 40.101 - What relationship may a laboratory have with an MRO?

Code of Federal Regulations, 2013 CFR

2013-10-01

... 49 Transportation 1 2013-10-01 2013-10-01 false What relationship may a laboratory have with an MRO? 40.101 Section 40.101 Transportation Office of the Secretary of Transportation PROCEDURES FOR TRANSPORTATION WORKPLACE DRUG AND ALCOHOL TESTING PROGRAMS Drug Testing Laboratories § 40.101 What relationship...

49 CFR 40.101 - What relationship may a laboratory have with an MRO?

Code of Federal Regulations, 2010 CFR

2010-10-01

... 49 Transportation 1 2010-10-01 2010-10-01 false What relationship may a laboratory have with an MRO? 40.101 Section 40.101 Transportation Office of the Secretary of Transportation PROCEDURES FOR TRANSPORTATION WORKPLACE DRUG AND ALCOHOL TESTING PROGRAMS Drug Testing Laboratories § 40.101 What relationship...

49 CFR 40.101 - What relationship may a laboratory have with an MRO?

Code of Federal Regulations, 2014 CFR

2014-10-01

... 49 Transportation 1 2014-10-01 2014-10-01 false What relationship may a laboratory have with an MRO? 40.101 Section 40.101 Transportation Office of the Secretary of Transportation PROCEDURES FOR TRANSPORTATION WORKPLACE DRUG AND ALCOHOL TESTING PROGRAMS Drug Testing Laboratories § 40.101 What relationship...

49 CFR 40.101 - What relationship may a laboratory have with an MRO?

Code of Federal Regulations, 2012 CFR

2012-10-01

... 49 Transportation 1 2012-10-01 2012-10-01 false What relationship may a laboratory have with an MRO? 40.101 Section 40.101 Transportation Office of the Secretary of Transportation PROCEDURES FOR TRANSPORTATION WORKPLACE DRUG AND ALCOHOL TESTING PROGRAMS Drug Testing Laboratories § 40.101 What relationship...

49 CFR 40.101 - What relationship may a laboratory have with an MRO?

Code of Federal Regulations, 2011 CFR

2011-10-01

... 49 Transportation 1 2011-10-01 2011-10-01 false What relationship may a laboratory have with an MRO? 40.101 Section 40.101 Transportation Office of the Secretary of Transportation PROCEDURES FOR TRANSPORTATION WORKPLACE DRUG AND ALCOHOL TESTING PROGRAMS Drug Testing Laboratories § 40.101 What relationship...

Mars Reconnaissance Orbiter Mission: Systems Engineering Challenges on the Mars Reconnaissance Orbiter Mission

NASA Technical Reports Server (NTRS)

Havens, Glen G.

2007-01-01

MRO project is a system of systems requiring system engineering team to architect, design, integrate, test, and operate these systems at each level of the project. The challenge of system engineering mission objectives into a single mission architecture that can be integrated tested, launched, and operated. Systems engineering must translate high-level requirements into integrated mission design. Systems engineering challenges were overcome utilizing a combination by creative designs built into MRO's flight and ground systems: a) Design of sophisticated spacecraft targeting and data management capabilities b) Establishment of a strong operations team organization; c) Implementation of robust operational processes; and d) Development of strategic ground tools. The MRO system has met the challenge of its driving requirements: a) MRO began its two-year primary science phase on November 7, 2006, and by July 2007, met it minimum requirement to collect 15 Tbits of data after only eight months of operations. Currently we have collected 22 Tbits. b) Based on current performance, mission data return could return 70 Tbits of data by the end of the primary science phase in 2008.

Design and Test of an Instrument for Measuring Microthermal Seeing on the Magdalena Ridge

NASA Astrophysics Data System (ADS)

Jorgensen, A. M.; Klinglesmith, D. A., III; Speights, J.; Clements, A.; Patel, J.

2009-05-01

We have constructed and operated an automated instrument for measuring ground-level microthermal seeing at the Magdalena Ridge Observatory (MRO). The MRO is located at an altitude of 10500' in the Cibola National Forest in New Mexico, USA. It is the planned site for the MRO Optical Interferometer (MROI) planned for up to 10 collecting elements, each with a diameter of 1.4 m, and baselines eventually up to approximately 400 m. As part of the preparation for construction we deployed a system to characterize the ground-level seeing across the observatory site. The instrument is built largely of off-the-shelf components, with only the sensor head and power supply requiring electronic board assembly. Even in those cases the board architecture is very simple. The first proof-of-concept system was deployed for several weeks in the autumn of 2004, and has since undergone several iterations. The latest configuration operates entirely off batteries, incorporates wireless data acquisition, and is thus able to operate in an area with no shelter, power, or communications. In this paper we present the design of the instrument, and show initial data. The microthermal tower has four sensor pairs at heights from 0.8 to 4.41 m, significantly lower than other microthermal experiments, because of the need to characterize the seeing near the ground. We find significant variation in the contribution of this range of heights to the seeing, contributing up to 0farcs3 of the seeing at some times and only 0farcs02 at other times. The individual sensor power spectra have a slope in the range of 1.4--1.5, which is lower than the 1.67 slope predicted by Kolmogorov turbulence theory. We measure the well known effect of improved seeing immediately around sunset. While we find significant variation in the microthermal seeing, we did not find a pattern of corresponding variations in weather conditions, suggesting that a complicated set of factors control microthermal turbulence.

49 CFR 40.21 - May an employer stand down an employee before the MRO has completed the verification process?

Code of Federal Regulations, 2011 CFR

2011-10-01

... positive, adulterated, or substituted by the MRO; (iii) Information about the work situation of the... which the employees work, the process through which employees will be informed of the stand-down... employee suffers no adverse personnel or financial consequences as a result; and (C) You maintain no...

49 CFR 40.135 - What does the MRO tell the employee at the beginning of the verification interview?

Code of Federal Regulations, 2010 CFR

2010-10-01

... beginning of the verification interview? 40.135 Section 40.135 Transportation Office of the Secretary of... verification interview? (a) As the MRO, you must tell the employee that the laboratory has determined that the... finding of adulteration or substitution. (b) You must explain the verification interview process to the...

49 CFR 40.145 - On what basis does the MRO verify test results involving adulteration or substitution?

Code of Federal Regulations, 2011 CFR

2011-10-01

...), except as otherwise provided in this section. (c) In the verification interview, you must explain the laboratory findings to the employee and address technical questions or issues the employee may raise. (d) You... at the time of the verification interview. As the MRO, you have discretion to extend the time...

49 CFR 40.145 - On what basis does the MRO verify test results involving adulteration or substitution?

Code of Federal Regulations, 2010 CFR

2010-10-01

...), except as otherwise provided in this section. (c) In the verification interview, you must explain the laboratory findings to the employee and address technical questions or issues the employee may raise. (d) You... at the time of the verification interview. As the MRO, you have discretion to extend the time...

Analysis of Employability for the Civil Aviation Maintenance Graduates of Turkey

ERIC Educational Resources Information Center

Denizhan, Berrin; Dogru, Alperen

2017-01-01

Purpose: With every passing day, the center of gravity for air traffic for the Middle East and Turkey is shifting toward becoming a center for airway transport, maintenance, repair, overhaul (MRO) and transfer. The MRO sector is gaining importance because of this increase in Turkey. The purpose of this study is to examine the future employability…

49 CFR 40.137 - On what basis does the MRO verify test results involving marijuana, cocaine, amphetamines, or PCP?

Code of Federal Regulations, 2012 CFR

2012-10-01

... involving marijuana, cocaine, amphetamines, or PCP? 40.137 Section 40.137 Transportation Office of the... results involving marijuana, cocaine, amphetamines, or PCP? (a) As the MRO, you must verify a confirmed positive test result for marijuana, cocaine, amphetamines, and/or PCP unless the employee presents a...

49 CFR 40.137 - On what basis does the MRO verify test results involving marijuana, cocaine, amphetamines, or PCP?

Code of Federal Regulations, 2010 CFR

2010-10-01

... involving marijuana, cocaine, amphetamines, or PCP? 40.137 Section 40.137 Transportation Office of the... results involving marijuana, cocaine, amphetamines, or PCP? (a) As the MRO, you must verify a confirmed positive test result for marijuana, cocaine, amphetamines, and/or PCP unless the employee presents a...

49 CFR 40.137 - On what basis does the MRO verify test results involving marijuana, cocaine, amphetamines, or PCP?

Code of Federal Regulations, 2011 CFR

2011-10-01

... involving marijuana, cocaine, amphetamines, or PCP? 40.137 Section 40.137 Transportation Office of the... results involving marijuana, cocaine, amphetamines, or PCP? (a) As the MRO, you must verify a confirmed positive test result for marijuana, cocaine, amphetamines, and/or PCP unless the employee presents a...

49 CFR 40.137 - On what basis does the MRO verify test results involving marijuana, cocaine, amphetamines, or PCP?

Code of Federal Regulations, 2013 CFR

2013-10-01

... involving marijuana, cocaine, amphetamines, or PCP? 40.137 Section 40.137 Transportation Office of the... results involving marijuana, cocaine, amphetamines, or PCP? (a) As the MRO, you must verify a confirmed positive test result for marijuana, cocaine, amphetamines, and/or PCP unless the employee presents a...

49 CFR 40.137 - On what basis does the MRO verify test results involving marijuana, cocaine, amphetamines, or PCP?

Code of Federal Regulations, 2014 CFR

2014-10-01

... involving marijuana, cocaine, amphetamines, or PCP? 40.137 Section 40.137 Transportation Office of the... results involving marijuana, cocaine, amphetamines, or PCP? (a) As the MRO, you must verify a confirmed positive test result for marijuana, cocaine, amphetamines, and/or PCP unless the employee presents a...

KSC-05PD-1072

NASA Technical Reports Server (NTRS)

2005-01-01

KENNEDY SPACE CENTER, FLA. In the Payload Hazardous Servicing Facility, technicians inspect the solar panels for the Mars Reconnaissance Orbiter (MRO) during an electromagnetic interference verification test. If no interference is found during the test, the Shallow Radar Antenna (SHARAD) will be installed on the spacecraft. The spacecraft is undergoing multiple mechanical assembly operations and electrical tests to verify its readiness for launch. The MRO was built by Lockheed Martin for NASAs Jet Propulsion Laboratory in California. It is the next major step in Mars exploration and scheduled for launch from Launch Complex 41 at Cape Canaveral Air Force Station in a window opening Aug. 10. The MRO is an important next step in fulfilling NASAs vision of space exploration and ultimately sending human explorers to Mars and beyond.

KSC-05PD-1784

NASA Technical Reports Server (NTRS)

2005-01-01

KENNEDY SPACE CENTER, FLA. Workers in the Payload Hazardous Servicing Facility make adjustments as they get ready to move the second half of the fairing (right) and install it with the first half around the Mars Reconnaissance Orbiter. The fairing protects the spacecraft during launch and flight through the atmosphere. Once in space, it is jettisoned. Launch of the MRO aboard an Atlas V rocket will be from Launch Complex 41 at Cape Canaveral Air Force Station in Florida. The MRO is the next major step in Mars exploration and scheduled for launch from Cape Canaveral Air Force Station in a window opening Aug. 10. The MRO is an important next step in fulfilling NASAs vision of space exploration and ultimately sending human explorers to Mars and beyond.

49 CFR 40.129 - What are the MRO's functions in reviewing laboratory confirmed non-negative drug test results?

Code of Federal Regulations, 2013 CFR

2013-10-01

... 49 Transportation 1 2013-10-01 2013-10-01 false What are the MRO's functions in reviewing laboratory confirmed non-negative drug test results? 40.129 Section 40.129 Transportation Office of the Secretary of Transportation PROCEDURES FOR TRANSPORTATION WORKPLACE DRUG AND ALCOHOL TESTING PROGRAMS Medical Review Officers and the Verification Proces...

49 CFR 40.145 - On what basis does the MRO verify test results involving adulteration or substitution?

Code of Federal Regulations, 2013 CFR

2013-10-01

... 49 Transportation 1 2013-10-01 2013-10-01 false On what basis does the MRO verify test results involving adulteration or substitution? 40.145 Section 40.145 Transportation Office of the Secretary of Transportation PROCEDURES FOR TRANSPORTATION WORKPLACE DRUG AND ALCOHOL TESTING PROGRAMS Medical Review Officers and the Verification Process §...

49 CFR 40.97 - What do laboratories report and how do they report it?

Code of Federal Regulations, 2011 CFR

2011-10-01

... review by the certifying scientist is completed. (e)(1) You must provide quantitative values for..., without a request from the MRO. (f) You must provide quantitative values for confirmed opiate results for morphine or codeine at 15,000 ng/mL or above, even if the MRO has not requested quantitative values for the...

49 CFR 40.97 - What do laboratories report and how do they report it?

Code of Federal Regulations, 2012 CFR

2012-10-01

... review by the certifying scientist is completed. (e)(1) You must provide quantitative values for..., without a request from the MRO. (f) You must provide quantitative values for confirmed opiate results for morphine or codeine at 15,000 ng/mL or above, even if the MRO has not requested quantitative values for the...

49 CFR 40.97 - What do laboratories report and how do they report it?

Code of Federal Regulations, 2013 CFR

2013-10-01

... review by the certifying scientist is completed. (e)(1) You must provide quantitative values for..., without a request from the MRO. (f) You must provide quantitative values for confirmed opiate results for morphine or codeine at 15,000 ng/mL or above, even if the MRO has not requested quantitative values for the...

49 CFR 40.97 - What do laboratories report and how do they report it?

Code of Federal Regulations, 2010 CFR

2010-10-01

... review by the certifying scientist is completed. (1) You must provide quantitative values for confirmed..., without a request from the MRO. (f) You must provide quantitative values for confirmed opiate results for morphine or codeine at 15,000 ng/mL or above, even if the MRO has not requested quantitative values for the...

49 CFR 40.97 - What do laboratories report and how do they report it?

Code of Federal Regulations, 2014 CFR

2014-10-01

... review by the certifying scientist is completed. (e)(1) You must provide quantitative values for..., without a request from the MRO. (f) You must provide quantitative values for confirmed opiate results for morphine or codeine at 15,000 ng/mL or above, even if the MRO has not requested quantitative values for the...

Using RFID Tagging in a Mining Industry Maintenance, Repair, and Operating (MRO) Supply Warehouse: A Case Study

ERIC Educational Resources Information Center

Smith, George D.

2008-01-01

The use of Radio Frequency Identification (RFID) technology has been shown to be successful by reducing operating costs in the retail and manufacturing industries, but has never been considered in the literature for a mining industry maintenance, repair, and operating (MRO) supply chain. This field study was conducted to determine whether or not…

49 CFR 40.327 - When must the MRO report medical information gathered in the verification process?

Code of Federal Regulations, 2011 CFR

2011-10-01

... 49 Transportation 1 2011-10-01 2011-10-01 false When must the MRO report medical information gathered in the verification process? 40.327 Section 40.327 Transportation Office of the Secretary of Transportation PROCEDURES FOR TRANSPORTATION WORKPLACE DRUG AND ALCOHOL TESTING PROGRAMS Confidentiality and Release of Information § 40.327 When must...

Child Temperament Moderates Effects of Parent-Child Mutuality on Self-Regulation: A Relationship-Based Path for Emotionally Negative Infants

ERIC Educational Resources Information Center

Kim, Sanghag; Kochanska, Grazyna

2012-01-01

This study examined infants' negative emotionality as moderating the effect of parent-child mutually responsive orientation (MRO) on children's self-regulation (n = 102). Negative emotionality was observed in anger-eliciting episodes and in interactions with parents at 7 months. MRO was coded in naturalistic interactions at 15 months.…

KSC-05PD-1003

NASA Technical Reports Server (NTRS)

2005-01-01

KENNEDY SPACE CENTER, FLA. In the Payload Hazardous Servicing Facility at NASAs Kennedy Space Center, engineers finish installing the gimbal on the Mars Reconnaissance Orbiter (MRO) solar panel. A gimbal is an appliance that allows an object to remain horizontal even as its support tips. In the PHSF, the spacecraft will undergo multiple mechanical assembly operations and electrical tests to verify its readiness for launch. A major deployment test will check out the spacecrafts large solar arrays. The MRO was built by Lockheed Martin for NASAs Jet Propulsion Laboratory in California. It is the next major step in Mars exploration and scheduled for launch from Cape Canaveral Air Force Station in a window opening Aug. 10. The MRO is an important next step in fulfilling NASAs vision of space exploration and ultimately sending human explorers to Mars and beyond.

KSC-05PD-1004

NASA Technical Reports Server (NTRS)

2005-01-01

KENNEDY SPACE CENTER, FLA. The Mars Reconnaissance Orbiter (MRO) spacecraft waits for installation of a second gimbal on its solar panel. A gimbal is an appliance that allows an object to remain horizontal even as its support tips. In the PHSF, the spacecraft will undergo multiple mechanical assembly operations and electrical tests to verify its readiness for launch. A major deployment test will check out the spacecrafts large solar arrays. The MRO was built by Lockheed Martin for NASAs Jet Propulsion Laboratory in California. It is the next major step in Mars exploration and scheduled for launch from Cape Canaveral Air Force Station in a window opening Aug. 10. The MRO is an important next step in fulfilling NASAs vision of space exploration and ultimately sending human explorers to Mars and beyond.

KSC-05PD-1002

NASA Technical Reports Server (NTRS)

2005-01-01

KENNEDY SPACE CENTER, FLA. In the Payload Hazardous Servicing Facility at NASAs Kennedy Space Center, engineers begin installing the gimbal on the Mars Reconnaissance Orbiter (MRO) solar panel. A gimbal is an appliance that allows an object to remain horizontal even as its support tips. In the PHSF, the spacecraft will undergo multiple mechanical assembly operations and electrical tests to verify its readiness for launch. A major deployment test will check out the spacecrafts large solar arrays. The MRO was built by Lockheed Martin for NASAs Jet Propulsion Laboratory in California. It is the next major step in Mars exploration and scheduled for launch from Cape Canaveral Air Force Station in a window opening Aug. 10. The MRO is an important next step in fulfilling NASAs vision of space exploration and ultimately sending human explorers to Mars and beyond.

KSC-05PD-1073

NASA Technical Reports Server (NTRS)

2005-01-01

KENNEDY SPACE CENTER, FLA. In the Payload Hazardous Servicing Facility, an electromagnetic interference verification test is being conducted on the solar arrays for the Mars Reconnaissance Orbiter (MRO) and an antenna simulator (yellow horizontal rod). If no interference is found during the test, the Shallow Radar Antenna (SHARAD) will be installed on the spacecraft. The spacecraft is undergoing multiple mechanical assembly operations and electrical tests to verify its readiness for launch. The MRO was built by Lockheed Martin for NASAs Jet Propulsion Laboratory in California. It is the next major step in Mars exploration and scheduled for launch from Launch Complex 41 at Cape Canaveral Air Force Station in a window opening Aug. 10. The MRO is an important next step in fulfilling NASAs vision of space exploration and ultimately sending human explorers to Mars and beyond.

Thermal kinetics and short range order parameters of Se80X20 (X = Te, Sb) binary glasses

NASA Astrophysics Data System (ADS)

Moharram, A. H.; Abu El-Oyoun, M.; Abdel-Baset, A. M.

2014-06-01

Bulk Se80Te20 and Se80Sb20 glasses were prepared using the melt-quench technique. Differential scanning calorimetry (DSC) curves measured at different heating rates (5 K/min≤ α≤50 K/min) and X-ray diffraction (XRD) are used to characterize the as-quenched specimens. Based on the obtained results, the activation energy of glass transition and the activation energy of crystallization ( E g, E c) of the Se80Te20 glass are (137.5, 105.1 kJ/mol) higher than the corresponding values of the Se80Sb20 glass (106.8, 71.2 kJ/mol). An integer n value ( n=2) of the Se80Te20 glass indicates that only one crystallization mechanism is occurring while a non-integer exponent ( n=1.79) in the Se80Sb20 glass means that two mechanisms are working simultaneously during the amorphous-crystalline transformations. The total structure factor, S( K), indicates the presence of the short-range order (SRO) and the absence of the medium-range order (MRO) inside the as-quenched alloys. In an opposite way to the activation energies, the values of the first peak position and the total coordination number ( r 1, η 1), obtained from a Gaussian fit of the radial distribution function, of the Se80Te20 glass are (2.42 nm, 1.99 atom) lower than the corresponding values (2.55 nm, 2.36 atom) of the Se80Sb20 specimens.

49 CFR 40.159 - What does the MRO do when a drug test result is invalid?

Code of Federal Regulations, 2010 CFR

2010-10-01

....160 for determining if there is clinical evidence that the individual is an illicit drug user. (5) If... is clinical evidence that the individual is an illicit drug user. (5) If the recollection was not... 49 Transportation 1 2010-10-01 2010-10-01 false What does the MRO do when a drug test result is...

Innovative Techniques to Predict Atmospheric Effects on Sensor Performance

DTIC Science & Technology

2009-10-15

since acquiring the MRO data, extensive tabulation of all of the data from all visible satellites (generally, non- resolved ) was also accomplished...efficient code has been written to run multiple OSC simulations in less time . Data from many passes of the same satellite is useful for SOI, whether it is...the data analyzed. Questions about the data were resolved using OSC to determine solar phase angle (SPA), range, time of penumbra entrance/exit and

Converting from DDOR SASF to APF

NASA Technical Reports Server (NTRS)

Gladden, Roy E.; Khanampompan, Teerapat; Fisher, Forest W.

2008-01-01

A computer program called ddor_sasf2apf converts delta-door (delta differential one-way range) request from an SASF (spacecraft activity sequence file) format to an APF (apgen plan file) format for use in the Mars Reconnaissance Orbiter (MRO) missionplanning- and-sequencing process. The APF is used as an input to APGEN/AUTOGEN in the MRO activity- planning and command-sequencegenerating process to sequence the delta-door (DDOR) activity. The DDOR activity is a spacecraft tracking technique for determining spacecraft location. The input to ddor_sasf2apf is an input request SASF provided by an observation team that utilizes DDOR. ddor_sasf2apf parses this DDOR SASF input, rearranging parameters and reformatting the request to produce an APF file for use in AUTOGEN and/or APGEN. The benefit afforded by ddor_sasf2apf is to enable the use of the DDOR SASF file earlier in the planning stage of the command-sequence-generating process and to produce sequences, optimized for DDOR operations, that are more accurate and more robust than would otherwise be possible.

KSC-05PD-1006

NASA Technical Reports Server (NTRS)

2005-01-01

KENNEDY SPACE CENTER, FLA. In the Payload Hazardous Servicing Facility at NASAs Kennedy Space Center, an engineer installs a second gimbal on a Mars Reconnaissance Orbiter (MRO) solar panel. A gimbal is an appliance that allows an object to remain horizontal even as its support tips. In the PHSF, the spacecraft will undergo multiple mechanical assembly operations and electrical tests to verify its readiness for launch. A major deployment test will check out the spacecrafts large solar arrays. The MRO was built by Lockheed Martin for NASAs Jet Propulsion Laboratory in California. It is the next major step in Mars exploration and scheduled for launch from Cape Canaveral Air Force Station in a window opening Aug. 10. The MRO is an important next step in fulfilling NASAs vision of space exploration and ultimately sending human explorers to Mars and beyond.

KSC-05PD-1005

NASA Technical Reports Server (NTRS)

2005-01-01

KENNEDY SPACE CENTER, FLA. In the Payload Hazardous Servicing Facility at NASAs Kennedy Space Center, engineers prepare a second gimbal for installation on a Mars Reconnaissance Orbiter (MRO) solar panel. A gimbal is an appliance that allows an object to remain horizontal even as its support tips. In the PHSF, the spacecraft will undergo multiple mechanical assembly operations and electrical tests to verify its readiness for launch. A major deployment test will check out the spacecrafts large solar arrays. The MRO was built by Lockheed Martin for NASAs Jet Propulsion Laboratory in California. It is the next major step in Mars exploration and scheduled for launch from Cape Canaveral Air Force Station in a window opening Aug. 10. The MRO is an important next step in fulfilling NASAs vision of space exploration and ultimately sending human explorers to Mars and beyond.

KSC-05PD-0999

NASA Technical Reports Server (NTRS)

2005-01-01

KENNEDY SPACE CENTER, FLA. In the Payload Hazardous Servicing Facility at NASAs Kennedy Space Center, engineers prepare to install the gimbal on the Mars Reconnaissance Orbiter (MRO) solar panel. A gimbal is an appliance that allows an object to remain horizontal even as its support tips. In the background is the orbiter. In the PHSF, the spacecraft will undergo multiple mechanical assembly operations and electrical tests to verify its readiness for launch. A major deployment test will check out the spacecrafts large solar arrays. The MRO was built by Lockheed Martin for NASAs Jet Propulsion Laboratory in California. It is the next major step in Mars exploration and scheduled for launch from Cape Canaveral Air Force Station in a window opening Aug. 10. The MRO is an important next step in fulfilling NASAs vision of space exploration and ultimately sending human explorers to Mars and beyond.

KSC-05PD-0998

NASA Technical Reports Server (NTRS)

2005-01-01

KENNEDY SPACE CENTER, FLA. In the Payload Hazardous Servicing Facility at NASAs Kennedy Space Center, engineers prepare to install the gimbal on the Mars Reconnaissance Orbiter (MRO) solar panel. A gimbal is an appliance that allows an object to remain horizontal even as its support tips. In the PHSF, the spacecraft will undergo multiple mechanical assembly operations and electrical tests to verify its readiness for launch. A major deployment test will check out the spacecrafts large solar arrays. The MRO was built by Lockheed Martin for NASAs Jet Propulsion Laboratory in California. It is the next major step in Mars exploration and scheduled for launch from Cape Canaveral Air Force Station in a window opening Aug. 10. The MRO is an important next step in fulfilling NASAs vision of space exploration and ultimately sending human explorers to Mars and beyond.

2018 Giant Dust Storm on Mars

NASA Image and Video Library

2018-06-13

This set of images from NASA's Mars Reconnaissance Orbiter (MRO) shows a fierce, giant dust storm is kicking up on Mars, with rovers on the surface indicated as icons. The spread of the storm can be seen in the salmon-colored overlay. These images from MRO's Mars Color Imager start from May 31, when the dust event was first detected, and go through June 11, 2018. MRO creates global maps of Mars but roll maneuvers for targeted observations produce gaps in the coverage, which appear as black gores in the maps. On some days there are data drops where partial or full orbits of coverage are missing. Green and purple observed in the south polar region indicate saturated pixels. Latitude is indicated along the vertical axis. Longitude is indicated along the horizontal axis. https://photojournal.jpl.nasa.gov/catalog/PIA22519

49 CFR 40.133 - Without interviewing the employee, under what circumstances may the MRO verify a test result as...

Code of Federal Regulations, 2010 CFR

2010-10-01

... 49 Transportation 1 2010-10-01 2010-10-01 false Without interviewing the employee, under what circumstances may the MRO verify a test result as positive, or as a refusal to test because of adulteration or substitution, or as cancelled because the test was invalid? 40.133 Section 40.133 Transportation Office of the Secretary of Transportation...

49 CFR 40.160 - What does the MRO do when a valid test result cannot be produced and a negative result is required?

Code of Federal Regulations, 2013 CFR

2013-10-01

... 49 Transportation 1 2013-10-01 2013-10-01 false What does the MRO do when a valid test result cannot be produced and a negative result is required? 40.160 Section 40.160 Transportation Office of the Secretary of Transportation PROCEDURES FOR TRANSPORTATION WORKPLACE DRUG AND ALCOHOL TESTING PROGRAMS Medical Review Officers and the Verification...

49 CFR 40.133 - Without interviewing the employee, under what circumstances may the MRO verify a test result as...

Code of Federal Regulations, 2012 CFR

2012-10-01

... 49 Transportation 1 2012-10-01 2012-10-01 false Without interviewing the employee, under what circumstances may the MRO verify a test result as positive, or as a refusal to test because of adulteration or substitution, or as cancelled because the test was invalid? 40.133 Section 40.133 Transportation Office of the Secretary of Transportation...

49 CFR 40.133 - Without interviewing the employee, under what circumstances may the MRO verify a test result as...

Code of Federal Regulations, 2011 CFR

2011-10-01

... 49 Transportation 1 2011-10-01 2011-10-01 false Without interviewing the employee, under what circumstances may the MRO verify a test result as positive, or as a refusal to test because of adulteration or substitution, or as cancelled because the test was invalid? 40.133 Section 40.133 Transportation Office of the Secretary of Transportation...

49 CFR 40.153 - How does the MRO notify employees of their right to a test of the split specimen?

Code of Federal Regulations, 2013 CFR

2013-10-01

... 49 Transportation 1 2013-10-01 2013-10-01 false How does the MRO notify employees of their right to a test of the split specimen? 40.153 Section 40.153 Transportation Office of the Secretary of Transportation PROCEDURES FOR TRANSPORTATION WORKPLACE DRUG AND ALCOHOL TESTING PROGRAMS Medical Review Officers and the Verification Process § 40.153 Ho...

49 CFR 40.133 - Without interviewing the employee, under what circumstances may the MRO verify a test result as...

Code of Federal Regulations, 2013 CFR

2013-10-01

... 49 Transportation 1 2013-10-01 2013-10-01 false Without interviewing the employee, under what circumstances may the MRO verify a test result as positive, or as a refusal to test because of adulteration or substitution, or as cancelled because the test was invalid? 40.133 Section 40.133 Transportation Office of the Secretary of Transportation...

49 CFR 40.133 - Without interviewing the employee, under what circumstances may the MRO verify a test result as...

Code of Federal Regulations, 2014 CFR

2014-10-01

... 49 Transportation 1 2014-10-01 2014-10-01 false Without interviewing the employee, under what circumstances may the MRO verify a test result as positive, or as a refusal to test because of adulteration or substitution, or as cancelled because the test was invalid? 40.133 Section 40.133 Transportation Office of the Secretary of Transportation...

Correlations between dynamics and atomic structures in Cu64.5Zr35.5 metallic glass

NASA Astrophysics Data System (ADS)

Wang, C. Z.; Zhang, Y.; Zhang, F.; Mendelev, M. I.; Kramer, M. J.; Ho, K. M.

2015-03-01

The atomic structure of Cu-Zr metallic glasses (MGs) has been widely accepted to be heterogeneous and dominated by icosahedral short range order (ISRO). However, the correlations between dynamics and atomic structures in Cu-Zr MGs remain an enigma. Using molecular dynamics (MD) simulations, we investigated the correlations between dynamics and atomic structures in Cu64.5Zr35.5 MG. The atomic structures are characterized using ISRO and the Bergman-type medium range order (BMRO). The simulation and analysis results show that the majority of the mobile atoms are not involved in ISRO or BMRO, indicating that the dynamical heterogeneity has a strong correlation to structural heterogeneity. Moreover, we found that the localized soft vibration modes below 1.0 THz are mostly concentrated on the mobile atoms. The diffusion was studied using the atomic trajectory collected in an extended time interval of 1.2 μs at 700 K in MD simulations. It was found that the long range diffusion in MGs is highly heterogeneous, which is confined to the liquid-like regions and strongly avoids the ISRO and the Bergman-type MRO. All These results clearly demonstrate strong correlations between dynamics (in terms of dynamical heterogeneity and diffusion) and atomic structures in Cu64.5Zr35.5 MGs. This work was supported by the U.S. Department of Energy, Basic Energy Sciences, Division of Materials Science and Engineering under the Contract No. DE-AC02-07CH11358.

From parent-child mutuality to security to socialization outcomes: developmental cascade toward positive adaptation in preadolescence.

PubMed

Kim, Sanghag; Boldt, Lea J; Kochanska, Grazyna

2015-01-01

A developmental cascade from positive early parent-child relationship to child security with the parent to adaptive socialization outcomes, proposed in attachment theory and often implicitly accepted but rarely formally tested, was examined in 100 mothers, fathers, and children followed from toddler age to preadolescence. Parent-child Mutually Responsive Orientation (MRO) was observed in lengthy interactions at 38, 52, 67, and 80 months; children reported their security with parents at age eight. Socialization outcomes (parent- and child-reported cooperation with parental monitoring and teacher-reported school competence) were assessed at age 10. Mediation was tested with PROCESS. The parent-child history of MRO significantly predicted both mother-child and father-child security. For mother-child dyads, security mediated links between history of MRO and cooperation with maternal monitoring and school competence, controlling for developmental continuity of the studied constructs. For father-child dyads, the mediation effect was not evident.

Link Design and Planning for Mars Reconnaissance Orbiter (MRO) Ka-band (32 GHz) Telecom Demonstration

NASA Technical Reports Server (NTRS)

Shambayati, Shervin; Davarian, Faramaz; Morabito, David

2004-01-01

NASA is planning an engineering telemetry demonstration with Mars Reconnaissance Orbiter (MRO). Capabilities of Ka-band (32 GHz) for use with deep space mission are demonstrated using the link optimization algorithms and weather forecasting. Furthermore, based on the performance of previous deep space missions with Ka-band downlink capabilities, experiment plans are developed for telemetry operations during superior solar conjunction. A general overview of the demonstration is given followed by a description of the mission planning during cruise, the primary science mission and superior conjunction. As part of the primary science mission planning the expected data return for various data optimization methods is calculated. These results indicate that, given MRO's data rates, a link optimized to use of at most two data rates, subject to a minimum availability of 90%, performs almost as well as a link with no limits on the number of data rates subject to the same minimum availability.

DESIGN AND TEST OF AN INSTRUMENT FOR MEASURING MICROTHERMAL SEEING ON THE MAGDALENA RIDGE

DOE Office of Scientific and Technical Information (OSTI.GOV)

Jorgensen, A. M.; Klinglesmith, D. A.; Speights, J.

2009-05-15

We have constructed and operated an automated instrument for measuring ground-level microthermal seeing at the Magdalena Ridge Observatory (MRO). The MRO is located at an altitude of 10500' in the Cibola National Forest in New Mexico, USA. It is the planned site for the MRO Optical Interferometer (MROI) planned for up to 10 collecting elements, each with a diameter of 1.4 m, and baselines eventually up to approximately 400 m. As part of the preparation for construction we deployed a system to characterize the ground-level seeing across the observatory site. The instrument is built largely of off-the-shelf components, with onlymore » the sensor head and power supply requiring electronic board assembly. Even in those cases the board architecture is very simple. The first proof-of-concept system was deployed for several weeks in the autumn of 2004, and has since undergone several iterations. The latest configuration operates entirely off batteries, incorporates wireless data acquisition, and is thus able to operate in an area with no shelter, power, or communications. In this paper we present the design of the instrument, and show initial data. The microthermal tower has four sensor pairs at heights from 0.8 to 4.41 m, significantly lower than other microthermal experiments, because of the need to characterize the seeing near the ground. We find significant variation in the contribution of this range of heights to the seeing, contributing up to 0.''3 of the seeing at some times and only 0.''02 at other times. The individual sensor power spectra have a slope in the range of 1.4--1.5, which is lower than the 1.67 slope predicted by Kolmogorov turbulence theory. We measure the well known effect of improved seeing immediately around sunset. While we find significant variation in the microthermal seeing, we did not find a pattern of corresponding variations in weather conditions, suggesting that a complicated set of factors control microthermal turbulence.« less

Spin State of Returning Fly-by Near Earth Asteroid 2012 TC4

NASA Astrophysics Data System (ADS)

Ryan, William; Ryan, Eileen V.

2017-10-01

The ten-meter class near-Earth asteroid 2012 TC4 will make a close approach to the Earth on October 12, 2017. As of July 2017, the close approach distance ranges from 0.003 to 0.64 lunar distances (LD) with a nominal value of 0.23 LD. However this is the second observable close approach that this object has made since its discovery. In particular, broadband photometry was obtained for 2012 TC4 on 10 and 11 October 2012 using the Magdalena Ridge Observatory (MRO) 2.4-meter telescope. A periodicity of ~12.2 minutes was immediately evident in the time-series data, which was in agreement with the reported values of Polishook (2013), Odden et al. (2012), Warner (2013), and Carbognani (2014). The lightcurve displays an amplitude of ~0.9 magnitude, which implies that it is highly elongated with an axial ratio of a/b>2.3. However, a second period is also clearly evident in the MRO data, indicating that the asteroid is in a state of non-principle axis rotation.The nature of its orbit has made 2012 TC4 an attractive Earth-impacting asteroid surrogate for an exercise testing the capabilities of the scientific and emergency response communities (Reddy, 2017). For this reason, it is anticipated that considerable resources, including MRO, will be utilized to take advantage of the 2017 flyby to study this asteroid. Here, we present the details of the tumbling nature of this fast-spinning object observed during the October 2012 discovery apparition. These data were acquired before closest approach in 2012 where the asteroid came within 0.25 lunar distances of Earth. Therefore, this analysis will be discussed in the context of the spin state observations planned for early October 2017 at MRO, for which preliminary results will also be reported. In particular, comparison of the observed rotation state from the two apparitions can be indicative of any effects of Earth’s gravity during the 2012 flyby.References:Odden, C.E., Verhaegh, J.C., McCullough, D.G., and Briggs, J.W. (2013). Minor Planet Bul. 40, 176-177.Warner, B.D. (2013). Minor Planet Bul. 40, 71-80.Polishook, D. (2013). Minor Planet Bul. 40, 42-43.Carbognani, A. (2014). Minor Planet Bul. 41, 4-8.Reddy, V. (2017), AMOS SSA Technical Conference, Maui, HI.

DOE Office of Scientific and Technical Information (OSTI.GOV)

Zhang, Pei; Maldonis, Jason J.; Besser, M. F.

Fluctuation electron microscopy experiments combined with hybrid reverse Monte Carlo modeling show a correlation between medium-range structure at the nanometer scale and glass forming ability in two Zr–Cu–Al bulk metallic glass (BMG) alloys. Both Zr 50Cu 35Al 15 and Zr 50Cu 45Al 5 exhibit two nanoscale structure types, one icosahedral and the other more crystal-like. In Zr 50Cu 35Al 15, the poorer glass former, the crystal-like structure is more stable under annealing below the glass transition temperature, T g, than in Zr 50Cu 45Al 5. Variable resolution fluctuation microscopy of the MRO clusters show that in Zr 50Cu 35Al 15more » on sub-Tg annealing, the crystal-like clusters shrink even as they grow more ordered, while icosahedral-like clusters grow. Furthermore, the results suggest that achieving better glass forming ability in this alloy system may depend more on destabilizing crystal-like structures than enhancing non-crystalline structures.« less

An Overview of the Mars Reconnaissance Orbiter (MRO) Science Mission

NASA Technical Reports Server (NTRS)

Zurek, Richard W.; Smrekar, Suzanne E.

2007-01-01

The Mars Reconnaissance Orbiter (MRO) is the latest addition to the suite of missions on or orbiting Mars as part of the NASA Mars Exploration Program. Launched on 12 August 2005, the orbiter successfully entered Mars orbit on 10 March 2006 and finished aerobraking on 30 August 2006. Now in its near-polar, near-circular, low-altitude (approximately 300 km), 3 p.m. orbit, the spacecraft is operating its payload of six scientific instruments throughout a one-Mars-year Primary Science Phase (PSP) of global mapping, regional survey, and targeted observations. Eight scientific investigations were chosen for MRO, two of which use either the spacecraft accelerometers or tracking of the spacecraft telecom signal to acquire data needed for analysis. Six instruments, including three imaging systems, a visible-near infrared spectrometer, a shallow-probing subsurface radar, and a thermal-infrared profiler, were selected to complement and extend the capabilities of current working spacecraft at Mars. Whether observing the atmosphere, surface, or subsurface, the MRO instruments are designed to achieve significantly higher resolution while maintaining coverage comparable to the current best observations. The requirements to return higher-resolution data, to target routinely from a low-altitude orbit, and to operate a complex suite of instruments were major challenges successfully met in the design and build of the spacecraft, as well as by the mission design. Calibration activities during the seven-month cruise to Mars and limited payload operations during a three-day checkout prior to the start of aerobraking demonstrated, where possible, that the spacecraft and payload still had the functions critical to the science mission. Two critical events, the deployment of the SHARAD radar antenna and the opening of the CRISM telescope cover, were successfully accomplished in September 2006. Normal data collection began 7 November 2006 after solar conjunction. As part of its science mission, MRO will also aid identification and characterization of the most promising sites for future landed missions, both in terms of safety and in terms of the scientific potential for future discovery. Ultimately, MRO data will advance our understanding of how Mars has evolved and by which processes that change occurs, all within a framework of identifying the presence, extent, and role of water in shaping the planet s climate over time.

MRO DKF Post-Processing Tool

NASA Technical Reports Server (NTRS)

Ayap, Shanti; Fisher, Forest; Gladden, Roy; Khanampompan, Teerapat

2008-01-01

This software tool saves time and reduces risk by automating two labor-intensive and error-prone post-processing steps required for every DKF [DSN (Deep Space Network) Keyword File] that MRO (Mars Reconnaissance Orbiter) produces, and is being extended to post-process the corresponding TSOE (Text Sequence Of Events) as well. The need for this post-processing step stems from limitations in the seq-gen modeling resulting in incorrect DKF generation that is then cleaned up in post-processing.

Visible-light OCT to quantify retinal oxygen metabolism (Conference Presentation)

NASA Astrophysics Data System (ADS)

Zhang, Hao F.; Yi, Ji; Chen, Siyu; Liu, Wenzhong; Soetikno, Brian T.

2016-03-01

We explored, both numerically and experimentally, whether OCT can be a good candidate to accurately measure retinal oxygen metabolism. We first used statistical methods to numerically simulate photon transport in the retina to mimic OCT working under different spectral ranges. Then we analyze accuracy of OCT oximetry subject to parameter variations such as vessel size, pigmentation, and oxygenation. We further developed an experimental OCT system based on the spectral range identified by our simulation work. We applied the newly developed OCT to measure both retinal hemoglobin oxygen saturation (sO2) and retinal retinal flow. After obtaining the retinal sO2 and blood velocity, we further measured retinal vessel diameter and calculated the retinal oxygen metabolism rate (MRO2). To test the capability of our OCT, we imaged wild-type Long-Evans rats ventilated with both normal air and air mixtures with various oxygen concentrations. Our simulation suggested that OCT working within visible spectral range is able to provide accurate measurement of retinal MRO2 using inverse Fourier transform spectral reconstruction. We called this newly developed technology vis-OCT, and showed that vis-OCT was able to measure the sO2 value in every single major retinal vessel around the optical disk as well as in micro retinal vessels. When breathing normal air, the averaged sO2 in arterial and venous blood in Long-Evans rats was measured to be 95% and 72%, respectively. When we challenge the rats using air mixtures with different oxygen concentrations, vis-OCT measurement followed analytical models of retinal oxygen diffusion and pulse oximeter well.

Mars Reconnaissance Orbiter: Aerobraking Science Analysis

NASA Astrophysics Data System (ADS)

Bougher, Stephen W.; Keating, G. M.

2006-09-01

The Mars Reconnaissance Orbiter (MRO) spacecraft was launched from the Kennedy Space Center in Florida on August 12, 2005, and arrived at Mars on March 10, 2006. Aerobraking in the martian thermosphere was conducted for nearly 5-months after arrival, enabling the desired MRO mapping orbit to be achieved. The MRO aerobraking phase began in early martian northern Spring (Ls = 36) and continued through early northern Summer (Ls 110), spanning approximately 500 orbits. The MRO periapsis latitude migrated slowly poleward/southward from 70ºS latitude upon aerobraking initiation, passed over the South pole (near Ls = 77), and moved rapidly northward to equatorial latitudes at aerobraking conclusion. Upper atmosphere sampling ( 100-200 km) was achieved on the dayside (LT 1900-2000) before polar crossing, and on the nightside (LT = 0200-0300) thereafter. These seasonal and latitude conditions are similar to a subset of those experienced by MGS during its post hiatus aerobraking Phase 2. Derived mass densities, scale heights, and estimated temperatures are the primary data products generated from each aeropass. The most important discovery of MRO aerobraking concerns the sampling of the thermosphere up to 200 km, far higher than previous MGS and Odyssey Accelerometers have achieved. This sampling contributes to the characterization of the Mars exobase region, which is required to predict and interpret atmospheric escape rates. In addition, thermospheric densities at a constant altitude were observed to decrease toward the southern (winter) pole, as expected from previous MGS experience. No winter polar warming was typically observed near the South pole. Thereafter, densities were measured to increase on the nightside as periapsis moved toward the equator. In general, thermospheric variability was observed to increase in the vicinity of the polar vortex boundary ( 70-80ºS), and decreased again inside the vortex (high southern latitudes). Finally, longitude wave features displayed wave#1 and 2 components.

Mars Reconnaissance Orbiter: Aerobraking Science Discoveries using the Accelerometer

NASA Astrophysics Data System (ADS)

Keating, Gerald M.; Bougher, S. W.

2006-09-01

The Mars Reconnaissance Orbiter (MRO) spacecraft was launched from the Kennedy Space Center in Florida on August 12, 2005, and arrived at Mars on March 10, 2006. Aerobraking in the martian thermosphere was conducted for nearly 5-months after arrival, enabling the desired MRO mapping orbit to be achieved. The MRO aerobraking phase began in early martian northern Spring (Ls = 36) and continued through early northern Summer (Ls 110), spanning approximately 500 orbits. The MRO periapsis latitude migrated slowly poleward/southward from 70ºS latitude upon aerobraking initiation, passed over the South pole (near Ls = 77), and moved rapidly northward to equatorial latitudes at aerobraking conclusion. Upper atmosphere sampling ( 100-200 km) was achieved on the dayside (LT 1900-2000) before polar crossing, and on the nightside (LT = 0200-0300) thereafter. These seasonal and latitude conditions are similar to a subset of those experienced by MGS during its post hiatus aerobraking Phase 2. Derived mass densities, scale heights, and estimated temperatures are the primary data products generated from each aeropass. The most important discovery of MRO aerobraking concerns the sampling of the thermosphere up to 200 km, far higher than previous MGS and Odyssey Accelerometers have achieved. This sampling contributes to the characterization of the Mars exobase region, which is required to predict and interpret atmospheric escape rates. In addition, thermospheric densities at a constant altitude were observed to decrease toward the southern (winter) pole, as expected from previous MGS experience. No winter polar warming was typically observed near the South pole. Thereafter, densities were measured to increase on the nightside as periapsis moved toward the equator. In general, thermospheric variability was observed to increase in the vicinity of the polar vortex boundary ( 70-80ºS), and decreased again inside the vortex (high southern latitudes). Finally, longitude wave features displayed wave#1 and 2 components.

Using polymerization, glass structure, and quasicrystalline theory to produce high level radioactive borosilicate glass remotely: a 20+ year legacy

DOE Office of Scientific and Technical Information (OSTI.GOV)

Jantzen, Carol M.

Vitrification is currently the most widely used technology for the treatment of high level radioactive wastes (HLW) throughout the world. Most of the nations that have generated HLW are immobilizing in borosilicate glass. One of the primary reasons that glass has become the most widely used immobilization media is the relative simplicity of the vitrification process, e.g. melt a highly variable waste with some glass forming additives such as SiO 2 and B 2O 3 in the form of a premelted frit and pour the molten mixture into a stainless steel canister. Seal the canister before moisture can enter themore » canister (10’ tall by 2’ in diameter) so the canister does not corrode from the inside out. Glass has also become widely used for HLW is that due to the fact that the short range order (SRO) and medium range order (MRO) found in the structure of glass atomistically bonds the radionuclides and hazardous species in the waste. The SRO and MRO have also been found to govern the melt properties such as viscosity and resistivity of the melt and the crystallization potential and solubility of certain species. Furthermore, the molecular structure of the glass also controls the glass durability, i.e. the contaminant/radionuclide release, by establishing the distribution of ion exchange sites, hydrolysis sites, and the access of water to those sites. The molecular structure is flexible and hence accounts for the flexibility of glass formulations to HLW waste variability. Nuclear waste glasses melt between 1050-1150°C which minimizes the volatility of radioactive components such as 99Tc, 137Cs, and 129I. Nuclear waste glasses have good long term stability including irradiation resistance. Process control models were developed based on the molecular structure of glass, polymerization theory of glass, and quasicrystalline theory of glass crystallization. These models create a glass which is durable, pourable, and processable with 95% accuracy without knowing from batch to batch what the composition of the waste coming out of the storage tanks will be. These models have operated the Savannah River Site Defense Waste Processing Facility (SRS DWPF), which is the world’s largest HLW Joule heated ceramic melter, since 1996. This unique “feed forward” process control, which qualifies the durability, pourability, and processability of the waste plus glass additive mixture before it enters the melter, has enabled ~8000 tons of HLW glass and 4242 canisters to be produced since 1996 with only one melter replacement.« less

Using polymerization, glass structure, and quasicrystalline theory to produce high level radioactive borosilicate glass remotely: a 20+ year legacy

DOE PAGES

Jantzen, Carol M.

2017-03-27

Vitrification is currently the most widely used technology for the treatment of high level radioactive wastes (HLW) throughout the world. Most of the nations that have generated HLW are immobilizing in borosilicate glass. One of the primary reasons that glass has become the most widely used immobilization media is the relative simplicity of the vitrification process, e.g. melt a highly variable waste with some glass forming additives such as SiO 2 and B 2O 3 in the form of a premelted frit and pour the molten mixture into a stainless steel canister. Seal the canister before moisture can enter themore » canister (10’ tall by 2’ in diameter) so the canister does not corrode from the inside out. Glass has also become widely used for HLW is that due to the fact that the short range order (SRO) and medium range order (MRO) found in the structure of glass atomistically bonds the radionuclides and hazardous species in the waste. The SRO and MRO have also been found to govern the melt properties such as viscosity and resistivity of the melt and the crystallization potential and solubility of certain species. Furthermore, the molecular structure of the glass also controls the glass durability, i.e. the contaminant/radionuclide release, by establishing the distribution of ion exchange sites, hydrolysis sites, and the access of water to those sites. The molecular structure is flexible and hence accounts for the flexibility of glass formulations to HLW waste variability. Nuclear waste glasses melt between 1050-1150°C which minimizes the volatility of radioactive components such as 99Tc, 137Cs, and 129I. Nuclear waste glasses have good long term stability including irradiation resistance. Process control models were developed based on the molecular structure of glass, polymerization theory of glass, and quasicrystalline theory of glass crystallization. These models create a glass which is durable, pourable, and processable with 95% accuracy without knowing from batch to batch what the composition of the waste coming out of the storage tanks will be. These models have operated the Savannah River Site Defense Waste Processing Facility (SRS DWPF), which is the world’s largest HLW Joule heated ceramic melter, since 1996. This unique “feed forward” process control, which qualifies the durability, pourability, and processability of the waste plus glass additive mixture before it enters the melter, has enabled ~8000 tons of HLW glass and 4242 canisters to be produced since 1996 with only one melter replacement.« less

Optical-resolution photoacoustic microscopy of the metabolic rate of oxygen in a mouse renal tumor model

NASA Astrophysics Data System (ADS)

Yeh, Chenghung; Hu, Song; Liang, Jinyang; Li, Lei; Soetikno, Brian; Lu, Zhi Hong; Sohn, Rebecca E.; Maslov, Konstantin; Arbeit, Jeffrey M.; Wang, Lihong V.

2015-03-01

We propose using noninvasive longitudinal optical-resolution photoacoustic microscopy (L-ORPAM) to quantify blood flow flux, oxygen saturation (sO2), and thereby the metabolic rate of oxygen (MRO2), for a renal tumor model in the same mouse over weeks to months. Experiments showed that the sO2 difference between the artery and vein decreased greatly due to the arteriovenous shunting effect during tumor growth. Moreover, hypermetabolism was exhibited by an increase in MRO2.

From Parent-Child Mutuality to Security to Socialization Outcomes: Developmental Cascade toward Positive Adaptation in Preadolescence

PubMed Central

Kim, Sanghag; Boldt, Lea J.; Kochanska, Grazyna

2016-01-01

A developmental cascade from positive early parent-child relationship to child security with the parent to adaptive socialization outcomes, proposed in attachment theory and often implicitly accepted but rarely formally tested, was examined in 100 mothers, fathers, and children followed from toddler age to preadolescence. Parent-child Mutually Responsive Orientation (MRO) was observed in lengthy interactions at 38, 52, 67, and 80 months; children reported their security with parents at age 8. Socialization outcomes (parent- and child-reported cooperation with parental monitoring and teacher-reported school competence) were assessed at age 10. Mediation was tested with PROCESS (Hayes, 2013). The parent-child history of MRO significantly predicted both mother-child and father-child security. For mother-child dyads, security mediated links between history of MRO and cooperation with maternal monitoring and school competence, controlling for developmental continuity of the studied constructs. For father-child dyads, the mediation effect was not evident. PMID:26258443

Prevalence of answers to orthopaedic in-training examination questions in 3 commonly used orthopedic review sources.

PubMed

Krueger, Chad A; Shakir, Irshad; Fuller, Brian C

2012-09-01

One of the greatest predictors for resident success on the Orthopaedic In-Training Examination (OITE) is reviewing previous OITE questions. However, no studies have examined which review sources contain the most answers to previously asked OITE questions. The goal of this study was to determine which review source contains the most answers to previously asked OITE questions. Each question from the 2006 to 2010 OITEs was examined. The questions were placed into 1 of 13 categories based on their topic. The publication date of the recommended readings associated with each question was recorded. The answer to each question was then searched for in 3 commonly used review sources: Miller's Review of Orthopaedics, 5th edition (MRO), American Academy of Orthopaedic Surgeons Comprehensive Orthopaedic Review (COR), and www.orthobullets.com (OB). Searchable electronic versions of each textbook were used, and each question had a 12-minute time limit. Of 1358 questions, 665 (49%) were found in all 3 sources. Significantly more answers were found on OB (99.4%) compared with MRO (60%) and COR (62%) (P<.0001). Significantly more answers to questions in each question category were found on OB compared with MRO or COR (P<.0001). More than 50% of all recommended readings for OITE questions were published within 5 years of the OITE. Residents using OB to review for the OITE will be exposed to significantly more answers of previously asked OITE questions than residents using MRO or COR (P<.0001). Copyright 2012, SLACK Incorporated.

Oxygen consumption estimation with combined color doppler ultrasound and photoacoustic microscopy: a phantom study

NASA Astrophysics Data System (ADS)

Jiang, Yan; Harrison, Tyler; Forbrich, Alex; Zemp, Roger J.

2011-03-01

The metabolic rate of oxygen consumption (MRO2) quantifies tissue metabolism, which is important for diagnosis of many diseases. For a single vessel model, the MRO2 can be estimated in terms of the mean flow velocity, vessel crosssectional area, total concentration of hemoglobin (CHB), and the difference between the oxygen saturation (sO2) of blood flowing into and out of the tissue region. In this work, we would like to show the feasibility to estimate MRO2 with our combined photoacoustic and high-frequency ultrasound imaging system. This system uses a swept-scan 25-MHz ultrasound transducer with confocal dark-field laser illumination optics. A pulse-sequencer enables ultrasonic and laser pulses to be interlaced so that photoacoustic and Doppler ultrasound images are co-registered. Since the mean flow velocity can be measured by color Doppler ultrasound, the vessel cross-sectional area can be measured by power Doppler or photoacoustic imaging, and multi-wavelength photoacoustic methods can be used to estimate sO2 and CHB, all of these parameters necessary for MRO2 estimation can be provided by our system. Experiments have been performed on flow phantoms to generate co-registered color Doppler and photoacoustic images. To verify the sO2 estimation, two ink samples (red and blue) were mixed in various concentration ratios to mimic different levels of sO2, and the result shows a good match between the calculated concentration ratios and actual values.

A New Method for Atmospheric Correction of MRO/CRISM Data.

NASA Astrophysics Data System (ADS)

Noe Dobrea, Eldar Z.; Dressing, C.; Wolff, M. J.

2009-09-01

The Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) aboard the Mars Reconnaissance Orbiter (MRO) collects hyperspectral images from 0.362 to 3.92 μm at 6.55 nanometers/channel, and at a spatial resolution of 20 m/pixel. The 1-2.6 μm spectral range is often used to identify and map the distribution of hydrous minerals using mineralogically diagnostic bands at 1.4 μm, 1.9 μm, and 2 - 2.5 micron region. Atmospheric correction of the 2-μm CO2 band typically employs the same methodology applied to OMEGA data (Mustard et al., Nature 454, 2008): an atmospheric opacity spectrum, obtained from the ratio of spectra from the base to spectra from the peak of Olympus Mons, is rescaled for each spectrum in the observation to fit the 2-μm CO2 band, and is subsequently used to correct the data. Three important aspects are not considered in this correction: 1) absorptions due to water vapor are improperly accounted for, 2) the band-center of each channel shifts slightly with time, and 3) multiple scattering due to atmospheric aerosols is not considered. The second issue results in miss-registration of the sharp CO2 features in the 2-μm triplet, and hence poor atmospheric correction. This leads to the necessity to ratio all spectra using the spectrum of a spectrally "bland” region in each observation in order to distinguish features 1.9 μm. Here, we present an improved atmospheric correction method, which uses emission phase function (EPF) observations to correct for molecular opacity, and a discrete ordinate radiative transfer algorithm (DISORT - Stamnes et al., Appl. Opt. 27, 1988) to correct for the effects of multiple scattering. This method results in a significant improvement in the correction of the 2-μm CO2 band, allowing us to forgo the use of spectral ratios that affect the spectral shape and preclude the derivation of reflectance values in the data.

Relay Support for the Mars Science Laboratory and the Coming Decade of Mars Relay Network Evolution

NASA Technical Reports Server (NTRS)

Edwards, Charles D., Jr.; Arnold, Bradford W.; Bell, David J.; Bruvold, Kristoffer N.; Gladden, Roy E.; Ilott, Peter A.; Lee, Charles H.

2012-01-01

Mars Relay Network is prepared to support MSL: a) ODY/MRO/MEX will all provide critical event comm support during EDL. b) New Electra/Electra-Lite capabilities on the MSL-MRO link will support >250 Mb/sol MSL data return. 2013 MAVEN orbiter will replenish on-orbit relay infrastructure as prior orbiters approach end-of-life. While NASA has withdrawn from the 2016 EMTGO and 2018 Joint Rover missions, analysis of the potential link shows a path to Gbit/sol relay capability 2012.

Extensive MRO CRISM Observations of 1.27 micron O2 Airglow in Mars Polar Night and Their Comparison to MRO MCS Temperature Profiles and LMD GCM Simulations

NASA Technical Reports Server (NTRS)

Clancy, R. Todd; Sandor, Brad J.; Wolff, Michael J.; Smith, Michael Doyle; Lefevre, Franck; Madeleine, Jean-Baptiste; Forget, Francois; Murchie, Scott L.; Seelos, Frank P.; Seelos, Kim D.;

Mars Reconnaissance Orbiter Ka-band (32 GHz) Demonstration: Cruise Phase Operations

NASA Technical Reports Server (NTRS)

Shambayati, Shervin; Morabito, David; Border, James S.; Davarian, Faramaz; Lee, Dennis; Mendoza, Ricardo; Britcliffe, Michael; Weinreb, Sander

2006-01-01

The X-band (8.41 GHz) frequency currently used for deep space telecommunications is too narrow (50 MHz) to support future high rate missions. Because of this NASA has decided to transition to Ka-band (32 GHz) frequencies. As weather effects cause much larger fluctuations on Ka-band than on X-band, the traditional method of using a few dBs of margin to cover these fluctuations is wasteful of power for Ka-band; therefore, a different operations concept is needed for Ka-band links. As part of the development of the operations concept for Ka-band, NASA has implemented a fully functioning Ka-band communications suite on its Mars Reconnaissance Orbiter (MRO). This suite will be used during the primary science phase to develop and refine the Ka-band operations concept for deep space missions. In order to test the functional readiness of the spacecraft and the Deep Space Network's (DSN) readiness to support the demonstration activities a series of passes over DSN 34-m Beam Waveguide (BWG) antennas were scheduled during the cruise phase of the mission. MRO was launched on August 12, 2005 from Kennedy Space Center, Cape Canaveral, Florida, USA and went into Mars Orbit on March 10, 2006. A total of ten telemetry demonstration and one high gain antenna (HGA) calibration passes were allocated to the Ka-band demonstration. Furthermore, a number of "shadow" passes were also scheduled where, during a regular MRO track over a Ka-band capable antenna, Ka-band was identically configured as the X-band and tracked by the station. In addition, nine Ka-band delta differential one way ranging ((delta)DOR) passes were scheduled. During these passes, the spacecraft and the ground system were put through their respective paces. Among the highlights of these was setting a single day record for data return from a deep space spacecraft (133 Gbits) achieved during one 10-hour pass; achieving the highest data rate ever from a planetary mission (6 Mbps) and successfully demonstrating Ka-band DDOR. In addition, DSN performed well. However, there are concerns with the active pointing of the Ka-band antennas as well as delivery of the monitor data from the stations. The spacecraft also presented challenges not normally associated with planetary missions mostly because of its very high equivalent isotropic radiated power (EIRP). This caused problems in accurately evaluating the in-flight EIRP of the spacecraft which led to difficulties evaluating the quality of the HGA calibration data. These led to the development of additional measurement techniques that could be used for future high-power deep space missions.

MRO's High Resolution Imaging Science Experiment (HiRISE): Polar Science Expectations

NASA Technical Reports Server (NTRS)

McEwen, A.; Herkenhoff, K.; Hansen, C.; Bridges, N.; Delamere, W. A.; Eliason, E.; Grant, J.; Gulick, V.; Keszthelyi, L.; Kirk, R.

2003-01-01

The Mars Reconnaissance Orbiter (MRO) is expected to launch in August 2005, arrive at Mars in March 2006, and begin the primary science phase in November 2006. MRO will carry a suite of remote-sensing instruments and is designed to routinely point off-nadir to precisely target locations on Mars for high-resolution observations. The mission will have a much higher data return than any previous planetary mission, with 34 Tbits of returned data expected in the first Mars year in the mapping orbit (255 x 320 km). The HiRISE camera features a 0.5 m telescope, 12 m focal length, and 14 CCDs. We expect to acquire approximately 10,000 observations in the primary science phase (approximately 1 Mars year), including approximately 2,000 images for 1,000 stereo targets. Each observation will be accompanied by a approximately 6 m/pixel image over a 30 x 45 km region acquired by MRO s context imager. Many HiRISE images will be full resolution in the center portion of the swath width and binned (typically 4x4) on the sides. This provides two levels of context, so we step out from 0.3 m/pixel to 1.2 m/pixel to 6 m/pixel (at 300 km altitude). We expect to cover approximately 1% of Mars at better than 1.2 m/pixel, approximately 0.1% at 0.3 m/pixel, approximately 0.1% in 3 colors, and approximately 0.05% in stereo. Our major challenge is to find the dey contacts, exposures and type morphologies to observe.

Novel Hydrogenosomes in the Microaerophilic Jakobid Stygiella incarcerata

PubMed Central

Leger, Michelle M.; Eme, Laura; Hug, Laura A.; Roger, Andrew J.

2016-01-01

Mitochondrion-related organelles (MROs) have arisen independently in a wide range of anaerobic protist lineages. Only a few of these organelles and their functions have been investigated in detail, and most of what is known about MROs comes from studies of parasitic organisms such as the parabasalid Trichomonas vaginalis. Here, we describe the MRO of a free-living anaerobic jakobid excavate, Stygiella incarcerata. We report an RNAseq-based reconstruction of S. incarcerata’s MRO proteome, with an associated biochemical map of the pathways predicted to be present in this organelle. The pyruvate metabolism and oxidative stress response pathways are strikingly similar to those found in the MROs of other anaerobic protists, such as Pygsuia and Trichomonas. This elegant example of convergent evolution is suggestive of an anaerobic biochemical ‘module’ of prokaryotic origins that has been laterally transferred among eukaryotes, enabling them to adapt rapidly to anaerobiosis. We also identified genes corresponding to a variety of mitochondrial processes not found in Trichomonas, including intermembrane space components of the mitochondrial protein import apparatus, and enzymes involved in amino acid metabolism and cardiolipin biosynthesis. In this respect, the MROs of S. incarcerata more closely resemble those of the much more distantly related free-living organisms Pygsuia biforma and Cantina marsupialis, likely reflecting these organisms’ shared lifestyle as free-living anaerobes. PMID:27280585

Elastic Anomaly and Polyamorphic Transition in (La, Ce)-based Bulk Metallic Glass under Pressure

DOE PAGES

Qi, Xintong; Zou, Yongtao; Wang, Xuebing; ...

2017-04-07

In this paper, we discovered that in association with the polyamorphism of La 32Ce 32Al 16Ni 5Cu 15 bulk metallic glass, the acoustic velocities, measured up to 12.3 GPa using ultrasonic interferometry, exhibit velocity minima at 1.8 GPa for P wave and 3.2 GPa for S wave. The low and high density amorphous states are distinguished by their distinct pressure derivatives of the bulk and shear moduli. The elasticity, permanent densification, and polyamorphic transition are interpreted by the topological rearrangement of solute-centered clusters in medium-range order (MRO) mediated by the 4f electron delocalization of Ce under pressure. The precisely measuredmore » acoustic wave travel times which were used to derive the velocities and densities provided unprecedented data to document the evolution of the bulk and shear elastic moduli associated with a polyamorphic transition in La 32Ce 32Al 16Ni 5Cu 15 bulk metallic glass and can shed new light on the mechanisms of polyamorphism and structural evolution in metallic glasses under pressure.« less

Mars Reconnaissance Orbiter Uplink Analysis Tool

NASA Technical Reports Server (NTRS)

Khanampompan, Teerapat; Gladden, Roy; Fisher, Forest; Hwang, Pauline

2008-01-01

This software analyzes Mars Reconnaissance Orbiter (MRO) orbital geometry with respect to Mars Exploration Rover (MER) contact windows, and is the first tool of its kind designed specifically to support MRO-MER interface coordination. Prior to this automated tool, this analysis was done manually with Excel and the UNIX command line. In total, the process would take approximately 30 minutes for each analysis. The current automated analysis takes less than 30 seconds. This tool resides on the flight machine and uses a PHP interface that does the entire analysis of the input files and takes into account one-way light time from another input file. Input flies are copied over to the proper directories and are dynamically read into the tool s interface. The user can then choose the corresponding input files based on the time frame desired for analysis. After submission of the Web form, the tool merges the two files into a single, time-ordered listing of events for both spacecraft. The times are converted to the same reference time (Earth Transmit Time) by reading in a light time file and performing the calculations necessary to shift the time formats. The program also has the ability to vary the size of the keep-out window on the main page of the analysis tool by inputting a custom time for padding each MRO event time. The parameters on the form are read in and passed to the second page for analysis. Everything is fully coded in PHP and can be accessed by anyone with access to the machine via Web page. This uplink tool will continue to be used for the duration of the MER mission's needs for X-band uplinks. Future missions also can use the tools to check overflight times as well as potential site observation times. Adaptation of the input files to the proper format, and the window keep-out times, would allow for other analyses. Any operations task that uses the idea of keep-out windows will have a use for this program.

Interannual Variability of Dust and Ice in the Mars Atmosphere: Comparison of MRO Mars Climate Sounder Retrievals with MGS-TES Limb Sounding Retrievals

NASA Technical Reports Server (NTRS)

Shirley, J. H.; McConnochie, T. H.; Kleinbohl, A.; Schofield, J. T.; Kass, D.; Heavens, N. G.; Benson, J.; McCleese, D. J.

2011-01-01

Dust and ice play important roles in Martian atmospheric dynamics on all time scales. Dust loading in particular exerts an important control on atmospheric temperatures and thereby on the strength of the atmospheric circulation in any given year. We present the first comparisons of MGS-TES aerosol opacity profiles with MRO-MCS aerosol opacity profiles. While the differences in vertical resolution are significant (a factor of 2), we find good agreement at particular seasons between nightside zonal average dust opacity profiles from the two instruments. Derived water ice opacities are likewise similar but show greater variability.

Mars Reconnaissance Orbiter Aerobraking Daily Operations and Collision Avoidance

NASA Technical Reports Server (NTRS)

Long, Stacia M.; You, Tung-Han; Halsell, C. Allen; Bhat, Ramachand S.; Demcak, Stuart W.; Graat, Eric J.; Higa, Earl S.; Highsmith, Dolan E.; Mottinger, Neil A.; Jah, Moriba K.

2007-01-01

The Mars Reconnaissance Orbiter reached Mars on March 10, 2006 and performed a Mars orbit insertion maneuver of 1 km/s to enter into a large elliptical orbit. Three weeks later, aerobraking operations began and lasted about five months. Aerobraking utilized the atmospheric drag to reduce the large elliptical orbit into a smaller, near circular orbit. At the time of MRO aerobraking, there were three other operational spacecraft orbiting Mars and the navigation team had to minimize the possibility of a collision. This paper describes the daily operations of the MRO navigation team during this time as well as the collision avoidance strategy development and implementation.

Relay Telecommunications for the Coming Decade of Mars Exploration

NASA Technical Reports Server (NTRS)

Edwards, C.; DePaula, R.

2010-01-01

Over the past decade, an evolving network of relay-equipped orbiters has advanced our capabilities for Mars exploration. NASA's Mars Global Surveyor, 2001 Mars Odyssey, and Mars Reconnaissance Orbiter (MRO), as well as ESA's Mars Express Orbiter, have provided telecommunications relay services to the 2003 Mars Exploration Rovers, Spirit and Opportunity, and to the 2007 Phoenix Lander. Based on these successes, a roadmap for continued Mars relay services is in place for the coming decade. MRO and Odyssey will provide key relay support to the 2011 Mars Science Laboratory (MSL) mission, including capture of critical event telemetry during entry, descent, and landing, as well as support for command and telemetry during surface operations, utilizing new capabilities of the Electra relay payload on MRO and the Electra-Lite payload on MSL to allow significant increase in data return relative to earlier missions. Over the remainder of the decade a number of additional orbiter and lander missions are planned, representing new orbital relay service providers and new landed relay users. In this paper we will outline this Mars relay roadmap, quantifying relay performance over time, illustrating planned support scenarios, and identifying key challenges and technology infusion opportunities.

Emplacement of the youngest flood lava on Mars: A short, turbulent story

USGS Publications Warehouse

Jaeger, W.L.; Keszthelyi, L.P.; Skinner, J.A.; Milazzo, M.P.; McEwen, A.S.; Titus, T.N.; Rosiek, M.R.; Galuszka, D.M.; Howington-Kraus, E.; Kirk, R.L.

2010-01-01

Recently acquired data from the High Resolution Imaging Science Experiment (HiRISE), Context (CTX) imager, and Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) onboard the Mars Reconnaissance Orbiter (MRO) spacecraft were used to investigate the emplacement of the youngest flood-lava flow on Mars. Careful mapping finds that the Athabasca Valles flood lava is the product of a single eruption, and it covers 250,000 km2 of western Elysium Planitia with an estimated 5000-7500 km3 of mafic or ultramafic lava. Calculations utilizing topographic data enhanced with MRO observations to refine the dimensions of the channel system show that this flood lava was emplaced turbulently over a period of only a few to several weeks. This is the first well-documented example of a turbulently emplaced flood lava anywhere in the Solar System. However, MRO data suggest that this same process may have operated in a number of martian channel systems. The magnitude and dynamics of these lava floods are similar to the aqueous floods that are generally believed to have eroded the channels, raising the intriguing possibility that mechanical erosion by lava could have played a role in their incision. ?? 2009.

Emplacement of the youngest flood lava on Mars: A short, turbulent story

USGS Publications Warehouse

Jaeger, W.L.; Keszthelyi, L.P.; Skinner, J.A.; Milazzo, M.P.; McEwen, A.S.; Titus, T.N.; Rosiek, M.R.; Galuszka, D.M.; Howington-Kraus, E.; Kirk, R.L.

2009-01-01

Recently acquired data from the High Resolution Imaging Science Experiment (HiRISE), Context (CTX) imager, and Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) onboard the Mars Reconnaissance Orbiter (MRO) spacecraft were used to investigate the emplacement of the youngest flood-lava flow on Mars. Careful mapping finds that the Athabasca Valles flood lava is the product of a single eruption, and it covers 250,000 km2 of western Elysium Planitia with an estimated 5000-7500 km3 of mafic or ultramafic lava. Calculations utilizing topographic data enhanced with MRO observations to refine the dimensions of the channel system show that this flood lava was emplaced turbulently over a period of only a few to several weeks. This is the first well-documented example of a turbulently emplaced flood lava anywhere in the Solar System. However, MRO data suggest that this same process may have operated in a number of martian channel systems. The magnitude and dynamics of these lava floods are similar to the aqueous floods that are generally believed to have eroded the channels, raising the intriguing possibility that mechanical erosion by lava could have played a role in their incision.

The Compositions, Particle Sizes, and Distributions of Ice Aerosols in the Mars Mesosphere from 2009-2016 CRISM Visible-NearIR Limb Spectra

NASA Astrophysics Data System (ADS)

Clancy, R. T.; Smith, M. D.; Wolff, M. J.; Toigo, A. D.; Seelos, K. D.; Murchie, S. L.

2016-12-01

Since 2009, the CRISM visible-nearIR imaging spectrometer onboard the Mars Reconnaissance Orbiter (MRO) has returned over 70 orbits of Mars limb image scans over the 0-130 km altitude range. Pole-to-pole latitudinal coverage is obtained from the near-polar, sun-synchronous (LT 3pm) MRO orbit for a limited set of surface longitudes centered on Tharsis, Valles Mariners, Meridioni, and Hellas regions. Seasonal coverage extends over the full seasonal range (Ls=0-360°), as accumulated over 2009-2016 (MY 29-33), supporting a range of aerosol and airglow studies (Smith et al., 2013; Clancy et al., 2012, 2013). The 0.4-4.0 μm wavelength range of these CRISM limb observations proves particularly suitable to characterizing aerosol composition and particle sizes, particularly for the Mars mesosphere (z=50-100 km), which has only recently been observed with any dedication by MCS (Sefton-Nash et al, 2013) and CRISM limb measurements. Dust and H2O, CO2 ice aerosols are clearly distinguished by their distinct scattering and absorption behaviors over the key 2-4 μm wavelength region, and their particle sizes are well determined by the 0.4-3 μm wavelength region. Several key attributes are determined for Mars mesospheric aerosols. Dust aerosols are largely undetected, and are apparently injected to such heights only during global dust storms (Clancy et al, 2010). Ice clouds are generally common at 55-75 km altitudes, although in separate halves of the Mars year. CO2 and H2O ice clouds are most prominent during the aphelion and perihelion portions of the Mars orbit, respectively. CO2 ice clouds, which occur at low latitudes over specific surface longitudes, present distinct particle size populations ranging from 0.5 to 1.5 μm (Reff). Mesospheric H2O ice clouds exhibit somewhat smaller particle sizes (Reff=0.3-1 μm) and extend over low to mid latitudes. This orbital dependence for mesospheric ice aerosol composition indicates extreme annual (orbital) variation in mesospheric water vapor.

Amorphous and nanocrystalline phase formation in highly-driven Al-based binary alloys

DOE Office of Scientific and Technical Information (OSTI.GOV)

Kalay, Yunus Eren

2009-01-01

Remarkable advances have been made since rapid solidification was first introduced to the field of materials science and technology. New types of materials such as amorphous alloys and nanostructure materials have been developed as a result of rapid solidification techniques. While these advances are, in many respects, ground breaking, much remains to be discerned concerning the fundamental relationships that exist between a liquid and a rapidly solidified solid. The scope of the current dissertation involves an extensive set of experimental, analytical, and computational studies designed to increase the overall understanding of morphological selection, phase competition, and structural hierarchy that occursmore » under far-from equilibrium conditions. High pressure gas atomization and Cu-block melt-spinning are the two different rapid solidification techniques applied in this study. The research is mainly focused on Al-Si and Al-Sm alloy systems. Silicon and samarium produce different, yet favorable, systems for exploration when alloyed with aluminum under far-from equilibrium conditions. One of the main differences comes from the positions of their respective T 0 curves, which makes Al-Si a good candidate for solubility extension while the plunging T 0 line in Al-Sm promotes glass formation. The rapidly solidified gas-atomized Al-Si powders within a composition range of 15 to 50 wt% Si are examined using scanning and transmission electron microscopy. The non-equilibrium partitioning and morphological selection observed by examining powders at different size classes are described via a microstructure map. The interface velocities and the amount of undercooling present in the powders are estimated from measured eutectic spacings based on Jackson-Hunt (JH) and Trivedi-Magnin-Kurz (TMK) models, which permit a direct comparison of theoretical predictions. For an average particle size of 10 {micro}m with a Peclet number of ~0.2, JH and TMK deviate from each other. This deviation indicates an adiabatic type solidification path where heat of fusion is reabsorbed. It is interesting that this particle size range is also consistent with the appearance of a microcellular growth. While no glass formation is observed within this system, the smallest size powders appear to consist of a mixture of nanocrystalline Si and Al. Al-Sm alloys have been investigated within a composition range of 34 to 42 wt% Sm. Gas atomized powders of Al-Sm are investigated to explore the morphological and structural hierarchy that correlates with different degrees of departure from full equilibrium conditions. The resultant powders show a variety of structural selection with respect to amount of undercooling, with an amorphous structure appearing at the highest cooling rates. Because of the chaotic nature of gas atomization, Cu-block melt-spinning is used to produce a homogeneous amorphous structure. The as-quenched structure within Al-34 to 42 wt% Sm consists of nanocrystalline fcc-Al (on the order of 5 nm) embedded in an amorphous matrix. The nucleation density of fcc-Al after initial crystallization is on the order of 10 22-10 23m -3, which is 10 5-10 6 orders of magnitude higher than what classical nucleation theory predicts. Detailed analysis of liquid and as-quenched structures using high energy synchrotron X-ray diffraction, high energy transmission electron microscopy, and atom probe tomography techniques revealed an Al-Sm network similar in appearance to a medium range order (MRO) structure. A model whereby these MRO clusters promote the observed high nucleation density of fcc-Al nanocrystals is proposed. The devitrification path was identified using high temperature, in-situ, high energy synchrotron X-ray diffraction techniques and the crystallization kinetics were described using an analytical Johnson-Mehl-Avrami (JMA) approach.« less

Critical needs for piston engine overhaul centre in Malaysia

NASA Astrophysics Data System (ADS)

Khairuddin, M. H.; Yahya, M. Y.; Johari, M. K.

2017-12-01

Piston engine overhaul centre (PEOC) is the branch of aviation Maintenance, Repair and Overhaul (MRO) providers, which plays a pivotal role in maintaining the fleet of business and commercial aircraft in the world. The centre typically offers three main MRO capabilities: airframe, engine and component services. Companies holding a PEOC(s) are all subjected to stringent procedures and conditions regulated and audited by the International Civil Aviation Organization. Currently, piston engine maintenance and repair for Asian countries is conducted only in Singapore. The focus of this study is to establish the needs for a PEOC in Malaysia, which will cater almost all small local aircraft companies such as transport and flying school companies.

Multi-instrument data analysis for interpretation of the Martian North polar layered deposits

NASA Astrophysics Data System (ADS)

Mirino, Melissa; Sefton-Nash, Elliot; Witasse, Olivier; Frigeri, Alessandro

2017-04-01

The Martian polar caps have engendered substantial study due to their spiral morphology, layered structure and the seasonal variability in thickness of the uppermost H2O and CO2 ice layers. We demonstrate a multi-instrument study of exposed and buried north polar layers using data from ESA's Mars Express (MEx) and NASA's Mars Reconnaissance Orbiter (MRO) missions. We perform analysis of high resolution images from MRO's HiRISE, which provide textural and morphological information about surface features larger than 0.3m, with NIR hyperspectral data from MRO CRISM, which allows study of surface mineralogy at a maximum resolution of 18 m/pixel. Stereo-derived topography is provided by MEx's HRSC. Together with these surficial observations we interpret radargrams from MRO SHARAD to obtain information about layered structures at a horizontal resolution between 0.3 and 3 kilometers and a free-space vertical resolution of 15 meters (vertical resolution depends on the dielectric properties of the medium). This combination of datasets allows us to attempt to correlate polar layering, made visible by dielectric interfaces between beds, with surface mineralogies and structures outcropping at specific stratigraphic levels. We analyse two opposite areas of the north polar cap with the intention to characterise in multiple datasets each geologic unit identified in the north polar cap's stratigraphy (mapped by e.g. [1]). We selected deposits observed in Chasma Boreale and Olympia Cavi because these areas allow us to observe and map strata at opposing sides of the north polar cap. Using the CRISM Analysis Tool and spectral summary parameters [2] we map the spectral characteristics of the two areas that show H2O and CO2 ice layering exposed on polar scarps. Through spatial-registration in a GIS with HRSC topography and HiRISE imagery we assess the mineralogical and morphological characteristics of exposed layers. In order to constrain the cross section between the two selected localities we choose SHARAD radargrams that most closely align with the transect between the sites. We interpret sub-horizontal features to be due to dielectric interfaces involving the deposits analysed. Our interpretation of radargrams in the context of compositional and structural constraints, from areas where pertinent beds outcrop, illustrates how joint analysis of surface and sub-surface data can benefit geological interpretation of planetary surfaces and subsurfaces. This technique applied to Mars' north polar layered deposits may offer additional constraint on morphology of internal layering resulting from seasonal deposition/sublimation cycles over varying obliquity [3]. References: [1] Tanaka et al. (2008), Icarus, 196, p. 318-358, doi:10.1016/j.icarus.2008.01.021. [2] Viviano-Beck et al. (2014), J. Geophys. Res. Planets, 119, p. 1403-1431, doi:10.1002/2014JE004627..[3] Putzig et al. (2009), Icarus, 204, p. 443-457, doi:10.1016/j.icarus.2009.07.034.

KSC-05pp1879

NASA Image and Video Library

2005-08-12

KENNEDY SPACE CENTER, FLA. - Trailing smoke and fire, the 19-stories-tall Atlas V launch vehicle, with a two-ton Mars Reconnaissance Orbiter (MRO) on top, roars away from Launch Complex 41 at Cape Canaveral Air Force Station at 7:43 a.m. EDT. All systems performed nominally for NASA's first launch of an Atlas V on an interplanetary mission. MRO established radio contact with controllers 61 minutes after launch and within four minutes of separation from the upper stage. Initial contact came through an antenna at the Japan Aerospace Exploration Agency's Uchinoura Space Center in southern Japan. Mars is 72 million miles from Earth today, but the spacecraft will travel more than four times that distance on its outbound-arc trajectory to intercept the red planet on March 10, 2006. The orbiter carries six scientific instruments for examining the surface, atmosphere and subsurface of Mars in unprecedented detail from low orbit. NASA expects to get several times more data about Mars from MRO than from all previous Martian missions combined. Researchers will use the instruments to learn more about the history and distribution of Mars' water. That information will improve understanding of planetary climate change and will help guide the quest to answer whether Mars ever supported life. The orbiter will also evaluate potential landing sites for future missions. (Photo Credit: Tom Rogers)

KSC-05pp1881

NASA Image and Video Library

2005-08-12

KENNEDY SPACE CENTER, FLA. - The 19-stories-tall Atlas V launch vehicle, with a two-ton Mars Reconnaissance Orbiter (MRO) on top, leaps away from Launch Complex 41 at Cape Canaveral Air Force Station at 7:43 a.m. EDT. All systems performed nominally for NASA's first launch of an Atlas V on an interplanetary mission. MRO established radio contact with controllers 61 minutes after launch and within four minutes of separation from the upper stage. Initial contact came through an antenna at the Japan Aerospace Exploration Agency's Uchinoura Space Center in southern Japan. Mars is 72 million miles from Earth today, but the spacecraft will travel more than four times that distance on its outbound-arc trajectory to intercept the red planet on March 10, 2006. The orbiter carries six scientific instruments for examining the surface, atmosphere and subsurface of Mars in unprecedented detail from low orbit. NASA expects to get several times more data about Mars from MRO than from all previous Martian missions combined. Researchers will use the instruments to learn more about the history and distribution of Mars' water. That information will improve understanding of planetary climate change and will help guide the quest to answer whether Mars ever supported life. The orbiter will also evaluate potential landing sites for future missions.

Mars Reconnaissance Orbiter In-flight Anomalies and Lessons Learned: An Update

NASA Technical Reports Server (NTRS)

Bayer, Todd J.

2008-01-01

The Mars Reconnaissance Orbiter mission has as its primary objectives: advance our understanding of the current Mars climate, the processes that have formed and modified the surface of the planet and the extent to which water has played a role in surface processes; identify sites of possible aqueous activity indicating environments that may have been or are conducive to biological activity; and thus identify and characterize sites for future landed missions; and provide forward and return relay services for current and future Mars landed assets. MRO's crucial role in the long term strategy for Mars exploration requires a high level of reliability during its 5.4 year mission. This requires an architecture which incorporates extensive redundancy and cross-strapping. Because of the distances and hence light-times involved, the spacecraft itself must be able to utilize this redundancy in responding to time-critical failures. For cases where fault protection is unable to recognize a potentially threatening condition, either due to known limitations or software flaws, intervention by ground operations is required. These aspects of MRO's design were discussed in a previous paper [Ref. 1]. This paper provides an update to the original paper, describing MRO's significant in-flight anomalies over the past year, with lessons learned for redundancy and fault protection architectures and for ground operations.

Gene expression in bovine rumen epithelium during weaning identifies molecular regulators of rumen development and growth.

PubMed

Connor, Erin E; Baldwin, Ransom L; Li, Cong-jun; Li, Robert W; Chung, Hoyoung

2013-03-01

During weaning, epithelial cell function in the rumen transitions in response to conversion from a pre-ruminant to a true ruminant environment to ensure efficient nutrient absorption and metabolism. To identify gene networks affected by weaning in bovine rumen, Holstein bull calves were fed commercial milk replacer only (MRO) until 42 days of age, then were provided diets of either milk + orchardgrass hay (MH) or milk + grain-based calf starter (MG). Rumen epithelial RNA was extracted from calves sacrificed at four time points: day 14 (n = 3) and day 42 (n = 3) of age while fed the MRO diet and day 56 (n = 3/diet) and day 70 (n = 3/diet) while fed the MH and MG diets for transcript profiling by microarray hybridization. Five two-group comparisons were made using Permutation Analysis of Differential Expression® to identify differentially expressed genes over time and developmental stage between days 14 and 42 within the MRO diet, between day 42 on the MRO diet and day 56 on the MG or MH diets, and between the MG and MH diets at days 56 and 70. Ingenuity Pathway Analysis (IPA) of differentially expressed genes during weaning indicated the top 5 gene networks involving molecules participating in lipid metabolism, cell morphology and death, cellular growth and proliferation, molecular transport, and the cell cycle. Putative genes functioning in the establishment of the rumen microbial population and associated rumen epithelial inflammation during weaning were identified. Activation of transcription factor PPAR-α was identified by IPA software as an important regulator of molecular changes in rumen epithelium that function in papillary development and fatty acid oxidation during the transition from pre-rumination to rumination. Thus, molecular markers of rumen development and gene networks regulating differentiation and growth of rumen epithelium were identified for selecting targets and methods for improving and assessing rumen development and function, particularly in the growing calf.

Dark Materials on Olympus Mons

NASA Image and Video Library

2018-01-23

This image from NASA's Mars Reconnaissance Orbiter (MRO) shows blocks of layered terrain within the Olympus Mons aureole. The aureole is a giant apron of chaotic material around the volcano, perhaps formed by enormous landslides off the flanks of the giant volcano. These blocks of layered material have been eroded by the wind into the scenic landscape we see here. The map is projected here at a scale of 25 centimeters (9.8 inches) per pixel. [The original image scale is 28.3 centimeters (11.1 inches) per pixel (with 1 x 1 binning); objects on the order of 85 centimeters (33.5 inches) across are resolved.] North is up. https://photojournal.jpl.nasa.gov/catalog/PIA22181

A Peek into a Cul-De-Sac and a Mews of Martian Dust Storm Activity: Western Hellas and Syria-Claritas Fossae During Mars Year 29

NASA Astrophysics Data System (ADS)

Heavens, N. G.

2016-12-01

Western Hellas Planitia (WHP) and the region encompassed by Syria Planum and Claritas Fossae are the main centers of textured dust storm activity in Mars's southern low to mid-latitudes. (Texture in this context refers to distinct fine structure at the cloud tops indicative of active lifting.) WHP is a well-known initiation zone for regional and global dust storm activity and often the end point of the Utopia "flushing storm" track. Syria-Claritas Fossae (SCF), too, can be a lifting center in global dust storm activity. Indeed, SCF and the area to its west was the region most denuded of dust by the Mars Year (MY) 25 global dust storm, perhaps suggesting that SCF contained the principal lifting center of the storm. Thus, if the Acidalia and Utopia storm tracks are Mars's dust storm alleys, through which dust storms pass quickly again and again; WHP might be a cul-de-sac and SCF something like a mews, where dust storm activity can enter more or less easily but may not as easily leave. In this presentation, I will focus on dust storm activity in these areas in a typical non-global dust storm year, MY 29. Synthesizing visible imagery by the Mars Color Imager (MARCI) on board Mars Reconnaissance Orbiter (MRO) and Mars Climate Sounder (MCS) also on board MRO, I will consider the climatology, morphology, texture, and vertical structure of dust storm activity in these areas in order to infer their governing dynamics. This investigation has two aims: (1) to understand why these areas are centers of textured dust storm activity; and (2) to connect the characteristics of smaller-scale dust storm activity in these regions to the underlying dynamics in order to understand the role of WHP and SCF in the dynamics of global dust storms. This work is supported by NASA's Mars Data Analysis Program (NNX14AM32G).

KSC-05pp1878

NASA Image and Video Library

2005-08-12

KENNEDY SPACE CENTER, FLA. - With the Atlantic Ocean as a backdrop, an Atlas V launch vehicle, 19 stories tall, with a two-ton Mars Reconnaissance Orbiter (MRO) on top, roars away from Launch Complex 41 at Cape Canaveral Air Force Station at 7:43 a.m. EDT. All systems performed nominally for NASA's first launch of an Atlas V on an interplanetary mission. MRO established radio contact with controllers 61 minutes after launch and within four minutes of separation from the upper stage. Initial contact came through an antenna at the Japan Aerospace Exploration Agency's Uchinoura Space Center in southern Japan. Mars is 72 million miles from Earth today, but the spacecraft will travel more than four times that distance on its outbound-arc trajectory to intercept the red planet on March 10, 2006. The orbiter carries six scientific instruments for examining the surface, atmosphere and subsurface of Mars in unprecedented detail from low orbit. NASA expects to get several times more data about Mars from MRO than from all previous Martian missions combined. Researchers will use the instruments to learn more about the history and distribution of Mars' water. That information will improve understanding of planetary climate change and will help guide the quest to answer whether Mars ever supported life. The orbiter will also evaluate potential landing sites for future missions. (Photo Credit: Pat Corkery/Lockheed Martin)

KSC-05pp1877

NASA Image and Video Library

2005-08-12

KENNEDY SPACE CENTER, FLA. - With the Atlantic Ocean as a backdrop, an Atlas V launch vehicle, 19 stories tall, with a two-ton Mars Reconnaissance Orbiter (MRO) on top, roars away from Launch Complex 41 at Cape Canaveral Air Force Station at 7:43 a.m. EDT. All systems performed nominally for NASA's first launch of an Atlas V on an interplanetary mission. MRO established radio contact with controllers 61 minutes after launch and within four minutes of separation from the upper stage. Initial contact came through an antenna at the Japan Aerospace Exploration Agency's Uchinoura Space Center in southern Japan. Mars is 72 million miles from Earth today, but the spacecraft will travel more than four times that distance on its outbound-arc trajectory to intercept the red planet on March 10, 2006. The orbiter carries six scientific instruments for examining the surface, atmosphere and subsurface of Mars in unprecedented detail from low orbit. NASA expects to get several times more data about Mars from MRO than from all previous Martian missions combined. Researchers will use the instruments to learn more about the history and distribution of Mars' water. That information will improve understanding of planetary climate change and will help guide the quest to answer whether Mars ever supported life. The orbiter will also evaluate potential landing sites for future missions. (Photo Credit: Pat Corkery/Lockheed Martin)

KSC-05pp1883

NASA Image and Video Library

2005-08-12

KENNEDY SPACE CENTER, FLA. - Viewed through a break in the greenscape around Launch Complex 41 at Cape Canaveral Air Force Station in Florida, the 19-stories-tall Atlas V launch vehicle roars off the launch pad, propelling the two-ton Mars Reconnaissance Orbiter (MRO) into a clear blue Florida sky and eventual orbit around Mars. Liftoff was at 7:43 a.m. EDT. All systems performed nominally for NASA's first launch of an Atlas V on an interplanetary mission. MRO established radio contact with controllers 61 minutes after launch and within four minutes of separation from the upper stage. Initial contact came through an antenna at the Japan Aerospace Exploration Agency's Uchinoura Space Center in southern Japan. Mars is 72 million miles from Earth today, but the spacecraft will travel more than four times that distance on its outbound-arc trajectory to intercept the red planet on March 10, 2006. The orbiter carries six scientific instruments for examining the surface, atmosphere and subsurface of Mars in unprecedented detail from low orbit. NASA expects to get several times more data about Mars from MRO than from all previous Martian missions combined. Researchers will use the instruments to learn more about the history and distribution of Mars' water. That information will improve understanding of planetary climate change and will help guide the quest to answer whether Mars ever supported life. The orbiter will also evaluate potential landing sites for future missions.

KSC-05pp1882

NASA Image and Video Library

2005-08-12

KENNEDY SPACE CENTER, FLA. - The 19-stories-tall Atlas V launch vehicle leaps above the trees near Launch Complex 41 at Cape Canaveral Air Force Station in Florida, propelling the two-ton Mars Reconnaissance Orbiter (MRO) into a clear blue Florida sky and eventual orbit around Mars. Liftoff was at 7:43 a.m. EDT. All systems performed nominally for NASA's first launch of an Atlas V on an interplanetary mission. MRO established radio contact with controllers 61 minutes after launch and within four minutes of separation from the upper stage. Initial contact came through an antenna at the Japan Aerospace Exploration Agency's Uchinoura Space Center in southern Japan. Mars is 72 million miles from Earth today, but the spacecraft will travel more than four times that distance on its outbound-arc trajectory to intercept the red planet on March 10, 2006. The orbiter carries six scientific instruments for examining the surface, atmosphere and subsurface of Mars in unprecedented detail from low orbit. NASA expects to get several times more data about Mars from MRO than from all previous Martian missions combined. Researchers will use the instruments to learn more about the history and distribution of Mars' water. That information will improve understanding of planetary climate change and will help guide the quest to answer whether Mars ever supported life. The orbiter will also evaluate potential landing sites for future missions.

KSC-05pp1876

NASA Image and Video Library

2005-08-12

KENNEDY SPACE CENTER, FLA. - With the Atlantic Ocean as a backdrop, an Atlas V launch vehicle, 19 stories tall, with a two-ton Mars Reconnaissance Orbiter (MRO) on top, roars away from Launch Complex 41 at Cape Canaveral Air Force Station at 7:43 a.m. EDT. All systems performed nominally for NASA's first launch of an Atlas V on an interplanetary mission. MRO established radio contact with controllers 61 minutes after launch and within four minutes of separation from the upper stage. Initial contact came through an antenna at the Japan Aerospace Exploration Agency's Uchinoura Space Center in southern Japan. Mars is 72 million miles from Earth today, but the spacecraft will travel more than four times that distance on its outbound-arc trajectory to intercept the red planet on March 10, 2006. The orbiter carries six scientific instruments for examining the surface, atmosphere and subsurface of Mars in unprecedented detail from low orbit. NASA expects to get several times more data about Mars from MRO than from all previous Martian missions combined. Researchers will use the instruments to learn more about the history and distribution of Mars' water. That information will improve understanding of planetary climate change and will help guide the quest to answer whether Mars ever supported life. The orbiter will also evaluate potential landing sites for future missions. (Photo Credit: Pat Corkery/Lockheed Martin)

KSC-05pp1875

NASA Image and Video Library

2005-08-12

KENNEDY SPACE CENTER, FLA. - With the Atlantic Ocean as a backdrop, an Atlas V launch vehicle, 19 stories tall, with a two-ton Mars Reconnaissance Orbiter (MRO) on top, roars away from Launch Complex 41 at Cape Canaveral Air Force Station at 7:43 a.m. EDT. All systems performed nominally for NASA's first launch of an Atlas V on an interplanetary mission. MRO established radio contact with controllers 61 minutes after launch and within four minutes of separation from the upper stage. Initial contact came through an antenna at the Japan Aerospace Exploration Agency's Uchinoura Space Center in southern Japan. Mars is 72 million miles from Earth today, but the spacecraft will travel more than four times that distance on its outbound-arc trajectory to intercept the red planet on March 10, 2006. The orbiter carries six scientific instruments for examining the surface, atmosphere and subsurface of Mars in unprecedented detail from low orbit. NASA expects to get several times more data about Mars from MRO than from all previous Martian missions combined. Researchers will use the instruments to learn more about the history and distribution of Mars' water. That information will improve understanding of planetary climate change and will help guide the quest to answer whether Mars ever supported life. The orbiter will also evaluate potential landing sites for future missions. (Photo Credit: Pat Corkery/Lockheed Martin)

KSC-05pp1880

NASA Image and Video Library

2005-08-12

KENNEDY SPACE CENTER, FLA. - Just minutes after liftoff, the 19-stories-tall Atlas V launch vehicle, with a two-ton Mars Reconnaissance Orbiter (MRO) on top, roars into the clear blue sky from Launch Complex 41 at Cape Canaveral Air Force Station. Liftoff was at 7:43 a.m. EDT. All systems performed nominally for NASA's first launch of an Atlas V on an interplanetary mission. MRO established radio contact with controllers 61 minutes after launch and within four minutes of separation from the upper stage. Initial contact came through an antenna at the Japan Aerospace Exploration Agency's Uchinoura Space Center in southern Japan. Mars is 72 million miles from Earth today, but the spacecraft will travel more than four times that distance on its outbound-arc trajectory to intercept the red planet on March 10, 2006. The orbiter carries six scientific instruments for examining the surface, atmosphere and subsurface of Mars in unprecedented detail from low orbit. NASA expects to get several times more data about Mars from MRO than from all previous Martian missions combined. Researchers will use the instruments to learn more about the history and distribution of Mars' water. That information will improve understanding of planetary climate change and will help guide the quest to answer whether Mars ever supported life. The orbiter will also evaluate potential landing sites for future missions. (Photo Credit: Tom Rogers)

Visible light optical coherence tomography measure retinal oxygen metabolic response to systemic oxygenation (Conference Presentation)

NASA Astrophysics Data System (ADS)

Yi, Ji; Liu, Wenzhong; Chen, Siyu; Backman, Vadim; Sheibani, Nader; Sorenson, Christine M.; Fawzi, Amani A.; Linsenmeier, Robert A.; Zhang, Hao F.

2016-03-01

The lack of capability to quantify oxygen metabolism noninvasively impedes both fundamental investigation and clinical diagnosis of a wide spectrum of diseases including all the major blinding diseases such as age-related macular degeneration, diabetic retinopathy, and glaucoma. Using visible light optical coherence tomography (vis-OCT), we demonstrated accurate and robust measurement of retinal oxygen metabolic rate (rMRO2) noninvasively in rat eyes. The rMRO2 was calculated by concurrent measurement of blood flow and blood oxygen saturation (sO2). Blood flow was calculated by the principle of Doppler optical coherence tomography, where the phase shift between two closely spaced A-lines measures the axial velocity. The distinct optical absorption spectra of oxy- and deoxy-hemoglobin provided the contrast for sO2 measurement, combined with the spectroscopic analysis of vis-OCT signal within the blood vessels. We continuously monitored the regulatory response of oxygen consumption to a progressive hypoxic challenge. We found that both oxygen delivery, and rMRO2 increased from the highly regulated retinal circulation (RC) under hypoxia, by 0.28+/-0.08 μL/min (p<0.001), and 0.20+/-0.04 μL/min (p<0.001) per 100 mmHg systemic pO2 reduction, respectively. The increased oxygen extraction compensated for the deficient oxygen supply from the poorly regulated choroidal circulation (CC).

Inner retinal oxygen metabolism in the 50/10 oxygen-induced retinopathy model

PubMed Central

Soetikno, Brian T.; Yi, Ji; Shah, Ronil; Liu, Wenzhong; Purta, Patryk; Zhang, Hao F.; Fawzi, Amani A.

2015-01-01

Retinopathy of prematurity (ROP) represents a major cause of childhood vision loss worldwide. The 50/10 oxygen-induced retinopathy (OIR) model mimics the findings of ROP, including peripheral vascular attenuation and neovascularization. The oxygen metabolism of the inner retina has not been previously explored in this model. Using visible-light optical coherence tomography (vis-OCT), we measured the oxygen saturation of hemoglobin and blood flow within inner retinal vessels, enabling us to compute the inner retinal oxygen delivery (irDO2) and metabolic rate of oxygen (irMRO2). We compared these measurements between age-matched room-air controls and rats with 50/10 OIR on postnatal day 18. To account for a 61% decrease in the irDO2 in the OIR group, we found an overall statistically significant decrease in retinal vascular density affecting the superficial and deep retinal vascular capillary networks in rats with OIR compared to controls. Furthermore, matching the reduced irDO2, we found a 59% decrease in irMRO2, which we correlated with a statistically significant reduction in retinal thickness in the OIR group, suggesting that the decreased irMRO2 was due to decreased neuronal oxygen utilization. By exploring these biological and metabolic changes in great detail, our study provides an improved understanding of the pathophysiology of OIR model. PMID:26576731

Super Resolution and Interference Suppression Technique applied to SHARAD Radar Data

NASA Astrophysics Data System (ADS)

Raguso, M. C.; Mastrogiuseppe, M.; Seu, R.; Piazzo, L.

2017-12-01

We will present a super resolution and interference suppression technique applied to the data acquired by the SHAllow RADar (SHARAD) on board the NASA's 2005 Mars Reconnaissance Orbiter (MRO) mission, currently operating around Mars [1]. The algorithms allow to improve the range resolution roughly by a factor of 3 and the Signal to Noise Ratio (SNR) by a several decibels. Range compression algorithms usually adopt conventional Fourier transform techniques, which are limited in the resolution by the transmitted signal bandwidth, analogous to the Rayleigh's criterion in optics. In this work, we investigate a super resolution method based on autoregressive models and linear prediction techniques [2]. Starting from the estimation of the linear prediction coefficients from the spectral data, the algorithm performs the radar bandwidth extrapolation (BWE), thereby improving the range resolution of the pulse-compressed coherent radar data. Moreover, the EMIs (ElectroMagnetic Interferences) are detected and the spectra is interpolated in order to reconstruct an interference free spectrum, thereby improving the SNR. The algorithm can be applied to the single complex look image after synthetic aperture processing (SAR). We apply the proposed algorithm to simulated as well as to real radar data. We will demonstrate the effective enhancement on vertical resolution with respect to the classical spectral estimator. We will show that the imaging of the subsurface layered structures observed in radargrams is improved, allowing additional insights for the scientific community in the interpretation of the SHARAD radar data, which will help to further our understanding of the formation and evolution of known geological features on Mars. References: [1] Seu et al. 2007, Science, 2007, 317, 1715-1718 [2] K.M. Cuomo, "A Bandwidth Extrapolation Technique for Improved Range Resolution of Coherent Radar Data", Project Report CJP-60, Revision 1, MIT Lincoln Laboratory (4 Dec. 1992).

System design of the CRISM (compact reconnaissance imaging spectrometer for Mars) hyperspectral imager

NASA Astrophysics Data System (ADS)

Silverglate, Peter R.; Fort, Dennis E.

2004-01-01

CRISM (Compact Reconnaissance Imaging Spectrometer for Mars) is a hyperspectral imager that will be launched on the MRO (Mars Reconnaissance Orbiter) in August 2005. The MRO will circle Mars in a polar orbit at a nominal altitude of 325 km. The CRISM spectral range spans the ultraviolet (UV) to the mid-wave infrared (MWIR), 400 nm to 4050 nm. The instrument utilizes a Ritchey-Chretien telescope with a 2.06º field of view (FOV) to focus light on the entrance slit of a dual spectrometer. Within the spectrometer light is split by a dichroic into VNIR (visible-near infrared) (λ <= 1.05 μm) and IR (infrared) (λ >= 1.05 μm) beams. Each beam is directed into a separate modified Offner spectrometer that focuses a spectrally dispersed image of the slit onto a two dimensional focal plane (FP). The IR FP is a 640 x 480 HgCdTe area array; the VNIR FP is a 640 x 480 silicon photodiode area array. The spectral image is contiguously sampled with a 6.55 nm spectral spacing and an instantaneous field of view of 60 μradians. The orbital motion of the MRO pushbroom scans the spectrometer slit across the Martian surface, allowing the planet to be mapped in 558 spectral bands. There are four major mapping modes: A quick initial multi-spectral mapping of a major portion of the Martian surface in 59 selected spectral bands at a spatial resolution of 600 μradians (10:1 binning); an extended multi-spectral mapping of the entire Martian surface in 59 selected spectral bands at a spatial resolution of 300 μradians (5:1 binning); a high resolution Target Mode, performing hyperspectral mapping of selected targets of interest at full spatial and spectral resolution; and an atmospheric Emission Phase Function (EPF) mode for atmospheric study and correction at full spectral resolution at a spatial resolution of 300 μradians (5:1 binning). The instrument is gimbaled to allow scanning over +/-60° for the EPF and Target modes. The scanning also permits orbital motion compensation, enabling longer integration times and consequently higher signal-to-noise ratios for selected areas on the Martian surface in Target Mode.

System design of the CRISM (compact reconnaissance imaging spectrometer for Mars) hyperspectral imager

NASA Astrophysics Data System (ADS)

Silverglate, Peter R.; Fort, Dennis E.

2003-12-01

CRISM (Compact Reconnaissance Imaging Spectrometer for Mars) is a hyperspectral imager that will be launched on the MRO (Mars Reconnaissance Orbiter) in August 2005. The MRO will circle Mars in a polar orbit at a nominal altitude of 325 km. The CRISM spectral range spans the ultraviolet (UV) to the mid-wave infrared (MWIR), 400 nm to 4050 nm. The instrument utilizes a Ritchey-Chretien telescope with a 2.06º field of view (FOV) to focus light on the entrance slit of a dual spectrometer. Within the spectrometer light is split by a dichroic into VNIR (visible-near infrared) (λ <= 1.05 μm) and IR (infrared) (λ >= 1.05 μm) beams. Each beam is directed into a separate modified Offner spectrometer that focuses a spectrally dispersed image of the slit onto a two dimensional focal plane (FP). The IR FP is a 640 x 480 HgCdTe area array; the VNIR FP is a 640 x 480 silicon photodiode area array. The spectral image is contiguously sampled with a 6.55 nm spectral spacing and an instantaneous field of view of 60 μradians. The orbital motion of the MRO pushbroom scans the spectrometer slit across the Martian surface, allowing the planet to be mapped in 558 spectral bands. There are four major mapping modes: A quick initial multi-spectral mapping of a major portion of the Martian surface in 59 selected spectral bands at a spatial resolution of 600 μradians (10:1 binning); an extended multi-spectral mapping of the entire Martian surface in 59 selected spectral bands at a spatial resolution of 300 μradians (5:1 binning); a high resolution Target Mode, performing hyperspectral mapping of selected targets of interest at full spatial and spectral resolution; and an atmospheric Emission Phase Function (EPF) mode for atmospheric study and correction at full spectral resolution at a spatial resolution of 300 μradians (5:1 binning). The instrument is gimbaled to allow scanning over +/-60° for the EPF and Target modes. The scanning also permits orbital motion compensation, enabling longer integration times and consequently higher signal-to-noise ratios for selected areas on the Martian surface in Target Mode.

Diverse Lithologies on a Crater Floor

NASA Image and Video Library

2018-04-16

This image from NASA's Mars Reconnaissance Orbiter (MRO) shows bedrock units with diverse colors indicating different mineral concentrations. More information is available at https://photojournal.jpl.nasa.gov/catalog/PIA22434

Thermal Model Correlation for Mars Reconnaissance Orbiter

NASA Technical Reports Server (NTRS)

Amundsen, Ruth M.; Dec, John A.; Gasbarre, Joseph F.

2007-01-01

The Mars Reconnaissance Orbiter (MRO) launched on August 12, 2005 and began aerobraking at Mars in March 2006. In order to save propellant, MRO used aerobraking to modify the initial orbit at Mars. The spacecraft passed through the atmosphere briefly on each orbit; during each pass the spacecraft was slowed by atmospheric drag, thus lowering the orbit apoapsis. The largest area on the spacecraft, most affected by aeroheating, was the solar arrays. A thermal analysis of the solar arrays was conducted at NASA Langley Research Center to simulate their performance throughout the entire roughly 6-month period of aerobraking. A companion paper describes the development of this thermal model. This model has been correlated against many sets of flight data. Several maneuvers were performed during the cruise to Mars, such as thruster calibrations, which involve large abrupt changes in the spacecraft orientation relative to the sun. The data obtained from these maneuvers allowed the model to be well-correlated with regard to thermal mass, conductive connections, and solar response well before arrival at the planet. Correlation against flight data for both in-cruise maneuvers and drag passes was performed. Adjustments made to the model included orientation during the drag pass, solar flux, Martian surface temperature, through-array resistance, aeroheating gradient due to angle of attack, and aeroheating accommodation coefficient. Methods of correlation included comparing the model to flight temperatures, slopes, temperature deltas between sensors, and solar and planet direction vectors. Correlation and model accuracy over 400 aeroheating drag passes were determined, with overall model accuracy better than 5 C.

Bedrock on a Crater Floor

NASA Image and Video Library

2018-04-30

This enhanced color image from NASA's Mars Reconnaissance Orbiter (MRO) shows eroded bedrock on the floor of a large ancient crater. For more information see https://photojournal.jpl.nasa.gov/catalog/PIA22439

Wave-Modulated CO2 Condensation in Mars' Polar Atmosphere From MGS/TES & MOLA and MRO/MCS.

NASA Astrophysics Data System (ADS)

Banfield, D. J.

2016-12-01

In Mars' polar night, atmospheric temperatures fall low enough to cause CO2 condensation. This has been empirically demonstrated by Mars Global Surveyor's (MGS) Mars Orbiter Laser Altimeter (MOLA), which identified reflections from above the surface, and MGS Radio Science (RS) and Thermal Emission Spectrometer (TES) and Mars Reconnaissance Orbiter's (MRO) Mars Climate Sounder (MCS), all of which showed polar night temperature profiles that were super-saturated. Detailed analysis of TES temperature profiles as well as numerical modeling both suggest that the stationary and traveling waves on the polar vortices are strong enough to significantly modulate the CO2 cloud condensation. However the extent to which this is actually occurring has not been quantified. The polar night CO2 condensation represents a significant amount of energy deposition, even if it were uniformly distributed. If instead it is concentrated in the cold sectors of the various waves, this can be a tremendous perturbation not only to the wave amplitudes (clipping them from going much below the CO2 condensation temperature), but also impacting their ability to transport heat and momentum poleward and upward, and thus it may also impact the maintenance and shape of the polar vortex itself. Mars' polar vortices remain barotropically unstable throughout the winter in spite of large amplitude waves in their vicinity. We have identified when and where the various waves (with their specific amplitudes and phases) in the vicinity of the polar vortex should modulate the CO2 condensation (see Figure of a meridional cross-section showing where no clouds are expected (blue), clouds should be ubiquitous (green) and waves should be required to form clouds (red)). We have also correlated this with the distribution of the actual observed cloud identifications from MGS MOLA and MRO MCS. We find only poor correlations between the MGS/TES identified wave modulated condensation predictions and actual simultaneous cloud identifications from MGS/MOLA. We will discuss the results of a similar study using only MRO/MCS to analyze the mean atmospheric temperature, the stationary and traveling waves along the polar vortex, and the actual locations where CO2 condensation is evident.

CRISM (Compact Reconnaissance Imaging Spectrometer for Mars) on MRO (Mars Reconnaissance Orbiter)

NASA Astrophysics Data System (ADS)

Murchie, Scott L.; Arvidson, Raymond E.; Bedini, Peter; Beisser, K.; Bibring, Jean-Pierre; Bishop, J.; Boldt, John D.; Choo, Tech H.; Clancy, R. Todd; Darlington, Edward H.; Des Marais, D.; Espiritu, R.; Fasold, Melissa J.; Fort, Dennis; Green, Richard N.; Guinness, E.; Hayes, John R.; Hash, C.; Heffernan, Kevin J.; Hemmler, J.; Heyler, Gene A.; Humm, David C.; Hutchison, J.; Izenberg, Noam R.; Lee, Robert E.; Lees, Jeffrey J.; Lohr, David A.; Malaret, Erick R.; Martin, T.; Morris, Richard V.; Mustard, John F.; Rhodes, Edgar A.; Robinson, Mark S.; Roush, Ted L.; Schaefer, Edward D.; Seagrave, Gordon G.; Silverglate, Peter R.; Slavney, S.; Smith, Mark F.; Strohbehn, Kim; Taylor, Howard W.; Thompson, Patrick L.; Tossman, Barry E.

2004-12-01

CRISM (Compact Reconnaissance Imaging Spectrometer for Mars) is a hyperspectral imager that will be launched on the MRO (Mars Reconnaissance Orbiter) spacecraft in August 2005. MRO"s objectives are to recover climate science originally to have been conducted on the Mars Climate Orbiter (MCO), to identify and characterize sites of possible aqueous activity to which future landed missions may be sent, and to characterize the composition, geology, and stratigraphy of Martian surface deposits. MRO will operate from a sun-synchronous, near-circular (255x320 km altitude), near-polar orbit with a mean local solar time of 3 PM. CRISM"s spectral range spans the ultraviolet (UV) to the mid-wave infrared (MWIR), 383 nm to 3960 nm. The instrument utilizes a Ritchey-Chretien telescope with a 2.12° field-of-view (FOV) to focus light on the entrance slit of a dual spectrometer. Within the spectrometer, light is split by a dichroic into VNIR (visible-near-infrared, 383-1071 nm) and IR (infrared, 988-3960 nm) beams. Each beam is directed into a separate modified Offner spectrometer that focuses a spectrally dispersed image of the slit onto a two dimensional focal plane (FP). The IR FP is a 640 x 480 HgCdTe area array; the VNIR FP is a 640 x 480 silicon photodiode area array. The spectral image is contiguously sampled with a 6.6 nm spectral spacing and an instantaneous field of view of 61.5 μradians. The Optical Sensor Unit (OSU) can be gimbaled to take out along-track smear, allowing long integration times that afford high signal-to-noise ratio (SNR) at high spectral and spatial resolution. The scan motor and encoder are controlled by a separately housed Gimbal Motor Electronics (GME) unit. A Data Processing Unit (DPU) provides power, command and control, and data editing and compression. CRISM acquires three major types of observations of the Martian surface and atmosphere. In Multispectral Mapping Mode, with the gimbal pointed at planet nadir, data are collected at frame rates of 15 or 30 Hz. A commandable subset of wavelengths is saved by the DPU and binned 5:1 or 10:1 cross-track. The combination of frame rates and binning yields pixel footprints of 100 or 200 m. In this mode, nearly the entire planet can be mapped at wavelengths of key mineralogic absorption bands to select regions of interest. In Targeted Mode, the gimbal is scanned over +/-60° from nadir to remove most along-track motion, and a region of interest is mapped at full spatial and spectral resolution. Ten additional abbreviated, pixel-binned observations are taken before and after the main hyperspectral image at longer atmospheric path lengths, providing an emission phase function (EPF) of the site for atmospheric study and correction of surface spectra for atmospheric effects. In Atmospheric Mode, the central observation is eliminated and only the EPF is acquired. Global grids of the resulting lower data volume observation are taken repeatedly throughout the Martian year to measure seasonal variations in atmospheric properties.

The Effect of Spatial Heterogeneities on Nucleation Kinetics in Amorphous Aluminum Alloys

NASA Astrophysics Data System (ADS)

Shen, Ye

The mechanical property of the Al based metallic glass could be enhanced significantly by introducing the high number density of Al-fcc nanocrystals (1021 ˜1023 m-3) to the amorphous matrix through annealing treatments, which motivates the study of the nucleation kinetics for the microstructure control. With the presence of a high number density (1025 m-3) of aluminum-like medium range order (MRO), the Al-Y-Fe metallic glass is considered to be spatially heterogeneous. Combining the classical nucleation theory with the structural configuration, a MRO seeded nucleation model has been proposed and yields theoretical steady state nucleation rates consistent with the experimental results. In addition, this model satisfies all the thermodynamic and kinetic constraints to be reasonable. Compared with the Al-Y-Fe system, the primary crystallization onset temperature decreases significantly and the transient delay time (tau) is shorter in the Al-Y-Fe-Pb(In) systems because the insoluble Pb and In nanoparticles in the amorphous matrix served as extrinsic spatial heterogeneity to provide the nucleation sites for Al-fcc precipitation and the high-resolution transmission electron microscopy (HRTEM) images of the Pb-Al interface revealed a good wetting behavior between the Al and Pb nanoparticles. The study of the transient delay time (tau) could provide insight on the transport behavior during the nucleation and a more convenient approach to evaluate the delay time has been developed by measuring the Al-Y-Fe amorphous alloy glass transition temperature (Tg) shift with the increasing annealing time (tannealing) in FlashDSC. The break point in the Tg vs. log(tannealing) plot has been identified to correspond to the delay time by the TEM characterization. FlashDSC tests with different heating rates and different compositions (Al-Y-Fe-Pb and Zn-Mg-Ca-Yb amorphous alloys) further confirmed the break point and delay time relationship. The amorphous matrix composition and the enthalpy analysis indicates that there are different mechanisms leading to the Tg shift before and after the break point. Before the break point, Tg shifts solely due to the increased glass stability through a relaxation process. However, after the break point, Tg shifts to higher temperatures because of both the relaxation and the composition change effects.

Fall Frosting

NASA Image and Video Library

2013-10-16

Richardson Crater is home to this sea of sand dunes. It was fall in the Southern hemisphere when NASA MRO acquired this image of the dunes frosted with the first bit of carbon dioxide ice condensed from the atmosphere.

Sequence History Update Tool

NASA Technical Reports Server (NTRS)

Khanampompan, Teerapat; Gladden, Roy; Fisher, Forest; DelGuercio, Chris

2008-01-01

The Sequence History Update Tool performs Web-based sequence statistics archiving for Mars Reconnaissance Orbiter (MRO). Using a single UNIX command, the software takes advantage of sequencing conventions to automatically extract the needed statistics from multiple files. This information is then used to populate a PHP database, which is then seamlessly formatted into a dynamic Web page. This tool replaces a previous tedious and error-prone process of manually editing HTML code to construct a Web-based table. Because the tool manages all of the statistics gathering and file delivery to and from multiple data sources spread across multiple servers, there is also a considerable time and effort savings. With the use of The Sequence History Update Tool what previously took minutes is now done in less than 30 seconds, and now provides a more accurate archival record of the sequence commanding for MRO.

Mars Reconnaissance Orbiter Operational Aerobraking Phase Assessment

NASA Technical Reports Server (NTRS)

Prince, Jill L.; Striepe, Scott A.

2007-01-01

The Mars Reconnaissance Orbiter (MRO) was inserted into orbit around Mars on March 10, 2005. After a brief delay, it began the process of aerobraking - using the atmospheric drag on the vehicle to reduce orbital period. The aerobraking phase lasted approximately 5 months (April 4 to August 30, 2006), during which teams from the Jet Propulsion Laboratory, Lockheed Martin Space Systems Corporation, and NASA Langley Research Center worked together to monitor and maneuver the spacecraft such that thermal margin on the solar arrays was maintained while schedule margin was upheld to provide a final local mean solar time (LMST) at ascending node of 3:00pm on the final aerobraking orbit. This paper will focus on the contribution of the flight mechanics team at NASA Langley Research Center (LaRC) during the aerobraking phase of the MRO mission.

On-Going Laboratory Efforts to Quantitatively Address Clay Abundance on Mars

NASA Technical Reports Server (NTRS)

Roush, Ted L.; Bishop, Janice L.; Brown, Adrian J.; Blake, David F.; Bristow, Thomas F.

2012-01-01

Data obtained at visible and near-infrared wavelengths by OMEGA on MarsExpress and CRISM on MRO provide definitive evidence for the presence of phyllosilicates and other hydrated phases on Mars. A diverse range of both Fe/Mg-OH and Al-OH-bearing phyllosilicates were identified including the smectites, nontronite, saponite, and montmorillonite. In order to constrain the abundances of these phyllosilicates spectral analyses of mixtures are needed. We report on our on-going effort to enable the quantitative evaluation of the abundance of hydrated-hydroxylated silicates when they are contained in mixtures. We include two component mixtures of hydrated/hydroxylated silicates with each other and with two analogs for other martian materials; pyroxene (enstatite) and palagonitic soil (an alteration product of basaltic glass). For the hydrated-hydroxylated silicates we include saponite and montmorillonite (Mg- and Al- rich smectites). We prepared three size separates of each end-member for study: 20-45, 63-90, and 125-150 µm. As the second phase of our effort we used scanning electron microscopy imaging and x-ray diffraction to characterize the grain size distribution, and structural nature, respectively, of the mixtures. Visible and near-infrared reflectance spectra of the 63-90 micrometers grain size of the mixture samples are shown in Figure 1. We discuss the results of our measurements of these mixtures.

Mars Weather Map, 2008

NASA Image and Video Library

2012-08-04

This global map of Mars was acquired on Oct. 28, 2008, by the Mars Color Imager instrument on NASA MRO. One global map is generated each day to forecast weather conditions for the entry, descent and landing of NASA Curiosity rover.

The Mars Reconnaissance Orbiter Mission: From Launch to the Primary Science Orbit

NASA Technical Reports Server (NTRS)

Johnston, Martin D.; Graf, James E.; Zurek, Richard W.; Eisen, Howard J.; Jai, Benhan; Erickson, James K.

2007-01-01

The Mars Reconnaissance Orbiter (MRO) was launched from Cape Canaveral Air Force Station, Florida, USA, aboard an Atlas V-401 launch vehicle on August 12, 2005. The MRO spacecraft carries a very sophisticated scientific payload. Its primary science mission is to to provide global, regional survey, and targeted observations from a low altitude orbit for one Martian year (687 Earth days). After a seven month interplanetary transit, the spacecraft fired its six main engines and established a highly elliptical capture orbit at Mars. During the post-MOI early check-out period, four instruments acquired engineering-quality data. This was followed by five months of aerobraking operations. After aerobraking was terminated, a series of propulsive maneuvers were used to establish the desired low altitude science orbit. As the spacecraft is readied for its primary science mission, spacecraft and instrument checkout and deployment activities have continued.

Telecommunications Relay Support of the Mars Phoenix Lander Mission

NASA Technical Reports Server (NTRS)

Edwards, Charles D., Jr.; Erickson, James K.; Gladden, Roy E.; Guinn, Joseph R.; Ilott, Peter A.; Jai, Benhan; Johnston, Martin D.; Kornfeld, Richard P.; Martin-Mur, Tomas J.; McSmith, Gaylon W.;

Water Flowing on Mars Today on This Week @NASA – October 2, 2015

NASA Image and Video Library

2015-10-02

A major scientific discovery was announced by NASA at a Sept. 28 news conference. From its vantage point high above the Martian surface, NASA’s Mars Reconnaissance Orbiter (MRO) spacecraft has found the strongest evidence yet, that under certain circumstances, liquid water has been found on Mars. Researchers say an imaging spectrometer on MRO detected signatures of hydrated minerals on slopes where downhill streaks, known as Recurring Slope Lineae (RSL) are seen. In the past, RSL flows have been described as possibly related to liquid water. But the new findings of hydrated minerals is key evidence. Hydrated salts can lower the freezing point of liquid brine – and produce liquid water. Also, Life beyond Earth in the next decade?, “The Martian” screening event, Cargo ship departs space station, New cargo ship delivers to space station, Rare double celestial treat and Espacio a Tierra!

Replacement Sequence of Events Generator

NASA Technical Reports Server (NTRS)

Fisher, Forest; Gladden, Daniel Wenkert Roy; Khanampompan, Teerpat

2008-01-01

The soeWINDOW program automates the generation of an ITAR (International Traffic in Arms Regulations)-compliant sub-RSOE (Replacement Sequence of Events) by extracting a specified temporal window from an RSOE while maintaining page header information. RSOEs contain a significant amount of information that is not ITAR-compliant, yet that foreign partners need to see for command details to their instrument, as well as the surrounding commands that provide context for validation. soeWINDOW can serve as an example of how command support products can be made ITAR-compliant for future missions. This software is a Perl script intended for use in the mission operations UNIX environment. It is designed for use to support the MRO (Mars Reconnaissance Orbiter) instrument team. The tool also provides automated DOM (Distributed Object Manager) storage into the special ITAR-okay DOM collection, and can be used for creating focused RSOEs for product review by any of the MRO teams.

KSC-05PD-0554

NASA Technical Reports Server (NTRS)

2005-01-01

KENNEDY SPACE CENTER, FLA. At the Cape Canaveral Air Force Station Skid Strip, workers inside a Russian Antonov AH-124-100 cargo airplane roll out the booster segment for a Lockheed Martin Atlas V. The Atlas V, designated AV-007, is the launch vehicle for the Mars Reconnaissance Orbiter (MRO). The MRO is designed for a series of global mapping, regional survey and targeted observations from a near-polar, low-altitude Mars orbit. These observations will be unprecedented in terms of the spatial resolution and coverage achieved by the orbiters instruments as they observe the atmosphere and surface of Mars while probing its shallow subsurface as part of a follow the water strategy. The orbiter is undergoing environmental tests in facilities at Lockheed Martin Space Systems in Denver, Colo., and is on schedule for a launch window that begins Aug. 10. Launch will be from Launch Pad 41 at Cape Canaveral Air Force Station in Florida.

Orbit Determination and Navigation Software Testing for the Mars Reconnaissance Orbiter

NASA Technical Reports Server (NTRS)

Pini, Alex

2011-01-01

During the extended science phase of the Mars Reconnaissance Orbiter's lifecycle, the operational duties pertaining to navigation primarily involve orbit determination. The orbit determination process utilizes radiometric tracking data and is used for the prediction and reconstruction of MRO's trajectories. Predictions are done twice per week for ephemeris updates on-board the spacecraft and for planning purposes. Orbit Trim Maneuvers (OTM-s) are also designed using the predicted trajectory. Reconstructions, which incorporate a batch estimator, provide precise information about the spacecraft state to be synchronized with scientific measurements. These tasks were conducted regularly to validate the results obtained by the MRO Navigation Team. Additionally, the team is in the process of converting to newer versions of the navigation software and operating system. The capability to model multiple densities in the Martian atmosphere is also being implemented. However, testing outputs among these different configurations was necessary to ensure compliance to a satisfactory degree.

[Recommendations for the diagnosis and prevention of infectious diseases in pediatric and adolescent refugees in Germany : Statement of the German Society of Pediatric Infectious Diseases, the Society of Tropical Pediatrics and International Child Health, and the Professional Association of Pediatricians].

PubMed

Pfeil, J; Kobbe, R; Trapp, S; Kitz, C; Hufnagel, M

2016-05-01

Child and adolescent refugees in Germany represent a particularly vulnerable social group and treating infectious diseases forms a crucial part of providing their medical care. From an infectious diseases perspective, refugees themselves, as a result of their difficult personal circumstances, are the ones at highest risk. Even in crisis situations, medical practitioners are medically and ethically obliged to provide a high standard of care. The guidelines presented here propose recommendations for diagnosing and preventing infectious diseases among refugees under 18 in Germany. The guidelines are intended to assist in optimizing vaccine protection and treatment of diseases while taking into consideration factors such as refugees' challenging living conditions, cultural differences and potential language barriers.Upon refugees' arrival at the first housing sites, it is recommended that a basic clinical screening (and not just a brief visual inspection) be provided in order to identify and initiate treatment for acute medical problems and potentially contagious diseases (including tuberculosis), as well as to close gaps in vaccination coverage. Documentation of the clinical findings is critical, both to avoid redundant investigations and to optimize individual medical care. For this, an effective communication system must be established.Once refugees have been transferred into their destination community, outpatient and inpatient care providers should collaborate to bring refugees up-to-date with all vaccines recommended by STIKO (German Standing Committee on Vaccination). The same high standard of medical care should be delivered to refugees as would be to the general population. Due to the high prevalence of multi-resistant organisms (MRO) in the refugees' countries of origin, MRO screening is recommended for most patients receiving inpatient care.

AutoGen Version 5.0

NASA Technical Reports Server (NTRS)

Gladden, Roy E.; Khanampornpan, Teerapat; Fisher, Forest W.

2010-01-01

Version 5.0 of the AutoGen software has been released. Previous versions, variously denoted Autogen and autogen, were reported in two articles: Automated Sequence Generation Process and Software (NPO-30746), Software Tech Briefs (Special Supplement to NASA Tech Briefs), September 2007, page 30, and Autogen Version 2.0 (NPO- 41501), NASA Tech Briefs, Vol. 31, No. 10 (October 2007), page 58. To recapitulate: AutoGen (now signifying automatic sequence generation ) automates the generation of sequences of commands in a standard format for uplink to spacecraft. AutoGen requires fewer workers than are needed for older manual sequence-generation processes, and greatly reduces sequence-generation times. The sequences are embodied in spacecraft activity sequence files (SASFs). AutoGen automates generation of SASFs by use of another previously reported program called APGEN. AutoGen encodes knowledge of different mission phases and of how the resultant commands must differ among the phases. AutoGen also provides means for customizing sequences through use of configuration files. The approach followed in developing AutoGen has involved encoding the behaviors of a system into a model and encoding algorithms for context-sensitive customizations of the modeled behaviors. This version of AutoGen addressed the MRO (Mars Reconnaissance Orbiter) primary science phase (PSP) mission phase. On previous Mars missions this phase has more commonly been referred to as mapping phase. This version addressed the unique aspects of sequencing orbital operations and specifically the mission specific adaptation of orbital operations for MRO. This version also includes capabilities for MRO s role in Mars relay support for UHF relay communications with the MER rovers and the Phoenix lander.

Controlling Precision Stepper Motors in Flight Using (Almost) No Parts

NASA Technical Reports Server (NTRS)

Randall, David

2010-01-01

This concept allows control of high-performance stepper motors with minimal parts count and minimal flight software complexity. Although it uses a small number of common flight-qualified parts and simple control algorithms, it is capable enough to meet demanding system requirements. Its programmable nature makes it trivial to implement changes to control algorithms both during integration & test and in flight. Enhancements such as microstepping, half stepping, back-emf compensation, and jitter reduction can be tailored to the requirements of a large variety of stepper motor based applications including filter wheels, focus mechanisms, antenna tracking subsystems, pointing and mobility. The hardware design (using an H-bridge motor controller IC) was adapted from JPL's MER mission, still operating on Mars. This concept has been fully developed and incorporated into the MCS instrument on MRO, currently operating in Mars orbit. It has been incorporated into the filter wheel mechanism and linear stage (focus) mechanism for the AMT instrument. On MCS/MRO, two of these circuits control the elevation and azimuth of the MCS telescope/radiometer assembly, allowing the instrument to continuously monitor the limb of the Martian atmosphere. Implementation on MCS/MRO resulted in a 4:1 reduction in the volume and mass required for the motor driver electronics (100:25 square inches of PCB space), producing a very compact instrument. In fact, all of the electronics for the MCS instrument are packaged within the movable instrument structure. It also saved approximately 3 Watts of power. Most importantly, the design enabled MCS to meet very its stringent maximum allowable torque disturbance requirements.

Curiosity Speaks Volumes

NASA Image and Video Library

2012-08-27

This chart shows increases in the volume of data coming back from NASA Mars Curiosity over recent sols. New capabilities of the Electra relay-radios on MRO and Curiosity have greatly increased the volume of data the rover is sending back from Mars.

Mars Weather Map, Aug. 5

NASA Image and Video Library

2012-08-10

This global map of Mars was acquired on Aug. 5, 2012, by the Mars Color Imager instrument on NASA MRO. One global map is generated each day to forecast weather conditions for the entry, descent and landing of NASA Curiosity rover.

POSSIBLE ESTUARY ASSOCIATED SYNDROME: SYMPTOMS, VISION & TREATMENT.

EPA Science Inventory

Evidence suggests that the estuarine dinoflagellate, Pfiesteria piscicida, and/or morphologically related organisms (Pf-MRO) may release a toxin(s) which kills fish and adversely affects human health. The North Carolina study investigated the potential for persistent health effec...

Channeled Southern Highlands

NASA Image and Video Library

2018-04-30

This enhanced color image from NASA's Mars Reconnaissance Orbiter (MRO) shows the heavily channeled and ancient southern highlands of Mars. The elongated and jagged features are windblown dunes, perhaps hardened and eroded. For more information see https://photojournal.jpl.nasa.gov/catalog/PIA22436

Automatic Command Sequence Generation

NASA Technical Reports Server (NTRS)

Fisher, Forest; Gladded, Roy; Khanampompan, Teerapat

2007-01-01

Automatic Sequence Generator (Autogen) Version 3.0 software automatically generates command sequences for the Mars Reconnaissance Orbiter (MRO) and several other JPL spacecraft operated by the multi-mission support team. Autogen uses standard JPL sequencing tools like APGEN, ASP, SEQGEN, and the DOM database to automate the generation of uplink command products, Spacecraft Command Message Format (SCMF) files, and the corresponding ground command products, DSN Keywords Files (DKF). Autogen supports all the major multi-mission mission phases including the cruise, aerobraking, mapping/science, and relay mission phases. Autogen is a Perl script, which functions within the mission operations UNIX environment. It consists of two parts: a set of model files and the autogen Perl script. Autogen encodes the behaviors of the system into a model and encodes algorithms for context sensitive customizations of the modeled behaviors. The model includes knowledge of different mission phases and how the resultant command products must differ for these phases. The executable software portion of Autogen, automates the setup and use of APGEN for constructing a spacecraft activity sequence file (SASF). The setup includes file retrieval through the DOM (Distributed Object Manager), an object database used to store project files. This step retrieves all the needed input files for generating the command products. Depending on the mission phase, Autogen also uses the ASP (Automated Sequence Processor) and SEQGEN to generate the command product sent to the spacecraft. Autogen also provides the means for customizing sequences through the use of configuration files. By automating the majority of the sequencing generation process, Autogen eliminates many sequence generation errors commonly introduced by manually constructing spacecraft command sequences. Through the layering of commands into the sequence by a series of scheduling algorithms, users are able to rapidly and reliably construct the desired uplink command products. With the aid of Autogen, sequences may be produced in a matter of hours instead of weeks, with a significant reduction in the number of people on the sequence team. As a result, the uplink product generation process is significantly streamlined and mission risk is significantly reduced. Autogen is used for operations of MRO, Mars Global Surveyor (MGS), Mars Exploration Rover (MER), Mars Odyssey, and will be used for operations of Phoenix. Autogen Version 3.0 is the operational version of Autogen including the MRO adaptation for the cruise mission phase, and was also used for development of the aerobraking and mapping mission phases for MRO.

Thermal Analysis Methods for Aerobraking Heating

NASA Technical Reports Server (NTRS)

Amundsen, Ruth M.; Gasbarre, Joseph F.; Dec, John A.

2005-01-01

As NASA begins exploration of other planets, a method of non-propulsively slowing vehicles at the planet, aerobraking, may become a valuable technique for managing vehicle design mass and propellant. An example of this is Mars Reconnaissance Orbiter (MRO), which will launch in late 2005 and reach Mars in March of 2006. In order to save propellant, MRO will use aerobraking to modify the initial orbit at Mars. The spacecraft will dip into the atmosphere briefly on each orbit, and during the drag pass, the atmospheric drag on the spacecraft will slow it, thus lowering the orbit apoapsis. The largest area on the spacecraft, and that most affected by the heat generated during the aerobraking process, is the solar arrays. A thermal analysis of the solar arrays was conducted at NASA Langley, to simulate their performance throughout the entire roughly 6-month period of aerobraking. Several interesting methods were used to make this analysis more rapid and robust. Two separate models were built for this analysis, one in Thermal Desktop for radiation and orbital heating analysis, and one in MSC.Patran for thermal analysis. The results from the radiation model were mapped in an automated fashion to the Patran thermal model that was used to analyze the thermal behavior during the drag pass. A high degree of automation in file manipulation as well as other methods for reducing run time were employed, since toward the end of the aerobraking period the orbit period is short, and in order to support flight operations the runs must be computed rapidly. All heating within the Patran Thermal model was combined in one section of logic, such that data mapped from the radiation model and aeroheating model, as well as skin temperature effects on the aeroheating and surface radiation, could be incorporated easily. This approach calculates the aeroheating at any given node, based on its position and temperature as well as the density and velocity at that trajectory point. Run times on several different processors, computer hard drives, and operating systems (Windows versus Linux) were evaluated.

78 FR 26024 - Combined Notice of Filings #1

Federal Register 2010, 2011, 2012, 2013, 2014

2013-05-03

... reliability filings: Docket Numbers: RR13-5-000. Applicants: North American Electric Reliability Corporation. Description: Petition of the North American Electric Reliability Corporation for Approval of Amendments to Delegation Agreement with Midwest Reliability Organization--Amendments to the MRO Regional Reliability...

Evidence Builds for Old Under-Ice Volcanoes on Mars

NASA Image and Video Library

2016-05-03

These mountains are in a region called Sisyphi Montes. The base image from NASA 2001 Mars Odyssey shows a portion of the region about 130 miles. Red outlines indicate possible subglacial volcanic structures. MRO CRISM data are at upper right.

49 CFR 40.129 - What are the MRO's functions in reviewing laboratory confirmed non-negative drug test results?

Code of Federal Regulations, 2010 CFR

2010-10-01

... scientist signed the form. You are not required to review any other documentation generated by the... of the CCF, containing the certifying scientist's signature. (c) With respect to verified positive...

49 CFR 40.129 - What are the MRO's functions in reviewing laboratory confirmed non-negative drug test results?

Code of Federal Regulations, 2011 CFR

2011-10-01

... scientist signed the form. You are not required to review any other documentation generated by the... of the CCF, containing the certifying scientist's signature. (c) With respect to verified positive...

77 FR 60318 - Procedures for Transportation Workplace Drug and Alcohol Testing Programs: 6-acetylmorphine (6-AM...

Federal Register 2010, 2011, 2012, 2013, 2014

2012-10-03

... final rule to harmonize with many aspects of the revised Department of Health and Human Services (HHS... (ODAPC). After consulting with ODAPC, the MRO would make a verified result determination, keeping in mind...

A synthesis of Martian aqueous mineralogy after 1 Mars year of observations from the Mars Reconnaissance Orbiter

USGS Publications Warehouse

Murchie, S.L.; Mustard, J.F.; Ehlmann, B.L.; Milliken, R.E.; Bishop, J.L.; McKeown, N.K.; Noe Dobrea, E.Z.; Seelos, F.P.; Buczkowski, D.L.; Wiseman, S.M.; Arvidson, R. E.; Wray, J.J.; Swayze, G.; Clark, R.N.; Des Marais, D.J.; McEwen, A.S.; Bibring, J.-P.

2009-01-01

Martian aqueous mineral deposits have been examined and characterized using data acquired during Mars Reconnaissance Orbiter's (MRO) primary science phase, including Compact Reconnaissance Imaging Spectrometer for Mars hyperspectral images covering the 0.4-3.9 ??m wavelength range, coordinated with higher-spatial resolution HiRISE and Context Imager images. MRO's new high-resolution measurements, combined with earlier data from Thermal Emission Spectrometer; Thermal Emission Imaging System; and Observatoire pour la Min??ralogie, L'Eau, les Glaces et l'Activiti?? on Mars Express, indicate that aqueous minerals are both diverse and widespread on the Martian surface. The aqueous minerals occur in 9-10 classes of deposits characterized by distinct mineral assemblages, morphologies, and geologic settings. Phyllosilicates occur in several settings: in compositionally layered blankets hundreds of meters thick, superposed on eroded Noachian terrains; in lower layers of intracrater depositional fans; in layers with potential chlorides in sediments on intercrater plains; and as thousands of deep exposures in craters and escarpments. Carbonate-bearing rocks form a thin unit surrounding the Isidis basin. Hydrated silica occurs with hydrated sulfates in thin stratified deposits surrounding Valles Marineris. Hydrated sulfates also occur together with crystalline ferric minerals in thick, layered deposits in Terra Meridiani and in Valles Marineris and together with kaolinite in deposits that partially infill some highland craters. In this paper we describe each of the classes of deposits, review hypotheses for their origins, identify new questions posed by existing measurements, and consider their implications for ancient habitable environments. On the basis of current data, two to five classes of Noachian-aged deposits containing phyllosilicates and carbonates may have formed in aqueous environments with pH and water activities suitable for life. Copyright 2009 by the American Geophysical Union.

The High Resolution Imaging Science Experiment (HiRISE) during MRO's Primary Science Phase (PSP)

USGS Publications Warehouse

McEwen, A.S.; Banks, M.E.; Baugh, N.; Becker, K.; Boyd, A.; Bergstrom, J.W.; Beyer, R.A.; Bortolini, E.; Bridges, N.T.; Byrne, S.; Castalia, B.; Chuang, F.C.; Crumpler, L.S.; Daubar, I.; Davatzes, A.K.; Deardorff, D.G.; DeJong, A.; Alan, Delamere W.; Dobrea, E.N.; Dundas, C.M.; Eliason, E.M.; Espinoza, Y.; Fennema, A.; Fishbaugh, K.E.; Forrester, T.; Geissler, P.E.; Grant, J. A.; Griffes, J.L.; Grotzinger, J.P.; Gulick, V.C.; Hansen, C.J.; Herkenhoff, K. E.; Heyd, R.; Jaeger, W.L.; Jones, D.; Kanefsky, B.; Keszthelyi, L.; King, R.; Kirk, R.L.; Kolb, K.J.; Lasco, J.; Lefort, A.; Leis, R.; Lewis, K.W.; Martinez-Alonso, S.; Mattson, S.; McArthur, G.; Mellon, M.T.; Metz, J.M.; Milazzo, M.P.; Milliken, R.E.; Motazedian, T.; Okubo, C.H.; Ortiz, A.; Philippoff, A.J.; Plassmann, J.; Polit, A.; Russell, P.S.; Schaller, C.; Searls, M.L.; Spriggs, T.; Squyres, S. W.; Tarr, S.; Thomas, N.; Thomson, B.J.; Tornabene, L.L.; Van Houten, C.; Verba, C.; Weitz, C.M.; Wray, J.J.

2010-01-01

The High Resolution Imaging Science Experiment (HiRISE) on the Mars Reconnaissance Orbiter (MRO) acquired 8 terapixels of data in 9137 images of Mars between October 2006 and December 2008, covering ???0.55% of the surface. Images are typically 5-6 km wide with 3-color coverage over the central 20% of the swath, and their scales usually range from 25 to 60 cm/pixel. Nine hundred and sixty stereo pairs were acquired and more than 50 digital terrain models (DTMs) completed; these data have led to some of the most significant science results. New methods to measure and correct distortions due to pointing jitter facilitate topographic and change-detection studies at sub-meter scales. Recent results address Noachian bedrock stratigraphy, fluvially deposited fans in craters and in or near Valles Marineris, groundwater flow in fractures and porous media, quasi-periodic layering in polar and non-polar deposits, tectonic history of west Candor Chasma, geometry of clay-rich deposits near and within Mawrth Vallis, dynamics of flood lavas in the Cerberus Palus region, evidence for pyroclastic deposits, columnar jointing in lava flows, recent collapse pits, evidence for water in well-preserved impact craters, newly discovered large rayed craters, and glacial and periglacial processes. Of particular interest are ongoing processes such as those driven by the wind, impact cratering, avalanches of dust and/or frost, relatively bright deposits on steep gullied slopes, and the dynamic seasonal processes over polar regions. HiRISE has acquired hundreds of large images of past, present and potential future landing sites and has contributed to scientific and engineering studies of those sites. Warming the focal-plane electronics prior to imaging has mitigated an instrument anomaly that produces bad data under cold operating conditions. ?? 2009 Elsevier Inc.

Preliminary Martian Atmospheric Water Vapour Column Abundances with Mars Climate Sounder

NASA Astrophysics Data System (ADS)

Lolachi, Ramin; Irwin, P. G. J.; Teanby, N.; Calcutt, S.; Howett, C. J. A.; Bowles, N. E.; Taylor, F. W.; Schofield, J. T.; Kleinboehl, A.; McCleese, D. J.

2007-12-01

Mars Climate Sounder (MCS) is an infra-red radiometer on board NASA's Mars Reconnaissance Orbiter (MRO) launched in August 2005 and now orbiting Mars in a near circular polar orbit. MCS has nine spectral channels in the range 0.3-50 µm. Goals of MCS include global characterization of atmospheric temperature, dust and water profiles observing temporal and spatial variation. Using Oxford University's multivariate retrieval algorithm, NEMESIS, we present preliminary determinations of the water vapour column abundance in the Martian atmosphere during the period September-October 2006 (Ls range 111-129°, i.e. northern hemisphere summer). A combination of spectral channels inside and outside the water vapour rotation band (at 50 µm) are used to retrieve the column abundances mainly using nadir observations (as aerosol opacity is less important relative to water vapour opacity in nadir viewing geometry). We then compare these column abundances to earlier results from the Viking Orbiter Mars Atmospheric Water Detectors (MAWD) and the Thermal Emission Spectrometer (TES) on Mars Global Surveyor.

49 CFR 40.327 - When must the MRO report medical information gathered in the verification process?

Code of Federal Regulations, 2010 CFR

2010-10-01

... results and medical information you learned as part of the verification process to third parties without... the course of an accident investigation. (c) If the law of a foreign country (e.g., Canada) prohibits...

49 CFR 40.167 - How are MRO reports of drug results transmitted to the employer?

Code of Federal Regulations, 2010 CFR

2010-10-01

... immediate reporting. Follow up your phone call with appropriate documentation (see § 40.163). (2) You are... (see § 40.163(b) and (c)). (2) Negative results reported electronically (i.e., computer data file) do...

49 CFR 40.139 - On what basis does the MRO verify test results for codeine and morphine?

Code of Federal Regulations, 2010 CFR

2010-10-01

... PROCEDURES FOR TRANSPORTATION WORKPLACE DRUG AND ALCOHOL TESTING PROGRAMS Medical Review Officers and the... the case of other drugs (see § 40.137). Consumption of food products (e.g., poppy seeds) must not be...

49 CFR 40.139 - On what basis does the MRO verify test results for codeine and morphine?

Code of Federal Regulations, 2011 CFR

2011-10-01

... PROCEDURES FOR TRANSPORTATION WORKPLACE DRUG AND ALCOHOL TESTING PROGRAMS Medical Review Officers and the... the case of other drugs (see § 40.137). Consumption of food products (e.g., poppy seeds) must not be...

10 CFR 26.37 - Protection of information.

Code of Federal Regulations, 2012 CFR

2012-01-01

... NUCLEAR REGULATORY COMMISSION FITNESS FOR DUTY PROGRAMS Program Elements § 26.37 Protection of information... program, including determinations of fitness, FFD program audits, or some human resources functions; (6... test results, MRO reviews, determinations of fitness, and management actions pertaining to the subject...

10 CFR 26.37 - Protection of information.

Code of Federal Regulations, 2014 CFR

2014-01-01

... NUCLEAR REGULATORY COMMISSION FITNESS FOR DUTY PROGRAMS Program Elements § 26.37 Protection of information... program, including determinations of fitness, FFD program audits, or some human resources functions; (6... test results, MRO reviews, determinations of fitness, and management actions pertaining to the subject...

10 CFR 26.37 - Protection of information.

Code of Federal Regulations, 2013 CFR

2013-01-01

... NUCLEAR REGULATORY COMMISSION FITNESS FOR DUTY PROGRAMS Program Elements § 26.37 Protection of information... program, including determinations of fitness, FFD program audits, or some human resources functions; (6... test results, MRO reviews, determinations of fitness, and management actions pertaining to the subject...

10 CFR 26.37 - Protection of information.

Code of Federal Regulations, 2010 CFR

2010-01-01

... NUCLEAR REGULATORY COMMISSION FITNESS FOR DUTY PROGRAMS Program Elements § 26.37 Protection of information... program, including determinations of fitness, FFD program audits, or some human resources functions; (6... test results, MRO reviews, determinations of fitness, and management actions pertaining to the subject...

10 CFR 26.37 - Protection of information.

Code of Federal Regulations, 2011 CFR

2011-01-01

... NUCLEAR REGULATORY COMMISSION FITNESS FOR DUTY PROGRAMS Program Elements § 26.37 Protection of information... program, including determinations of fitness, FFD program audits, or some human resources functions; (6... test results, MRO reviews, determinations of fitness, and management actions pertaining to the subject...

Mars-Flyby Comet in False Color

NASA Image and Video Library

2014-11-07

This frame from a movie sequence of images from NASA Mars Reconnaissance Orbiter MRO shows comet C/2013 A1 Siding Spring before and after its close pass by Mars in October 2014. False color enhances subtle variations in brightness in the comet coma.

Clays of Ladon Basin

NASA Image and Video Library

2018-01-23

Ladon Basin was a large impact structure that was filled in by the deposits from Ladon Valles, a major ancient river on Mars as seen in this image from NASA's Mars Reconnaissance Orbiter (MRO). These wet sediments were altered into minerals such as various clay minerals. Clays imply chemistry that may have been favorable for life on ancient Mars, if anything lived there, so this could be a good spot for future exploration by rovers and perhaps return of samples to Earth. The map is projected here at a scale of 50 centimeters (19.7 inches) per pixel. [The original image scale is 52.1 centimeters (20.5 inches) per pixel (with 2 x 2 binning); objects on the order of 156 centimeters (61.4 inches) across are resolved.] North is up. https://photojournal.jpl.nasa.gov/catalog/PIA22183

Hexagons in Icy Terrain

NASA Image and Video Library

2018-01-23

Ground cemented by ice cover the high latitudes of Mars, much as they do on Earth's cold climates. A common landform that occurs in icy terrain are polygons as shown in this image from NASA's Mars Reconnaissance Orbiter (MRO). Polygonal patterns form by winter cooling and contraction cracking of the frozen ground. Over time these thin cracks develop and coalesce into a honeycomb network, with a few meters spacing between neighboring cracks. Shallow troughs mark the locations of the underground cracks, which are clearly visible form orbit. The map is projected here at a scale of 25 centimeters (9.8 inches) per pixel. [The original image scale is 30.2 centimeters (11.9 inches) per pixel (with 1 x 1 binning); objects on the order of 91 centimeters (35.8 inches) across are resolved.] North is up. https://photojournal.jpl.nasa.gov/catalog/PIA22180

The resolved nucleus of Comet Siding Spring (C/2013 A1) in MRO HiRISE images

NASA Astrophysics Data System (ADS)

Farnham, Tony; Kelley, Michael S.; Bodewits, Dennis; Bauer, James M.

2017-10-01

Comet Siding Spring (C/2013 A1) passed within 140,000 km of Mars on 19 Oct 2014. The MRO spacecraft, in orbit around Mars, used its HiRISE camera to monitor the comet during the encounter, obtaining the first resolved images of the nucleus of a dynamically new comet.MRO observed Siding Spring from 60 hr before, to 15 hr after close approach, obtaining 122 images in three different color filters. Close approach images, with a spatial scale as small as 138 m/pix, reveal an elongated crescent that changes shape over the course of the sequence, indicating that we are seeing a ~1 km non-spherical body from different viewpoints as the comet rapidly sweeps past. To better constrain the characteristics of the nucleus, we are performing detailed analyses, including modeling of the inner coma to separate its flux contribution from that of the nucleus. In conjunction with the coma removal, we will model the nucleus as a prolate/triaxial ellipsoid and, combined with the known illumination and viewing conditions, will use the changing aspect in the images to constrain the size, shape, orientation, albedo and possibly the phase dependence of the nucleus.In addition to the close approach observations, the images before and after close approach capture the coma structure and brightness. The photometric lightcurve from these images shows variability with an 8.1 hr period, which is presumed to be the rotational modulation of the coma activity. The observed morphology changes as well, promising to provide a measure of the nucleus' spin axis orientation.We will report on the results from our analyses, and provide the first direct measurements of the nucleus of a dynamically new comet.

Supporting parent-child interactions: music therapy as an intervention for promoting mutually responsive orientation.

PubMed

Pasiali, Varvara

2012-01-01

Music therapists working with families address relationship and interpersonal communication issues. Few controlled studies exist in the literature but a growing body of documented practice is emerging. This study makes a contribution by documenting how music therapy supports mutuality and reciprocity in parent-child interactions. This study investigated mutually responsive orientation (MRO) behaviors of young children (aged 3-5) and their family members during music therapy. Participants were 4 families with low income and history of maternal depression as common risk factors. Data were collected by videotaping sessions, creating field notes and analytic memos, conducting parent interviews and reviewing parent journals. A cross-case analysis using MRO theory as a conceptualizing framework was used for the purpose of data reduction. Greeting and farewell rituals, and the flexibility of music-based therapeutic applications facilitated development of coordinated routines. Therapist's actions (e.g., encouraging and modeling musical interactions) and bidirectional parent-child actions (e.g., joint attention, turn-taking, being playful) facilitated harmonious communication. Behaviors promoting mutual cooperation were evident when adults attempted to scaffold a child's participation or when children sought comfort from parents, engaged in social referencing and made requests that shaped the direction of the session. The novelty of musical tasks captivated attention, increasing impulse inhibition. Parent actions (e.g., finding delight in watching their child participate, acting silly) and parent-child interactions (e.g., play exploration, shared excitement, cuddling) contributed to positive emotional ambiance. Music therapy assisted development of MRO within parent-child dyads by providing opportunities to rehearse adaptive ways of connecting with each other. Results of this study may serve as an archetypal model guiding clinical treatment planning.

POSSIBLE EFFECTS OF CHRONIC EXPOSURE TO ENVIRONMENTAL AIRBORNE MANGANESE ON NEUROLOGICAL FUNCTION IN CHILDREN.

EPA Science Inventory

Evidence suggests that the estuarine dinoflagellate, Pfiesteria piscicida, and/or morphologically related organisms (Pf-MRO) may release a toxin(s) which kills fish and adversely affects human health. The North Carolina study investigated the potential for persistent health effec...

Mars Global Coverage by Context Camera on MRO

NASA Image and Video Library

2017-03-29

In early 2017, after more than a decade of observing Mars, the Context Camera (CTX) on NASA's Mars Reconnaissance Orbiter (MRO) surpassed 99 percent coverage of the entire planet. This mosaic shows that global coverage. No other camera has ever imaged so much of Mars in such high resolution. The mosaic offers a resolution that enables zooming in for more detail of any region of Mars. It is still far from the full resolution of individual CTX observations, which can reveal the shapes of features smaller than the size of a tennis court. As of March 2017, the Context Camera has taken about 90,000 images since the spacecraft began examining Mars from orbit in late 2006. In addition to covering 99.1 percent of the surface of Mars at least once, this camera has observed more than 60 percent of Mars more than once, checking for changes over time and providing stereo pairs for 3-D modeling of the surface. http://photojournal.jpl.nasa.gov/catalog/PIA21488

Three-and-a-Half Mars Years of Surface Albedo Changes Observed by the Mars Reconnaissance Orbiter MARCI Investigation

NASA Astrophysics Data System (ADS)

Wellington, D. F.; Bell, J. F.

2013-12-01

The Mars Color Imager (MARCI) wide-angle camera aboard the Mars Reconnaissance Orbiter (MRO) has gathered over three-and-a-half Mars years' worth of observations at approximately 1 km/pixel resolution. The MARCI instrument has seven bands in the ultraviolet, visible, and near-infrared, five of which (the longer wavelength 420, 550, 600, 650, and 750 nm bands) are amenable to observations of surface albedo (the two short-wave ultraviolet bands are primarily intended for ozone measurements). MRO's near-polar orbit and MARCI's wide angle field-of-view (180°) allows it to make almost daily observations of large portions of the planet. As a global multi-year dataset, the MARCI observations are well-suited to examining surface albedo changes on both local and regional scales, including investigating any repeatability and seasonality in such changes. Because Mars displays considerable interannual variability, long-term continuous observations such as MARCI's are necessary in order to adequately describe and distinguish typical surface variance from unusual and longer-term secular changes. We have produced time-lapse animations of sections of the Martian surface from calibrated, map-projected, and mosaicked MARCI observations, altogether comprising the surface of Mars within +/- 65 degrees of the equator. These animations show many albedo changes that have occurred on the surface since 2006, including changes in traditionally variable regions such as Syrtis Major, Alcyonius, Hyblaeus, and Cerberus, as well as a dramatic brightening of Propontis and variations in the appearance and orientation of mesoscale linear streaks in Amazonis. Many regions show alternating periods of dust deposition and removal that, while not producing a persistent change in the surface albedo, nevertheless yield information on the local near-surface conditions that drive these variations. We present a descriptive classification of the types and locations of surface albedo changes observed on Mars over the course of the MRO mission (2006-present), including the nature, seasonal timing, and extent of such changes. The surface albedo features are shown to vary quasi-seasonally, with changes sometimes in concurrence with local or regional dust storms. Dust storm events typically brighten the surface and are followed by months of subsequent darkening, though occasionally an associated darkening or brightening may persist. Changes in the boundaries of albedo features usually occur in discrete episodes, followed by periods of stasis, and often affect regions with historical precedent for variability. These observations and analyses can yield information on near-surface wind conditions, which can be used to test existing atmospheric circulation and climate models. Furthermore, changes in surface albedo markings can provide constraints on surface albedo as an important input parameter to global and mesoscale climate models.

10 CFR 26.169 - Reporting Results.

Code of Federal Regulations, 2012 CFR

2012-01-01

... request. The laboratory shall routinely provide quantitative values for confirmatory opiate test results... requested quantitative values for the test result. (3) For a specimen that has an adulterated or substituted... of the standard curve, the laboratory may report to the MRO that the quantitative value “exceeds the...

10 CFR 26.169 - Reporting Results.

Code of Federal Regulations, 2013 CFR

2013-01-01

... request. The laboratory shall routinely provide quantitative values for confirmatory opiate test results... requested quantitative values for the test result. (3) For a specimen that has an adulterated or substituted... of the standard curve, the laboratory may report to the MRO that the quantitative value “exceeds the...

10 CFR 26.169 - Reporting Results.

Code of Federal Regulations, 2010 CFR

2010-01-01

... request. The laboratory shall routinely provide quantitative values for confirmatory opiate test results... requested quantitative values for the test result. (3) For a specimen that has an adulterated or substituted... of the standard curve, the laboratory may report to the MRO that the quantitative value “exceeds the...

10 CFR 26.169 - Reporting Results.

Code of Federal Regulations, 2011 CFR

2011-01-01

... request. The laboratory shall routinely provide quantitative values for confirmatory opiate test results... requested quantitative values for the test result. (3) For a specimen that has an adulterated or substituted... of the standard curve, the laboratory may report to the MRO that the quantitative value “exceeds the...

10 CFR 26.169 - Reporting Results.

Code of Federal Regulations, 2014 CFR

2014-01-01

... request. The laboratory shall routinely provide quantitative values for confirmatory opiate test results... requested quantitative values for the test result. (3) For a specimen that has an adulterated or substituted... of the standard curve, the laboratory may report to the MRO that the quantitative value “exceeds the...

49 CFR 40.17 - Is an employer responsible for obtaining information from its service agents?

Code of Federal Regulations, 2011 CFR

2011-10-01

... you. For example, suppose an applicant for a safety-sensitive job takes a pre-employment drug test, but there is a significant delay in your receipt of the test result from an MRO or C/TPA. You must not...

49 CFR 40.17 - Is an employer responsible for obtaining information from its service agents?

Code of Federal Regulations, 2013 CFR

2013-10-01

... you. For example, suppose an applicant for a safety-sensitive job takes a pre-employment drug test, but there is a significant delay in your receipt of the test result from an MRO or C/TPA. You must not...

A First Step Toward Understanding Nucleation Processes: in situ High-Temperature X-ray Diffraction and Absorption Investigations

NASA Astrophysics Data System (ADS)

Strukelj, E.; Neuville, D. R.; Cochain, B.; Hennet, L.; Thiaudière, D.; Guillot, B.; Roskosz, M.; Comte, M.; Richet, P.

2009-05-01

Nucleation is the first step of the transition between the amorphous and crystalline states and thus plays a key role in Earth and Materials sciences whenever crystallization takes place. In spite of its considerable importance in igneous petrology and industrial applications (ceramics, glass-ceramics, etc.), nucleation remains known poorly because of the difficulties of investigating the structural rearrangements that take place at a nm scale when an ordered atomic packing begins to develop in a melt. In addition, the structure of amorphous phases is not only difficult to determine, but the wealth of information available for glasses is not necessarily applicable to nucleation because of the existence of temperature-induced structural changes in melts. In view of the basic geological and industrial importance of the SiO2-Al2O3-CaO system, we have investigated a calcium aluminosilicate whose crystallization has already been studied. And because elements such as Ti or Zr can promote rapid nucleation, information can be gained about the structural changes they induce by probing specifically their own environment. In this work we have thus performed a high-temperature study of the very first steps of crystallization in a calcium aluminosilicate with 7 mol percent ZrO2 by X-ray absorption measurements at the Zr K-edge et 1873 K on the homogenous melt and 1173 K on a nucleating supercooled liquid. To complement these results with information on medium range order (MRO) X-Ray diffraction experiments have also been performed under the same conditions. As a reference, the glass has been investigated by both techniques at room temperature.

10 CFR 26.183 - Medical review officer.

Code of Federal Regulations, 2012 CFR

2012-01-01

... construed as a potential conflict of interest. Examples of relationships between laboratories and MROs that... licensee's or other entity's discretion, dilute test result. This action may include, but is not limited to... physiology of the donor. (2) The MRO may only consider the results of tests of specimens that are collected...

10 CFR 26.183 - Medical review officer.

Code of Federal Regulations, 2013 CFR

2013-01-01

... construed as a potential conflict of interest. Examples of relationships between laboratories and MROs that... licensee's or other entity's discretion, dilute test result. This action may include, but is not limited to... physiology of the donor. (2) The MRO may only consider the results of tests of specimens that are collected...

10 CFR 26.183 - Medical review officer.

Code of Federal Regulations, 2014 CFR

2014-01-01

... construed as a potential conflict of interest. Examples of relationships between laboratories and MROs that... licensee's or other entity's discretion, dilute test result. This action may include, but is not limited to... physiology of the donor. (2) The MRO may only consider the results of tests of specimens that are collected...

Atmospheric Modeling of the Martian Polar Regions: One Mars Year of CRISM EPF Observations of the South Pole

NASA Astrophysics Data System (ADS)

Brown, A. J.; Wolff, M. J.

2009-03-01

We have used CRISM Emission Phase Function gimballed observations to investigate atmospheric dust/ice opacity and surface albedo in the south polar region for the first Mars year of MRO operations. This covers the MY28 "dust event" and cap recession.

49 CFR 40.121 - Who is qualified to act as an MRO?

Code of Federal Regulations, 2010 CFR

2010-10-01

... physician (Doctor of Medicine or Osteopathy). If you are a licensed physician in any U.S., Canadian, or... states or provinces without becoming licensed to practice medicine in the other jurisdictions. (b) Basic... clinical experience in controlled substances abuse disorders, including detailed knowledge of alternative...

49 CFR 40.121 - Who is qualified to act as an MRO?

Code of Federal Regulations, 2012 CFR

2012-10-01

... physician (Doctor of Medicine or Osteopathy). If you are a licensed physician in any U.S., Canadian, or... states or provinces without becoming licensed to practice medicine in the other jurisdictions. (b) Basic... clinical experience in controlled substances abuse disorders, including detailed knowledge of alternative...

49 CFR 40.121 - Who is qualified to act as an MRO?

Code of Federal Regulations, 2013 CFR

2013-10-01

... physician (Doctor of Medicine or Osteopathy). If you are a licensed physician in any U.S., Canadian, or... states or provinces without becoming licensed to practice medicine in the other jurisdictions. (b) Basic... clinical experience in controlled substances abuse disorders, including detailed knowledge of alternative...

49 CFR 40.121 - Who is qualified to act as an MRO?

Code of Federal Regulations, 2014 CFR

2014-10-01

... physician (Doctor of Medicine or Osteopathy). If you are a licensed physician in any U.S., Canadian, or... states or provinces without becoming licensed to practice medicine in the other jurisdictions. (b) Basic... clinical experience in controlled substances abuse disorders, including detailed knowledge of alternative...

49 CFR 40.121 - Who is qualified to act as an MRO?

Code of Federal Regulations, 2011 CFR

2011-10-01

... physician (Doctor of Medicine or Osteopathy). If you are a licensed physician in any U.S., Canadian, or... states or provinces without becoming licensed to practice medicine in the other jurisdictions. (b) Basic... clinical experience in controlled substances abuse disorders, including detailed knowledge of alternative...

The Role of Intraverbal Exchanges in Assessing Parent-Child Relationships

ERIC Educational Resources Information Center

Gokhan, Nurper; Dennis, Tracy A.; Crossman, Angela M.

2012-01-01

The present investigation evaluated the role of verbal exchanges between parent and child (intraverbal exchanges) in relation to two contemporary measurements of the parent-child relationship, mutual responsive orientation (MRO) and synchrony. Data were collected from 30 mother-preschool child dyads (19 girls, 11 boys) during a laboratory…

CHRONIC LYME DISEASE: SYMPTOMS, VISION AND A NEW APPROACH TO TREATMENT BASED ON A THEORY OF NEUROTOXIN-MEDIATED ILLNESS.

EPA Science Inventory

Evidence suggests that the estuarine dinoflagellate, Pfiesteria piscicida, and/or morphologically related organisms (Pf-MRO) may release a toxin(s) which kills fish and adversely affects human health. The North Carolina study investigated the potential for persistent health effec...

49 CFR 199.109 - Review of drug testing results.

Code of Federal Regulations, 2013 CFR

2013-10-01

... 49 Transportation 3 2013-10-01 2013-10-01 false Review of drug testing results. 199.109 Section... MATERIALS SAFETY ADMINISTRATION, DEPARTMENT OF TRANSPORTATION (CONTINUED) PIPELINE SAFETY DRUG AND ALCOHOL TESTING Drug Testing § 199.109 Review of drug testing results. (a) MRO appointment. Each operator shall...

49 CFR 199.109 - Review of drug testing results.

Code of Federal Regulations, 2010 CFR

2010-10-01

... 49 Transportation 3 2010-10-01 2010-10-01 false Review of drug testing results. 199.109 Section... MATERIALS SAFETY ADMINISTRATION, DEPARTMENT OF TRANSPORTATION (CONTINUED) PIPELINE SAFETY DRUG AND ALCOHOL TESTING Drug Testing § 199.109 Review of drug testing results. (a) MRO appointment. Each operator shall...

49 CFR 199.109 - Review of drug testing results.

Code of Federal Regulations, 2012 CFR

2012-10-01

... 49 Transportation 3 2012-10-01 2012-10-01 false Review of drug testing results. 199.109 Section... MATERIALS SAFETY ADMINISTRATION, DEPARTMENT OF TRANSPORTATION (CONTINUED) PIPELINE SAFETY DRUG AND ALCOHOL TESTING Drug Testing § 199.109 Review of drug testing results. (a) MRO appointment. Each operator shall...

49 CFR 199.109 - Review of drug testing results.

Code of Federal Regulations, 2011 CFR

2011-10-01

... 49 Transportation 3 2011-10-01 2011-10-01 false Review of drug testing results. 199.109 Section... MATERIALS SAFETY ADMINISTRATION, DEPARTMENT OF TRANSPORTATION (CONTINUED) PIPELINE SAFETY DRUG AND ALCOHOL TESTING Drug Testing § 199.109 Review of drug testing results. (a) MRO appointment. Each operator shall...

49 CFR 199.109 - Review of drug testing results.

Code of Federal Regulations, 2014 CFR

2014-10-01

... 49 Transportation 3 2014-10-01 2014-10-01 false Review of drug testing results. 199.109 Section... MATERIALS SAFETY ADMINISTRATION, DEPARTMENT OF TRANSPORTATION (CONTINUED) PIPELINE SAFETY DRUG AND ALCOHOL TESTING Drug Testing § 199.109 Review of drug testing results. (a) MRO appointment. Each operator shall...

10 CFR 26.4 - FFD program applicability to categories of individuals.

Code of Federal Regulations, 2011 CFR

2011-01-01

....4 Section 26.4 Energy NUCLEAR REGULATORY COMMISSION FITNESS FOR DUTY PROGRAMS Administrative... entity, monitors the fitness of the individuals specified in paragraph (f) of this section; (4) Witnesses... not limited to the MRO; (2) All persons who make determinations of fitness; (3) All persons who make...

10 CFR 26.183 - Medical review officer.

Code of Federal Regulations, 2010 CFR

2010-01-01

... 10 Energy 1 2010-01-01 2010-01-01 false Medical review officer. 26.183 Section 26.183 Energy NUCLEAR REGULATORY COMMISSION FITNESS FOR DUTY PROGRAMS Determining Fitness-for-Duty Policy Violations and Determining Fitness § 26.183 Medical review officer. (a) Qualifications. The MRO shall be knowledgeable of...

10 CFR 26.183 - Medical review officer.

Code of Federal Regulations, 2011 CFR

2011-01-01

... 10 Energy 1 2011-01-01 2011-01-01 false Medical review officer. 26.183 Section 26.183 Energy NUCLEAR REGULATORY COMMISSION FITNESS FOR DUTY PROGRAMS Determining Fitness-for-Duty Policy Violations and Determining Fitness § 26.183 Medical review officer. (a) Qualifications. The MRO shall be knowledgeable of...

10 CFR 26.185 - Determining a fitness-for-duty policy violation.

Code of Federal Regulations, 2012 CFR

2012-01-01

... was marijuana and the confirmatory assay for delta-9-tetrahydrocannabinol-9-carboxylic acid yields a positive result, the MRO shall determine whether the confirmatory test result indicates further marijuana... delta-9-tetrahydrocannabinol-9-carboxylic acid that would be expected if no further marijuana use had...

10 CFR 26.185 - Determining a fitness-for-duty policy violation.

Code of Federal Regulations, 2013 CFR

2013-01-01

... was marijuana and the confirmatory assay for delta-9-tetrahydrocannabinol-9-carboxylic acid yields a positive result, the MRO shall determine whether the confirmatory test result indicates further marijuana... delta-9-tetrahydrocannabinol-9-carboxylic acid that would be expected if no further marijuana use had...

10 CFR 26.185 - Determining a fitness-for-duty policy violation.

Code of Federal Regulations, 2014 CFR

2014-01-01

... was marijuana and the confirmatory assay for delta-9-tetrahydrocannabinol-9-carboxylic acid yields a positive result, the MRO shall determine whether the confirmatory test result indicates further marijuana... delta-9-tetrahydrocannabinol-9-carboxylic acid that would be expected if no further marijuana use had...

Interannual Similarity in the Martian Atmosphere During the Dust Storm Season

NASA Technical Reports Server (NTRS)

Kass, D. M.; Kleinboehl, A.; McCleese, D. J.; Schofield, J. T.; Smith, M. D.

2016-01-01

We find that during the dusty season on Mars (southern spring and summer) of years without a global dust storm there are three large regional-scale dust storms. The storms are labeled A, B, and C in seasonal order. This classification is based on examining the zonal mean 50 Pa (approximately 25 km) daytime temperature retrievals from TES/MGS and MCS/MRO over 6 Mars Years. Regional-scale storms are defined as events where the temperature exceeds 200 K. Examining the MCS dust field at 50 Pa indicates that warming in the Southern Hemisphere is dominated by direct heating, while northern high latitude warming is a dynamical response. A storms are springtime planet encircling Southern Hemisphere events. B storms are southern polar events that begin near perihelion and last through the solstice. C storms are southern summertime events starting well after the end of the B storm. C storms show the most interannual variability.

Interannual similarity in the Martian atmosphere during the dust storm season

NASA Astrophysics Data System (ADS)

Kass, D. M.; Kleinböhl, A.; McCleese, D. J.; Schofield, J. T.; Smith, M. D.

2016-06-01

We find that during the dusty season on Mars (southern spring and summer) of years without a global dust storm there are three large regional-scale dust storms. The storms are labeled A, B, and C in seasonal order. This classification is based on examining the zonal mean 50 Pa (˜25 km) daytime temperature retrievals from TES/MGS and MCS/MRO over 6 Mars Years. Regional-scale storms are defined as events where the temperature exceeds 200 K. Examining the MCS dust field at 50 Pa indicates that warming in the Southern Hemisphere is dominated by direct heating, while northern high latitude warming is a dynamical response. A storms are springtime planet encircling Southern Hemisphere events. B storms are southern polar events that begin near perihelion and last through the solstice. C storms are southern summertime events starting well after the end of the B storm. C storms show the most interannual variability.

Chemical and Mineralogical Characterization of Acid-Sulfate Alteration of Basaltic Material on Mauna Kea Volcano, Hawaii: Jarosite and Hydrated Halloysite

NASA Technical Reports Server (NTRS)

Graff, Trevor G.; Morris, R. V.; Archilles C. N.; Agresti, D. G.; Ming, D. W.; Hamilton, J. C.; Mertzman, S. A.; Smith, J.

2012-01-01

Sulfates have been identified on the martian surface during robotic surface exploration and by orbital remote sensing. Measurements at Meridiani Planum (MP) by the Alpha-Particle X-ray Spectrometer (APXS) and Mossbauer (MB) instruments on the Mars Exploration Rover Opportunity document the presence of a ubiquitous sulfate-rich outcrop (20-40% SO3) that has jarosite as an anhydrous Fe3+-sulfate [1- 3]. The presence of jarosite implies a highly acidic (pH <3) formation environment [4]. Jarosite and other sulfate minerals, including kieserite, gypsum, and alunite have also been identified in several locations in orbital remote sensing data from the MEx OMEGA and MRO CRISM instruments [e.g. 5-8]. Acid sulfate weathering of basaltic materials is an obvious pathway for formation of sulfate-bearing phases on Mars [e.g. 4, 9, 10]. In order to constrain acid-sulfate pathways on Mars, we are studying the mineralogical and chemical manifestations of acid-sulfate alteration of basaltic compositions in terrestrial environments. We have previously shown that acidsulfate alteration of tephra under hydrothermal conditions on the Puu Poliahu cone (summit region of Mauna Kea volcano, Hawaii) resulted in jarosite and alunite as sulfate-bearing alteration products [11-14]. Other, more soluble, sulfates may have formed, but were leached away by rain and melting snow. Acidsulfate processes on Puu Poliahu also formed hematite spherules similar (except in size) to the hematite spherules observed at MP as an alteration product [14]. Phyllosilicates, usually smectite }minor kaolinite are also present as alteration products [13]. We discuss here an occurrence of acid-sulfate alteration on Mauna Kea Volcano (Hawaii). We report VNIR spectra (0.35-2.5 microns ASD spectrometer), Mossbauer spectra (MER-like ESPI backscatter spectrometer), powder XRD (PANalytical), and major element chemical compositions (XRF with LOI and Fe redox) for comparison to similar data acquired or to be acquired by MRO-CRISM and MEx OMEGA, MERMB, MSL-CheMin, and MER and MSL APXS, respectively.

Comparative analysis between Payen and Daedalia Planum lava fields

NASA Astrophysics Data System (ADS)

Giacomini, Lorenza; Massironi, Matteo; Pasquarè, Giorgio; Carli, Cristian; Martellato, Elena; Frigeri, Alessandro; Cremonese, Gabriele; Bistacchi, Andrea; Federico, Costanzo

The Payen volcanic complex is a large Quaternary fissural structure belonging to the back-arc extensional area of the Andes in the Mendoza Province (Argentina). From the eastern portion of this volcanic structure huge pahoehoe lava flows were emitted, extending more than 180 km from the feeding vents. These huge flows propagated over the nearly flat surface of the Pampean foreland (ca 0.3° slope). The very low viscosity of the olivine basalt lavas, coupled with the inflation process are the most probable explanation for their considerable length. In an inflation process a thin viscoelastic crust, produced at an early stage, is later inflated by the underlying fluid core, which remains hot and fluid thanks to the thermal-shield effect of the crust. The inflation shows some typical morphological fingerprints like tumuli, lava lobes, lava rises and lava ridges. In order to compare the morphology of the Argentinean Payen flows with lava flows on Mars, MOLA, THEMIS, MOC, MRO/HIRISE, and MEX/OMEGA data have been analysed, providing a multi-scale characterisation of Martian flows. Mars Global Surveyor/MOLA data were used to investigate the topographic environment over which flows propagated on Mars in order to detect very low angle slopes where possibly inflation processes could have developed. Then Mars Odyssey/THEMIS and Mars Global Surveyor's MOC data were used to detect Martian lava flows with inflation "fingerprints", whereas OMEGA data were used to obtain some inferences about their composition. Finally the MRO/HIRISE images recently acquired, can provide further details and constraints on surface morphologies and lava fronts. All these data were used to analyze Daedalia Planum lava field, at about 300 km southwest of Arsia Mons, and clear morphological similarities with the longest flows of the Payen lava fields were found. These striking morphological analogies suggest that inflation process is quite common also for the Daedalia field. This is also supported by simple calculation of effusion rates for not inflated lava flows foreseeing for the Daedalia Planum long lava flows improbable huge rates. Consequently lower effusion rates coupled with very efficient spreading process are more likely. Nonetheless the comparison of typology vs frequency and dimension of inflation related features of Payen and Daedalia Planum field suggest that even the effusion rates responsible of inflated flows on Mars are by far higher than the one on the Earth.

49 CFR 40.141 - How does the MRO obtain information for the verification decision?

Code of Federal Regulations, 2013 CFR

2013-10-01

... PROCEDURES FOR TRANSPORTATION WORKPLACE DRUG AND ALCOHOL TESTING PROGRAMS Medical Review Officers and the... must conduct a medical interview. You must review the employee's medical history and any other relevant... evaluation by you or another physician. (b) If the employee asserts that the presence of a drug or drug...

49 CFR 40.141 - How does the MRO obtain information for the verification decision?

Code of Federal Regulations, 2011 CFR

2011-10-01

... PROCEDURES FOR TRANSPORTATION WORKPLACE DRUG AND ALCOHOL TESTING PROGRAMS Medical Review Officers and the... must conduct a medical interview. You must review the employee's medical history and any other relevant... evaluation by you or another physician. (b) If the employee asserts that the presence of a drug or drug...

49 CFR 40.141 - How does the MRO obtain information for the verification decision?

Code of Federal Regulations, 2014 CFR

2014-10-01

... PROCEDURES FOR TRANSPORTATION WORKPLACE DRUG AND ALCOHOL TESTING PROGRAMS Medical Review Officers and the... must conduct a medical interview. You must review the employee's medical history and any other relevant... evaluation by you or another physician. (b) If the employee asserts that the presence of a drug or drug...

49 CFR 40.141 - How does the MRO obtain information for the verification decision?

Code of Federal Regulations, 2012 CFR

2012-10-01

... PROCEDURES FOR TRANSPORTATION WORKPLACE DRUG AND ALCOHOL TESTING PROGRAMS Medical Review Officers and the... must conduct a medical interview. You must review the employee's medical history and any other relevant... evaluation by you or another physician. (b) If the employee asserts that the presence of a drug or drug...

49 CFR 40.125 - What relationship may an MRO have with a laboratory?

Code of Federal Regulations, 2010 CFR

2010-10-01

... TRANSPORTATION WORKPLACE DRUG AND ALCOHOL TESTING PROGRAMS Medical Review Officers and the Verification Process... relationship with an employer's laboratory that creates a conflict of interest or the appearance of a conflict... that the Department views as creating a conflict of interest or the appearance of such a conflict, see...

49 CFR 40.141 - How does the MRO obtain information for the verification decision?

Code of Federal Regulations, 2010 CFR

2010-10-01

... PROCEDURES FOR TRANSPORTATION WORKPLACE DRUG AND ALCOHOL TESTING PROGRAMS Medical Review Officers and the... must conduct a medical interview. You must review the employee's medical history and any other relevant... evaluation by you or another physician. (b) If the employee asserts that the presence of a drug or drug...

49 CFR 40.21 - May an employer stand down an employee before the MRO has completed the verification process?

Code of Federal Regulations, 2010 CFR

2010-10-01

... which DOT agencies regulate your employees. (2) Your proposed written company policy concerning stand... temporary removal from performance of safety-sensitive functions becomes available, directly or indirectly... a covered employee will be subject to stand-down only with respect to the actual performance of...

Pathways to Conscience: Early Mother-Child Mutually Responsive Orientation and Children's Moral Emotion, Conduct, and Cognition

ERIC Educational Resources Information Center

Kochanska, Grazyna; Forman, David R.; Aksan, Nazan; Dunbar, Stephen B.

2005-01-01

Background: Associations between early mother-child mutually responsive orientation (MRO) and children's conscience have been previously established, but the mechanisms accounting for those links are not understood. We examined three such mediational mechanisms: (a) the child's enhanced enjoyment of interactions with the mother, (b) increased…

10 CFR 26.159 - Assuring specimen security, chain of custody, and preservation.

Code of Federal Regulations, 2010 CFR

2010-01-01

... licensee testing facility has retained the specimen in Bottle B, the licensee testing facility shall... the licensee testing facility. (2) The following are exclusive grounds requiring the MRO to cancel the... or legal challenge until they are no longer needed. (j) The laboratory shall discard a valid specimen...

Evidences of early aqueous Mars: Implications on the origin of branched valleys in the Ius Chasma, Mars

NASA Astrophysics Data System (ADS)

Martha, Tapas R.; Jain, Nirmala; Vamshi, Gasiganti T.; Vinod Kumar, K.

2017-11-01

This study shows results of morphological and spectroscopic analyses of Ius Chasma and its southern branched valleys using Orbiter datasets such as Mars Reconnaissance Orbiter (MRO)-Compact Reconnaissance Imaging Spectrometer for Mars (CRISM), High Resolution Imaging Science Experiment (MRO-HiRISE) and digital terrain model (HRSC-DTM). Result of the spectral analysis reveals presence of hydrated minerals such as opal, nontronite and vermiculite in the floor and wall rock areas Ius Chasma indicating alteration of parent rock in an water rich environment of early Mars. Topographic gradient and morphological evidences such as V-shaped valleys with theatre shaped stubby channels, dendritic drainage and river piracy indicate that these valleys were initially developed by surface runoff due to episodic floods and further expanded due to groundwater sapping controlled by faults and fractures. Minerals formed by aqueous alteration during valley formation and their intricate association with different morphological domains suggest that surface runoff played a key role in the development of branched valleys south of Ius Chasma on Mars.

Adaptive Local Spatiotemporal Features from RGB-D Data for One-Shot Learning Gesture Recognition

PubMed Central

Lin, Jia; Ruan, Xiaogang; Yu, Naigong; Yang, Yee-Hong

2016-01-01

Noise and constant empirical motion constraints affect the extraction of distinctive spatiotemporal features from one or a few samples per gesture class. To tackle these problems, an adaptive local spatiotemporal feature (ALSTF) using fused RGB-D data is proposed. First, motion regions of interest (MRoIs) are adaptively extracted using grayscale and depth velocity variance information to greatly reduce the impact of noise. Then, corners are used as keypoints if their depth, and velocities of grayscale and of depth meet several adaptive local constraints in each MRoI. With further filtering of noise, an accurate and sufficient number of keypoints is obtained within the desired moving body parts (MBPs). Finally, four kinds of multiple descriptors are calculated and combined in extended gradient and motion spaces to represent the appearance and motion features of gestures. The experimental results on the ChaLearn gesture, CAD-60 and MSRDailyActivity3D datasets demonstrate that the proposed feature achieves higher performance compared with published state-of-the-art approaches under the one-shot learning setting and comparable accuracy under the leave-one-out cross validation. PMID:27999337

Adaptive Local Spatiotemporal Features from RGB-D Data for One-Shot Learning Gesture Recognition.

PubMed

Lin, Jia; Ruan, Xiaogang; Yu, Naigong; Yang, Yee-Hong

2016-12-17

Noise and constant empirical motion constraints affect the extraction of distinctive spatiotemporal features from one or a few samples per gesture class. To tackle these problems, an adaptive local spatiotemporal feature (ALSTF) using fused RGB-D data is proposed. First, motion regions of interest (MRoIs) are adaptively extracted using grayscale and depth velocity variance information to greatly reduce the impact of noise. Then, corners are used as keypoints if their depth, and velocities of grayscale and of depth meet several adaptive local constraints in each MRoI. With further filtering of noise, an accurate and sufficient number of keypoints is obtained within the desired moving body parts (MBPs). Finally, four kinds of multiple descriptors are calculated and combined in extended gradient and motion spaces to represent the appearance and motion features of gestures. The experimental results on the ChaLearn gesture, CAD-60 and MSRDailyActivity3D datasets demonstrate that the proposed feature achieves higher performance compared with published state-of-the-art approaches under the one-shot learning setting and comparable accuracy under the leave-one-out cross validation.

Planet Four: Terrains - Pointing the Highest Resolution Camera Ever Sent to Mars with the Help of 10,000 Earthlings

NASA Astrophysics Data System (ADS)

Schwamb, Megan Elizabeth; Aye, Klaus-Michael; Portyankina, Ganna; Hansen, Candice; Lintott, Chris; Carstensen, Brian; Duca, Simone; Parrish, Michael; Miller, Grant

2016-10-01

Mars' south pole is sculpted by the never-ending cycle of freezing and thawing of exposed carbon dioxide ice. In the summer, carbon dioxide jets loft dust and dirt through cracks in the thawing carbon dioxide ice sheet to the surface where winds blow the material into the hundreds of thousands of dark fans observed from orbit. Built with the Zooniverse's project builder platform (http://www.zooniverse.org/lab), Planet Four: Terrains (http://terrains.planetfour.org/) is a citizen science project enlisting the general public to review mid-resolution Mars Reconnaissance Orbiter (MRO) Context Camera subimages to identify the channels and pits (dubbed araneiforms) carved during the gas jet formation process, as well as other surface features including craters and carbon dioxide ice pits dubbed 'swiss cheese terrain.'One of the key goals of the project was to identify jet locations on the Martian south pole and create a set of new targets regions for further detailed monitoring over the next southern Spring and Summer with MRO's HiRISE (High Resolution Imaging Experiment) camera. HiRISE has ~20x higher resolution than CTX, while CTX on the other hand covers more area in a single observation. In less than a year, thanks to the effort of over 10,000 volunteers worldwide, Planet Four: Terrains was able to categorize ~20,000 subimages from 90 CTX images, and identify 20+ regions selected for further HiRISE monitoring to explore the on-going seasonal processes.We present an overview of Planet Four: Terrains including the project's goals and public engagement. We will also present a summary of the over 20 target regions selected for HiRISE monitoring.Acknowledgements: This work uses data generated via the Zooniverse.org platform, development of which was supported by a Global Impact Award from Google, and by the Alfred P. Sloan Foundation. We also thank theHiRISE and MRO Teams for their help in scheduling and acquiring ourrequested observations.

Effect of Lactobacillus plantarum isolated from digestive tract of wild shrimp on growth and survival of white shrimp (Litopenaeus vannamei) challenged with Vibrio harveyi.

PubMed

Kongnum, Khanitta; Hongpattarakere, Tipparat

2012-01-01

Two hundred and two strains of lactic acid bacteria (LAB) isolated from digestive tracts of cultivated and wild adult shrimp, including Litopenaeus vannamei, Metapenaeus brevicornis and Penaeus merguiensis were selected based on their antibacterial activity against Vibrio harveyi. LAB strain of MRO3.12 exhibiting highest reduction of V. harveyi was identified as Lactobacillus plantarum MRO3.12 based on the nucleotide sequence of its 16S rDNA, which showed 99% (780/786 bp) homology to L. plantarum strain L5 (GenBank accession number DQ 239698.1). Co-cultivation of V. harveyi and L. plantarum MRO3.12 showed complete reduction of V. harveyi at 24 h under aerobic and anaerobic conditions, whereas L. plantarum increased from 5.29 to 9.47 log CFU ml(-1). After 6-week feeding trial with L. plantarum supplemented diet, white shrimp (L. vannamei) exhibited significant differences (p < 0.05) in relative growth rate (% RGR), feed conversion ratio (FCR) and survival compared to the control group fed with non-supplemented diet. LAB-fed group showed 98.89% survival, whereas only 68.89% survival was observed in the control group. LAB from the digestive tract of probiotic-fed shrimp showed higher level of 5.0 ± 0.14 log CFU/g than the non-supplemented ones (3.34 ± 0.21 log CFU/g). However, total bacterial and non-fermenting vibrios counts decreased in shrimps fed on L. plantarum. Ten days after infection with V. harveyi (5.3-5.5 log CFU ml(-1)), significant survival (p < 0.05) of 77% was observed in LAB supplemented shrimp, while only 67% survival was observed in the control. Copyright © 2011 Elsevier Ltd. All rights reserved.

Identification of hydrated silicate minerals on Mars using MRO-CRISM: Geologic context near Nili Fossae and implications for aqueous alteration

USGS Publications Warehouse

Ehlmann, B.L.; Mustard, J.F.; Swayze, G.A.; Clark, R.N.; Bishop, J.L.; Poulet, F.; Des Marais, D.J.; Roach, L.H.; Milliken, R.E.; Wray, J.J.; Barnouin-Jha, O.; Murchie, S.L.

2009-01-01

The Noachian terrain west of the Isidis basin hosts a diverse collection of alteration minerals in rocks comprising varied geomorphic units within a 100,000 km2 region in and near the Nili Fossae. Prior investigations in this region by the Observatoire pour l'Min??ralogie, l'Eau, les Glaces, et l'Activit?? (OMEGA) instrument on Mars Express revealed large exposures of both mafic minerals and iron magnesium phyllosilicates in stratigraphic context. Expanding on the discoveries of OMEGA, the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) aboard the Mars Reconnaissance Orbiter (MRO) has found more spatially widespread and mineralogically diverse alteration minerals than previously realized, which represent multiple aqueous environments. Using CRISM near-infrared spectral data, we detail the basis for identification of iron and magnesium smectites (including both nontronite and more Mg-rich varieties), chlorite, prehnite, serpentine, kaolinite, potassium mica (illite or muscovite), hydrated (opaline) silica, the sodium zeolite analcime, and magnesium carbonate. The detection of serpentine and analcime on Mars is reported here for the first time. We detail the geomorphic context of these minerals using data from high-resolution imagers onboard MRO in conjunction with CRISM. We find that the distribution of alteration minerals is not homogeneous; rather, they occur in provinces with distinctive assemblages of alteration minerals. Key findings are (1) a distinctive stratigraphy, in and around the Nili Fossae, of kaolinite and magnesium carbonate in bedrock units always overlying Fe/Mg smectites and (2) evidence for mineral phases and assemblages indicative of low-grade metamorphic or hydrothermal aqueous alteration in cratered terrains. The alteration minerals around the Nili Fossae are more typical of those resulting from neutral to alkaline conditions rather than acidic conditions, which appear to have dominated much of Mars. Moreover, the mineralogic diversity and geologic context of alteration minerals found in the region around the Nili Fossae indicates several episodes of aqueous activity in multiple distinct environments. Copyright 2009 by the American Geophysical Union.

Mechanical Design of NESSI: New Mexico Tech Extrasolar Spectroscopic Survey Instrument

NASA Technical Reports Server (NTRS)

Santoro, Fernando G.; Olivares, Andres M.; Salcido, Christopher D.; Jimenez, Stephen R.; Jurgenson, Colby A.; Hrynevych, Michael A.; Creech-Eakman, Michelle J.; Boston, Penny J.; Schmidt, Luke M.; Bloemhard, Heather;

Mars Atmospheric CO2 Condensation Above the North and South Poles as Revealed by Radio Occultation, Climate Sounder, and Laser Ranging Observations

NASA Technical Reports Server (NTRS)

Hu, Renyu; Cahoy, Kerri; Zuber, Maria T.

2012-01-01

We study the condensation of CO2 in Mars atmosphere using temperature profilesretrieved from radio occultation measurements from Mars Global Surveyor (MGS) as wellas the climate sounding instrument onboard the Mars Reconnaissance Orbiter (MRO),and detection of reflective clouds by the MGS Mars Orbiter Laser Altimeter (MOLA). Wefind 11 events in 1999 where MGS temperature profiles indicate CO2 condensation andMOLA simultaneously detects reflective clouds. We thus provide causal evidence thatMOLA non-ground returns are associated with CO2 condensation, which strongly indicatestheir nature being CO2 clouds. The MGS and MRO temperature profiles together revealthe seasonal expansion and shrinking of the area and the vertical extent of atmosphericsaturation. The occurrence rate of atmospheric saturation is maximized at high latitudes inthe middle of winter. The atmospheric saturation in the northern polar region exhibits moreintense seasonal variation than in the southern polar region. In particular, a shrinking ofsaturation area and thickness from LS 270 to 300 in 2007 is found; this is probablyrelated to a planet-encircling dust storm. Furthermore, we integrate the condensation areaand the condensation occurrence rate to estimate cumulative masses of CO2 condensatesdeposited onto the northern and southern seasonal polar caps. The precipitation flux isapproximated by the particle settling flux which is estimated using the impulse responses ofMOLA filter channels. With our approach, the total atmospheric condensation mass canbe estimated from these observational data sets with average particle size as the onlyfree parameter. By comparison with the seasonal polar cap masses inferred from thetime-varying gravity of Mars, our estimates indicate that the average condensate particleradius is 822 mm in the northern hemisphere and 413 mm in the southern hemisphere.Our multi-instrument data analysis provides new constraints on modeling the global climateof Mars.

CRISM Multispectral and Hyperspectral Mapping Data - A Global Data Set for Hydrated Mineral Mapping

NASA Astrophysics Data System (ADS)

Seelos, F. P.; Hash, C. D.; Murchie, S. L.; Lim, H.

2017-12-01

The Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) is a visible through short-wave infrared hyperspectral imaging spectrometer (VNIR S-detector: 364-1055 nm; IR L-detector: 1001-3936 nm; 6.55 nm sampling) that has been in operation on the Mars Reconnaissance Orbiter (MRO) since 2006. Over the course of the MRO mission, CRISM has acquired 290,000 individual mapping observation segments (mapping strips) with a variety of observing modes and data characteristics (VNIR/IR; 100/200 m/pxl; multi-/hyper-spectral band selection) over a wide range of observing conditions (atmospheric state, observation geometry, instrument state). CRISM mapping data coverage density varies primarily with latitude and secondarily due to seasonal and operational considerations. The aggregate global IR mapping data coverage currently stands at 85% ( 80% at the equator with 40% repeat sampling), which is sufficient spatial sampling density to support the assembly of empirically optimized radiometrically consistent mapping mosaic products. The CRISM project has defined a number of mapping mosaic data products (e.g. Multispectral Reduced Data Record (MRDR) map tiles) with varying degrees of observation-specific processing and correction applied prior to mosaic assembly. A commonality among the mosaic products is the presence of inter-observation radiometric discrepancies which are traceable to variable observation circumstances or associated atmospheric/photometric correction residuals. The empirical approach to radiometric reconciliation leverages inter-observation spatial overlaps and proximal relationships to construct a graph that encodes the mosaic structure and radiometric discrepancies. The graph theory abstraction allows the underling structure of the msaic to be evaluated and the corresponding optimization problem configured so it is well-posed. Linear and non-linear least squares optimization is then employed to derive a set of observation- and wavelength- specific model parameters for a series of transform functions that minimize the total radiometric discrepancy across the mosaic. This empirical approach to CRISM data radiometric reconciliation and the utility of the resulting mapping data mosaic products for hydrated mineral mapping will be presented.

Mars atmospheric CO2 condensation above the north and south poles as revealed by radio occultation, climate sounder, and laser ranging observations

NASA Astrophysics Data System (ADS)

Hu, Renyu; Cahoy, Kerri; Zuber, Maria T.

2012-07-01

We study the condensation of CO2 in Mars' atmosphere using temperature profiles retrieved from radio occultation measurements from Mars Global Surveyor (MGS) as well as the climate sounding instrument onboard the Mars Reconnaissance Orbiter (MRO), and detection of reflective clouds by the MGS Mars Orbiter Laser Altimeter (MOLA). We find 11 events in 1999 where MGS temperature profiles indicate CO2 condensation and MOLA simultaneously detects reflective clouds. We thus provide causal evidence that MOLA non-ground returns are associated with CO2 condensation, which strongly indicates their nature being CO2 clouds. The MGS and MRO temperature profiles together reveal the seasonal expansion and shrinking of the area and the vertical extent of atmospheric saturation. The occurrence rate of atmospheric saturation is maximized at high latitudes in the middle of winter. The atmospheric saturation in the northern polar region exhibits more intense seasonal variation than in the southern polar region. In particular, a shrinking of saturation area and thickness from LS ˜ 270° to ˜300° in 2007 is found; this is probably related to a planet-encircling dust storm. Furthermore, we integrate the condensation area and the condensation occurrence rate to estimate cumulative masses of CO2 condensates deposited onto the northern and southern seasonal polar caps. The precipitation flux is approximated by the particle settling flux which is estimated using the impulse responses of MOLA filter channels. With our approach, the total atmospheric condensation mass can be estimated from these observational data sets with average particle size as the only free parameter. By comparison with the seasonal polar cap masses inferred from the time-varying gravity of Mars, our estimates indicate that the average condensate particle radius is 8-22 μm in the northern hemisphere and 4-13 μm in the southern hemisphere. Our multi-instrument data analysis provides new constraints on modeling the global climate of Mars.

Spectral Evidence for Hydrated Salts in Seasonal Brine Flows on Mars

NASA Astrophysics Data System (ADS)

Ojha, L.

2015-12-01

Recurring Slope Lineae (RSL) are narrow, low-reflectance features forming on present-day Mars that have been hypothesized to be due to the transient flow of liquid water. RSL extend incrementally downslope on steep, warm slopes, fade when inactive, and reappear annually over multiple Mars years as monitored by the HiRISE camera on board the Mars Reconnaissance Orbiter (MRO). In the southern mid-latitudes of Mars, RSL are observed to form most commonly on equator facing slopes, but in equatorial regions RSL often "follow the sun", forming and growing on slopes that receive the greatest insolation during a particular season. The temperature on slopes where RSL are active typically exceeds 250 K and often but not always exceeds 273 K, although sub-surface temperatures would be colder. These characteristics suggest a possible role of salts in lowering the freezing point of water, allowing briny solutions to flow. Confirmation of this wet origin hypothesis for RSL would require either (i) detection of liquid water absorptions on the surface, or (ii) detection of hydrated salts precipitated from that water. The mineralogical composition of RSL and their surroundings can be investigated using orbital data acquired by the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) also on board MRO, which acquires spectral cubes with 544 spectral channels in the visible to near-infrared range of ~0.36 μm to 3.92 μm [13], within which both liquid water and hydrated salts have diagnostic absorption bands at ~1.4 μm, ~1.9 μm, ~3.0 μm. Additionally, hydrated salts may have combination of overtones at other wavelengths from 1.7 μm to 2.4 μm. We present results from examination of individual pixels containing RSL at four different sites that confirm the hypothesis that RSL are due to present-day activity of briny water.

Ultrahigh resolution topographic mapping of Mars with MRO HiRISE stereo images: Meter-scale slopes of candidate Phoenix landing sites

USGS Publications Warehouse

Kirk, R.L.; Howington-Kraus, E.; Rosiek, M.R.; Anderson, J.A.; Archinal, B.A.; Becker, K.J.; Cook, D.A.; Galuszka, D.M.; Geissler, P.E.; Hare, T.M.; Holmberg, I.M.; Keszthelyi, L.P.; Redding, B.L.; Delamere, W.A.; Gallagher, D.; Chapel, J.D.; Eliason, E.M.; King, R.; McEwen, A.S.

2009-01-01

The objectives of this paper are twofold: first, to report our estimates of the meter-to-decameter-scale topography and slopes of candidate landing sites for the Phoenix mission, based on analysis of Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) images with a typical pixel scale of 3 m and Mars Reconnaissance Orbiter (MRO) High Resolution Imaging Science Experiment (HiRISE) images at 0.3 m pixel-1 and, second, to document in detail the geometric calibration, software, and procedures on which the photogrammetric analysis of HiRISE data is based. A combination of optical design modeling, laboratory observations, star images, and Mars images form the basis for software in the U.S. Geological Survey Integrated Software for Imagers and Spectrometers (ISIS) 3 system that corrects the images for a variety of distortions with single-pixel or subpixel accuracy. Corrected images are analyzed in the commercial photogrammetric software SOCET SET (??BAE Systems), yielding digital topographic models (DTMs) with a grid spacing of 1 m (3-4 pixels) that require minimal interactive editing. Photoclinometry yields DTMs with single-pixel grid spacing. Slopes from MOC and HiRISE are comparable throughout the latitude zone of interest and compare favorably with those where past missions have landed successfully; only the Mars Exploration Rover (MER) B site in Meridiani Planum is smoother. MOC results at multiple locations have root-mean-square (RMS) bidirectional slopes of 0.8-4.5?? at baselines of 3-10 m. HiRISE stereopairs (one per final candidate site and one in the former site) yield 1.8-2.8?? slopes at 1-m baseline. Slopes at 1 m from photoclinometry are also in the range 2-3?? after correction for image blur. Slopes exceeding the 16?? Phoenix safety limit are extremely rare. Copyright 2008 by the American Geophysical Union.

2013: A Year in Space

NASA Image and Video Library

2014-01-24

2013 was a big year for Ames Research Center's space exploration programs, including several new launches, and continuing a long history of cutting-edge innovations. Projects listed include: LADEE, IRIS, Kepler, PhoneSat, TechEdSat, NLAS, K10 Rover, Seedling Growth-1, Cell Biology Tech Demonstration, ADEPT, Spaceloft 7 and 8, CheMin, MSL, MRO, Bion-M1, Pioneer 11.

49 CFR 40.139 - On what basis does the MRO verify test results involving opiates?

Code of Federal Regulations, 2014 CFR

2014-10-01

... FOR TRANSPORTATION WORKPLACE DRUG AND ALCOHOL TESTING PROGRAMS Medical Review Officers and the... legitimate medical explanation for the presence of the drug or drug metabolite in his or her system, as in the case of other drugs (see § 40.137). Consumption of food products (e.g., poppy seeds) must not be...

49 CFR 40.139 - On what basis does the MRO verify test results involving opiates?

Code of Federal Regulations, 2012 CFR

2012-10-01

... FOR TRANSPORTATION WORKPLACE DRUG AND ALCOHOL TESTING PROGRAMS Medical Review Officers and the... legitimate medical explanation for the presence of the drug or drug metabolite in his or her system, as in the case of other drugs (see § 40.137). Consumption of food products (e.g., poppy seeds) must not be...

49 CFR 40.139 - On what basis does the MRO verify test results involving opiates?

Code of Federal Regulations, 2013 CFR

2013-10-01

... FOR TRANSPORTATION WORKPLACE DRUG AND ALCOHOL TESTING PROGRAMS Medical Review Officers and the... legitimate medical explanation for the presence of the drug or drug metabolite in his or her system, as in the case of other drugs (see § 40.137). Consumption of food products (e.g., poppy seeds) must not be...

49 CFR Appendix D to Part 40 - Report Format: Split Specimen Failure To Reconfirm

Code of Federal Regulations, 2010 CFR

2010-10-01

.... The following items are required on each report: 1. MRO name, address, phone number, and fax number. 2. Collection site name, address, and phone number. 3. Date of collection. 4. Specimen I.D. number. 5. Laboratory accession number. 6. Primary specimen laboratory name, address, and phone number. 7. Date result...

49 CFR 40.329 - What information must laboratories, MROs, and other service agents release to employees?

Code of Federal Regulations, 2010 CFR

2010-10-01

... other service agents release to employees? 40.329 Section 40.329 Transportation Office of the Secretary... Confidentiality and Release of Information § 40.329 What information must laboratories, MROs, and other service agents release to employees? (a) As an MRO or service agent you must provide, within 10 business days of...

Inventory Management

NASA Technical Reports Server (NTRS)

1983-01-01

Known as MRO for Maintenance, Repair and Operating supplies, Tropicana Products, Inc.'s automated inventory management system is an adaptation of the Shuttle Inventory Management System (SIMS) developed by NASA to assure adequate supply of every item used in support of the Space Shuttle. The Tropicana version monitors inventory control, purchasing receiving and departmental costs for eight major areas of the company's operation.

76 FR 21889 - Nebraska Public Power District; Southwest Power Pool Regional Entity; Notice of Extension of Time

Federal Register 2010, 2011, 2012, 2013, 2014

2011-04-19

... Time On April 8, 2011, the Midwest Reliability Organization (MRO) filed a motion for an extension of time to file comments in connection with the March 18, 2011 Petition of Nebraska Public Power District... may oppose both petitions. Upon consideration, notice is hereby given that an extension of time for...

A Winter's View of a Gullied Crater

NASA Image and Video Library

2017-04-18

This image from NASA's Mars Reconnaissance Orbiter (MRO) shows the location with the most impressive known gully activity in Mars' northern hemisphere. Gullies are active in the winter due to carbon dioxide frost, but northern winters are shorter and warmer than southern winters, so there is less frost and less gully activity.. https://photojournal.jpl.nasa.gov/catalog/PIA21593

49 CFR Appendix D to Part 40 - Report Format: Split Specimen Failure To Reconfirm

Code of Federal Regulations, 2014 CFR

2014-10-01

.... The following items are required on each report: 1. MRO name, address, phone number, and fax number. 2. Collection site name, address, and phone number. 3. Date of collection. 4. Specimen I.D. number. 5. Laboratory accession number. 6. Primary specimen laboratory name, address, and phone number. 7. Date result...

49 CFR Appendix D to Part 40 - Report Format: Split Specimen Failure To Reconfirm

Code of Federal Regulations, 2013 CFR

2013-10-01

.... The following items are required on each report: 1. MRO name, address, phone number, and fax number. 2. Collection site name, address, and phone number. 3. Date of collection. 4. Specimen I.D. number. 5. Laboratory accession number. 6. Primary specimen laboratory name, address, and phone number. 7. Date result...

49 CFR Appendix D to Part 40 - Report Format: Split Specimen Failure To Reconfirm

Code of Federal Regulations, 2012 CFR

2012-10-01

.... The following items are required on each report: 1. MRO name, address, phone number, and fax number. 2. Collection site name, address, and phone number. 3. Date of collection. 4. Specimen I.D. number. 5. Laboratory accession number. 6. Primary specimen laboratory name, address, and phone number. 7. Date result...

49 CFR 40.145 - On what basis does the MRO verify test results involving adulteration or substitution?

Code of Federal Regulations, 2014 CFR

2014-10-01

... the adulterant found by the laboratory entered the specimen through physiological means. (2) To meet... produce or could have produced urine through physiological means, meeting the creatinine concentration criterion of less than 2 mg/dL and the specific gravity criteria of less than or equal to 1.0010 or greater...

Dunes in Nectaris Montes

NASA Image and Video Library

2018-05-14

This image from NASA's Mars Reconnaissance Orbiter (MRO) shows some of these on the slopes of Nectaris Montes within Coprates Chasma. Sand dunes in Valles Marineris can be impressive in size, with steep slopes that seem to climb and descend. The brighter bedforms are inactive while the bigger dunes move over the landscape, burying and exhuming the surface. https://photojournal.jpl.nasa.gov/catalog/PIA22455

49 CFR 40.160 - What does the MRO do when a valid test result cannot be produced and a negative result is required?

Code of Federal Regulations, 2010 CFR

2010-10-01

... determine if there is clinical evidence that the individual is currently an illicit drug user. You must make... Secretary of Transportation PROCEDURES FOR TRANSPORTATION WORKPLACE DRUG AND ALCOHOL TESTING PROGRAMS...., blood) as part of the medically appropriate procedures in determining clinical evidence of drug use. (d...

Transcriptional regulators transforming growth factor-beta 1 and estrogen-related receptor-alpha identified as putative mediators of calf rumen epithelial tissue development and function during weaning

USDA-ARS?s Scientific Manuscript database

Molecular mechanisms controlling rumen epithelial development at weaning remain largely unknown. To identify gene networks and regulatory factors responsive to concentrate versus forage feeding at weaning, Holstein bull calves (n = 18) were fed commercial milk replacer only (MRO) until 42 d of age. ...

49 CFR 40.149 - May the MRO change a verified drug test result?

Code of Federal Regulations, 2011 CFR

2011-10-01

... identifying (e.g., a paperwork mistake) or testing (e.g., a false positive or negative) the employee's primary... result only in the following situations: (1) When you have reopened a verification that was done without... laboratory notifies you that it mixed up the two test results, and X was really negative and Y was really...

49 CFR 40.149 - May the MRO change a verified drug test result?

Code of Federal Regulations, 2014 CFR

2014-10-01

... identifying (e.g., a paperwork mistake) or testing (e.g., a false positive or negative) the employee's primary... result only in the following situations: (1) When you have reopened a verification that was done without... laboratory notifies you that it mixed up the two test results, and X was really negative and Y was really...

49 CFR 40.149 - May the MRO change a verified drug test result?

Code of Federal Regulations, 2012 CFR

2012-10-01

... identifying (e.g., a paperwork mistake) or testing (e.g., a false positive or negative) the employee's primary... result only in the following situations: (1) When you have reopened a verification that was done without... laboratory notifies you that it mixed up the two test results, and X was really negative and Y was really...

49 CFR 40.149 - May the MRO change a verified drug test result?

Code of Federal Regulations, 2013 CFR

2013-10-01

... identifying (e.g., a paperwork mistake) or testing (e.g., a false positive or negative) the employee's primary... result only in the following situations: (1) When you have reopened a verification that was done without... laboratory notifies you that it mixed up the two test results, and X was really negative and Y was really...

49 CFR 40.163 - How does the MRO report drug test results?

Code of Federal Regulations, 2014 CFR

2014-10-01

... tests, the drug(s)/metabolite(s) for which the test was positive; (8) For cancelled tests, the reason... for this purpose, you must provide a written report (e.g., a letter) for each test result. This report... for the test, if indicated on the CCF (e.g., random, post-accident); (4) Date of the collection; (5...

Ionic Transport Through Metal-Rich Organic Coatings

DTIC Science & Technology

2016-08-19

COVERED October 2013-Septermber 2015 4. TITLE AND SUBTITLE Ionic Transport Through Metal-Rich Organic Coatings 5a. CONTRACT NUMBER 5b. GRANT...NOTES 14. ABSTRACT Organic coatings are commonly used on aircraft and in the automotive industry to protect against corrosive environments. Although...volume (MPV) percent, solvent polarity, and resin molecular weight impact corrosion protection of metal-rich organic (MRO) coatings. Following design

Ionic Transport Through Metal-Rich Organic Coatings

DTIC Science & Technology

2016-08-19

COVERED October 2013-Septermber 2015 4. TITLE AND SUBTITLE Ionic Transport Through Metal-Rich Organic Coatings 5a. CONTRACT NUMBER 5b. GRANT...14. ABSTRACT Organic coatings are commonly used on aircraft and in the automotive industry to protect against corrosive environments. Although...volume (MPV) percent, solvent polarity, and resin molecular weight impact corrosion protection of metal-rich organic (MRO) coatings. Following design of

Retrospective study of urinalysis for dl-amphetamine and dl-methamphetamine analysis under current Department of Defense guidelines.

PubMed

Shippee, R L; Kippenberger, D J

2000-09-01

Under current Department of Defense (DOD) directive, the laboratories certified to conduct urinalyis testing in support of the DOD Drug Deterrence Program are required to conduct dl-isomer analysis on all specimens that confirm at a concentration greater than 500 ng/mL methamphetamine (METH). Although the same cutoff concentration is required for amphetamine (AMP) reporting, there is no requirement for dl-isomer analysis of AMP-positive specimens. Of the 894,823 specimens screened by the Army Drug Testing Laboratory at Ft. Meade, MD during a 19-month period, 339 confirmed positive for METH. From this positive population, seven specimens failed to confirm at or above the DOD cutoff of > 20% d-isomer. One of the seven specimens contained 534 ng/mL l-AMP and was reported positive for AMP. Although 100% of the AMP was the l-isomer, under current DOD directive, this information was not passed along to the Medical Review Officers (MRO) to assist them during the interview process. Although this situation appears to be a rare event, consideration should be given to requiring dl-isomer analysis of AMP-positive specimens and forwarding this information to the MRO.

Visible light optical coherence tomography measures retinal oxygen metabolic response to systemic oxygenation

PubMed Central

Yi, Ji; Liu, Wenzhong; Chen, Siyu; Backman, Vadim; Sheibani, Nader; Sorenson, Christine M.; Fawzi, Amani A.; Linsenmeier, Robert A.; Zhang, Hao F.

2015-01-01

The lack of capability to quantify oxygen metabolism noninvasively impedes both fundamental investigation and clinical diagnosis of a wide spectrum of diseases including all the major blinding diseases such as age-related macular degeneration, diabetic retinopathy, and glaucoma. Using visible light optical coherence tomography (vis-OCT), we demonstrated accurate and robust measurement of retinal oxygen metabolic rate (rMRO2) noninvasively in rat eyes. We continuously monitored the regulatory response of oxygen consumption to a progressive hypoxic challenge. We found that both oxygen delivery, and rMRO2 increased from the highly regulated retinal circulation (RC) under hypoxia, by 0.28 ± 0.08 μL min−1 (p < 0.001), and 0.20 ± 0.04 μL min−1 (p < 0.001) per 100 mmHg systemic pO2 reduction, respectively. The increased oxygen extraction compensated for the deficient oxygen supply from the poorly regulated choroidal circulation. Results from an oxygen diffusion model based on previous oxygen electrode measurements corroborated our in vivo observations. We believe that vis-OCT has the potential to reveal the fundamental role of oxygen metabolism in various retinal diseases. PMID:26658555

15O PET Measurement of Blood Flow and Oxygen Consumption in Cold-Activated Human Brown Fat

PubMed Central

Muzik, Otto; Mangner, Thomas J.; Leonard, William R.; Kumar, Ajay; Janisse, James; Granneman, James G.

2013-01-01

Although it has been believed that brown adipose tissue (BAT) depots disappear shortly after the perinatal period in humans, PET imaging using the glucose analog 18F-FDG has shown unequivocally the existence of functional BAT in adult humans, suggesting that many humans retain some functional BAT past infancy. The objective of this study was to determine to what extent BAT thermogenesis is activated in adults during cold stress and to establish the relationship between BAT oxidative metabolism and 18F-FDG tracer uptake. Methods Twenty-five healthy adults (15 women and 10 men; mean age ± SD, 30 ± 7 y) underwent triple-oxygen scans (H215O, C15O, and 15O2) as well as measurements of daily energy expenditure (DEE; kcal/d) both at rest and after exposure to mild cold (15.5°C [60°F]) using indirect calorimetry. The subjects were divided into 2 groups (high BAT and low BAT) based on the presence or absence of 18F-FDG tracer uptake (standardized uptake value [SUV] > 2) in cervical–supraclavicular BAT. Blood flow and oxygen extraction fraction (OEF) were calculated from dynamic PET scans at the location of BAT, muscle, and white adipose tissue. Regional blood oxygen saturation was determined by near-infrared spectroscopy. The total energy expenditure during rest and mild cold stress was measured by indirect calorimetry. Tissue-level metabolic rate of oxygen (MRO2) in BAT was determined and used to calculate the contribution of activated BAT to DEE. Results The mass of activated BAT was 59.1 ± 17.5 g (range, 32–85 g) in the high-BAT group (8 women and 1 man; mean age, 29.6 ± 5.5 y) and 2.2 ± 3.6 g (range, 0–9.3 g) in the low-BAT group (9 men and 7 women; mean age, 31.4 ± 10 y). Corresponding maximal SUVs were significantly higher in the high-BAT group than in the low-BAT group (10.7 ± 3.9 vs. 2.1 ± 0.7, P = 0.01). Blood flow values were significantly higher in the high-BAT group than in the low-BAT group for BAT (12.9 ± 4.1 vs. 5.9 ± 2.2 mL/100 g/min, P = 0.03) and white adipose tissue (7.2 ± 3.4 vs. 5.7 ± 2.3 mL/100 g/min, P = 0.03) but were similar for muscle (4.4 ± 1.9 vs. 3.9 ± 1.7 mL/100 g/min). Moreover, OEF in BAT was similar in the 2 groups (0.51 ± 0.17 in high-BAT group vs. 0.47 ± 0.18 in low-BAT group, P = 0.39). During mild cold stress, calculated MRO2 values in BAT increased from 0.97 ± 0.53 to 1.42 ± 0.68 mL/100 g/min (P = 0.04) in the high-BAT group and were significantly higher than those determined in the low-BAT group (0.40 ± 0.28 vs. 0.51 ± 0.23, P = 0.67). The increase in DEE associated with BAT oxidative metabolism was highly variable in the high-BAT group, with an average of 3.2 ± 2.4 kcal/d (range, 1.9–4.6 kcal/d) at rest, and increased to 6.3 ± 3.5 kcal/d (range, 4.0–9.9 kcal/d) during exposure to mild cold. Although BAT accounted for only a small fraction of the cold-induced increase in DEE, such increases were not observed in subjects lacking BAT. Conclusion Mild cold-induced thermogenesis in BAT accounts for 15–25 kcal/d in subjects with relatively large BAT depots. Thus, although the presence of active BAT is correlated with cold-induced energy expenditure, direct measurement of MRO2 indicates that BAT is a minor source of thermogenesis in humans. PMID:23362317

Correlating High Resolution Radar Reflectors with Visible Layering of the Polar Layered Deposits, Mars

NASA Astrophysics Data System (ADS)

Christian, S.; Holt, J. W.; Choudhary, P.; Fishbaugh, K. E.; Plaut, J. J.

2010-12-01

The Shallow Radar (SHARAD) onboard NASA’s Mars Reconnaissance Orbiter (MRO) has successfully detected many subsurface reflectors in the North Polar Layered Deposits (NPLD) of Mars. Confirming that these reflectors are caused by varying fractions of dust within the ice will be of primary importance in any attempt to model the composition of the NPLD, particularly if such a study incorporates optical data based on the assumption of a shared mechanism between layering and radar reflectance. As a first step towards examining this assumption, we have quantitatively studied the relationship between radar reflectors and adjacent visible layers exposed in an NPLD outcrop using statistical analyses and geometric comparisons. A clustering analysis of vertical separation distances between radar reflectors returned strong values at 11.8, 15.8, 20.3, 27.9, and 35.3 m, which strongly agree with published visible layer clusters [Fishbaugh et al., LPSC, 2009] and known frequency analysis results [Milkovich and Head, JGR, 2005]. Furthermore, in order to understand subsurface structures and reflector geometry we have gridded reflector surfaces in three dimensions, taking into account the influence of surface slopes to obtain accurate subsurface geometries. These geometries reveal average reflector dips of 0.4°, which are consistent with optical layer slopes on the order of 1.0°. Unexpected long wavelength topography resulting from subsurface structures visible to SHARAD complicated the attempt to compare radar reflector geometries with layer boundary elevation profiles obtained from the stratigraphic column produced using a digital elevation model (DEM) of High Resolution Imaging Science Experiment (HiRISE) stereo imagery [Fishbaugh et al., GRL, 2010]. The limitation imposed by the small extent of the DEM was resolved by increasing exposure coverage through the incorporation of images from Context Camera (CTX), also on MRO. In doing so, we were able to resolve the disparity between geometries and have now determined visible layers demonstrate similar subsurface topographic features as those revealed by SHARAD. Direct elevation comparisons between individual reflectors and discrete optical layers, while considered necessary for a correlation, are complicated by variations in subsurface structure that exist between the outcrop and the SHARAD tracks, as inferred from our mapping. While a direct correlation has not yet been accomplished, we have confirmed a genetic link between radar reflectors and visible layers; furthermore, we have generalized and improved the techniques for conducting such correlations so this can be undertaken at additional locations.

49 CFR 40.131 - How does the MRO or DER notify an employee of the verification process after receiving laboratory...

Code of Federal Regulations, 2010 CFR

2010-10-01

... result. In making this contact, you must explain to the employee that, if he or she declines to discuss... staff person must document the employee's decision, including the date and time. (2) A staff person must... numbers listed on the CCF. If you or your staff cannot reach the employee directly after making these...

49 CFR 40.203 - What problems cause a drug test to be cancelled unless they are corrected?

Code of Federal Regulations, 2010 CFR

2010-10-01

... 49 Transportation 1 2010-10-01 2010-10-01 false What problems cause a drug test to be cancelled... What problems cause a drug test to be cancelled unless they are corrected? (a) As the MRO, when a... the CCF, you must cancel the test unless the flaw is corrected. (d) The following are correctable...

River Ice Data Instrumentation

DTIC Science & Technology

1997-06-01

transmission and storage of data. Fi- nally, recommendations are made for further work in the field of ice data collection. North Atlantic \\N...Missouri River Division (MRD) Kansas City Omaha MRK MRO 7 32 20 11 North Atlantic Division (NAD) Baltimore New York Norfolk Philadelphia... Western 1 r~ T T Ice Thickness U Water Temperature < > Air Temperature i ► Discharge < | Water Stage < [ Ice Areal Coverage a Ice

CRISM Observations of Water Vapor and Carbon Monoxide

NASA Technical Reports Server (NTRS)

Smith, Michael D.; Wolff, Michael J.; Clancy, R. Todd

2008-01-01

Near-infrared spectra returned by the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM, [1]) on-board the Mars Reconnaissance Orbiter (MRO) contain the clear spectral signature of several atmospheric gases including carbon dioxide (CO2), water vapor (H2O), and carbon monoxide (CO). Here we describe the seasonal and spatial mapping of water vapor and carbon dioxide for one full Martian year using CRISM spectra.

Imaging of Stellar Surfaces with the Navy Precision Optical Interferometer

DTIC Science & Technology

2015-09-18

geostationary satel- lite with the Navy Prototype Optical Interferome- ter,” in Proc. Optical and Infrared Interferometry II, W. C. Danchi, F...Cormier, “Imag- ing of geostationary satellites with the MRO inter- ferometer,” in Proc. Advanced Maui Optical and Space Surveillance Technologies... geostationary satellites: Signal-to-noise considerations,” in Proc. Advanced Maui Optical and Space Surveillance Technologies Conference, 2011. 6. D

10 CFR 707.13 - Medical review of results of tests for illegal drug use.

Code of Federal Regulations, 2010 CFR

2010-01-01

... 10 Energy 4 2010-01-01 2010-01-01 false Medical review of results of tests for illegal drug use... Procedures § 707.13 Medical review of results of tests for illegal drug use. (a) All test results shall be submitted for medical review by the MRO. A confirmed positive test for drugs shall consist of an initial...

Global Albedo Variations on Mars from Recent MRO/MARCI and Other Space-Based Observations

NASA Astrophysics Data System (ADS)

Bell, J. F., III; Wellington, D. F.

2017-12-01

Dramatic changes in Mars surface albedo have been quantified by telescopic, orbital, and surface-based observations over the last 40 years. These changes provide important inputs for global and mesoscale climate models, enabling characterization of seasonal and secular variations in the distribution of mobile surface materials (dust, sand) in the planet's current climate regime. Much of the modern record of dust storms and albedo changes comes from synoptic-scale global imaging from the Viking Orbiter, Mars Global Surveyor (MGS), Hubble Space Telescope (HST), and Mars Reconnaissance Orbiter (MRO) missions, as well as local-scale observations from long-lived surface platforms like the Spirit and Opportunity rovers. Here we focus on the substantial time history of global-scale images acquired from the MRO Mars Color Imager (MARCI). MARCI is a wide-angle multispectral imager that acquires daily coverage of most of the surface at up to 1 km/pixel. MARCI has been in orbit since 2006, providing six Mars years of continuous surface and atmospheric observations, and building on the nearly five previous Mars years of global-scale imaging from the MGS Mars Orbiter Camera Wide Angle (MOC/WA) imager, which operated from 1997 to 2006. While many of the most significant MARCI-observed changes in the surface albedo are the result of large dust storms, other regions experience seasonal darkening events that repeat with different degrees of annual regularity. Some of these are associated with local dust storms, while for others, frequent surface changes take place with no associated evidence for dust storms, suggesting action by seasonally-variable winds and/or small-scale storms/dust devils too small to resolve. Discrete areas of dramatic surface changes across widely separated regions of Tharsis and in portions of Solis Lacus and Syrtis Major are among the regions where surface changes have been observed without a direct association to specific detectable dust storm events. Deposition following the annual southern summer dusty season plays a significant role in maintaining the cyclic nature of these changes. These and other historical observations also show that major regional or global-scale dust storms produce unique changes that may require several Mars years to reverse.

Recurring Slope Lineae (RSL) and Future Exploration of Mars and Europa

NASA Astrophysics Data System (ADS)

McEwen, Alfred S.

2014-11-01

Recurring slope lineae (RSL) are narrow (<5 m), dark markings on steep (25°-40°) slopes that incrementally grow during warm seasons over low-albedo surfaces, fade when inactive, and recur over multiple Mars years. RSL often follow small gullies, but no topographic changes (with one exception) have been detected via 30 cm/pixel images from MRO/HiRISE. Mid-latitude RSL appear and lengthen in the late spring through summer favoring equator-facing slopes. RSL also occur in equatorial regions of Mars, especially in the deep canyons of Valles Marineris; some of these lineae are over 1 km long, again usually following pristine gullies. The fans on which many RSL terminate have distinctive color and spectral properties, but lack water absorption bands in MRO/CRISM. RSL are active at places with peak surface temperatures >250 K, but we do not know what time of day they are active. Laboratory experiments show that water or brines darken basaltic soils but produce weak water absorption bands after partial dehydration during the low-humidity middle afternoon conditions when MRO observes. The primary question is whether RSL are really due to water at or near the surface. All observations can be explained in this way, and no entirely dry model has been offered, but there is no direct detection of water. If they are due to water, where does the water come from and how is it replenished each year? Multiple hypotheses exist. RSL may be evidence for seepage of water today, and may mark the most promising sites to search for extraterrestrial life. There are 2 key unknowns: (1) Does the water originate from the subsurface where microbes would be protected from radiation, or does it have an atmospheric origin and is only skin deep? (2) Is the water too salty for life as we know it? RSL occur on steep, rocky slopes on which landing is dangerous, but several concepts for surface exploration of RSL were presented in http://www.lpi.usra.edu/meetings/marsconcepts2012/. Landing in RSL sites will require additional expenses for planetary protection. For these reasons, it is important to learn as much as possible about RSL from orbital observations.

Initial Estimates of Optical Constants of Mars Candidate Materials

NASA Technical Reports Server (NTRS)

Rousch, Ted L.; Brown, Adrian Jon; Bishop, Janice L.; Blake, David F.; Bristow, Thomas F.

2013-01-01

Data obtained at visible and near-infrared wavelengths by OMEGA on Mars Express and CRISM on MRO provide definitive evidence for the presence of phyllosilicates and other hydrated phases on Mars. A diverse range of both Fe/Mg-OH and Al- OH-bearing phyllosilicates were identified including the smectites, nontronite, saponite, and montmorillonite. To constrain the abundances of these phyllosilicates, spectral analyses of mixtures are needed. We report on our effort to enable the quantitative evaluation of the abundance of hydrated-hydroxylated silicates when they are contained in mixtures. We include two component mixtures of hydrated/ hydroxylated silicates with each other and with two analogs for other Martian materials; pyroxene (enstatite) and palagonitic soil (an alteration product of basaltic glass, hereafter referred to as palagonite). For the hydrated-hydroxylated silicates we include saponite and montmorillonite (Mg- and Al-rich smectites). We prepared three size separates of each end-member for study: 20-45, 63-90, and 125-150 micron.

Optical Constants of Mars Candidate Materials used to Model Laboratory Reflectance Spectra of Mixtures

NASA Technical Reports Server (NTRS)

Roush, Ted L.; Brown, Adrian Jon; Blake, D.; Bristow, T.

2014-01-01

Data obtained at visible and nearinfrared wavelengths by OMEGA on MarsExpress and CRISM on MRO provide definitive evidence for the presence of phyllosilicates and other hydrated phases on Mars. A diverse range of both Fe/Mg-OH and Al- OH-bearing phyllosilicates were identified including the smectites nontronite, saponite, and montmorillonite. To constrain the abundances of these phyllosilicates, spectral analyses of mixtures are needed. We report on our effort to enable the quantitative evaluation of the abundance of hydrated-hydroxylated silicates when they are contained in mixtures. Here we focus on two component mixtures of the hydrated/ hydroxylated silicates, saponite and montmorillonite (Mg- and Al-rich smectites) with each other and with two analogs for other Martian materials; pyroxene (enstatite) and palagonitic soil (an alteration product of basaltic glass, hereafter referred to as palagonite). We prepared three size separates of each end-member for study: 20-45, 63-90, and 125-150 micron. Here we focus upon mixtures of the 63-90 m size fractions.

A New Impact Crater

NASA Image and Video Library

2018-05-29

NASA's Mars Reconnaissance Orbiter (MRO) keeps finding new impact sites on Mars. This one occurred within the dense secondary crater field of Corinto Crater, to the north-northeast. The new crater and its ejecta have distinctive color patterns. Once the colors have faded in a few decades, this new crater will still be distinctive compared to the secondaries by having a deeper cavity compared to its diameter. https://photojournal.jpl.nasa.gov/catalog/PIA22462

49 CFR 40.201 - What problems always cause a drug test to be cancelled and may result in a requirement for...

Code of Federal Regulations, 2010 CFR

2010-10-01

... cancelled and may result in a requirement for another collection? 40.201 Section 40.201 Transportation... TESTING PROGRAMS Problems in Drug Tests § 40.201 What problems always cause a drug test to be cancelled and may result in a requirement for another collection? As the MRO, you must cancel a drug test when a...

New results from the MRO/CRISM investigation

NASA Astrophysics Data System (ADS)

Murchie, Scott L.; Mustard, John; Arvidson, Raymond; Bishop, Janice; Clancy, R. Todd; Ehlmann, Bethany; Skok, J. R.; Wray, James; Lichtenberg, Kimberly; Andrews-Hanna, Jeffrey

The CRISM visible-infrared imaging spectrometer on the MRO spacecraft has completed over 1.7 Mars years of its investigation. During that time CRISM has acquired over 11,500 hyper-spectral observations at 20-40 m/pixel (typically coordinated with 30 cm/pixel HiRISE images and 6 m/pixel CTX images), 12,500 globally distributed measurements of aerosol opacity and trace gas abundances, and 200 m/pixel mapping of 70% of Mars at 72 wavelengths. Ma-jor results from the first Mars year of operation include characterization of the composition, stratigraphy, and geologic setting of ten distinct classes of deposits containing minerals diagnos-tic of past aqueous processes, and monitoring of spatial and seasonal variations in atmospheric properties during the year of a global dust event. New results during the second Mars year of operations include: (a) discovery of Noachian-aged hydrothermal alteration of the crust, includ-ing formation of serpentine; (b) Hesperian-aged hydrothermal deposits, for example in Syrtis Major; (c) more complete mapping of late Noachian-to Hesperian-aged sulfate-bearing layered deposits, revealing correlation with expected locations of groundwater discharge; (d) detailed mineral mapping of candidate MSL landing sites, and characterization of seasonal change at the Phoenix site; and (e) limb profiles of gases and aerosols showing their distribution at vertical scales <1 km.

Pangolin distribution and conservation status in Bangladesh

PubMed Central

Trageser, Scott J.; Mro, Passing; Mro, Poroy

2017-01-01

Asian pangolins are a highly-threatened species group, mainly due to the perceived medicinal value of their scales. Increased demand from China has resulted in pangolins being the most trafficked mammal in the world. Three pangolin species are reported to occur in Bangladesh: Manis pentadactyla, M. crassicaudata, and M. javanica. No peer-reviewed studies exist detailing these species’ current distribution or status within Bangladesh. A literature review was conducted resulting in the clarification of conflicting reports and misidentified observations and specimen records. In this paper, we also report the current status of pangolins (Manis spp.) in Bangladesh based on semi-structured interviews, camera trapping, media queries, and field surveys employing traditional ecological knowledge and non-randomized transect surveys. Ethnozoological knowledge pertaining to the natural history of M. pentadactyla is also reported from experienced Mro tribal hunters. The critically endangered M. pentadactyla was verified to occur in northwest, northeast, and southeast Bangladesh in natural and degraded habitats. Interviews with the Mro tribe in the southeast indicate that pangolin populations there were likely extirpated in 2014 due to skilled commercial collection beginning in 2010. Evidence of extant M. crassicaudata and M. javanica populations remain unverified and questionable, and historical records of M. crassicaudata and M. javanica are likely a result of misidentification. PMID:28388644

Using Mean Orbit Period in Mars Reconnaissance Orbiter Maneuver Design

NASA Technical Reports Server (NTRS)

Chung, Min-Kun J.; Menon, Premkumar R.; Wagner, Sean V.; Williams, Jessica L.

2014-01-01

Mars Reconnaissance Orbiter (MRO) has provided communication relays for a number of Mars spacecraft. In 2016 MRO is expected to support a relay for NASA's Interior Exploration using Seismic Investigations, Geodesy and Heat Transport (InSight) spacecraft. In addition, support may be needed by another mission, ESA's ExoMars EDL Demonstrator Module's (EDM), only 21 days after the InSight coverage. The close proximity of these two events presents a unique challenge to a conventional orbit synchronization maneuver where one deterministic maneuver is executed prior to each relay. Since the two events are close together and the difference in required phasing between InSight and EDM may be up to half an orbit (yielding a large execution error), the downtrack timing error can increase rapidly at the EDM encounter. Thus, a new maneuver strategy that does not require a deterministic maneuver in-between the two events (with only a small statistical cleanup) is proposed in the paper. This proposed strategy rests heavily on the stability of the mean orbital period. The ability to search and set the specified mean period is fundamental in the proposed maneuver design as well as in understanding the scope of the problem. The proposed strategy is explained and its result is used to understand and solve the problem in the flight operations environment.

The Australian SKA Pathfinder: project update and initial operations

NASA Astrophysics Data System (ADS)

Schinckel, Antony E. T.; Bock, Douglas C.-J.

2016-08-01

The Australian Square Kilometre Array Pathfinder (ASKAP) will be the fastest dedicated cm-wave survey telescope, and will consist of 36 12-meter 3-axis antennas, each with a large chequerboard phased array feed (PAF) receiver operating between 0.7 and 1.8 GHz, and digital beamforming prior to correlation. The large raw data rates involved ( 100 Tb/sec), and the need to do pipeline processing, has led to the antenna incorporating a third axis to fix the parallactic angle with respect to the entire optical system (blockages and phased array feed). It also results in innovative technical solutions to the data transport and processing issues. ASKAP is located at the Murchison Radio-astronomy Observatory (MRO), a new observatory developed for the Square Kilometre Array (SKA), 315 kilometres north-east of Geraldton, Western Australia. The MRO also hosts the SKA low frequency pathfinder instrument, the Murchison Widefield Array and will host the initial low frequency instrument of the SKA, SKA1-Low. Commissioning of ASKAP using six antennas equipped with first-generation PAFs is now complete and installation of second-generation PAFs and digital systems is underway. In this paper we review technical progress and commissioning to date, and refer the reader to relevant technical and scientific publications.

MARS Science Laboratory Post-Landing Location Estimation Using Post2 Trajectory Simulation

NASA Technical Reports Server (NTRS)

Davis, J. L.; Shidner, Jeremy D.; Way, David W.

2013-01-01

The Mars Science Laboratory (MSL) Curiosity rover landed safely on Mars August 5th, 2012 at 10:32 PDT, Earth Received Time. Immediately following touchdown confirmation, best estimates of position were calculated to assist in determining official MSL locations during entry, descent and landing (EDL). Additionally, estimated balance mass impact locations were provided and used to assess how predicted locations compared to actual locations. For MSL, the Program to Optimize Simulated Trajectories II (POST2) was the primary trajectory simulation tool used to predict and assess EDL performance from cruise stage separation through rover touchdown and descent stage impact. This POST2 simulation was used during MSL operations for EDL trajectory analyses in support of maneuver decisions and imaging MSL during EDL. This paper presents the simulation methodology used and results of pre/post-landing MSL location estimates and associated imagery from Mars Reconnaissance Orbiter s (MRO) High Resolution Imaging Science Experiment (HiRISE) camera. To generate these estimates, the MSL POST2 simulation nominal and Monte Carlo data, flight telemetry from onboard navigation, relay orbiter positions from MRO and Mars Odyssey and HiRISE generated digital elevation models (DEM) were utilized. A comparison of predicted rover and balance mass location estimations against actual locations are also presented.

Pangolin distribution and conservation status in Bangladesh.

PubMed

Trageser, Scott J; Ghose, Animesh; Faisal, Muzaffar; Mro, Passing; Mro, Poroy; Rahman, Shahriar Caesar

2017-01-01

Asian pangolins are a highly-threatened species group, mainly due to the perceived medicinal value of their scales. Increased demand from China has resulted in pangolins being the most trafficked mammal in the world. Three pangolin species are reported to occur in Bangladesh: Manis pentadactyla, M. crassicaudata, and M. javanica. No peer-reviewed studies exist detailing these species' current distribution or status within Bangladesh. A literature review was conducted resulting in the clarification of conflicting reports and misidentified observations and specimen records. In this paper, we also report the current status of pangolins (Manis spp.) in Bangladesh based on semi-structured interviews, camera trapping, media queries, and field surveys employing traditional ecological knowledge and non-randomized transect surveys. Ethnozoological knowledge pertaining to the natural history of M. pentadactyla is also reported from experienced Mro tribal hunters. The critically endangered M. pentadactyla was verified to occur in northwest, northeast, and southeast Bangladesh in natural and degraded habitats. Interviews with the Mro tribe in the southeast indicate that pangolin populations there were likely extirpated in 2014 due to skilled commercial collection beginning in 2010. Evidence of extant M. crassicaudata and M. javanica populations remain unverified and questionable, and historical records of M. crassicaudata and M. javanica are likely a result of misidentification.

History of the University of Washington Astronomy Department: 1965-1995

NASA Astrophysics Data System (ADS)

Lutz, Julie H.

2015-01-01

The Department of Astronomy of the University of Washington (UW) is celebrating its fiftieth anniversary this year, starting in 1965 when George Wallerstein and Paul Hodge joined Theodor Jacobsen to significantly expand research and initiate a graduate program. Three additional faculty members in astrophysical theory were added before the end of the decade: James Bardeen, Karl-Heinz Böhm and Erika Böhm-Vitense. In addition, plans were started to establish a research telescope in the State of Washington, primarily for training graduate students. The site survey for what eventually became Manastash Ridge Observatory (MRO) started in 1965. The 30-inch telescope at MRO in the eastern Cascades was dedicated in 1972.Four more faculty with a broad range of expertise were added in the 1970s and the number of graduate students expanded to about 15. Wallerstein was Chair of the department from 1965-1980. Part of his vision for the department was for UW astronomers to have access to a large, well-equipped telescope at a good observing site. He realized that such a goal would have to be accomplished in collaboration with other institutions and he spent years seeking partners.Newly-arrived faculty member Bruce Margon served as Chair from 1981-87 and from 1990-1995. In 1983 the Astrophysical Research Consortium (ARC) was formed with UW as a partner. UW played a major role in the construction of the ARC 3.5-m telescope in New Mexico, which was dedicated in 1994 and continues to function robustly. The department hired several more faculty with a variety of interests, both in multi-wavelength studies and astrophysical theory. An undergraduate astronomy major was added in the mid-1980s.In the mid-1980s ARC started to think about a sky survey which would encompass both imaging and spectroscopy. This became the original Sloan Digital Sky Survey (SDSS), which took place between 1990 and 1995, again with the UW as a major partner. At this time, UW Astronomy experienced growth in faculty, graduate students, postdoctoral fellows, research scientists and undergraduate majors.

Modeling Floods in Athabasca Valles, Mars, Using CTX Stereo Topography

NASA Astrophysics Data System (ADS)

Dundas, C. M.; Keszthelyi, L. P.; Denlinger, R. P.; Thomas, O. H.; Galuszka, D.; Hare, T. M.; Kirk, R. L.; Howington-Kraus, E.; Rosiek, M.

2012-12-01

Among the most remarkable landforms on Mars are the outflow channels, which suggest the occurrence of catastrophic water floods in the past. Athabasca Valles has long been thought to be the youngest of these channels [1-2], although it has recently become clear that the young crater age applies to a coating lava flow [3]. Simulations with a 2.5-dimensional flood model have provided insight into the details of flood dynamics but have also demonstrated that the Digital Elevation Model (DEM) from the Mars Orbiter Laser Altimeter (MOLA) Mission Experiment Gridded Data Records includes significant artifacts at this latitude at the scales relevant for flood modeling [4]. In order to obtain improved topography, we processed stereo images from the Context Camera (CTX) of the Mars Reconnaissance Orbiter (MRO) using methods developed for producing topographic models of the Moon with images from the Lunar Reconnaissance Orbiter Camera, a derivative of the CTX camera. Some work on flood modeling with CTX stereo has been published by [5], but we will present several advances, including corrections to the published CTX optical distortion model and improved methods to combine the stereo and MOLA data. The limitations of current methods are the accuracy of control to MOLA and the level of error introduced when the MRO spacecraft is not in a high-stability mode during stereo imaging, leading to jitter impacting the derived topography. Construction of a mosaic of multiple stereo pairs, controlled to MOLA, allows us to consider flow through the cluster of streamlined islands in the upper part of the channel [6], including what is suggested to be the best example of flood-formed subaqueous dunes on Mars [7]. We will present results from running a flood model [4, 8] through the high-resolution (100 m/post) DEM covering the streamlined islands and subaqueous dunes, using results from a lower-resolution model as a guide to the inflow. By considering a range of flow levels below estimated peak flow, we can examine the flow behavior at the site of the apparent subaqueous dunes and, in particular, assess whether the flow in this area is uniquely conducive to the formation of such bedforms [e.g., 9]. [1] Berman D. C. and Hartmann W. K. (2002) Icarus 159, 1-17. [2] Burr D. M. et al. (2002) Icarus 159, 53-73. [3] Jaeger W. L. et al. (2010) Icarus 205, 230-243. [4] Keszthelyi L. P. et al. (2007) GRL 34, L21206. [5] McIntyre et al. (2012) JGR 117, E03009. [6] Burr D. (2005) Geomorphology 69, 242-252. [7] Burr D. M. et al. (2004) Icarus 171, 68-83. [8] Denlinger R. P. and O'Connell D. R. H. (2008) J. Hyd. Eng. 134, 1590-1602. [9] Kleinhans M. G. (2005) JGR 110, E12003.

Investigating Functional Extension of Optical Coherence Tomography for Spectroscopic Analysis of Blood Oxygen Saturation

NASA Astrophysics Data System (ADS)

Chen, Siyu

Over the past two decades, optical coherence tomography (OCT) has been successfully applied to various fields of biomedical researching and clinical studies, including cardiology, urology, dermatology, dentistry, oncology, and most successfully, ophthalmology. This dissertation seeks to extend the current OCT practice, which is still largely morphology-based, into a new dimension, functional analysis of metabolic activities in vivo. More specifically, the investigation is focused on retrieving blood oxygen saturation (sO2) using intrinsic hemoglobin optical absorption contrast. Most mammalian cells rely on aerobic respiration to support cellular function, which means they consume oxygen to create adenosine triphosphate (ATP). Metabolic rate of oxygen (MRO2), a key hemodynamic parameter, characterizes how much oxygen is consumed during a given period of time, reflecting the metabolic activity of the target tissue. For example, retinal neurons are highly active and almost entirely rely on the moment-to-moment oxygen supply from retinal circulations. Thus, variation in MRO2 reveals the instantaneous activity of these neurons, shedding light on the physiological and pathophysiological change of cellular functions. Eventually, measuring MRO2 can potentially provide a biomarker for early-stage disease diagnosis, and serve as one benchmark for evaluating effectiveness of medical intervention during disease management. Essential in calculating MRO2, blood sO2 measurements using spectroscopic OCT analysis has been attempted as early as 2003. OCT is intrinsically sensitive to the blood optical absorption spectrum due to its wide-band illumination and detection scheme relying on back-scattered photon. However, accurate retrieval of blood sO2 using conventional near infrared (NIR) OCT systems in vivo has remained challenging. It was not until the development of OCT systems using visible light illumination (vis-OCT) when accurate measurement of blood sO2 was reported in live animals in situ. Thus, one question demanding immediate investigation is how the choice of illumination wavelength bands affect the performance of OCT oximetry. This is addressed using two approaches, (1) a numerical study using Monte Carlo methods, and (2) animal experiments involving the development of a vis- and NIR- dual band OCT imaging system. It is indicated that visible light is more suitable for OCT oximetry applications due to the higher absorption contrast between oxyhemoglobin and deoxyhemoglobin. The accuracy of OCT retinal oximetry is established to be around 5 percentage points (pp) regardless of physiological variation of blood sO2, vessel diameter, and is robust over a reasonable selection of sampling geometry. Despite the higher optical scattering experienced in the visible wavelength range, vis-OCT also demonstrated comparable or better imaging capability in terms of resolving anatomical features, imaging resolution, and retrieving other functional indicators such as blood flow. Besides retrieving blood sO2 from vessels directly visualized in structural OCT images, the possibility of using dynamic motion contrast to enhance otherwise non-resolvable micro vessels is investigated. Using this approach, it is subsequently proved that OCT angiography (OCTA) encodes blood absorption contrast and can be used to calculate sO2 within microvasculature. For the first time, measurements of relative sO2 change are reported in choroidal capillaries following inhalation oxygen challenge. This dissertation also represents a translational study that seeks to move technologies developed in the laboratory into real clinical applications. A vis-OCT imaging system with integrated scanning laser ophthalmoscope (SLO) is developed for human subjects. This prototype system can provide three-dimensional (3D) structural images and cross-sections of human fundus similar to that from commercial NIR-OCT systems. In addition, blood sO2 within retinal circulation is successfully retrieved from healthy subjects following spectroscopic analysis. To improve the accuracy of sO2 measurements, a statistical model is formulized. This model describes the noise intensity distribution in Fourier domain (FD) OCT amplitude image, which enables retrieving unbiased true OCT intensity from low signal-to-noise ratio (SNR) images. Finally, a vis-OCT microscope is developed to monitor dynamic changes within the cerebral circulation following ischemic stroke. This study demonstrates the application of vis-OCT beyond ophthalmic imaging, and serves as a proof of concept that vis-OCT has the potential to be employed in a wide-array of biomedical research.

Once in a Blue Dune

NASA Image and Video Library

2018-06-11

Sand dunes often accumulate in the floors of craters. In this region of Lyot Crater NASA's Mars Reconnaissance Orbiter (MRO) shows a field of classic barchan dunes. Just to the south of the group of barchan dunes is one large dune with a more complex structure. This particular dune, appearing like turquoise blue in enhanced color, is made of finer material and/or has a different composition than the surrounding. https://photojournal.jpl.nasa.gov/catalog/PIA22512

Summaries of Research 1986

DTIC Science & Technology

1986-01-01

PSEUDOMONAS AERUGINOSA AD A177 399 NMRI 86-0009 3CMILLAN M CHERNOW B ROTH BL PHOROOL ESTERS INHIBIT ALPHA I-ADRENERGIC RECEPTOR- STIlULATED...PHORBOL ESTERS PHOSPHOINOSITIDES RATS RECEPTORS, ADRENERGIC, ALPHA TASOMOTOR SYSTEM AD A171 091 NMRI 86-0010 QUESADA M MILLAR DB SMEJKAL R TUEULIN SYNTHESIS...UPTAKE AND RELEASE OF CALCIUM BY BRAIN SYNAPTOSOMES. JOURNAL OF APPLIED PHYSIOLOGY 1966 APR;60(4):1446-50 HYPERBARIC MEDICINE MRO41.O.1.1124 REPORT NO

Improved Acquisition for System Sustainment: Availability-Based Importance Framework for Maintenance, Repair, and Overhaul Acquisition

DTIC Science & Technology

2015-06-30

when these equipment failures cause some of the worst accidents and environmental damages in human history such as the March 2011 Fukushima Nuclear ...ultimately facilitate the MRO acquisition process through effective maintenance triggers and supplier selection Task 2. Stochastic Availability Importance...dollars with a replacement plan lasting for several decades [GAO 2004]. A budget reduction of about 29 percent since 1990 has “forced the branches of the

26TH AFOSR Chemical & Atmospheric Sciences Program Review FY81.

DTIC Science & Technology

1982-03-01

AFOSR-80-0020, 2310/A2 N. Larsen Department of Electrical Engineering Cornell University Ithaca, New York 14853 Light Scattering and Absorption Kuo-Nan...0011; University of Florida 80-0015 (To MRO Contract DAAM 1816 NW G Street 29-78-G-0024), 2310/Al Gainesville, FL 32601 Atmospheric Absorption of...parameters for use in the theoretical spectroscopy, for updating the transmission/emission codes, and for computing molecular absorption /emission line

Ridges near Nirgal Valles

NASA Image and Video Library

2018-03-05

In this observation from NASA's Mars Reconnaissance Orbiter (MRO), we see a set of straight ridges in ancient bedrock near Nirgal Valles. The patterns indicate fractures from tectonic stresses, but how have they been hardened to now stand in positive relief after billions of years of erosion? It is possible that groundwater flowed through the fractures, depositing various durable minerals, some of which we see in diverse colors. https://photojournal.jpl.nasa.gov/catalog/PIA22333

49 CFR 40.153 - How does the MRO notify employees of their right to a test of the split specimen?

Code of Federal Regulations, 2011 CFR

2011-10-01

... must have the ability to receive the employee's calls at all times during the 72 hour period (e.g., by use of an answering machine with a “time stamp” feature when there is no one in your office to answer... 72 hours from the time you provide this notification to him or her to request a test of the split...

The Effects of Employing HVM on C-130 Aircraft at WR-ALC to Aircraft Availability

DTIC Science & Technology

2011-06-01

processes of numerous commercial companies such as American Airlines, TIMCO, the Royal Canadian Air Force, and Hon Furniture to determine how and why...commercial industry best practices that best achieve higher labor burn rates and the challenges of implementing these practices into the traditional...Challenges According to Jerry Mobley, the HVM team in 2007 initiated the study and industrial analysis of the Maintenance, Repair, and Overhaul (MRO

Glorious Glacier

NASA Image and Video Library

2016-07-15

This image has low-sun lighting that accentuates the many transverse ridges on this slope, extending from Euripus Mons (mountains). These flow-like structures were previously called "lobate debris aprons," but the Shallow Radar (SHARAD) instrument on MRO has shown that they are actually debris-covered flows of ice, or glaciers. There is no evidence for present-day flow of these glaciers, so they appear to be remnants of past climates. http://photojournal.jpl.nasa.gov/catalog/PIA20745

The Fault in Our Mars

NASA Image and Video Library

2017-12-12

Lyot Crater (220-kilometers in diameter) is located in the Northern lowlands of Mars. The crater's floor marks the lowest elevation in the Northern Hemisphere as seen in this image from NASA's Mars Reconnaissance Orbiter (MRO). On the crater's floor, we see a network of channels. connecting a series of irregular shaped pits. These resemble terrestrial beaded streams, which are common in the Arctic regions of Earth and develop from uneven permafrost thawing. If terrestrial beaded streams are a good analog, these landforms suggest liquid water flow in the past. If not then these pits may result from the process of sublimation and would indicate pockets of easily accessible near-surface ground ice, which might have potentially preserved evidence of past habitability. The map is projected here at a scale of 25 centimeters (9.8 inches) per pixel. [The original image scale is 12.2 centimeters (9.8 inches) per pixel (with 1 x 1 binning); objects on the order of 93 centimeters (36.6 inches) across are resolved.] North is up. https://photojournal.jpl.nasa.gov/catalog/PIA22186

Depressions and Channels on the Floor of Lyot Crater

NASA Image and Video Library

2017-12-12

Lyot Crater (220-kilometers in diameter) is located in the Northern lowlands of Mars. The crater's floor marks the lowest elevation in the Northern Hemisphere as seen in this image from NASA's Mars Reconnaissance Orbiter (MRO). On the crater's floor, we see a network of channels. connecting a series of irregular shaped pits. These resemble terrestrial beaded streams, which are common in the Arctic regions of Earth and develop from uneven permafrost thawing. If terrestrial beaded streams are a good analog, these landforms suggest liquid water flow in the past. If not then these pits may result from the process of sublimation and would indicate pockets of easily accessible near-surface ground ice, which might have potentially preserved evidence of past habitability. The map is projected here at a scale of 25 centimeters (9.8 inches) per pixel. [The original image scale is 12.2 centimeters (9.8 inches) per pixel (with 1 x 1 binning); objects on the order of 93 centimeters (36.6 inches) across are resolved.] North is up. https://photojournal.jpl.nasa.gov/catalog/PIA22186

Water maser emission in the Saturnian system

NASA Astrophysics Data System (ADS)

Horiuchi, Shinji; Cimo, Giuseppe; Gurvits, Leonid; Pogrebenko, Sergei; Molera Calves, Guifré

2010-10-01

Prompted by the recent discovery of a water vapour plume of Enceladus by the Cassini spacecraft, our team started an observational programme to search for possible 22 GHz water vapour maser emission associated with different objects in the Kronian system. The observations have been conducted so far with the 32 m Medicina radio telescope (INAF-IRA, Italy) and the 14 m Metsahovi radio telescope (Aalto University, MRO, Finland). During the 2006-2008 campaigns, more than 300 hours of data have been analysed, and initial results including maser detections up to 7.0 sigma level have been presented. The detections attracted considerable interest and attempts to confirm them and investigate the phenomenon in depth. No confirmations have been published so far. In order to provide critical verification of these detections and study the details of masing conditions efficiently, we request a total of 20 hours on the Tidbinbilla 70 m telescope (DSS43) to observe Saturn and its moons during several, non-consecutive days. Due to natural changes of the planetary target positions, targets' coordinates will be provided after the antenna time is allocated.

12 years of Phobos observations by Omega and Spicam on board MEX

NASA Astrophysics Data System (ADS)

Gondet, Brigitte; Bertaux, Jean-Loup; Omega Team, Spicam Team

2016-10-01

Mars Express made several encounters with Phobos and a few with Deimos since 2004. Observations with SPICAM and OMEGA imaging spectrometers on board Mars Express covers the range from UV (110-312 nm) to visible and mid IR up to 5 µm. In the following we consider the ultraviolet (UV) channel of SPICAM and only the visible channel of OMEGA and its small UV extension down to 390 nm, in order to compare with SPICAM. Preliminary results were presented already in the past [1]. Since then, a more detailed analysis was carried out, subtracting some internally scattered light affecting the SPICAM UV retrieved reflectance.The combined spectrum of Radiance Factor from SPICAM and OMEGA suggests the presence of a deep absorption feature. Both instruments, taken separately, support also this absorption feature.In the visible part of CRISM [2] on board MRO and recently confirmed by Omega, one feature is centered at 0.65 µm, with an absorption depth varying from 0 to 4%, an other one is centered at 2.8µm. These two Visible IR features were interpreted [2] either to highly desiccated Fe-phyllosilicate minerals indigenous to the bodies, or to a surface process involving Rayleigh scattering and absorption of small iron particles formed by exogenic space weathering processing.In this rather uncertain situation, the UV band detected by SPICAM and OMEGA on board Mars Express is of great importance to attempt discriminating between the two scenarios proposed above to explain the Visible-IR reflectance spectra of Phobos.[1] Bertaux J.L. et al. (2011) EPSC/DPS conference abstract, Nantes, November 2011. [[2] Freaman A.A. et al. (2014) Icarus, 229 , 196-205.

UV-Visible reflectance of Phobos from SPICAM and OMEGA and comparison with Deimos

NASA Astrophysics Data System (ADS)

Gondet, Brigitte; Bertaux, Jean-Loup; Montmessin, Franck; Reberarc, Aurelie

2016-04-01

Mars Express made several encounters with Phobos and a few with Deimos since 2004. Observations with SPICAM and OMEGA imaging spectrometers on board Mars Express covers the range from UV (110-312 nm) to visible and mid IR up to 5 μm. In the following we consider the ultraviolet (UV) channel of SPICAM and only the visible channel of OMEGA and its small UV extension down to 390 nm, in order to compare with SPICAM. Preliminary results were presented already in the past [1]. Since then, a more detailed analysis was carried out, subtracting some internally scattered light affecting the SPICAM UV retrieved reflectance. The combined spectrum of Radiance Factor from SPICAM and OMEGA suggests the presence of a deep absorption feature. Both instruments, taken separately, support also this absorption feature. In the visible part of CRISM [2] on board MRO, one feature is centered at 0.65 μm, with an absorption depth varying from 0 to 4%, an other one is centered at 2.8μm. These two Visible IR features were interpreted [2] either to highly desiccated Fe-phyllosilicate minerals indigenous to the bodies, or to a surface process involving Rayleigh scattering and absorption of small iron particles formed by exogenic space weathering processing. In this rather uncertain situation, the UV band detected by SPICAM and OMEGA on board Mars Express is of great importance to attempt discriminating between the two scenarios proposed above to explain the Visible-IR reflectance spectra of Phobos. [1] Bertaux J.L. et al. (2011) EPSC/DPS conference abstract, Nantes, November 2011, [5] Freaman A.A. et al. (2014) Icarus, 229 , 196-205.

Diurnal Variations of Dust from Mars Climate Sounder Observations: Initial Results

NASA Astrophysics Data System (ADS)

Kleinboehl, A.

2017-12-01

Over the recent years, research on the Martian atmosphere has been focusing increasingly on aerosols. One recent focus has been on detached dust layers (DDL) as they have a significant radiative impact on the atmosphere. The dust distribution in the Martian atmosphere is affected by transport processes like lifting, advection, and sedimentation. However, lifting and sedimentation processes are only poorly understood, and the formation mechanism of DDLs is unclear. Significant variations in the occurrence of DDLs have been observed in comparisons of nearly co-located daytime and nighttime dust extinction measurements by the Mars Climate Sounder (MCS). However, the detailed behavior of changes in the vertical profile of dust over the course of a day has largely been unexplored. To date, aerosol studies by MCS have been limited to observations around 3 am and 3 pm local time due to the sun-synchronous orbit of the Mars Reconnaissance Orbiter (MRO), from which MCS is operated. MCS nominally observes in the direction of the MRO orbit track. Since Sep. 2010 the MCS instrument has been performing frequent sideways scans to obtain measurements at various local times. These special measurements yield nearly global coverage while sampling local times within a few hours of the nominal local time determined by the MRO orbit track. Of particular interest is the behavior at latitudes where cross-track measurements intersect with in-track measurements such that the same airmass is sampled 3 times in intervals of 2 hours at mid-latitudes. Here I present initial analyses of dust vertical profiles retrieved from these MCS observations during the dusty season of the Martian year. Dust opacities tend to be highest within 25 km of the surface and decreasing above. Numerous sets of profiles have been identified in the southern mid-latitudes in which this dust opacity slope is lofted by several kilometers in altitude between 4 pm and 6 pm local time. The behavior is largely restricted to ice-free conditions and suggestive of convective lofting of dust to higher altitudes due to absorption of incoming sunlight by dust particles. Most of these events are located in the vicinity of the Hellas basin, suggesting that topographic features may also play a role in their formation.

Demonstration of Regional Discrimination of Eurasian Seismic Events Using Observations at Soviet IRIS and CDSN Stations

DTIC Science & Technology

1992-03-01

Propagation of Lg Waves Across Eastern Europe and Asia, Lawrence Livermore National Laboratory Report, LLNL Report No. UCRL -52494. Press, F., and M. Ewing...the Nuclear Testing Ground in Eastern Kazakhstan, Lawrence Livermore National Laboratory Report, LLNL Report No. UCRL -52856. Ruzaikin, A., I. Nersesov...Derring Hall University Park, PA 16802 Blacksburg, VA 24061 Dr. Ralph Alewine, III Dr. Stephen Bratt DARPAftMRO Center for Seismic Studies 3701 North Fairax

A History of the U.S. Army Construction Engineering Research Laboratory (CERL) 1964-1985

DTIC Science & Technology

1987-12-01

Advlwry Cu.rctl Lqu i fWTU1l rv.lu.1 tl~ CLmn!tteo.o r t"l..kral .... m.ro . • Progr.n UJmntl t"t’ H,Hl er PI~ Camu (t~ M.I:soe.uch oInJ ~1 0fTTU...Illinois, 16 Dec. 1983, Records of Prof. William J. Hall, University of Illinois. 21. Ibid.; James J. Costello, University Counsel, to Albert E. Jenner

3-D Imaging of Mars’ Polar Ice Caps Using Orbital Radar Data

PubMed Central

Foss, Frederick J.; Putzig, Nathaniel E.; Campbell, Bruce A.; Phillips, Roger J.

2018-01-01

Since its arrival in early 2006, various instruments aboard NASA’s Mars Reconnaissance Orbiter (MRO) have been collecting a variety of scientific and engineering data from orbit around Mars. Among these is the SHAllow RADar (SHARAD) instrument, supplied by Agenzia Spaziale Italiana (ASI) and designed for subsurface sounding in the 15–25 MHz frequency band. As of this writing, MRO has completed over 46,000 nearly polar orbits of Mars, 30% of which have included active SHARAD data collection. By 2009, a sufficient density of SHARAD coverage had been obtained over the polar regions to support 3-D processing and analysis of the data. Using tools and techniques commonly employed in terrestrial seismic data processing, we have processed subsets of the resulting collection of SHARAD observations covering the north and south polar regions as SHARAD 3-D volumes, imaging the interiors of the north and south polar ice caps known, respectively, as Planum Boreum and Planum Australe. After overcoming a series of challenges revealed during the 3-D processing and analysis, a completed Planum Boreum 3-D volume is currently being used for scientific research. Lessons learned in the northern work fed forward into our 3-D processing and analysis of the Planum Australe 3-D volume, currently under way. We discuss our experiences with these projects and present results and scientific insights stemming from these efforts. PMID:29400351

Deep Space Ka-band Link Management and the MRO Demonstration: Long-term Weather Statistics Versus Forecasting

NASA Technical Reports Server (NTRS)

Davarian, Faramaz; Shambayati, Shervin; Slobin, Stephen

2004-01-01

During the last 40 years, deep space radio communication systems have experienced a move toward shorter wavelengths. In the 1960s a transition from L- to S-band occurred which was followed by a transition from S- to X-band in the 1970s. Both these transitions provided deep space links with wider bandwidths and improved radio metrics capability. Now, in the 2000s, a new change is taking place, namely a move to the Ka-band region of the radio frequency spectrum. Ka-band will soon replace X-band as the frequency of choice for deep space communications providing ample spectrum for the high data rate requirements of future missions. The low-noise receivers of deep space networks have a great need for link management techniques that can mitigate weather effects. In this paper, three approaches for managing Ka-band Earth-space links are investigated. The first approach uses aggregate annual statistics, the second one uses monthly statistics, and the third is based on the short-term forecasting of the local weather. An example of weather forecasting for Ka-band link performance prediction is presented. Furthermore, spacecraft commanding schemes suitable for Ka-band link management are investigated. Theses schemes will be demonstrated using NASA's Mars Reconnaissance Orbiter (MRO) spacecraft in the 2007 to 2008 time period, and the demonstration findings will be reported in a future publication.

Compact Reconnaissance Imaging Spectrometer for Mars investigation and data set from the Mars Reconnaissance Orbiter's primary science phase

USGS Publications Warehouse

Murchie, S.L.; Seelos, F.P.; Hash, C.D.; Humm, D.C.; Malaret, E.; McGovern, J.A.; Choo, T.H.; Seelos, K.D.; Buczkowski, D.L.; Morgan, M.F.; Barnouin-Jha, O. S.; Nair, H.; Taylor, H.W.; Patterson, G.W.; Harvel, C.A.; Mustard, J.F.; Arvidson, R. E.; McGuire, P.; Smith, M.D.; Wolff, M.J.; Titus, T.N.; Bibring, J.-P.; Poulet, F.

2009-01-01

The part of the Compact Reconnaissance Imaging Spectrometer (CRISM) for Mars investigation conducted during the Mars Reconnaissance Orbiter's (MRO's) primary science phase was a comprehensive investigation of past aqueous environments, structure of the planet's crust, past climate, and current meteorology. The measurements to implement this investigation include over 9500 targeted observations of surface features taken at spatial resolutions of better than 40 m/pixel, monitoring of seasonal variations in atmospheric aerosols and trace gases, and acquisition of a 200 m/pixel map covering over 55% of Mars in 72 selected wavelengths under conditions of relatively low atmospheric opacity. Key results from these data include recognition of a diversity of aqueous mineral-containing deposits, discovery of a widespread distribution of phyllosilicates in early to middle Noachian units, the first definitive detection of carbonates in bedrock, new constraints on the sequence of events that formed Hesperian-aged, sulfate-rich layered deposits, characterization of seasonal polar processes, and monitoring of the 2007 global dust event. Here we describe CRISM's science investigations during the Primary Science Phase, the data sets that were collected and their calibration and uncertainties, and how they have been processed and made available to the scientific community. We also describe the ongoing investigation during MRO's extended science phase. Copyright 2009 by the American Geophysical Union.

Temperature and dust profiles of Mars' atmosphere derived from Mars Climate Sounder (Mars Reconnaissance Orbiter)

NASA Astrophysics Data System (ADS)

Teanby, N. A.; Irwin, P. G.; Howett, C.; Calcutt, S. B.; Lolachi, R.; Bowles, N. E.; Taylor, F. W.; Schofield, J. T.; Kleinboehl, A.; McCleese, D. J.

2007-12-01

Mars Climate Sounder (MCS) on board NASA's Mars Reconnaissance Orbiter (MRO) primarily operates as a limb sounding infrared radiometer. The small field of view and limb scanning mode allow retrieval of atmospheric temperature and dust properties from the surface up to approximately 80km with 5km vertical resolution. The polar orbit of MRO gives coverage of all latitudes at 3pm and 3am Mars local-time. The ability of MCS to sounds these altitudes at high spatial and temporal resolution gives a unique dataset with which to test our understanding of the Martian atmosphere. It also complements and extends upon previous climatalogical datasets (for example TES). Measured mid-infrared radiances from MCS were analysed using the correlated-k approximation with Oxford's NEMESIS retrieval software. The correlated-k approximation was compared with a line-by-line model to confirm its accuracy under Martian atmospheric conditions. Dust properties were taken from analysis of TES data by Wolff and Clancy (2003). We present profiles of temperature and dust for data covering September to December 2006. During this period Mars' north pole was experiencing summer and the south pole was in winter. Preliminary results show that high altitude warming over the southern winter pole is greater than that predicted by models. Our results will be compared to numerical models of the Martian atmosphere and the implications discussed.

Vertical Profiles Of Temperature And Dust Derived From Mars Climate Sounder

NASA Astrophysics Data System (ADS)

Teanby, Nicholas; Irwin, P. G.; Howett, C.; Calcutt, S.; Lolachi, R.; Bowles, N.; Taylor, F.; Schofield, J. T.; Kleinboehl, A.; McCleese, D. J.

2007-10-01

Mars Climate Sounder (MCS) on board NASA's Mars Reconnaissance Orbiter (MRO) primarily operates as a limb sounding infrared radiometer. The small field of view and limb scanning mode allow retrieval of temperature and dust properties from the surface up to approximately 80km with 5km vertical resolution. The polar orbit of MRO gives coverage of all latitudes at 3pm and 3am local time. The ability of MCS to sounds these altitudes at high spatial and temporal resolution gives a unique dataset with which to test our understanding of the Martian atmosphere. It also complements and extends upon previous climatalogical datasets (for example TES). Measured mid-infrared radiances from MCS were analysed using the correlated-k approximation with Oxford's NEMESIS retrieval software. The correlated-k approximation was compared with a line-by-line model to confirm its accuracy under Martian atmospheric conditions. Dust properties were taken from analysis of TES data by Wolff and Clancy (2003). We present profiles of temperature and dust for data covering September to December 2006. During this period Mars' north pole was experiencing summer and the south pole was in winter. Preliminary results show that high altitude warming over the southern winter pole is greater than that predicted by models. Our results will be compared to numerical models of the Martian atmosphere and the implications discussed.

A New Blind Pointing Model Improves Large Reflector Antennas Precision Pointing at Ka-Band (32 GHz)

NASA Technical Reports Server (NTRS)

Rochblatt, David J.

2009-01-01

The National Aeronautics and Space Administration (NASA), Jet Propulsion Laboratory (JPL)-Deep Space Network (DSN) subnet of 34-m Beam Waveguide (BWG) Antennas was recently upgraded with Ka-Band (32-GHz) frequency feeds for space research and communication. For normal telemetry tracking a Ka-Band monopulse system is used, which typically yields 1.6-mdeg mean radial error (MRE) pointing accuracy on the 34-m diameter antennas. However, for the monopulse to be able to acquire and lock, for special radio science applications where monopulse cannot be used, or as a back-up for the monopulse, high-precision open-loop blind pointing is required. This paper describes a new 4th order pointing model and calibration technique, which was developed and applied to the DSN 34-m BWG antennas yielding 1.8 to 3.0-mdeg MRE pointing accuracy and amplitude stability of 0.2 dB, at Ka-Band, and successfully used for the CASSINI spacecraft occultation experiment at Saturn and Titan. In addition, the new 4th order pointing model was used during a telemetry experiment at Ka-Band (32 GHz) utilizing the Mars Reconnaissance Orbiter (MRO) spacecraft while at a distance of 0.225 astronomical units (AU) from Earth and communicating with a DSN 34-m BWG antenna at a record high rate of 6-megabits per second (Mb/s).

Windblown Sand in Ganges Chasma

NASA Image and Video Library

2017-04-25

Dark, windblown sand covers intricate sedimentary rock layers in this image captured by NASA's Mars Reconnaissance Orbiter (MRO) from Ganges Chasma, a canyon in the Valles Marineris system. These features are at once familiar and unusual to those familiar with Earth's beaches and deserts. Most sand dunes on Earth are made of silica-rich sand, giving them a light color; these Martian dunes owe their dark color to the iron and magnesium-rich sand found in the region. https://photojournal.jpl.nasa.gov/catalog/PIA21600

Colorful Equatorial Gullies in Krupac Crater

NASA Image and Video Library

2017-05-02

Although large gullies (ravines) are concentrated at higher latitudes, there are gullies on steep slopes in equatorial regions, as seen in this image captured by NASA's Mars Reconnaissance Orbiter (MRO). The colors of the gully deposits match the colors of the eroded source materials. Krupac is a relatively young impact crater, but exposes ancient bedrock. Krupac Crater also hosts some of the most impressive recurring slope lineae (RSL) on equatorial Mars outside of Valles Marineris. https://photojournal.jpl.nasa.gov/catalog/PIA21605

Applying Best Practices to Military Commercial-Derivative Aircraft Engine Sustainment: Assessment of Using Parts Manufacturer Approval (PMA) Parts and Designated Engineering Representative (DER) Repairs

DTIC Science & Technology

2016-01-01

Company HPT high-pressure turbine LPT low-pressure turbine MARPA Modification and Replacement Parts Association MRO maintenance , repair, and overhaul...Corporation R® is a registered trademark. Cover image: A KC-10 F103 (CF6-50) engine at the MTU Vancouver facility (courtesy of MTU Maintenance Canada Ltd...representative (DER) repairs to decrease the cost of their aircraft engine maintenance . These parts and repairs are provided by third-party companies and

Cracks in a Debris Apron

NASA Image and Video Library

2015-03-11

This observation from NASA Mars Reconnaissance Orbiter shows the nature of large fissures in a smooth apron around a mound in the Phlegra region. The apron could be (or could have been) ice-rich, so one possibility is that the fissures are related to ice loss. Based on radar data from MRO combined with studies of the region's geology from other orbiters, scientists think that extensive glaciers covered this region several hundred million years ago. http://photojournal.jpl.nasa.gov/catalog/PIA19307

Expanded Craters on Mars: Implications for Shallow, Mid-latitude Excess Ice

NASA Astrophysics Data System (ADS)

Viola, Donna

Understanding the age and distribution of shallow ice on Mars is valuable for interpreting past and present climate conditions, and has implications on habitability and future in situ resource utilization. Many ice-related features, such as lobate debris aprons and concentric crater fill, have been studied using a range of remote sensing techniques. Here, I explore the distribution of expanded craters, a form of sublimation thermokarst where shallow, excess ice has been destabilized and sublimated following an impact event. This leads to the collapse of the overlying dry regolith to produce the appearance of diameter widening. The modern presence of these features suggests that excess ice has remained preserved in the terrain immediately surrounding the craters since the time of their formation in order to maintain the surface. High-resolution imagery is ideal for observing thermokarst features, and much of the work described here will utilize data from the Context Camera (CTX) and High Resolution Imaging Science Experiment (HiRISE) on the Mars Reconnaissance Orbiter (MRO). Expanded craters tend to be found in clusters that emanate radially from at least four primary craters in Arcadia Planitia, and are interpreted as secondary craters that formed nearly simultaneously with their primaries. Crater age dates of the primaries indicate that the expanded secondaries, as well as the ice layer into which they impacted, must be at least tens of millions of years old. Older double-layer ejecta craters in Arcadia Planitia commonly have expanded craters superposed on their ejecta - and they tend to be more expanded (with larger diameters) in the inner ejecta layer. This has implications on the formation mechanisms for craters with this unique ejecta morphology. Finally, I explore the distribution of expanded craters south of Arcadia Planitia and across the southern mid-latitudes, along with scalloped depressions (another form of sublimation thermokarst), in order to identify the modern excess ice boundary in this region and any longitudinal variations. This study identifies some potential low-latitude locations with patchy excess ice, possibly preserved during a past climate. Through these studies, I will infer regions that contain abundant ice today and consider the implications that this ice has on both the martian climate and future exploration.

NASA Tech Briefs, November 2008

NASA Technical Reports Server (NTRS)

2008-01-01

Topics covered include: Digital Phase Meter for a Laser Heterodyne Interferometer; Vision System Measures Motions of Robot and External Objects; Advanced Precipitation Radar Antenna to Measure Rainfall From Space; Wide-Band Radar for Measuring Thickness of Sea Ice; Vertical Isolation for Photodiodes in CMOS Imagers; Wide-Band Microwave Receivers Using Photonic Processing; L-Band Transmit/Receive Module for Phase-Stable Array Antennas; Microwave Power Combiner/Switch Utilizing a Faraday Rotator; Compact Low-Loss Planar Magic-T; Using Pipelined XNOR Logic to Reduce SEU Risks in State Machines; Quasi-Optical Transmission Line for 94-GHz Radar; Next Generation Flight Controller Trainer System; Converting from DDOR SASF to APF; Converting from CVF to AAF; Documenting AUTOGEN and APGEN Model Files; Sequence History Update Tool; Extraction and Analysis of Display Data; MRO DKF Post-Processing Tool; Rig Diagnostic Tools; MRO Sequence Checking Tool; Science Activity Planner for the MER Mission; UAVSAR Flight-Planning System; Templates for Deposition of Microscopic Pointed Structures; Adjustable Membrane Mirrors Incorporating G-Elastomers; Hall-Effect Thruster Utilizing Bismuth as Propellant; High-Temperature Crystal-Growth Cartridge Tubes Made by VPS; Quench Crucibles Reinforced with Metal; Deep-Sea Hydrothermal-Vent Sampler; Mars Rocket Propulsion System; Two-Stage Passive Vibration Isolator; Improved Thermal Design of a Compression Mold; Enhanced Pseudo-Waypoint Guidance for Spacecraft Maneuvers; Altimetry Using GPS-Reflection/Occultation Interferometry; Thermally Driven Josephson Effect; Perturbation Effects on a Supercritical C7H16/N2 Mixing Layer; Gold Nanoparticle Labels Amplify Ellipsometric Signals; Phase Matching of Diverse Modes in a WGM Resonator; WGM Resonators for Terahertz-to-Optical Frequency Conversion; Determining Concentration of Nanoparticles from Ellipsometry; Microwave-to-Optical Conversion in WGM Resonators; Four-Pass Coupler for Laser-Diode-Pumped Solid-State Laser; Low-Resolution Raman-Spectroscopy Combustion Thermometry; Temperature Sensors Based on WGM Optical Resonators; Varying the Divergence of Multiple Parallel Laser Beams; Efficient Algorithm for Rectangular Spiral Search; Algorithm-Based Fault Tolerance Integrated with Replication; Targeting and Localization for Mars Rover Operations; Terrain-Adaptive Navigation Architecture; Self-Adjusting Hash Tables for Embedded Flight Applications; Schema for Spacecraft-Command Dictionary; Combined GMSK Communications and PN Ranging; System-Level Integration of Mass Memory; Network-Attached Solid-State Recorder Architecture; Method of Cross-Linking Aerogels Using a One-Pot Reaction Scheme; An Efficient Reachability Analysis Algorithm.

Paths from Mother-Child and Father-Child Relationships to Externalizing Behavior Problems in Children Differing in Electrodermal Reactivity: a Longitudinal Study from Infancy to Age 10

PubMed Central

Kochanska, Grazyna; Brock, Rebecca L.; Chen, Kuan-Hua; Aksan, Nazan; Anderson, Steven W.

2014-01-01

Electrodermal hyporeactivity (or low skin conductance level, SCL) has been long established as a correlate of and diathesis for antisocial behavior, aggression, disregard for rules of conduct and feelings of others, and generally, externalizing behavior problems in children and adults. Much less is known, however, about how individual differences in children’s SCL and qualities of their early experiences in relationships with parents interact to produce antisocial outcomes. In a community sample of 102 families (51 girls), we examined children’s SCL, assessed in standard laboratory tasks at age 8 (N=81), as a moderator of the links between parent–child socialization history and children’s externalizing behavior problems at ages 8 and 10, reported by mothers and fathers in well-established instruments and by children in clinical interviews. Mother- and father-child socialization history was assessed in frequent, intensive observations. Parent–child mutually responsive orientation (MRO) was observed from infancy to age 10, parental power assertion was observed from 15 months to age 6 ½, and children reported their attachment security in interviews at age 8 and 10. For children with lower SCL, variations in mothers’ power assertion and father-child MRO were associated with parent-rated externalizing problems. The former interaction was consistent with diathesis-stress, and the latter with differential susceptibility. For children with higher SCL, there were no links between socialization history and externalizing problems. PMID:25218772

Nine martian years of dust optical depth observations: A reference dataset

NASA Astrophysics Data System (ADS)

Montabone, Luca; Forget, Francois; Kleinboehl, Armin; Kass, David; Wilson, R. John; Millour, Ehouarn; Smith, Michael; Lewis, Stephen; Cantor, Bruce; Lemmon, Mark; Wolff, Michael

2016-07-01

We present a multi-annual reference dataset of the horizontal distribution of airborne dust from martian year 24 to 32 using observations of the martian atmosphere from April 1999 to June 2015 made by the Thermal Emission Spectrometer (TES) aboard Mars Global Surveyor, the Thermal Emission Imaging System (THEMIS) aboard Mars Odyssey, and the Mars Climate Sounder (MCS) aboard Mars Reconnaissance Orbiter (MRO). Our methodology to build the dataset works by gridding the available retrievals of column dust optical depth (CDOD) from TES and THEMIS nadir observations, as well as the estimates of this quantity from MCS limb observations. The resulting (irregularly) gridded maps (one per sol) were validated with independent observations of CDOD by PanCam cameras and Mini-TES spectrometers aboard the Mars Exploration Rovers "Spirit" and "Opportunity", by the Surface Stereo Imager aboard the Phoenix lander, and by the Compact Reconnaissance Imaging Spectrometer for Mars aboard MRO. Finally, regular maps of CDOD are produced by spatially interpolating the irregularly gridded maps using a kriging method. These latter maps are used as dust scenarios in the Mars Climate Database (MCD) version 5, and are useful in many modelling applications. The two datasets (daily irregularly gridded maps and regularly kriged maps) for the nine available martian years are publicly available as NetCDF files and can be downloaded from the MCD website at the URL: http://www-mars.lmd.jussieu.fr/mars/dust_climatology/index.html

Paths from mother-child and father-child relationships to externalizing behavior problems in children differing in electrodermal reactivity: a longitudinal study from infancy to age 10.

PubMed

Kochanska, Grazyna; Brock, Rebecca L; Chen, Kuan-Hua; Aksan, Nazan; Anderson, Steven W

2015-05-01

Electrodermal hyporeactivity (or low skin conductance level, SCL) has been long established as a correlate of and diathesis for antisocial behavior, aggression, disregard for rules of conduct and feelings of others, and generally, externalizing behavior problems in children and adults. Much less is known, however, about how individual differences in children's SCL and qualities of their early experiences in relationships with parents interact to produce antisocial outcomes. In a community sample of 102 families (51 girls), we examined children's SCL, assessed in standard laboratory tasks at age 8 (N = 81), as a moderator of the links between parent-child socialization history and children's externalizing behavior problems at ages 8 and 10, reported by mothers and fathers in well-established instruments and by children in clinical interviews. Mother- and father-child socialization history was assessed in frequent, intensive observations. Parent-child mutually responsive orientation (MRO) was observed from infancy to age 10, parental power assertion was observed from 15 months to age 6 ½, and children reported their attachment security in interviews at age 8 and 10. For children with lower SCL, variations in mothers' power assertion and father-child MRO were associated with parent-rated externalizing problems. The former interaction was consistent with diathesis-stress, and the latter with differential susceptibility. For children with higher SCL, there were no links between socialization history and externalizing problems.

CRISM/HiRISE Correlative Spectroscopy

NASA Astrophysics Data System (ADS)

Seelos, F. P.; Murchie, S. L.; McGovern, A.; Milazzo, M. P.; Herkenhoff, K. E.

2011-12-01

The Mars Reconnaissance Orbiter (MRO) Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) and High Resolution Imaging Science Experiment (HiRISE) are complementary investigations with high spectral resolution and broad wavelength coverage (CRISM ~20 m/pxl; ~400 - 4000 nm, 6.55 nm sampling) and high spatial resolution with broadband color capability (HiRISE ~25 cm/pxl; ~500, 700, 900 nm band centers, ~200-300 nm FWHM). Over the course of the MRO mission it has become apparent that spectral variations in the IR detected by CRISM (~1000 nm - 4000 nm) sometimes correlate spatially with visible and near infrared 3-band color variations observed by HiRISE. We have developed a data processing procedure that establishes a numerical mapping between HiRISE color and CRISM VNIR and IR spectral data and provides a statistical evaluation of the uncertainty in the mapping, with the objective of extrapolating CRISM-inferred mineralogy to the HiRISE spatial scale. The MRO mission profile, spacecraft capabilities, and science planning process emphasize coordinated observations - the simultaneous observation of a common target by multiple instruments. The commonalities of CRISM/HiRISE coordinated observations present a unique opportunity for tandem data analysis. Recent advances in the systematic processing of CRISM hyperspectral targeted observations account for gimbal-induced photometric variations and transform the data to a synthetic nadir acquisition geometry. The CRISM VNIR (~400 nm - 1000 nm) data can then be convolved to the HiRISE Infrared, Red, and Blue/Green (IRB) response functions to generate a compatible CRISM IRB product. Statistical evaluation of the CRISM/HiRISE spatial overlap region establishes a quantitative link between the data sets. IRB spectral similarity mapping for each HiRISE color spatial pixel with respect to the CRISM IRB product allows a given HiRISE pixel to be populated with information derived from the coordinated CRISM observation, including correlative VNIR or IR spectral data, spectral summary parameters, or browse products. To properly characterize the quality and fidelity of the IRB correlation, a series of ancillary information bands that record the numerical behavior of the procedure are also generated. Prototype CRISM/HiRISE correlative data products have been generated for a small number of coordinated observation pairs. The resulting products have the potential to support integrated spectral and morphological mapping at sub-meter spatial scales. Such data products would be invaluable for strategic and tactical science operations on landed missions, and would allow observations from a landed platform to be evaluated in a CRISM-based spectral and mineralogical context.

Layered Ice Near the South Pole of Mars

NASA Image and Video Library

2017-12-12

The two largest ice sheets in the inner solar system are here on Earth, Antarctica and Greenland. The third largest is at the South Pole of Mars and a small part of it is shown in this image from NASA's Mars Reconnaissance Orbiter (MRO). Much like the terrestrial examples, this ice sheet is layered and scientists refer to it as the South Polar layered deposits. The ice layers contain information about past climates on Mars and deciphering this record has been a major goal of Mars science for decades. This slope, near the ice sheet's edge, shows the internal layers that have this climate record. With stereo images, we can tell the heights of these layers so we can measure their thickness and try to unravel the climatic information they contain. (Be sure to view the digital terrain model for this observation.) The map is projected here at a scale of 25 centimeters (9.8 inches) per pixel. [The original image scale is 25.0 centimeters (9.8 inches) per pixel (with 1 x 1 binning); objects on the order of 75 centimeters (29.5 inches) across are resolved.] North is up. https://photojournal.jpl.nasa.gov/catalog/PIA22125

Monitoring Sand Sheets and Dunes

NASA Image and Video Library

2017-06-12

NASA's Mars Reconnaissance Orbiter (MRO) captured this crater featuring sand dunes and sand sheets on its floor. What are sand sheets? Snow fall on Earth is a good example of sand sheets: when it snows, the ground gets blanketed with up to a few meters of snow. The snow mantles the ground and "mimics" the underlying topography. Sand sheets likewise mantle the ground as a relatively thin deposit. This kind of environment has been monitored by HiRISE since 2007 to look for movement in the ripples covering the dunes and sheets. This is how scientists who study wind-blown sand can track the amount of sand moving through the area and possibly where the sand came from. Using the present environment is crucial to understanding the past: sand dunes, sheets, and ripples sometimes become preserved as sandstone and contain clues as to how they were deposited The map is projected here at a scale of 25 centimeters (9.8 inches) per pixel. [The original image scale is 25 centimeters (9.8 inches) per pixel (with 1 x 1 binning); objects on the order of 75 centimeters (29.5 inches) across are resolved.] North is up. https://photojournal.jpl.nasa.gov/catalog/PIA21757

An Undergraduate Endeavor: Assembling a Live Planetarium Show About Mars

NASA Astrophysics Data System (ADS)

McGraw, Allison M.

2016-10-01

Viewing the mysterious red planet Mars goes back thousands of years with just the human eye but in more recent years the growth of telescopes, satellites and lander missions unveil unrivaled detail of the Martian surface that tells a story worth listening to. This planetarium show will go through the observations starting with the ancients to current understandings of the Martian surface, atmosphere and inner-workings through past and current Mars missions. Visual animations of its planetary motions, display of high resolution images from the Hi-RISE (High Resolution Imaging Science Experiment) and CTX (Context Camera) data imagery aboard the MRO (Mars Reconnaissance Orbiter) as well as other datasets will be used to display the terrain detail and imagery of the planet Mars with a digital projection system. Local planetary scientists and Mars specialists from the Lunar and Planetary Lab at the University of Arizona (Tucson, AZ) will be interviewed and used in the show to highlight current technology and understandings of the red planet. This is an undergraduate project that is looking for collaborations and insight in order gain structure in script writing that will teach about this planetary body to all ages in the format of a live planetarium show.

Ultrastructural and Functional Effects of Lipopolysaccharide and Interleukin-2 on Human NK Cells

DTIC Science & Technology

1988-01-01

Leu-lla antibody was Fixation in 1% glut 1% paraf Incubation with stained by HRP using the ABC method via a bio - in ice gold-linked tinylated anti...iilnAd rcsofrCa~Arsloaiti.A.Mro graji~howaweakataintig fr th enzye actvityNn h cl iRfaoo ~u1a el.1.ilvngl cain fa mllprioi(arw nfi.l~X)ofte niecl soin ol... Riccardi C, Santoni A, Stadler BM, Tarameill D, In: Immunobiology of Natural Killer Cells, Vol. 1, Timonen T, Varesio L (1980) Immunoregulation in- Lotzova E

Spectral Analysis of the Shuttle Glow. SPAS II/IBSS Mission - AIS hardware

DTIC Science & Technology

1992-04-23

Mirror Lens C Reflection) CiraCylindrical/-Lens • Plane Mirror j _Slit Slit Mro Fig. 7. Cross section through the reflective foreoptics of the UV Fig. 6...selection. The gratings in the The slit width of 0.045 mm restricted the angular spectrograph are deposited on Zerodur blanks, which width of the FOV...of th*i short fee-1 hlaa, t do, lmw b*WdW 3Wa APO=E OPTIC I VOL 31, ft. 16 1 1~ toes I 48 Secondary Mlirror Primary Mirror - lntaeranas Ptten Image

Mars Briefing

NASA Image and Video Library

2011-08-04

Colin Dundas, a research geologist with the U.S. Geological Survey, speaks during a briefing, Thursday, Aug. 4, 2011, at NASA Headquarters in Washington. Observations from NASA's Mars Reconnaissance Orbiter (MRO) have revealed possible flowing water during the warmest months on Mars. Dark, finger-like features appear and extend down some Martian slopes during late spring through summer, fade in winter, and return during the next spring. Repeated observations have tracked the seasonal changes in these recurring features on several steep slopes in the middle latitudes of Mars' southern hemisphere. Photo Credit: (NASA/Paul E. Alers)

Identification of Martian Cave Skylights Using the Temperature Change During Day and Night

NASA Astrophysics Data System (ADS)

Jung, Jongil; Yi, Yu; Kim, Eojin

2014-06-01

Recently, cave candidates have been discovered on other planets besides the Earth, such as the Moon and Mars. When we go to other planets, caves could be possible human habitats providing natural protection from cosmic threats. In this study, seven cave candidates have been found on Pavonis Mons and Ascraeus Mons in Tharsis Montes on Mars. The cave candidates were selected using the images of the Context Camera (CTX) on the Mars Reconnaissance Orbiter (MRO). The Context Camera could provide images with the high resolution of 6 meter per pixel. The diameter of the candidates ranges from 50 to 100m. Cushing et al. (2007) have analyzed the temperature change at daytime and nighttime using the Thermal Emission Imaging System (THEMIS) for the sites of potential cave candidates. Similarly, we have examined the temperature change at daytime and at nighttime for seven cave candidates using the method of Cushing et al. (2007). Among those, only one candidate showed a distinct temperature change. However, we cannot verify a cave based on the temperature change only and further study is required for the improvement of this method to identify caves more clearly.

Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) on Mars Reconnaissance Orbiter (MRO)

NASA Astrophysics Data System (ADS)

Murchie, S.; Arvidson, R.; Bedini, P.; Beisser, K.; Bibring, J.-P.; Bishop, J.; Boldt, J.; Cavender, P.; Choo, T.; Clancy, R. T.; Darlington, E. H.; Des Marais, D.; Espiritu, R.; Fort, D.; Green, R.; Guinness, E.; Hayes, J.; Hash, C.; Heffernan, K.; Hemmler, J.; Heyler, G.; Humm, D.; Hutcheson, J.; Izenberg, N.; Lee, R.; Lees, J.; Lohr, D.; Malaret, E.; Martin, T.; McGovern, J. A.; McGuire, P.; Morris, R.; Mustard, J.; Pelkey, S.; Rhodes, E.; Robinson, M.; Roush, T.; Schaefer, E.; Seagrave, G.; Seelos, F.; Silverglate, P.; Slavney, S.; Smith, M.; Shyong, W.-J.; Strohbehn, K.; Taylor, H.; Thompson, P.; Tossman, B.; Wirzburger, M.; Wolff, M.

2007-05-01

The Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) is a hyperspectral imager on the Mars Reconnaissance Orbiter (MRO) spacecraft. CRISM consists of three subassemblies, a gimbaled Optical Sensor Unit (OSU), a Data Processing Unit (DPU), and the Gimbal Motor Electronics (GME). CRISM's objectives are (1) to map the entire surface using a subset of bands to characterize crustal mineralogy, (2) to map the mineralogy of key areas at high spectral and spatial resolution, and (3) to measure spatial and seasonal variations in the atmosphere. These objectives are addressed using three major types of observations. In multispectral mapping mode, with the OSU pointed at planet nadir, data are collected at a subset of 72 wavelengths covering key mineralogic absorptions and binned to pixel footprints of 100 or 200 m/pixel. Nearly the entire planet can be mapped in this fashion. In targeted mode the OSU is scanned to remove most along-track motion, and a region of interest is mapped at full spatial and spectral resolution (15-19 m/pixel, 362-3920 nm at 6.55 nm/channel). Ten additional abbreviated, spatially binned images are taken before and after the main image, providing an emission phase function (EPF) of the site for atmospheric study and correction of surface spectra for atmospheric effects. In atmospheric mode, only the EPF is acquired. Global grids of the resulting lower data volume observations are taken repeatedly throughout the Martian year to measure seasonal variations in atmospheric properties. Raw, calibrated, and map-projected data are delivered to the community with a spectral library to aid in interpretation.

MRO CTX-based Digital Terrain Models

NASA Astrophysics Data System (ADS)

Dumke, Alexander

2016-04-01

In planetary surface sciences, digital terrain models (DTM) are paramount when it comes to understanding and quantifying processes. In this contribution an approach for the derivation of digital terrain models from stereo images of the NASA Mars Reconnaissance Orbiter (MRO) Context Camera (CTX) are described. CTX consists of a 350 mm focal length telescope and 5000 CCD sensor elements and is operated as pushbroom camera. It acquires images with ~6 m/px over a swath width of ~30 km of the Mars surface [1]. Today, several approaches for the derivation of CTX DTMs exist [e. g. 2, 3, 4]. The discussed approach here is based on established software and combines them with proprietary software as described below. The main processing task for the derivation of CTX stereo DTMs is based on six steps: (1) First, CTX images are radiometrically corrected using the ISIS software package [5]. (2) For selected CTX stereo images, exterior orientation data from reconstructed NAIF SPICE data are extracted [6]. (3) In the next step High Resolution Stereo Camera (HRSC) DTMs [7, 8, 9] are used for the rectification of CTX stereo images to reduce the search area during the image matching. Here, HRSC DTMs are used due to their higher spatial resolution when compared to MOLA DTMs. (4) The determination of coordinates of homologous points between stereo images, i.e. the stereo image matching process, consists of two steps: first, a cross-correlation to obtain approximate values and secondly, their use in a least-square matching (LSM) process in order to obtain subpixel positions. (5) The stereo matching results are then used to generate object points from forward ray intersections. (6) As a last step, the DTM-raster generation is performed using software developed at the German Aerospace Center, Berlin. Whereby only object points are used that have a smaller error than a threshold value. References: [1] Malin, M. C. et al., 2007, JGR 112, doi:10.1029/2006JE002808 [2] Broxton, M. J. et al., 2008, LPSC XXXIX, Abstract#2419 [3] Yershov, V. et al., 2015 EPSC 10, EPSC2015-343 [4] Kim, J. R. et al., 2013 EPS 65, 799-809 [5] https://isis.astrogeology.usgs.gov/index.html [6] http://naif.jpl.nasa.gov/naif/index.html [7] Gwinner et al., 2010, EPS 294, 543-540 [8] Gwinner et al., 2015, PSS [9] Dumke, A. et al., 2008, ISPRS, 37, Part B4, 1037-1042

The Role of Passive Film Growth Kinetics and Properties in Stress Corrosion and Crevice Corrosion Susceptibility

DTIC Science & Technology

1975-10-01

Kleinzack-Mathieu Cl. Mertens, J. Meunier, Cl. Vanlengenhaghe, L. de Munck, L. Laureys , L. N. Nellmans, and M . Warzu, Corrosion Science, 3, 239 (1963). 10) H...312O448 DEPARTMENT OF COMMERCE 11. CoMfact/Grat No. WASHINGTON. D.C. 20234 M 1 mRO36-082 12. Spoasoring Organizstion N~me and Complete Address (Street...Ill. Undw Swnay Dr. 111"y Alu-Juhws. AsnluaM ScWaty fr Salome and T0e@* M /WY NATIONAL UMAU OF STANDAWS. Ernest Ambler. Acting Dimwt PART I (To be

Big Fans

NASA Image and Video Library

2018-03-05

Shown in this image from NASA's Mars Reconnaissance Orbiter (MRO) are alluvial fans, fan-shaped deposits emerging from regions of steep topography. Alluvial fans on Mars are thought to be ancient and record past episodes of flowing water. This image shows part of one of those fans, which has been eroded. The old stream channels now stand above the rest of the fan as ridges, mostly in the southern (bottom) part of the image. This can occur because the channel materials are more resistant to erosion; perhaps they had larger grains (gravel) or because minerals deposited from the water cemented together. https://photojournal.jpl.nasa.gov/catalog/PIA22332

Helicopter Electro-Optical System Display Requirements. 1. The Effects of CRT Display Size, System Gamma Function, and Terrain Type on Pilots’ Required Display Luminance

DTIC Science & Technology

1980-03-01

full-color terrain model designed to 6 ,. .. ., CINE MA ICiINE h MRO FILM To’ N U Ix v M C CTMIRROR MONITOR FRESNEL REAR- PROJECTION SCREEN Z...ments of NOE flight, recorded on videotape. One segment was filmed at the Hunter-Liggett, Calif., ntilitary reservation, and the other segment was... filmed near Fort Rucker, Ala. The tapes were viewed by each participant pilot on the 13-cm and the 26-cm CRT displays. They could attenuate the display

A Volcanic Fissure

NASA Image and Video Library

2017-04-26

Although Mars is known for having the largest volcano in our solar system, Olympus Mons, we also find small-scale volcanic features on its surface, as shown in this image from HiRISE onboard NASA's Mars Reconnaissance Orbiter (MRO). This fissure, less than 500 meters across at its widest point, lies in the Tharsis region and is believed to be a vent from which lava flowed in ancient eruptions. The total volume of lava released from this fissure is much less than what would erupt from nearby volcanoes, but the mark left on the landscape is dramatic nonetheless. https://photojournal.jpl.nasa.gov/catalog/PIA21601

Smoke and fire Rocket-engine ablaze on This Week @NASA – August 14, 2015

NASA Image and Video Library

2015-08-14

On Aug. 13, NASA conducted a test firing of the RS-25 rocket engine at Stennis Space Center. The 535 second test was the sixth in the current series of seven developmental tests of the former space shuttle main engine. Four RS-25 engines will power the core stage of the new Space Launch System (SLS) rocket, which will carry humans deeper into space than ever before, including to an asteroid and Mars. Also, Veggies in space, Russian spacewalk, Supply ship undocks from ISS, Smallest giant black hole, 10th anniversary of MRO launch and more!

Osteopoikilosis and multiple exostoses caused by novel mutations in LEMD3 and EXT1 genes respectively - coincidence within one family

PubMed Central

2010-01-01

Background Osteopoikilosis is a rare autosomal dominant genetic disorder, characterised by the occurrence of the hyperostotic spots preferentially localized in the epiphyses and metaphyses of the long bones, and in the carpal and tarsal bones [1]. Heterozygous LEMD3 gene mutations were shown to be the primary cause of the disease [2]. Association of the primarily asymptomatic osteopokilosis with connective tissue nevi of the skin is categorized as Buschke-Ollendorff syndrome (BOS) [3]. Additionally, osteopoikilosis can coincide with melorheostosis (MRO), a more severe bone disease characterised by the ectopic bone formation on the periosteal and endosteal surface of the long bones [4-6]. However, not all MRO affected individuals carry germ-line LEMD3 mutations [7]. Thus, the genetic cause of MRO remains unknown. Here we describe a familial case of osteopoikilosis in which a novel heterozygous LEMD3 mutation coincides with a novel mutation in EXT1, a gene involved in aetiology of multiple exostosis syndrome. The patients affected with both LEMD3 and EXT1 gene mutations displayed typical features of the osteopoikilosis. There were no additional skeletal manifestations detected however, various non-skeletal pathologies coincided in this group. Methods We investigated LEMD3 and EXT1 in the three-generation family from Poland, with 5 patients affected with osteopoikilosis and one child affected with multiple exostoses. Results We found a novel c.2203C > T (p.R735X) mutation in exon 9 of LEMD3, resulting in a premature stop codon at amino acid position 735. The mutation co-segregates with the osteopoikilosis phenotype and was not found in 200 ethnically matched controls. Another new substitution G > A was found in EXT1 gene at position 1732 (cDNA) in Exon 9 (p.A578T) in three out of five osteopoikilosis affected family members. Evolutionary conservation of the affected amino acid suggested possible functional relevance, however no additional skeletal manifestations were observed other then those specific for osteopoikilosis. Finally in one member of the family we found a splice site mutation in the EXT1 gene intron 5 (IVS5-2 A > G) resulting in the deletion of 9 bp of cDNA encoding three evolutionarily conserved amino acid residues. This child patient suffered from a severe form of exostoses, thus a causal relationship can be postulated. Conclusions We identified a new mutation in LEMD3 gene, accounting for the familial case of osteopoikilosis. In the same family we identified two novel EXT1 gene mutations. One of them A598T co-incided with the LEMD3 mutation. Co-incidence of LEMD3 and EXT1 gene mutations was not associated with a more severe skeletal phenotype in those patients. PMID:20618940

Probiotics [LGG-BB12 or RC14-GR1] versus placebo as prophylaxis for urinary tract infection in persons with spinal cord injury [ProSCIUTTU]: a study protocol for a randomised controlled trial.

PubMed

Lee, Bonsan Bonne; Toh, Swee-Ling; Ryan, Suzanne; Simpson, Judy M; Clezy, Kate; Bossa, Laetitia; Rice, Scott A; Marial, Obaydullah; Weber, Gerard; Kaur, Jasbeer; Boswell-Ruys, Claire; Goodall, Stephen; Middleton, James; Tudehope, Mark; Kotsiou, George

2016-04-16

Urinary tract infections [UTIs] are very common in people with Spinal Cord Injury [SCI]. UTIs are increasingly difficult and expensive to treat as the organisms that cause them become more antibiotic resistant. Among the SCI population, there is a high rate of multi-resistant organism [MRO] colonisation. Non-antibiotic prevention strategies are needed to prevent UTI without increasing resistance. Probiotics have been reported to be beneficial in preventing UTIs in post-menopausal women in several in vivo and in vitro studies. The main aim of this study is to determine whether probiotic therapy with combinations of Lactobacillus reuteri RC-14 + Lactobacillus rhamnosus GR-1 [RC14-GR1] and/or Lactobacillus rhamnosus GG + Bifidobacterium BB-12 [LGG-BB12] are effective in preventing UTI in people with SCI compared to placebo. This is a multi-site randomised double-blind double-dummy placebo-controlled factorial design study conducted in New South Wales, Australia. All participants have a neurogenic bladder as a result of spinal injury. Recruitment started in April 2011. Participants are randomised to one of four arms, designed for factorial analysis of LGG-BB12 and/or RC14-GR1 v Placebo. This involves 24 weeks of daily oral treatment with RC14-GR1 + LGG-BB12, RC14-GR1 + placebo, LGG-BB12 + placebo or two placebo capsules. Randomisation is stratified by bladder management type and inpatient status. Participants are assessed at baseline, three months and six months for Short Form Health Survey [SF-36], microbiological swabs of rectum, nose and groin; urine culture and urinary catheters for subjects with indwelling catheters. A bowel questionnaire is administered at baseline and three months to assess effect of probiotics on bowel function. The primary outcome is time from randomisation to occurrence of symptomatic UTI. The secondary outcomes are change of MRO status and bowel function, quality of life and cost-effectiveness of probiotics in persons with SCI. The primary outcome will be analysed using survival analysis of factorial groups, with Cox regression modelling to test the effect of each treatment while allowing for the other, assuming no interaction effect. Hazard ratios and Kaplan-Meier survival curves will be used to summarise results. If these probiotics are shown to be effective in preventing UTI and MRO colonisation, they would be a very attractive alternative for UTI prophylaxis and for combating the increasing rate of antibiotic resistance after SCI. Australian New Zealand Clinical Trials Registry [ ACTRN 12610000512022 ]. Date of registration: 21 June 2010.

Mars-GRAM 2010: Additions and Resulting Improvements

NASA Technical Reports Server (NTRS)

Justh, Hilary L.; Burns, K. Lee

2013-01-01

The Mars Global Reference Atmospheric Model (Mars-GRAM) is an engineering-level atmospheric model widely used for diverse mission applications. Mars-GRAM has been utilized during previous aerobraking operations in the atmosphere of Mars. Mars-GRAM has also been used in the prediction and validation of Mars Pathfinder hypersonic aerodynamics, the aerothermodynamic and entry dynamics studies for Mars Polar Lander, the landing site selection process for the Mars Science Laboratory (MSL), the Mars Aerocapture System Study (MASS) as well as the Aerocapture Technology Assessment Group (TAG). Most recently, Mars-GRAM 2010 was used to develop the onboard atmospheric density estimator that is part of the Autonomous Aerobraking Development Plan. The most recent release of Mars-GRAM 2010 contains several changes including an update to Fortran 90/95 and the addition of adjustment factors. Following the completion of a comparison analysis between Mars-GRAM, Thermal Emission Spectrometer (TES), as well as Mars Global Surveyor (MGS), Mars Odyssey (ODY), and Mars Reconnaissance Orbiter (MRO) aerobraking density data, adjustment factors were added to Mars-GRAM 2010 that alter the input data from National Aeronautics and Space Administration (NASA) Ames Mars General Circulation Model (MGCM) and the University of Michigan Mars Thermospheric General Circulation Model (MTGCM) for the mapping year 0 user-controlled dust case. The addition of adjustment factors resolved the issue of previous versions of Mars-GRAM being less than realistic when used for sensitivity studies for mapping year 0 and large optical depth values, such as tau equal to 3. Mars-GRAM was evaluated at locations and times of TES limb observations and adjustment factors were determined. For altitudes above 80 km and below 135 km, Mars-GRAM (MTGCM) densities were compared to aerobraking densities measured by Mars Global Surveyor (MGS), Mars Odyssey (ODY), and Mars Reconnaissance Orbiter (MRO) to determine the adjustment factors. The adjustment factors generated by this process had to satisfy the gas law as well as the hydrostatic relation and are expressed as a function of height (z), Latitude (Lat) and areocentric solar longitude (Ls). The greatest adjustments are made at large optical depths such as tau greater than 1. The addition of the adjustment factors has led to better correspondence to TES Limb data from 0-60 km altitude as well as better agreement with MGS, ODY and MRO data at approximately 90-130 km altitude. Improved Mars-GRAM atmospheric simulations for various locations, times and dust conditions on Mars will be presented at the workshop session. The latest results validating Mars-GRAM 2010 versus Mars Climate Sounder data will also be presented. Mars-GRAM 2010 updates have resulted in improved atmospheric simulations which will be very important when beginning systems design, performance analysis, and operations planning for future aerocapture, aerobraking or landed missions to Mars.

Vertical Distribution of Aerosols and Water Vapor Using CRISM Limb Observations

NASA Astrophysics Data System (ADS)

Smith, M. D.; Wolff, M. J.; Clancy, R. T.; CRISM Science; Operations Teams

2011-12-01

Near-infrared spectra taken in a limb-viewing geometry by the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) on-board the Mars Reconnaissance Orbiter (MRO) provide a useful tool for probing atmospheric structure. Specifically, the observed radiance as a function of wavelength and height above the limb allows the vertical distribution of both dust and ice aerosols to be retrieved. These data serve as an important supplement to the aerosol profiling provided by the MRO/MCS instrument allowing independent validation and giving additional information on particle physical and scattering properties through multi-wavelength studies. A total of at least ten CRISM limb observations have been taken so far covering a full Martian year. Each set of limb observations nominally contains about four dozen scans across the limb giving pole-to-pole coverage for two orbits at roughly 100 and 290 W longitude over the Tharsis and Syrtis/Hellas regions, respectively. At each longitude, limb scans are spaced roughly 10 degrees apart in latitude, with a vertical spatial resolution on the limb of roughly 800 m. Radiative transfer modeling is used to model the observations. We compute synthetic CRISM limb spectra using a discrete-ordinates radiative transfer code that accounts for multiple scattering from aerosols and accounts for spherical geometry of the limb observations by integrating the source functions along curved paths in that coordinate system. Retrieved are 14-point vertical profiles for dust and water ice aerosols with resolution of 0.4 scale heights between one and six scale heights above the surface. After the aerosol retrieval is completed, the abundances of CO2 (or surface pressure) and H2O gas are retrieved by matching the depth of absorption bands at 2000 nm for carbon dioxide and at 2600 nm for water vapor. In addition to the column abundance of water vapor, limited information on its vertical structure can also be retrieved depending on the signal available from aerosol scattering. Significant differences are seen in the retrieved vertical profiles of dust and water ice as a function of season. Dust typically extends to higher altitudes during the perihelion season. Ice aerosols are often observed to cap the dust layer during all seasons. Water vapor is observed to be deeply mixed in the perihelion season and confined near the surface in the aphelion season. The CRISM limb-geometry observations support the quantitative retrieval of aerosol and gas vertical profiles. These quantities cannot be retrieved using nadir observations, and they enable the study of important new science questions. The CRISM limbs also serve as a valuable supplement to the MRO/MCS limb profiles, enabling validation and multi-wavelength comparisons. Additional CRISM limb-geometry sets will continue to be taken approximately every two months (~30 degrees of Ls) as operations allow.

Transient Slope Lineae Formation in a Well-Preserved Crater

NASA Image and Video Library

2017-11-20

This enhanced color image from NASA's Mars Reconnaissance Orbiter (MRO) shows what are called "recurring slope lineae"s in Tivat Crater. The narrow, dark flows descend downhill (towards the upper left). Analysis shows that the flows all end at approximately the same slope, which is similar to the angle of repose for sand. RSL are mostly found on steep rocky slopes in dark regions of Mars, such as the southern mid-latitudes, Valles Marineris near the equator, and in Acidalia Planitia on the northern plains. The appearance and growth of these features resemble seeping liquid water, but how they form remains unclear, and this research demonstrated that the RSL flows seen by HiRISE are likely moving granular material like sand and dust. These findings indicate that present-day Mars may not have a significant volume of liquid water. The water-restricted conditions that exist on Mars would make it difficult for Earth-like life to exist near the surface of the planet. The map is projected here at a scale of 25 centimeters (9.8 inches) per pixel. [The original image scale is 25.6 centimeters (10.8 inches) per pixel (with 1 x 1 binning); objects on the order of 77 centimeters (30.3 inches) across are resolved.] North is up. https://photojournal.jpl.nasa.gov/catalog/PIA22114

Honeycomb-Textured Landforms in Northwestern Hellas Planitia

NASA Image and Video Library

2017-11-28

This image from NASA's Mars Reconnaissance Orbiter (MRO) targets a portion of a group of honeycomb-textured landforms in northwestern Hellas Planitia, which is part of one of the largest and most ancient impact basins on Mars. In a larger Context Camera image, the individual "cells" are about 5 to 10 kilometers wide. With HiRISE, we see much greater detail of these cells, like sand ripples that indicate wind erosion has played some role here. We also see distinctive exposures of bedrock that cut across the floor and wall of the cells. These resemble dykes, which are usually formed by volcanic activity. Additionally, the lack of impact craters suggests that the landscape, along with these features, have been recently reshaped by a process, or number of processes that may even be active today. Scientists have been debating how these honeycombed features are created, theorizing from glacial events, lake formation, volcanic activity, and tectonic activity, to wind erosion. The map is projected here at a scale of 50 centimeters (19.7 inches) per pixel. [The original image scale is 53.8 centimeters (21.2 inches) per pixel (with 2 x 2 binning); objects on the order of 161 centimeters (23.5 inches) across are resolved.] North is up. https://photojournal.jpl.nasa.gov/catalog/PIA22118

A New Impact Site in the Southern Middle Latitudes

NASA Image and Video Library

2017-04-05

Over 500 new impact events have been detected from before-and-after images from NASA's Mars Reconnaissance Orbiter, mostly from MRO's Context Camera, with a HiRISE followup. Those new craters that expose shallow ice are of special interest, especially at latitudes where not previously detected, to better map the ice distribution. We hope to find ice at relatively low latitudes both for understanding recent climate change and as a resource for possible future humans on Mars. This new impact, which occurred between August and December 2016 (at 42.5 degree South latitude) would provide an important constraint if ice was detected. Alas, the HiRISE color image does not indicate that ice is exposed. There is an elongated cluster of new craters (or just dark spots where the craters are too small to resolve), due to an oblique impact in which the bolide fragmented in the Martian atmosphere. The map is projected here at a scale of 25 centimeters (9.8 inches) per pixel. [The original image scale is 25.1 centimeters (9.9 inches) per pixel (with 1 x 1 binning); objects on the order of 75 centimeters (29.5 inches) across are resolved.] North is up. https://photojournal.jpl.nasa.gov/catalog/PIA21578

Discovery of jarosite within the Mawrth Vallis region of Mars: Implications for the geologic history of the region

NASA Astrophysics Data System (ADS)

Farrand, William H.; Glotch, Timothy D.; Rice, James W.; Hurowitz, Joel A.; Swayze, Gregg A.

2009-12-01

Analysis of visible to near infrared reflectance data from the MRO CRISM hyperspectral imager has revealed the presence of an ovoid-shaped landform, approximately 3 by 5 km in size, within the layered terrains surrounding the Mawrth Vallis outflow channel. This feature has spectral absorption features consistent with the presence of the ferric sulfate mineral jarosite, specifically a K-bearing jarosite (KFe 3(SO 4) 2(OH) 6). Terrestrial jarosite is formed through the oxidation of iron sulfides in acidic environments or from basaltic precursor minerals with the addition of sulfur. Previously identified phyllosilicates in the Mawrth Vallis layered terrains include a basal sequence of layers containing Fe-Mg smectites and an upper set of layers of hydrated silica and aluminous phyllosilicates. In terms of its fine scale morphology revealed by MRO HiRISE imagery, the jarosite-bearing unit has fracture patterns very similar to that observed in Fe-Mg smectite-bearing layers, but unlike that observed in the Al-bearing phyllosilicate unit. The ovoid-shaped landform is situated in an east-west bowl-shaped depression superposed on a north sloping surface. Spectra of the ovoid-shaped jarosite-bearing landform also display an anomalously high 600 nm shoulder, which may be consistent with the presence of goethite and a 1.92 μm absorption which could indicate the presence of ferrihydrite. Goethite, jarosite, and ferrihydrite can be co-precipitated and/or form through transformation of schwertmannite, both processes generally occurring under low pH conditions (pH 2-4). To date, this location appears to be unique in the Mawrth Vallis region and could represent precipitation of jarosite in acidic, sulfur-rich ponded water during the waning stages of drying.

Disappearance of the Propontis Regional Dark Albedo Feature on Mars

NASA Astrophysics Data System (ADS)

Lee, Steven W.; Thomas, P. C.; Cantor, B. A.

2013-10-01

The appearance of Propontis, one of many distinct classical dark albedo features on Mars, has been documented by ground-based observers for well over a century; Propontis was once thought to be the location of a “typical Martian canal”. The roughly circular feature (centered at 38°N, 179°W) covers about 500km in north-south extent. Modern spacecraft observations have shown the northern plains in which Propontis is located to include many subdued craters, knobs, and troughs. Observations by the Mars Color Imager (MARCI) onboard the Mars Reconnaissance Orbiter (MRO) have documented dramatic changes in the Propontis feature during August 2009. Daily MARCI mosaics (spatial resolution of 1 km/pixel) revealed extensive dust storm activity in this region over a ten day period (August 16-25, Ls ~ 322°-327°). At this time, the north polar seasonal ice cap was at maximum extent (reaching southward to about 55°N), and dust storm activity was frequently observed southward of the seasonal cap. These storms apparently led to sufficient deposition of bright dust to effectively “erase” the dark Propontis feature - yielding one of the most significant changes in regional albedo since Mars Global Surveyor began routine global mapping in 1997. Only minor changes have been detected over the course of repeated MARCI observations of this region since late-2009 - Propontis has not yet “recovered” to its previous extent and appearance. MRO is expected to provide ongoing MARCI mapping, enhanced with regular Context Imager (CTX, spatial resolution of 6 m/pixel) monitoring. An overview of the accumulated observations to date will be presented, along with interpretation of the magnitude of sediment transport required to account for the observed changes in Propontis.

Field reconnaissance geologic mapping of the Columbia Hills, Mars, based on Mars Exploration Rover Spirit and MRO HiRISE observations

NASA Astrophysics Data System (ADS)

Crumpler, L. S.; Arvidson, R. E.; Squyres, S. W.; McCoy, T.; Yingst, A.; Ruff, S.; Farrand, W.; McSween, Y.; Powell, M.; Ming, D. W.; Morris, R. V.; Bell, J. F., III; Grant, J.; Greeley, R.; DesMarais, D.; Schmidt, M.; Cabrol, N. A.; Haldemann, A.; Lewis, Kevin W.; Wang, A. E.; Schröder, C.; Blaney, D.; Cohen, B.; Yen, A.; Farmer, J.; Gellert, R.; Guinness, E. A.; Herkenhoff, K. E.; Johnson, J. R.; Klingelhöfer, G.; McEwen, A.; Rice, J. W., Jr.; Rice, M.; deSouza, P.; Hurowitz, J.

2011-07-01

Chemical, mineralogic, and lithologic ground truth was acquired for the first time on Mars in terrain units mapped using orbital Mars Reconnaissance Orbiter's High Resolution Imaging Science Experiment (MRO HiRISE) image data. Examination of several dozen outcrops shows that Mars is geologically complex at meter length scales, the record of its geologic history is well exposed, stratigraphic units may be identified and correlated across significant areas on the ground, and outcrops and geologic relationships between materials may be analyzed with techniques commonly employed in terrestrial field geology. Despite their burial during the course of Martian geologic time by widespread epiclastic materials, mobile fines, and fall deposits, the selective exhumation of deep and well-preserved geologic units has exposed undisturbed outcrops, stratigraphic sections, and structural information much as they are preserved and exposed on Earth. A rich geologic record awaits skilled future field investigators on Mars. The correlation of ground observations and orbital images enables construction of a corresponding geologic reconnaissance map. Most of the outcrops visited are interpreted to be pyroclastic, impactite, and epiclastic deposits overlying an unexposed substrate, probably related to a modified Gusev crater central peak. Fluids have altered chemistry and mineralogy of these protoliths in degrees that vary substantially within the same map unit. Examination of the rocks exposed above and below the major unconformity between the plains lavas and the Columbia Hills directly confirms the general conclusion from remote sensing in previous studies over past years that the early history of Mars was a time of more intense deposition and modification of the surface. Although the availability of fluids and the chemical and mineral activity declined from this early period, significant later volcanism and fluid convection enabled additional, if localized, chemical activity.

Discovery of araneiforms outside of the South Polar Layered Deposits

NASA Astrophysics Data System (ADS)

Schwamb, Megan E.; Aye, K.-Michael; Portyankina, Ganna; Hansen, Candice; Lintott, Chris J.; Allen, Campbell; Allen, Sarah; Calef, Fred J.; Duca, Simone; McMaster, Adam; R. M Miller, Grant

2017-10-01

Mars' south polar region is sculpted by the seasonal cycle of freezing and thawing of exposed carbon dioxide (CO2) ice. In the Southern Spring, CO2 jets loft dust and dirt through cracks in the sublimating CO2 ice sheet to the surface where winds blow the material into the hundreds of thousands of dark fans observed from orbit. During this seasonal process, it is thought that the CO2 gas also exploits weaknesses in the surface below the ice sheet to carve dendritic channels known as araneiforms. Planet Four: Terrains (http://terrains.planetfour.org) is a citizen science project enlisting the general public to review ~6 m/pixel resolution Mars Reconnaissance Orbiter (MRO) Context Camera (CTX) subimages to identify: (1) araneiforms (including features with a central pit and radiating channels known as ‘spiders’) (2) erosional depressions, troughs, mesas, ridges, and quasi-circular pits characteristic of the South Polar Residual Cap (SPRC) which we collectively refer to as ‘Swiss cheese terrain’, and (3) craters.We provide an overview of Planet Four: Terrains and discuss the distributions of our high confidence classic spider araneiforms and Swiss cheese terrain identifications in CTX images covering 11% of the South polar regions at latitudes ≤ -75 degrees N. Previously spiders were reported as being confined to the South Polar Layered Deposits (SPLD). We present the first identification of araneiforms at locations outside of the SPLD and discuss the implications for the CO2 jet hypothesis.Acknowledgements: This work uses data generated via the Zooniverse.org platform, development of which was supported by a Global Impact Award from Google, and by the Alfred P. Sloan Foundation. We also thank the HIRSE and MRO Teams for their help in scheduling and acquiring our requested observations.

Field Reconnaissance Geologic Mapping of the Columbia Hills, Mars: Results from MER Spirit and MRO HiRISE Observations

USGS Publications Warehouse

Crumpler, L.S.; Arvidson, R. E.; Squyres, S. W.; McCoy, T.; Yingst, A.; Ruff, S.; Farrand, W.; McSween, Y.; Powell, M.; Ming, D. W.; Morris, R.V.; Bell, J.F.; Grant, J.; Greeley, R.; DesMarais, D.; Schmidt, M.; Cabrol, N.A.; Haldemann, A.; Lewis, Kevin W.; Wang, A.E.; Schroder, C.; Blaney, D.; Cohen, B.; Yen, A.; Farmer, J.; Gellert, Ralf; Guinness, E.A.; Herkenhoff, K. E.; Johnson, J. R.; Klingelhofer, G.; McEwen, A.; Rice, J. W.; Rice, M.; deSouza, P.; Hurowitz, J.

2011-01-01

Chemical, mineralogic, and lithologic ground truth was acquired for the first time on Mars in terrain units mapped using orbital Mars Reconnaissance Orbiter's High Resolution Imaging Science Experiment (MRO HiRISE) image data. Examination of several dozen outcrops shows that Mars is geologically complex at meter length scales, the record of its geologic history is well exposed, stratigraphic units may be identified and correlated across significant areas on the ground, and outcrops and geologic relationships between materials may be analyzed with techniques commonly employed in terrestrial field geology. Despite their burial during the course of Martian geologic time by widespread epiclastic materials, mobile fines, and fall deposits, the selective exhumation of deep and well-preserved geologic units has exposed undisturbed outcrops, stratigraphic sections, and structural information much as they are preserved and exposed on Earth. A rich geologic record awaits skilled future field investigators on Mars. The correlation of ground observations and orbital images enables construction of a corresponding geologic reconnaissance map. Most of the outcrops visited are interpreted to be pyroclastic, impactite, and epiclastic deposits overlying an unexposed substrate, probably related to a modified Gusev crater central peak. Fluids have altered chemistry and mineralogy of these protoliths in degrees that vary substantially within the same map unit. Examination of the rocks exposed above and below the major unconformity between the plains lavas and the Columbia Hills directly confirms the general conclusion from remote sensing in previous studies over past years that the early history of Mars was a time of more intense deposition and modification of the surface. Although the availability of fluids and the chemical and mineral activity declined from this early period, significant later volcanism and fluid convection enabled additional, if localized, chemical activity.

Terrestrial rock glaciers: a potential analog for Martian lobate flow features (LFF)

NASA Astrophysics Data System (ADS)

Sinha, Rishitosh K.; Vijayan, Sivaprahasam; Bharti, Rajiv R.

2016-05-01

Rock glaciers, regarded as cryospheric ice/water resource in the terrestrial-glacial systems based on their tongue/lobate-shaped flow characteristic and subsurface investigation using ground-penetrating radar. We examined the subsurface, geomorphology, climate-sensitivity and thermophysical properties of a Lobate Flow Feature (LFF) on Mars (30°-60° N and S hemispheres) to compare/assess the potentials of rock glaciers as an analog in suggesting LFFs to be a source of subsurface ice/water. LFFs are generally observed at the foot of impact craters' wall. HiRISE/CTX imageries from MRO spacecraft were used for geomorphological investigation of LFF using ArcMap-10.0 and subsurface investigation was carried out using data from MRO-SHARAD (shallow radar) after integrating with SiesWare-8.0. ENVI-5.0 was used to retrieve thermophysical properties of LFF from nighttime datasets (12.57 μm) acquired by THEMIS instrument-onboard the Mars Odyssey spacecraft and derive LFFs morphometry from MOLA altimeter point tracks onboard MGS spacecraft. Integrating crater chronology tool (Craterstats) with Arc Map, we have derived the formation age of LFF. Our investigation and comparison of LFF to rock glaciers revealed: (1) LFFs have preserved ice at depth 50m as revealed from SHARAD radargram and top-layer composed of rocky-debris material with thermal inertia ( 300-350 Jm-2 K-1s-1/2). (2) LFF formation age ( 10-100 Ma) corresponds to moderate scale debris covered glaciation of a shorter-span suggesting high sensitivity to obliquity-driven climatic shifts. (3) Presence of polygon cracks and high linear-arcuate furrow-and-ridges on the surface indicates presence of buried ice. This work is a significant step towards suggesting LFF to be a potential source of present-day stored ice/water on Mars.

Investigating social functioning after early mild TBI: the quality of parent-child interactions.

PubMed

Lalonde, Gabrielle; Bernier, Annie; Beaudoin, Cindy; Gravel, Jocelyn; Beauchamp, Miriam H

2018-03-01

The young brain is particularly vulnerable to injury due to inherent physiological and developmental factors, and even mild forms of traumatic brain injury (mTBI) can sometimes result in cognitive and behavioural difficulties. Despite the high prevalence of paediatric mTBI, little is known of its impact on children's social functioning. Parent-child relationships represent the centre of young children's social environments and are therefore ideal contexts for studying the potential effects of mTBI on children's social functioning. The aim of this study was to assess the quality of parent-child interactions after mTBI using observational assessment methods and parental report. The sample included 130 children (18-60 months at recruitment) divided into three groups: children with uncomplicated mTBI (n = 47), children with orthopaedic injury (OI, n = 27), and non-injured children (NI, n = 56). The quality of parent-child interactions was assessed 6 months post-injury using the Mutually Responsive Orientation (MRO) scale, an observational measure which focuses on the dyadic nature of parent-child exchanges, and the Parental Stress Index questionnaire (Parent-Child Dysfunctional Interaction (PCDI) domain). Significant differences with medium effect sizes were found between the mTBI group and the NI group on the MRO, but not between the OI group and the other two groups. PCDI scores did not differ across groups, suggesting that observational measures may be more sensitive to changes in parent-child interactions after TBI. The current findings have implications for children's post-injury social development and highlight the importance of monitoring social outcomes even after minor head injuries. © 2016 The British Psychological Society.

Discovery of jarosite within the Mawrth Vallis region of Mars: Implications for the geologic history of the region

USGS Publications Warehouse

Farrand, W. H.; Glotch, T.D.; Rice, J. W.; Hurowitz, J.A.; Swayze, G.A.

2009-01-01

Analysis of visible to near infrared reflectance data from the MRO CRISM hyperspectral imager has revealed the presence of an ovoid-shaped landform, approximately 3 by 5 km in size, within the layered terrains surrounding the Mawrth Vallis outflow channel. This feature has spectral absorption features consistent with the presence of the ferric sulfate mineral jarosite, specifically a K-bearing jarosite (KFe3(SO4)2(OH)6). Terrestrial jarosite is formed through the oxidation of iron sulfides in acidic environments or from basaltic precursor minerals with the addition of sulfur. Previously identified phyllosilicates in the Mawrth Vallis layered terrains include a basal sequence of layers containing Fe-Mg smectites and an upper set of layers of hydrated silica and aluminous phyllosilicates. In terms of its fine scale morphology revealed by MRO HiRISE imagery, the jarosite-bearing unit has fracture patterns very similar to that observed in Fe-Mg smectite-bearing layers, but unlike that observed in the Al-bearing phyllosilicate unit. The ovoid-shaped landform is situated in an east-west bowl-shaped depression superposed on a north sloping surface. Spectra of the ovoid-shaped jarosite-bearing landform also display an anomalously high 600 nm shoulder, which may be consistent with the presence of goethite and a 1.92 ??m absorption which could indicate the presence of ferrihydrite. Goethite, jarosite, and ferrihydrite can be co-precipitated and/or form through transformation of schwertmannite, both processes generally occurring under low pH conditions (pH 2-4). To date, this location appears to be unique in the Mawrth Vallis region and could represent precipitation of jarosite in acidic, sulfur-rich ponded water during the waning stages of drying. ?? 2009 Elsevier Inc. All rights reserved.

Investigation of small scale roughness properties of Martian terrains using Mars Reconnaissance Orbiter data.

NASA Astrophysics Data System (ADS)

Ivanov, A. B.; Rossi, A.

2009-04-01

Studies of layered terrains in polar regions as well as inside craters and other areas on Mars often require knowledge of local topography at much finer resolution than global MOLA topography allows. For example, in the polar layered deposits spatial relationships are important to understand unconformities that are observed on the edges of the layered terrains [15,3]. Their formation process is not understood at this point, yet fine scale topography, joint with ground penetrating radar like SHARAD and MARSIS may shed light on their 3D structure. Landing site analysis also requires knowledge of local slopes and roughness at scales from 1 to 10 m [1,2]. Mars Orbiter Camera [13] has taken stereo images at these scales, however interpretation was difficult due to unstable behavior of the Mars Global Surveyor spacecraft during image take (wobbling effect). Mars Reconnaissance Orbiter (MRO) is much better stabilized, since it is required for optimal operation of its high resolution camera. In this work we have utilized data from MRO sensors (CTX camera [11] and HIRISE camera [12] in order to derive digital elevation models (DEM) from images targeted as stereo pairs. We employed methods and approaches utilized for the Mars Orbiter Camera (MOC) stereo data [4,5]. CTX data varies in resolution and stereo pairs analyzed in this work can be derived at approximately 10m scale. HIRISE images allow DEM post spacing at around 1 meter. The latter are very big images and our computer infrastructure was only able to process either reduced resolution images, covering larger surface or working with smaller patches at the original resolution. We employed stereo matching technique described in [5,9], in conjunction with radiometric and geometric image processing in ISIS3 [16]. This technique is capable of deriving tiepoint co-registration at subpixel precision and has proven itself when used for Pathfinder and MER operations [8]. Considerable part of this work was to accommodate CTX and HIRISE image processing in the existing data processing pipeline and improve it at the same time. Currently the workflow is not finished: DEM units are relative and are not in elevation. We have been able to derive successful DEMs from CTX data Becquerel [14] and Crommelin craters as well as for some areas in the North Polar Layered Terrain. Due to its tremendous resolution HIRISE data showing great surface detail, hence allowing better correlation than other sensors considered in this work. In all cases DEM were showing considerable potential for exploration of terrain characteristics. Next steps include cross validation results with DEM produced by other teams and sensors (HRSC [6], HIRISE [7]) and providing elevation in terms of absolute height over a MOLA areoid. MRO imaging data allows us an unprecedented look at Martian terrain. This work provides a step forward derivation of DEM from HIRISE and CTX datasets and currently undergoing validation vs. other existing datasets. We will present our latest results for layering structures in both North and South Polar Layered deposits as well as layered structures inside Becquerel and Crommelin craters. Digital Elevation models derived from the CTX sensor can also be utilized effectively as a input for clutter reduction models, which are in turn used for the ground penetrating SHARAD instrument [13]. References. [1] R. Arvidson, et al. Mars exploration program 2007 phoenix landing site selection and characteristics. Journal of Geophysical Research-Planets, 113, JUN 19 2008. [2] M. Golombek, et al. Assessment of mars exploration rover landing site predictions. Nature, 436(7047):44-48, JUL 7 2005. [3] K. E. Herkenhoff, et al. Meter-scale morphology of the north polar region of mars. Science, 317(5845):1711-1715, SEP 21 2007. [4] A. B. Ivanov. Ten-Meter Scale Topography and Roughness of Mars Exploration Rovers Landing Sites and Martian Polar Regions. volume 34 of Lunar and Planetary Inst. Technical Report, pages 2084-+, Mar. 2003. [5] A. B. Ivanov and J. J. Lorre. Analysis of Mars Orbiter Camera Stereo Pairs. In Lunar and Planetary Institute Conference Abstracts, volume 33 of Lunar and Planetary Inst. Technical Report, pages 1845-+, Mar. 2002. [6] R. Jaumann, et al. The high-resolution stereo camera (HRSC) experiment on mars express: Instrument aspects and experiment conduct from interplanetary cruise through the nominal mission. Planetary and Space Science, 55(7-8):928-952, MAY 2007. [7] R. L. Kirk, et al. Ultrahigh resolution topographic mapping of mars with MRO HIRISE stereo images: Meter-scale slopes of candidate phoenix landing sites. Journal of Geophysical Research-Planets, 113, NOV 15 2008. [8] S. Lavoie, et al. Processing and analysis of mars pathfinder science data at the jet propulsion laboratory's science data processing systems section. Journal of Geophysical Research-Planets, 104(E4):8831-8852, APR 25 1999. [9] J. J. Lorre, et al. Recent developments at JPL in the application of image processing to astronomy. In D. L. Crawford, editor, Instrumentation in Astronomy III, volume 172 of Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, pages 394-402, 1979. [10] M. Malin, et al. Early views of the martian surface from the mars orbiter camera of mars global surveyor. Science, 279(5357):1681-1685, MAR 13 1998. [11] M. C. Malin,et al. Context camera investigation on board the mars reconnaissance orbiter. Journal of Geophysical Research-Planets, 112(E5), MAY 18 2007. [12] A. S. McEwen, et al.. Mars reconnaissance orbiter's high resolution imaging science experiment (HIRISE). Journal of Geophysical Research-Planets, 112(E5), MAY 17 2007. [13] A. Rossi, et al. Multi-spacecraft synergy with MEX HRSC and MRO SHARAD: Light-Toned Deposits in crater bulges. AGU Fall Meeting Abstracts, pages B1371+, Dec. 2008. [14] A. P. Rossi, et al. Stratigraphic architecture and structural control on sediment emplacement in Becquerel crater (Mars). volume 40. Lunar and Planetary Science Institute, 2009. [15] K. L. Tanaka,et al. North polar region of mars: Advances in stratigraphy, structure, and erosional modification, AUG 2008. Icarus. [16] USGS. Planetary image processing software: ISIS3. http://isis.astrogeology.usgs.gov/

On the Linear Stability of Two-Dimensional Barium Clouds. I. The Inviscid Case.

DTIC Science & Technology

1984-04-30

MECVRDT FKPR--7;PG ON13& TYPE OF REPORT 13R1. TIME 8 CIEDO 1 4 AT OF REOT .Y,. Mo.. Day, 37PAECON Interim FROM 10183 TO17’I April 30, 1984 I37 IS...Note that if we write our perturbation ( 8 ) in terms of arc length ro 0 multiplied by a wavenumber k then cos m6 - cos k r0 and m/ro - k (10) 4 ...38 APR 84 NRL-MR-53i2 UNCLASSIFIED F/G 4 /1 NI I EEEEEEEEE L &, 12 am... ~ a m II) ,uut_ _- 7-_ MICROCOPY RESOLUTION TEST CHART NATIONAL BUREAU OF

Thermal Modeling of the Mars Reconnaissance Orbiter's Solar Panel and Instruments during Aerobraking

NASA Technical Reports Server (NTRS)

Dec, John A.; Gasbarre, Joseph F.; Amundsen, Ruth M.

2007-01-01

The Mars Reconnaissance Orbiter (MRO) launched on August 12, 2005 and started aerobraking at Mars in March 2006. During the spacecraft s design phase, thermal models of the solar panels and instruments were developed to determine which components would be the most limiting thermally during aerobraking. Having determined the most limiting components, thermal limits in terms of heat rate were established. Advanced thermal modeling techniques were developed utilizing Thermal Desktop and Patran Thermal. Heat transfer coefficients were calculated using a Direct Simulation Monte Carlo technique. Analysis established that the solar panels were the most limiting components during the aerobraking phase of the mission.

Ice Block Avalanche

NASA Image and Video Library

2018-06-25

One of the most actively changing areas on Mars are the steep edges of the North Polar layered deposits. This image from NASA's Mars Reconnaissance Orbiter (MRO) shows many new ice blocks compared to an earlier image in December 2006. An animation shows one example, where a section of ice cliff collapsed. The older image (acquired in bin-2 mode) is not as sharp as the newer one. HiRISE has been re-imaging regions first photographed in 2006 through 2007, six Mars years ago. This long baseline allows us to see large, rare changes as well as many smaller changes. More information is available at https://photojournal.jpl.nasa.gov/catalog/PIA22535

The Geology of Mars as Seen by MRO's HiRISE

NASA Astrophysics Data System (ADS)

McEwen, A. S.

2007-12-01

By September 2007 the High Resolution Imaging Science Experiment (HiRISE) had acquired more than 3,000 images of Mars at resolutions as high as 25 cm/pixel in the 3 PM mapping orbit of Mars Reconnaissance Orbiter, covering about 0.2 percent of the surface. These images are helping to address a broad range of science issues, as presented in dozens of abstracts to this conference. In this talk I will focus on several topics. (1) The color data is proving quite valuable to reduce the ambiguities of B&W images; to correlate deposits and better define the stratigraphy; and to extend mineral identifications to the scale of outcrops. (2) The nature of the Martian highlands is being revealed, with the identification of megabreccia, hydrous minerals (by OMEGA and CRISM spectrometers), and the detailed nature of the layered or massive stratigraphy where exposed in cross- section. (3) There is new evidence for the roles of water in the most recent large (at least 1 km diameter) impact craters, which may have implications for the altered mineralogy of the ancient crust. (4) New observations and measurements are leading to improved understanding of slope processes such as gullies, creep, and mass wasting. We are producing meter-scale digital elevation models to test high-priority science questions.

Failure of Harmonic Gears During Verification of a Two-Axis Gimbal for the Mars Reconnaissance Orbiter Spacecraft

NASA Technical Reports Server (NTRS)

Johnson, Michael R.; Gehling, Russ; Head, Ray

2006-01-01

The Mars Reconnaissance Orbiter (MRO) spacecraft has three two-axis gimbal assemblies that support and move the High Gain Antenna and two solar array wings. The gimbal assemblies are required to move almost continuously throughout the mission's seven-year lifetime, requiring a large number of output revolutions for each actuator in the gimbal assemblies. The actuator for each of the six axes consists of a two-phase brushless dc motor with a direct drive to the wave generator of a size-32 cup-type harmonic gear. During life testing of an actuator assembly, the harmonic gear teeth failed completely, leaving the size-32 harmonic gear with a maximum output torque capability less than 10% of its design capability. The investigation that followed the failure revealed limitations of the heritage material choices that were made for the harmonic gear components that had passed similar life requirements on several previous programs. Additionally, the methods used to increase the stiffness of a standard harmonic gear component set, while accepted practice for harmonic gears, is limited in its range. The stiffness of harmonic gear assemblies can be increased up to a maximum stiffness point that, if exceeded, compromises the reliability of the gear components for long life applications.

Correcting spacecraft jitter in HiRISE images

USGS Publications Warehouse

Sutton, S. S.; Boyd, A.K.; Kirk, Randolph L.; Cook, Debbie; Backer, Jean; Fennema, A.; Heyd, R.; McEwen, A.S.; Mirchandani, S.D.; Wu, B.; Di, K.; Oberst, J.; Karachevtseva, I.

2017-01-01

Mechanical oscillations or vibrations on spacecraft, also called pointing jitter, cause geometric distortions and/or smear in high resolution digital images acquired from orbit. Geometric distortion is especially a problem with pushbroom type sensors, such as the High Resolution Imaging Science Experiment (HiRISE) instrument on board the Mars Reconnaissance Orbiter (MRO). Geometric distortions occur at a range of frequencies that may not be obvious in the image products, but can cause problems with stereo image correlation in the production of digital elevation models, and in measuring surface changes over time in orthorectified images. The HiRISE focal plane comprises a staggered array of fourteen charge-coupled devices (CCDs) with pixel IFOV of 1 microradian. The high spatial resolution of HiRISE makes it both sensitive to, and an excellent recorder of jitter. We present an algorithm using Fourier analysis to resolve the jitter function for a HiRISE image that is then used to update instrument pointing information to remove geometric distortions from the image. Implementation of the jitter analysis and image correction is performed on selected HiRISE images. Resulting corrected images and updated pointing information are made available to the public. Results show marked reduction of geometric distortions. This work has applications to similar cameras operating now, and to the design of future instruments (such as the Europa Imaging System).

Liquid Water on the Surface of Mars Today: Present Gully Activity Observed by the Mars Reconnaissance Orbiter (MRO) and Mars Global Surveyor (MGS) and Direction for Future Missions

NASA Astrophysics Data System (ADS)

Harrison, T. N.; Malin, M. C.; Edgett, K. S.

2009-12-01

Eight new flows in martian mid-latitude gullies have been found using the MRO Context Camera and MGS Mars Orbiter Camera. Each formed during 1999-2009. Using MRO HiRISE images, we find that the morphology and inferred emplacement behavior of these features is consistent with those of debris flows fluidized by a liquid medium and not by dry, granular flows. Evidence comes from the patterns of flow around obstacles, ponding in and subsequent overtopping of topographic depressions, and super-elevation of deposits on channel banks where the channels change direction, attributes consistent with a liquid but not with fluid-like granular flow. Additional evidence includes anastomoses in distal reaches and lobate terminations. Of the 8 flows, 3 have formation dates constrained to within a single Mars year (although not the same year); these 3 formed during autumn to early spring, demonstrating that summer warming is not participating in creating the liquid (i.e., that would melt snow or ice). The new gully deposits indicate that some gullies are currently active, suggesting that Mars has liquid water today and it occasionally appears on the planet’s surface. NASA’s Mars Exploration Program has focused on the “follow the water” theme and is now shifting toward “habitability” and life detection. Places where liquid water comes to the Martian surface today warrant detailed investigation. Martian astrobiology involves the search for evidence of extinct and extant life. Discovery of ancient sedimentary rocks shifted emphasis from the Viking-era pursuit of present-day microbial life to MSL’s focus on habitable environments. Recent descriptions of contemporary methane production have renewed interest in searching for extant life. Missions to locations of potential present day life, whether indicated by methane or liquid water, must deal with the associated planetary protection issues (they are “special regions”). More information about such locations is critical. Present mission planning is focused on methane (a 2016 trace gas orbiter), while the on-going gully activity is not being subjected to the same level of examination. Active gully locations might represent the optimum landing site for the much-discussed astrobiology rover mission (2018), provided additional information can be developed (i.e., the occurrence and recurrence rates and locations, and further evidence of the role of water). Long-term orbital monitoring at high resolution plus lander deployment from orbit after activity is detected are key gully mission objectives, as are the development of vehicles that can negotiate steep slopes and instruments that can detect sub-surface ice and/or water. As an added benefit, rather than learning only about a specific landing site, the knowledge gained from a single landed mission at a gullied site would be applicable to thousands of other locations on Mars.

An Inverted Crater West of Mawrth Vallis

NASA Image and Video Library

2017-11-28

This image from NASA's Mars Reconnaissance Orbiter (MRO) captures details of an approximately 1-kilometer inverted crater west of Mawrth Vallis. A Context Camera image provides context for the erosional features observed at this site. The location of this HiRISE image is north of the proposed landing ellipse for the ExoMars 2020 rover mission that will investigate diverse rocks and minerals related to ancient water-related activity in this region. Prolonged erosion removed less resistant rocks leaving behind other rocks that stand up locally such as the crater seen here and other nearby remnants. These resistant layers may belong to a phase of volcanism and/or water-related activity that carved Mawrth Vallis and filled in existing craters, and other lower-lying depressions, with darker materials. Erosion has also exposed these layers down to older, more resistant lighter rocks that are clay-bearing. The diversity of exposed bedrock made this location an ideal candidate for exploring a potentially water-rich ancient environment that might have once harbored life. The map is projected here at a scale of 25 centimeters (9.8 inches) per pixel. [The original image scale is 28.7 centimeters (11.3 inches) per pixel (with 1 x 1 binning); objects on the order of 86 centimeters (33.9 inches) across are resolved.] North is up. https://photojournal.jpl.nasa.gov/catalog/PIA22117

Yardangs: Nature's Weathervanes

NASA Image and Video Library

2017-11-28

The prominent tear-shaped features in this image from NASA's Mars Reconnaissance Orbiter (MRO) are erosional features called yardangs. Yardangs are composed of sand grains that have clumped together and have become more resistant to erosion than their surrounding materials. As the winds of Mars blow and erode away at the landscape, the more cohesive rock is left behind as a standing feature. (This Context Camera image shows several examples of yardangs that overlie the darker iron-rich material that makes up the lava plains in the southern portion of Elysium Planitia.) Resistant as they may be, the yardangs are not permanent, and will eventually be eroded away by the persistence of the Martian winds. For scientists observing the Red Planet, yardangs serve as a useful indicator of regional prevailing wind direction. The sandy structures are slowly eroded down and carved into elongated shapes that point in the downwind direction, like giant weathervanes. In this instance, the yardangs are all aligned, pointing towards north-northwest. This shows that the winds in this area generally gust in that direction. The map is projected here at a scale of 50 centimeters (19.7 inches) per pixel. [The original image scale is 55.8 centimeters (21 inches) per pixel (with 2 x 2 binning); objects on the order of 167 centimeters (65.7 inches) across are resolved.] North is up. https://photojournal.jpl.nasa.gov/catalog/PIA22119

2016 Mars Insight Mission Design and Navigation

NASA Technical Reports Server (NTRS)

Abilleira, Fernando; Frauenholz, Ray; Fujii, Ken; Wallace, Mark; You, Tung-Han

2014-01-01

Scheduled for a launch in the 2016 Earth to Mars opportunity, the Interior Exploration using Seismic Investigations, Geodesy, and Heat Transport (InSight) Mission will arrive to Mars in late September 2016 with the primary objective of placing a science lander on the surface of the Red Planet followed by the deployment of two science instruments to investigate the fundamental processes of terrestrial planet formation and evolution. In order to achieve a successful landing, the InSight Project has selected a launch/arrival strategy that satisfies the following key and driving requirements: (1) Deliver a total launch mass of 727 kg, (2) target a nominal landing site with a cumulative Delta V99 less than 30 m/s, and (3) approach EDL with a V-infinity upper limit of 3.941 km/s and (4) an entry flight-path angle (EFPA) of -12.5 +/- 0.26 deg, 3-sigma; the InSight trajectories have been designed such that they (5) provide UHF-band communications via Direct-To-Earth and MRO from Entry through landing plus 60 s, (6) with injection aimpoints biased away from Mars such that the probability of the launch vehicle upper stage impacting Mars is less than 1.0 X 10(exp 4) for fifty years after launch, and (7) non-nominal impact probabilities due to failure during the Cruise phase less than 1.0 X 10(exp 2).

Phobos MRO/CRISM visible and near-infrared (0.5-2.5 μm) spectral modeling

NASA Astrophysics Data System (ADS)

Pajola, Maurizio; Roush, Ted; Dalle Ore, Cristina; Marzo, Giuseppe A.; Simioni, Emanuele

2018-05-01

This paper focuses on the spectral modeling of the surface of Phobos in the wavelength range between 0.5 and 2.5 μm. We exploit the Phobos Mars Reconnaissance Orbiter/Compact Reconnaissance Imaging Spectrometer for Mars (MRO/CRISM) dataset and extend the study area presented by Fraeman et al. (2012) including spectra from nearly the entire surface observed. Without a priori selection of surface locations we use the unsupervised K-means partitioning algorithm developed by Marzo et al. (2006) to investigate the spectral variability across Phobos surface. The statistical partitioning identifies seven clusters. We investigate the compositional information contained within the average spectra of four clusters using the radiative transfer model of Shkuratov et al. (1999). We use optical constants of Tagish Lake meteorite (TL), from Roush (2003), and pyroxene glass (PM80), from Jaeger et al. (1994) and Dorschner et al. (1995), as previously suggested by Pajola et al. (2013) as inputs for the calculations. The model results show good agreement in slope when compared to the averages of the CRISM spectral clusters. In particular, the best fitting model of the cluster with the steepest spectral slope yields relative abundances that are equal to those of Pajola et al. (2013), i.e. 20% PM80 and 80% TL, but grain sizes that are 12 μm smaller for PM80 and 4 μm smaller for TL (the grain sizes are 11 μm for PM80 and 20 μm for TL in Pajola et al. (2013), respectively). This modest discrepancy may arise from the fact that the areas observed by CRISM and those analyzed in Pajola et al. (2013) are on opposite locations on Phobos and are characterized by different morphological and weathering settings. Instead, as the clusters spectral slopes decrease, the best fits obtained show trends related to both relative abundance and grain size that is not observed for the cluster with the steepest spectral slope. With a decrease in slope there is general increase of relative percentage of PM80 from 12% to 18% and the associated decrease of TL from 88% to 82%. Simultaneously the PM80 grain sizes decrease from 9 to 5 μm and TL grain sizes increase from 13 to 16 μm. The best fitting models show relative abundances and grain sizes that partially overlap. This supports the hypothesis that from a compositional perspective the transition between the highest and lowest slopes on Phobos is subtle, and it is characterized by a smooth change of relative abundances and grain sizes, instead of a distinct dichotomy between the areas.

The Mars Reconnaissance Orbiter Mission: 10 Years of Exploration from Mars Orbit

NASA Technical Reports Server (NTRS)

Johnston, M. Daniel; Zurek, Richard W.

2016-01-01

The Mars Reconnaissance Orbiter ( MRO ) entered Mars orbit on March 10, 2006. After five months of aerobraking, a series of propulsive maneuvers were used to establish the desired low -altitude science orbit. The spacecraft has been on station in its 255 x 320 k m, sun -synchronous (approximately 3 am -pm ), primary science orbit since September 2006 performing both scientific and Mars programmatic support functions. This paper will provide a summary of the major achievements of the mission to date and the major flight activities planned for the remainder of its third Extended Mission (EM3). Some of the major flight challenges the flight team has faced are also discussed.

Solar System Visualization (SSV) Project

NASA Technical Reports Server (NTRS)

Todd, Jessida L.

2005-01-01

The Solar System Visualization (SSV) project aims at enhancing scientific and public understanding through visual representations and modeling procedures. The SSV project's objectives are to (1) create new visualization technologies, (2) organize science observations and models, and (3) visualize science results and mission Plans. The SSV project currently supports the Mars Exploration Rovers (MER) mission, the Mars Reconnaissance Orbiter (MRO), and Cassini. In support of the these missions, the SSV team has produced pan and zoom animations of large mosaics to reveal details of surface features and topography, created 3D animations of science instruments and procedures, formed 3-D anaglyphs from left and right stereo pairs, and animated registered multi-resolution mosaics to provide context for microscopic images.

Visible and Near-IR Reflectance Spectra of Mars Analogue Materials Under Arid Conditions for Interpretation of Martian Surface Mineralogy

NASA Technical Reports Server (NTRS)

Morris, R. V.; Graff, T. G.; Achilles, C. N.; Agresti, D. G.; Ming, D. W.; Golden, D. C.

2011-01-01

Visible and near-IR (VNIR) spectra from the hyper-spectral imagers MRO-CRISM and Mars Express OMEGA in martian orbit have signatures from Fe-bearing phases (e.g., olivine, pyroxene, and jarosite), H2O/OH-bearing phases (e.g., smectites and other phyllosilicates, sulfates, and high-SiO2 phases), and carbonate [e.g., 1-5]. Mineralogical assignments of martian spectral features are made on the basis of VNIR spectra acquired in the laboratory under appropriate environmental conditions on samples whose mineralogical composition is known. We report here additional results for our ongoing project [6] to acquire VNIR spectra under arid conditions.

Meter-scale morphology of the north polar region of Mars.

PubMed

Herkenhoff, K E; Byrne, S; Russell, P S; Fishbaugh, K E; McEwen, A S

2007-09-21

Mars' north pole is covered by a dome of layered ice deposits. Detailed ( approximately 30 centimeters per pixel) images of this region were obtained with the High-Resolution Imaging Science Experiment on board the Mars Reconnaissance Orbiter (MRO). Planum Boreum basal unit scarps reveal cross-bedding and show evidence for recent mass wasting, flow, and debris accumulation. The north polar layers themselves are as thin as 10 centimeters but appear to be covered by a dusty veneer in places, which may obscure thinner layers. Repetition of particular layer types implies that quasi-periodic climate changes influenced the stratigraphic sequence in the polar layered deposits, informing models for recent climate variations on Mars.

MRO's High Resolution Imaging Science Experiment (HiRISE): Education and Public Outreach Plans

NASA Technical Reports Server (NTRS)

Gulick, V.; McEwen, A.; Delamere, W. A.; Eliason, E.; Grant, J.; Hansen, C.; Herkenhoff, K.; Keszthelyi, L.; Kirk, R.; Mellon, M.

2003-01-01

The High Resolution Imaging Experiment, described by McEwen et al. and Delamere et al., will fly on the Mars 2005 Orbiter. In conjunction with the NASA Mars E/PO program, the HiRISE team plans an innovative and aggressive E/PO effort to complement the unique high-resolution capabilities of the camera. The team is organizing partnerships with existing educational outreach programs and museums and plans to develop its own educational materials. In addition to other traditional E/PO activities and a strong web presence, opportunities will be provided for the public to participate in image targeting and science analysis. The main aspects of our program are summarized.

Diverse Orbits Around Mars Graphic

NASA Image and Video Library

2015-05-04

This graphic depicts the relative shapes and distances from Mars for five active orbiter missions plus the planet's two natural satellites. It illustrates the potential for intersections of the spacecraft orbits. The number of active orbiter missions at Mars increased from three to five in 2014. With the increased traffic, NASA has augmented a process for anticipating orbit intersections and avoiding collisions. NASA's Mars Odyssey and MRO (Mars Reconnaissance Orbiter) travel near-circular orbits. The European Space Agency's Mars Express, NASA's MAVEN (Mars Atmosphere and Volatile Evolution) and India's MOM (Mars Orbiter Mission), travel more elliptical orbits. Phobos and Deimos are the two natural moons of Mars. http://photojournal.jpl.nasa.gov/catalog/PIA19396

Meter-scale morphology of the north polar region of mars

USGS Publications Warehouse

Herkenhoff, K. E.; Byrne, S.; Russell, P.S.; Fishbaugh, K.E.; McEwen, A.S.

2007-01-01

Mars' north pole is covered by a dome of layered ice deposits. Detailed (???30 centimeters per pixel) images of this region were obtained with the High-Resolution Imaging Science Experiment on board the Mars Reconnaissance Orbiter (MRO). Planum Boreum basal unit scarps reveal cross-bedding and show evidence for recent mass wasting, flow, and debris accumulation. The north polar layers themselves are as thin as 10 centimeters but appear to be covered by a dusty veneer in places, which may obscure thinner layers. Repetition of particular layer types implies that quasi-periodic climate changes influenced the stratigraphic sequence in the polar layered deposits, informing models for recent climate variations on Mars.

Gram-negative Biomass in Clay Minerals Analogs: Testing Habitability Potential for the 2011 Mars Science Laboratory Mission

NASA Astrophysics Data System (ADS)

Bonaccorsi, R.; McKay, C. P.

2009-12-01

Landing sites of next missions to Mars i.e., the US 2011 Mars Science Laboratory (MSL11) and the ESA2016 Pasteur ExoMars, will include phyllosilicate outcrops as targets for investigating the geological and biological history of that planet. In this context, we present a study assessing the living biomass and habitability potential in mineralogical Mars analogs such as phyllosilicates and hematite-rich deposits encompassing a broad arid-hyper-arid climate range (annual rainfall <0.2 to ~700mm/y). Samples from the Atacama Desert (Chile), the Death Valley (CA), and the California Coast (USA) were analyzed for microbial lipopolysaccharide (LPS) as proxy for Gram-negatives biomass with the Limulus-Amebocite-Lysate (LAL) assay. Mineral phases were identified using X-Ray-Diffraction (XRD). These samples resulted to contain phyllosilicate phases similar to those identified, or inferred [1], on the surface of Mars by the OMEGA-Mars/Express [e.g., 2], the Mars Reconnaissance Orbiter (MRO) instruments (HiRISE and CRISM) [3]. Basic observations were: 1) there is no systematic pattern in biomass content of clays vs. non-clays (oxidized) materials from the study sites; 2) Atacama desiccation polygons (muscovite and kaolinite) and contiguous hematite-rich hyper-arid deposits contain the lowest biomass, i.e., ~104to-105 cells/g, respectively; 3) the hyper-arid clays contain three-order magnitude lower Gram-negative biomass than those (montmorillonite, illite, and chlorite) from the arid Death Valley site (~107cells/g); and 4) finally, the Gram-negative (~107cells/g) of clay minerals-rich materials from the arid site is about the same than that (~1.5 to ~3.0 x 107cells/g) of water-saturated massive deposits (kaolinite, illite, and vermiculite) from the wetter California coast. Results from this investigation will help testing for the habitability potential of phyllosilicate deposits sampled by the MSL11 Mission. REFERENCES:[1] Bibring et al., 2006, Science 312:400-404; [2] Wang et al., 2006 JGR E02S16 Vol.111; [3] Bishop et al., 2008. Science, 321,830-833.

Vertical Distribution of Aersols and Water Vapor Using CRISM Limb Observations

NASA Technical Reports Server (NTRS)

Smith, Michael D.; Wolff, Michael J.; Clancy, R. Todd

2011-01-01

Near-infrared spectra taken in a limb-viewing geometry by the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) on-board the Mars Reconnaissance Orbiter (MRO) provide a useful tool for probing atmospheric structure. Specifically, the observed radiance as a function of wavelength and height above the limb allows the vertical distribution of both dust and ice aerosols to be retrieved. These data serve as an important supplement to the aerosol profiling provided by the MRO/MCS instrument allowing independent validation and giving additional information on particle physical and scattering properties through multi-wavelength studies. A total of at least ten CRISM limb observations have been taken so far covering a full Martian year. Each set of limb observations nominally contains about four dozen scans across the limb giving pole-to-pole coverage for two orbits at roughly 100 and 290 W longitude over the Tharsis and Syrtis/Hellas regions, respectively. At each longitude, limb scans are spaced roughly 10 degrees apart in latitude, with a vertical spatial resolution on the limb of roughly 800 m. Radiative transfer modeling is used to model the observations. We compute synthetic CRISM limb spectra using a discrete-ordinates radiative transfer code that accounts for multiple scattering from aerosols and accounts for spherical geometry of the limb observations by integrating the source functions along curved paths in that coordinate system. Retrieved are 14-point vertical profiles for dust and water ice aerosols with resolution of 0.4 scale heights between one and six scale heights above the surface. After the aerosol retrieval is completed, the abundances of C02 (or surface pressure) and H20 gas are retrieved by matching the depth of absorption bands at 2000 nm for carbon dioxide and at 2600 run for water vapor. In addition to the column abundance of water vapor, limited information on its vertical structure can also be retrieved depending on the signal available from aerosol scattering.

Field reconnaissance geologic mapping of the Columbia Hills, Mars, based on Mars Exploration Rover Spirit and MRO HiRISE observations

USGS Publications Warehouse

Crumpler, L.S.; Arvidson, R. E.; Squyres, S. W.; McCoy, T.; Yingst, A.; Ruff, S.; Farrand, W.; McSween, Y.; Powell, M.; Ming, D. W.; Morris, R.V.; Bell, J.F.; Grant, J.; Greeley, R.; DesMarais, D.; Schmidt, M.; Cabrol, N.A.; Haldemann, A.; Lewis, K.W.; Wang, A.E.; Schroder, C.; Blaney, D.; Cohen, B.; Yen, A.; Farmer, J.; Gellert, Ralf; Guinness, E.A.; Herkenhoff, K. E.; Johnson, J. R.; Klingelhfer, G.; McEwen, A.; Rice, J.W.; Rice, M.; deSouza, P.; Hurowitz, J.

2011-01-01

Chemical, mineralogic, and lithologic ground truth was acquired for the first time on Mars in terrain units mapped using orbital Mars Reconnaissance Orbiter's High Resolution Imaging Science Experiment (MRO HiRISE) image data. Examination of several dozen outcrops shows that Mars is geologically complex at meter length scales, the record of its geologic history is well exposed, stratigraphic units may be identified and correlated across significant areas on the ground, and outcrops and geologic relationships between materials may be analyzed with techniques commonly employed in terrestrial field geology. Despite their burial during the course of Martian geologic time by widespread epiclastic materials, mobile fines, and fall deposits, the selective exhumation of deep and well-preserved geologic units has exposed undisturbed outcrops, stratigraphic sections, and structural information much as they are preserved and exposed on Earth. A rich geologic record awaits skilled future field investigators on Mars. The correlation of ground observations and orbital images enables construction of a corresponding geologic reconnaissance map. Most of the outcrops visited are interpreted to be pyroclastic, impactite, and epiclastic deposits overlying an unexposed substrate, probably related to a modified Gusev crater central peak. Fluids have altered chemistry and mineralogy of these protoliths in degrees that vary substantially within the same map unit. Examination of the rocks exposed above and below the major unconformity between the plains lavas and the Columbia Hills directly confirms the general conclusion from remote sensing in previous studies over past years that the early history of Mars was a time of more intense deposition and modification of the surface. Although the availability of fluids and the chemical and mineral activity declined from this early period, significant later volcanism and fluid convection enabled additional, if localized, chemical activity. Copyright ?? 2011 by the American Geophysical Union.

Transient bright "halos" on the South Polar Residual Cap of Mars: Implications for mass-balance

NASA Astrophysics Data System (ADS)

Becerra, Patricio; Byrne, Shane; Brown, Adrian J.

2015-05-01

Spacecraft imaging of Mars' south polar region during mid-southern summer of Mars year 28 (2007) observed bright halo-like features surrounding many of the pits, scarps and slopes of the heavily eroded carbon dioxide ice of the South Polar Residual Cap (SPRC). These features had not been observed before, and have not been observed since. We report on the results of an observational study of these halos, and spectral modeling of the SPRC surface at the time of their appearance. Image analysis was performed using data from MRO's Context Camera (CTX), and High Resolution Imaging Science Experiment (HiRISE), as well as images from Mars Global Surveyor's (MGS) Mars Orbiter Camera (MOC). Data from MRO's Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) were used for the spectral analysis of the SPRC ice at the time of the halos. These data were compared with a Hapke reflectance model of the surface to constrain their formation mechanism. We find that the unique appearance of the halos is intimately linked to a near-perihelion global dust storm that occurred shortly before they were observed. The combination of vigorous summertime sublimation of carbon dioxide ice from sloped surfaces on the SPRC and simultaneous settling of dust from the global storm, resulted in a sublimation wind that deflected settling dust particles away from the edges of these slopes, keeping these areas relatively free of dust compared to the rest of the cap. The fact that the halos were not exhumed in subsequent years indicates a positive mass-balance for flat portions of the SPRC in those years. A net accumulation mass-balance on flat surfaces of the SPRC is required to preserve the cap, as it is constantly being eroded by the expansion of the pits and scarps that populate its surface.

Active and Recent Volcanism and Hydrogeothermal Activity on Mars

NASA Astrophysics Data System (ADS)

Edgett, Kenneth S.; Cantor, B. A.; Harrison, T. N.; Kennedy, M. R.; Lipkaman, L. J.; Malin, M. C.; Posiolova, L. V.; Shean, D. E.

2010-10-01

There are no active volcanoes or geysers on Mars today, nor in the very recent past. Since 1997, we have sought evidence from targeted narrow angle camera images and daily, global wide angle images for active or very recent (decades to < 10 Ma) volcanism or hydrogeothermal events on Mars. Despite > 11 years of daily global imaging and coverage of > 60% of Mars at ≤ 6 m/pixel (with the remaining < 40% largely outside of volcanic regions), we have found no such evidence, although one lava field in Aeolis (5°N, 220°W) stands out as possibly the site of the most recent volcanism. Authors of impact crater size-frequency studies suggest some volcanic landforms on Mars are as young as tens to hundreds of Ma. This interpreted youth has implications for understanding the internal geophysical state of Mars and has encouraged those seeking sources for trace gases (methane) in the atmosphere and those seeking "warm havens for life” (Jakosky 1996, New Scientist 150, 38-42). We targeted thousands of Mars Global Surveyor (MGS) MOC and Mars Reconnaissance Orbiter (MRO) CTX (and HiRISE) images to examine volcanic regions; we also studied every MGS MOC and MRO MARCI wide angle image. For evidence of active volcanism, we sought eruption plumes, new vents, new tephra deposits, and new volcanogenic flows not observed in earlier images. For recent volcanism, we sought volcanogenic flows with zero or few superposed impact craters and minimal regolith development or superposed eolian sediment. Targets included all volcanic landforms identified in research papers as "recent” as well as areas speculated to have exhibited eruptive plumes. An independent search for endogenic heat sources, a key Mars Odyssey THEMIS objective, has also not produced a positive result (Christensen et al. 2005, P24A-01, Eos, Trans. Am. Geophys. Union 86/52).

A Window into the Past

NASA Image and Video Library

2017-10-23

The layered sedimentary deposits inside the giant canyons of Mars have puzzled scientists for decades. These light toned deposits have fine, horizontal laminations that are unlike the rugged rim rock of the Valles Marineris as seen by NASA's Mars Reconnaisance Orbiter (MRO). Various ideas for the origin of the layered sediments have suggested lake deposits, wind blown dust and sand, or volcanic materials that erupted after the canyon was formed, and possibly filled with water. One particular layered deposit, called Ceti Mensa, attracted attention because its deep red color in images collected by the Viking Orbiter mission during the 1970s. Located in west Candor Chasma in the north of the Valles Marineris, Ceti Mensa is an undulating plateau that rises 3 kilometers above the canyon floor and is bounded by steep scarps up to 1.5 kilometers in height. Deep red hues are on the west-facing scarp in particular. The red tint may be due to the presence of crystalline ferric oxide, suggesting that the material may have been exposed to heat or water, or both. Spectral measurements by the Mars Express OMEGA and MRO CRISM instruments confirm the presence of hydrated sulfate salts, such as gypsum and kieserite . These minerals are important for two reasons. On Earth, they typically form in wet environments, suggesting that the deposits in Ceti Mensa may have formed under water. On Mars, these deposits could be valuable to future Martian colonists as fertilizer for growing crops. In a view of the colorful west-facing scarp of Ceti Mensa, we see the interior layers of the deposit, giving us a window into the past history of the sediments as they accumulated over time. We also see layers that were previously too small to view, and a surface that is thoroughly fractured, eroded into knobs, and partially covered by young dark sand dunes. https://photojournal.jpl.nasa.gov/catalog/PIA22051

Upgrades to the Mars Initial Reference Ionosphere (MIRI) Model Due to Observations from MAVEN, MEX and MRO.

NASA Astrophysics Data System (ADS)

Narvaez, C.; Mendillo, M.; Trovato, J.

2017-12-01

A semi-empirical model of the maximum electron density (Nmax) of the martian ionosphere [MIRI-mark-1](1) was derived from an initial set radar observations by the MEX/MARSIS instrument. To extend the model to full electron density profiles, normalized shapes of Ne(h) from a theoretical model(2) were calibrated by MIRI's Nmax. Subsequent topside ionosphere observations from MAVEN indicated that topside shapes from MEX/MARSIS(3) offered improved morphology. The MEX topside shapes were then merged to the bottomside shapes from the theoretical model. Using a larger set of MEX/MARSIS observations (07/31/2005 - 05/24/2015), a new specification of Nmax as a function of solar zenith angle and solar flux is now used to calibrate the normalized Ne(h) profiles. The MIRI-mark-2 model includes the integral with height of Ne(h) to form total electron content (TEC) values. Validation of the MIRI TEC was accomplished using an independent set of TEC derived from the SHARAD(4) experiment on MRO. (1) M. Mendillo, A. Marusiak, P. Withers, D. Morgan and D. Gurnett, A New Semi-empirical Model of the Peak Electron Density of the Martian Ionosphere, Geophysical Research Letters, 40, 1-5, doi:10.1002/2013GL057631, 2013. (2) Mayyasi, M. and M. Mendillo (2015), Why the Viking descent probes found only one ionospheric layer at Mars, Geophys. Res. Lett., 42, 7359-7365, doi:10.1002/2015GL065575 (3) Němec, F., D. Morgan, D. Gurnett, and D. Andrews (2016), Empirical model of the Martian dayside ionosphere: Effects of crustal magnetic fields and solar ionizing flux at higher altitudes, J. Geophys. Res. Space Physics, 121, 1760-1771, doi:10.1002/2015/A022060.(4) Campbell, B., and T. Watters (2016), Phase compensation of MARSIS subsurface sounding and estimation of ionospheric properties: New insights from SHARAD results, J.Geophys. Res. Planets, 121, 180-193, doi:10.1002/2015JE004917.

Ongoing Mars Missions: Extended Mission Plans

NASA Astrophysics Data System (ADS)

Zurek, Richard; Diniega, Serina; Crisp, Joy; Fraeman, Abigail; Golombek, Matt; Jakosky, Bruce; Plaut, Jeff; Senske, David A.; Tamppari, Leslie; Thompson, Thomas W.; Vasavada, Ashwin R.

2016-10-01

Many key scientific discoveries in planetary science have been made during extended missions. This is certainly true for the Mars missions both in orbit and on the planet's surface. Every two years, ongoing NASA planetary missions propose investigations for the next two years. This year, as part of the 2016 Planetary Sciences Division (PSD) Mission Senior Review, the Mars Odyssey (ODY) orbiter project submitted a proposal for its 7th extended mission, the Mars Exploration Rover (MER-B) Opportunity submitted for its 10th, the Mars Reconnaissance Orbiter (MRO) for its 4th, and the Mars Science Laboratory (MSL) Curiosity rover and the Mars Atmosphere and Volatile Evolution (MVN) orbiter for their 2nd extended missions, respectively. Continued US participation in the ongoing Mars Express Mission (MEX) was also proposed. These missions arrived at Mars in 2001, 2004, 2006, 2012, 2014, and 2003, respectively. Highlights of proposed activities include systematic observations of the surface and atmosphere in twilight (early morning and late evening), building on a 13-year record of global mapping (ODY); exploration of a crater rim gully and interior of Endeavour Crater, while continuing to test what can and cannot be seen from orbit (MER-B); refocused observations of ancient aqueous deposits and polar cap interiors, while adding a 6th Mars year of change detection in the atmosphere and the surface (MRO); exploration and sampling by a rover of mineralogically diverse strata of Mt. Sharp and of atmospheric methane in Gale Crater (MSL); and further characterization of atmospheric escape under different solar conditions (MVN). As proposed, these activities follow up on previous discoveries (e.g., recurring slope lineae, habitable environments), while expanding spatial and temporal coverage to guide new detailed observations. An independent review panel evaluated these proposals, met with project representatives in May, and made recommendations to NASA in June 2016. In this presentation, we will highlight the planned activities of these NASA Mars missions, as they start new chapters in their historic exploration of the dynamic and complex planet that is Mars.

Limb clouds and dust on Mars from images obtained by the Visual Monitoring Camera (VMC) onboard Mars Express

NASA Astrophysics Data System (ADS)

Sánchez-Lavega, A.; Chen-Chen, H.; Ordoñez-Etxeberria, I.; Hueso, R.; del Río-Gaztelurrutia, T.; Garro, A.; Cardesín-Moinelo, A.; Titov, D.; Wood, S.

2018-01-01

The Visual Monitoring Camera (VMC) onboard the Mars Express (MEx) spacecraft is a simple camera aimed to monitor the release of the Beagle-2 lander on Mars Express and later used for public outreach. Here, we employ VMC as a scientific instrument to study and characterize high altitude aerosols events (dust and condensates) observed at the Martian limb. More than 21,000 images taken between 2007 and 2016 have been examined to detect and characterize elevated layers of dust in the limb, dust storms and clouds. We report a total of 18 events for which we give their main properties (areographic location, maximum altitude, limb projected size, Martian solar longitude and local time of occurrence). The top altitudes of these phenomena ranged from 40 to 85 km and their horizontal extent at the limb ranged from 120 to 2000 km. They mostly occurred at Equatorial and Tropical latitudes (between ∼30°N and 30°S) at morning and afternoon local times in the southern fall and northern winter seasons. None of them are related to the orographic clouds that typically form around volcanoes. Three of these events have been studied in detail using simultaneous images taken by the MARCI instrument onboard Mars Reconnaissance Orbiter (MRO) and studying the properties of the atmosphere using the predictions from the Mars Climate Database (MCD) General Circulation Model. This has allowed us to determine the three-dimensional structure and nature of these events, with one of them being a regional dust storm and the two others water ice clouds. Analyses based on MCD and/or MARCI images for the other cases studied indicate that the rest of the events correspond most probably to water ice clouds.

The Era After the ELT: Optical Interferometry With Kilometer Baselines

NASA Astrophysics Data System (ADS)

Bakker, Eric J.

2007-12-01

The 8-meter class telescopes seen first light in 1993-1998 (Keck, 1993, VLT 1998). The ELT will see first light in the 2013-2018 time frame. The follow-up of the ELT will see first light around 2023. That is 15 years from today. The sequence from 8-meter to 30 meter telescopes (started as a goal of 100m), will suggest a follow-up telescope with an aperture of 300 meter as initial goal. Cleary a 300 meter or more ambitiously a 1000-meter telescope can no longer be structural one piece that has to point to any point on the sky and track the objects. The more likely scenario is to follow the process applied in radio astronomy and move from single telescopes to interferometers. Optical interferometry is maturing very quickly with the de-commissioning of experimental instruments (COAST, GT2I, IOTA, and probably PTI and ISI in the near future) and the use of precision mechanics and automation. The remaining interferometers are grouped in three categories: large telescopes (VLTI and KECK-I), mid-size interferometers (MROI) and small interferometers (CHARA and NPOI). The Magdalena Ridge Observatory Interferometer (MROI) is scheduled for first light/fringe in 2009 and will provide unique observing capabilities to astronomers with limiting magnitudes in the same range as those currently achieved by Keck-I and VLTI. The Magdalena Ridge Observatory Interferometer (near Socorro, NM) invites interested engineers, scientists, and astronomers to participate in the construction and science program of MRO at all levels. Ranging from visitors instruments, support of large procurements in return for access, to individual contributions related to the science program, shared risk observations, etc. For more information, contact the Project Manager at the Magdalena Ridge Observatory Interferometer.

Ligand field splittings in core level transitions for transition metal (TM) oxides: Tanabe-Sugano diagrams and (TM) dangling bonds in vacated O-atom defects

NASA Astrophysics Data System (ADS)

Lucovsky, Gerry; Wu, Kun; Pappas, Brian; Whitten, Jerry

2013-04-01

Defect states in the forbidden band-gap below the conduction band edge are active as electron traps in nano-grain high-) transition metal (TM) oxides with thickness >0.3 nm, e.g., ZrO2 and HfO2. These oxides have received considerable attention as gate-dielectrics in complementary metal oxide semiconductor (CMOS) devices, and more recently are emerging as candidates for charge storage and memory devices. To provide a theoretical basis for device functionality, ab-initio many-electron theory is combined with X-ray absorption spectroscopy (XAS) to study O K edge and TM core level transitions. These studies identify ligand field splittings (ΔLF) for defect state features,. When compared with those obtained from O-atom and TM-atom core spectroscopic transitions, this provides direct information about defect state sun-nm bonding arrangements. comparisons are made for (i) elemental TiO2 and Ti2O3 with different formal ionic charges, Ti4+ and Ti3+ and for (ii) Magneli Phase alloys, TinO2n-1, n is an integer 9>=n>3, and (TiO2)x(HfO2)1-x alloys. The alloys display multi-valent behavior from (i) different ionic-charge states, (ii} local bond-strain, and (iii) metallic hopping transport. The intrinsic bonding defects in TM oxides are identified as pairs of singly occupied dangling bonds. For 6-fold coordinated Ti-oxides defect excited states in 2nd derivative O K pre-edge spectra are essentially the same as single Ti-atom d2 transitions in Tanabe-Sugano (T-S) diagrams. O-vacated site defects in 8-fold coordinated ZrO2 and HfO2 are described by d8 T-S diagrams. T-S defect state ordering and splittings are functions of the coordination and symmetry of vacated site bordering TM atoms. ΔLF values from the analysis of T-S diagrams indicate medium range order (MRO) extending to 3rd and 4th nearest-neighbor (NN) TM-atoms. Values are different for 6-fold Ti, and 8-fold ZrO2 and HfO2, and scale inversely with differences in respective formal ionic radii. O-vacated site bonding defects in TM nano-grain oxides are qualitatively similar to vacant-site defects in non-crystalline SiO2 and GeO2 for ulta-thin films, < 0.2 nm thick, and yield similar performance in MOSCAPs on Ge substrates heralding applications in aggressively-scale CMOS devices.

Vertical profiles of Mars 1.27 μm O2 dayglow from MRO CRISM limb spectra: Seasonal/global behaviors, comparisons to LMDGCM simulations, and a global definition for Mars water vapor profiles

NASA Astrophysics Data System (ADS)

Todd Clancy, R.; Smith, Michael D.; Lefèvre, Franck; McConnochie, Timothy H.; Sandor, Brad J.; Wolff, Michael J.; Lee, Steven W.; Murchie, Scott L.; Toigo, Anthony D.; Nair, Hari; Navarro, Thomas

2017-09-01

Since July of 2009, The Compact Reconnaissance Imaging Spectral Mapper (CRISM) onboard the Mars Reconnaissance Orbiter (MRO) has periodically obtained pole-to-pole observations (i.e., full MRO orbits) of limb scanned visible/near IR spectra (λ = 0.4 - 4.0 μ m, △λ ∼ 10 nm- Murchie et al., 2007). These CRISM limb observations support the first seasonally and spatially extensive set of Mars 1.27 μm O2(1△g) dayglow profile retrievals (∼ 1100) over ≥ 8-80 km altitudes. Their comparison to Laboratoire de Météorologie Dynamique (LMD) global climate model (GCM) simulated O2(1△g) volume emission rate (VER) profiles, as a function of altitude, latitude, and season (solar longitude, Ls), supports several key conclusions regarding Mars atmospheric water vapor (which is derived from O2(1△g) emission rates), Mars O3, and the collisional de-excitation of O2(1△g) in the Mars CO2 atmosphere. Current (Navarro et al., 2014) LMDGCM simulations of Mars atmospheric water vapor fall 2-3 times below CRISM derived water vapor abundances at 20-40 km altitudes over low-to-mid latitudes in northern spring (Ls = 30-60°), and northern mid-to-high latitudes over northern summer (Ls = 60-140°). In contrast, LMDGCM simulated water vapor is 2-5 times greater than CRISM derived values at all latitudes and seasons above 40 km, within the aphelion cloud belt (ACB), and over high-southern to mid-southern latitudes in southern summer (Ls = 190-340°) at 15-35 km altitudes. Overall, the solstitial summer-to-winter hemisphere gradients in water vapor are reversed between the LMDGCM modeled versus the CRISM derived water vapor abundances above 10-30 km altitudes. LMDGCM-CRISM differences in water vapor profiles correlate with LMDGCM-CRISM differences in cloud mixing profiles; and likely reflect limitations in simulating cloud microphysics and radiative forcing, both of which restrict meridional transport of water from summer-to-winter hemispheres on Mars (Clancy et al., 1996; Montmessin et al., 2004; Steele et al., 2014; Navarro et al., 2014) and depend on uncertain cloud microphysical properties (Navarro et al., 2014). The derived low-to-mid latitude changes in Mars water vapor vertical distributions should reduce current model-data disagreements in column O3 and H2O2 abundances over low-to-mid latitudes (e.g., within the ACB; Lefèvre et al., 2008; Encrenaz et al., 2015; Clancy et al., 2016). Lastly, the global/seasonal average comparison of CRISM and LMDGCM O2(1△g) VER below 20 km altitudes indicates a factor of ∼3 times lower value (0.25 ×10-20 cm3sec-1) for the CO2 collisional de-excitation rate coefficient of O2(1△g) than derived recently by Guslyakova et al. (2016).

A Multi-mission Event-Driven Component-Based System for Support of Flight Software Development, ATLO, and Operations first used by the Mars Science Laboratory (MSL) Project

NASA Technical Reports Server (NTRS)

Dehghani, Navid; Tankenson, Michael

2006-01-01

This viewgraph presentation reviews the architectural description of the Mission Data Processing and Control System (MPCS). MPCS is an event-driven, multi-mission ground data processing components providing uplink, downlink, and data management capabilities which will support the Mars Science Laboratory (MSL) project as its first target mission. MPCS is designed with these factors (1) Enabling plug and play architecture (2) MPCS has strong inheritance from GDS components that have been developed for other Flight Projects (MER, MRO, DAWN, MSAP), and are currently being used in operations and ATLO, and (3) MPCS components are Java-based, platform independent, and are designed to consume and produce XML-formatted data

Windy Mars: A Dynamic Planet as Seen by the HiRISE Camera

NASA Technical Reports Server (NTRS)

Bridges, N. T.; Geissler, P. E.; McEwen, A. S.; Thomson, B. J.; Chuang, F. C.; Herkenhoff, K. E.; Keszthelyi, L. P.; Martnez-Alonso, S.

2007-01-01

With a dynamic atmosphere and a large supply of particulate material, the surface of Mars is heavily influenced by wind-driven, or aeolian, processes. The High Resolution Imaging Science Experiment (HiRISE) camera on the Mars Reconnaissance Orbiter (MRO) provides a new view of Martian geology, with the ability to see decimeter-size features. Current sand movement, and evidence for recent bedform development, is observed. Dunes and ripples generally exhibit complex surfaces down to the limits of resolution. Yardangs have diverse textures, with some being massive at HiRISE scale, others having horizontal and cross-cutting layers of variable character, and some exhibiting blocky and polygonal morphologies. 'Reticulate' (fine polygonal texture) bedforms are ubiquitous in the thick mantle at the highest elevations.

Martian Analogue Sample Characterization and Spectral Library Development at the Johnson Space Center

NASA Technical Reports Server (NTRS)

Morris, Richard V.

2002-01-01

An extensive collection of Martian analogue samples housed at the Johnson Space Center is the focus of ongoing research by the JSC Mars soil genesis group and their collaborators. Because the major element composition of Martian meteorites and in situ analyses of Martian soils and rocks indicate that Mars is predominantly an iron-rich basaltic world, the focus of active sample collection and analysis is basaltic materials and their hydrolytic (both aqueous and hydrothermal) and sulfatetic alteration products. Described below are the scope of the JSC Mars analogue sample collection, the characterization process, and plans to incorporate the data into spectral libraries for the Mars 2003 Mars Exploration Rover (MER) and Mars 2005 Mars Reconnaissance Orbiter (MRO) CRISM missions.

A Review of Laboratory Experiments in Support of Interpretation of Hyperspectral Data from the Mars South Polar Residual Cap

NASA Astrophysics Data System (ADS)

Campbell, Jacqueline; Sidiropoulos, Panagiotis; Muller, Jan Peter

2017-04-01

The Martian South Polar Residual Cap (SPRC) is a permanent region of CO2 ice exhibiting unique, dynamic, flat floored, quasi-circular sublimation features known colloquially as Swiss Cheese Terrain (SCT). Sublimation processes can expose dust particles trapped within the ice during winter, which can be analysed using hyperspectral data from the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) on board NASA's Mars Reconnaissance Orbiter (MRO). Work is being carried out to establish the composition of these dust particles, and look for evidence of organic molecules that may have been afforded protection within the SPRC from the deleterious effects of ultraviolet radiation on the Martian surface. In this work we review laboratory experiments that have been carried out in order to better interpret CRISM spectra. In particular, SWIR (short-wave infrared) studies of CO2 and H2O ice/frost and dust mixtures, the behaviour of organic molecules in Martian conditions, and the angular reflectance measurements of such spectra. We will then briefly discuss what further work should be carried out to enable these measurements to be used to improve the interpretation of orbital hyperspectral data. Acknowledgements Part of the research leading to these results has received partial funding from the European Union's Seventh Framework Programme (FP7/2007-2013) under iMars grant agreement n˚ 607379; MSSL STFC Consolidated grant no. ST/K000977/1 and the first author is supported by STFC under PhD studentship no. 526933.

Assessment of Oxidative Metabolism in Brown Fat Using PET Imaging

PubMed Central

Muzik, Otto; Mangner, Thomas J.; Granneman, James G.

2011-01-01

Objective: Although it has been believed that brown adipose tissue (BAT) depots disappear shortly after the perinatal period in humans, positron emission tomography (PET) imaging using the glucose analog 18F-deoxy-d-glucose (FDG) has shown unequivocally the existence of functional BAT in humans, suggesting that most humans have some functional BAT. The objective of this study was to determine, using dynamic oxygen-15 (15O) PET imaging, to what extent BAT thermogenesis is activated in adults during cold stress and to establish the relationship between BAT oxidative metabolism and FDG tracer uptake. Methods: Fourteen adult normal subjects (9F/5M, 30 ± 7 years) underwent triple oxygen scans (H215O, C15O, 15O2) as well as indirect calorimetric measurements at both rest and following exposure to mild cold (16°C). Subjects were divided into two groups (BAT+ and BAT−) based on the presence or absence of FDG tracer uptake (SUV > 2) in cervical–supraclavicular BAT. Blood flow and oxygen extraction fraction (OEF) was calculated from dynamic PET scans at the location of BAT, muscle, and white adipose tissue (WAT). The metabolic rate of oxygen (MRO2) in BAT was determined and used to calculate the contribution of activated BAT to daily energy expenditure (DEE). Results: The median mass of activated BAT in the BAT+ group (5F, age 31 ± 8) was 52.4 g (range 14–68 g) and was 1.7 g (range 0–6.3 g) in the BAT − group (5M/4F, age 29 ± 6). Corresponding SUV values were significantly higher in the BAT+ as compared to the BAT− group (7.4 ± 3.7 vs. 1.9 ± 0.9; p = 0.03). Blood flow values in BAT were significantly higher in the BAT+ group as compared to the BAT− group (13.1 ± 4.4 vs. 5.7 ± 1.1 ml/100 g/min, p = 0.03), but were similar in WAT (4.1 ± 1.6 vs. 4.2 ± 1.8 ml/100 g/min) and muscle (3.7 ± 0.8 vs. 3.3 ± 1.2 ml/100 g/min). Moreover, OEF in BAT was similar in the two groups (0.56 ± 0.18 in BAT+ vs. 0.46 ± 0.19 in BAT−, p = 0.39). Calculated MRO2 values in BAT increased from 0.95 ± 0.74 to 1.62 ± 0.82 ml/100 g/min in the BAT+ group and were significantly higher than those determined in the BAT− group (0.43 ± 0.27 vs. 0.56 ± 0.24, p = 0.67). The DEE associated with BAT oxidative metabolism was highly variable in the BAT+ group, with an average of 5.5 ± 6.4 kcal/day (range 0.57–15.3 kcal/day). Conclusion: BAT thermogenesis in humans accounts for less than 20 kcal/day during moderate cold stress, even in subjects with relatively large BAT depots. Furthermore, due to the large differences in blood flow and glucose metabolic rates in BAT between humans and rodents, the application of rodent data to humans is problematic and needs careful evaluation. PMID:22649408

Possible Sulfates in the Northeast Syrtis Major Region

NASA Image and Video Library

2015-09-16

A variety of diverse morphological features are present in this image (21 by 5.5 kilometers) located in the southeastern area of the Nili Fossae region and just northeast of Syrtis Major. This particular region has been studied intensely due to the presence of volcanics from Syrtis Major and impact ejecta from the Isidis Basin. The region is rich in unaltered mafic deposits, in contact with diverse altered deposits rich in clays, carbonates, and sulfates. These deposits make the Nili Fossae region one of the most colorful regions on Mars, which is most distinctive in infrared color composites (IRB). HiRISE IRB color aids in chemical and mineral-type mapping, especially when correlated with other MRO instruments such as CRISM. http://photojournal.jpl.nasa.gov/catalog/PIA19940

Gullies and Voids

NASA Image and Video Library

2018-02-05

Intricate gullies have formed on the northern wall of this impact crater located in the Terra Cimmeria region in this image from NASA's Mars Reconnaissance Orbiter (MRO). This crater may have formed in a region rich in ground water. This ground water likely flowed down the wall, eventually eroding numerous gullies while carrying sediments to form fan deposits. Ultimately the water likely infiltrated and froze beneath the surface. Other hypotheses say gullies form through carbon dioxide frost avalanches that we can see today. What about this chain of pits snaking their way downhill? After material was transported, subsurface voids may have formed, removing support for the overlying material. The collapse of the surface into the cavities below likely resulted in the pits and troughs, perhaps beginning a new cycle of gully formation. https://photojournal.jpl.nasa.gov/catalog/PIA22239

A nonlinear model for gas chromatograph systems

NASA Technical Reports Server (NTRS)

Feinberg, M. P.

1975-01-01

Fundamental engineering design techniques and concepts were studied for the optimization of a gas chromatograph-mass spectrometer chemical analysis system suitable for use on an unmanned, Martian roving vehicle. Previously developed mathematical models of the gas chromatograph are found to be inadequate for predicting peak heights and spreading for some experimental conditions and chemical systems. A modification to the existing equilibrium adsorption model is required; the Langmuir isotherm replaces the linear isotherm. The numerical technique of Crank-Nicolson was studied for use with the linear isotherm to determine the utility of the method. Modifications are made to the method eliminate unnecessary calculations which result in an overall reduction of the computation time of about 42 percent. The Langmuir isotherm is considered which takes into account the composition-dependent effects on the thermodynamic parameter, mRo.

VNIR Multispectral Observations of Rocks at Spirit of St. Louis Crater and Marathon Valley on Th Rim of Endeavour Crater Made by the Opportunity Rover Pancam

NASA Technical Reports Server (NTRS)

Farrand, W. H.; Johnson, J. R.; Bell, J. F., III; Mittlefehldt, D.W.

2016-01-01

The Mars Exploration Rover Opportunity has been exploring the western rim of the 22 km diameter Endeavour crater since August, 2011. Recently, Opportunity has reached a break in the Endeavour rim that the rover team has named Mara-thon Valley. This is the site where orbital observations from the MRO CRISM imaging spectrometer indicated the presence of iron smectites. On the outer western portion of Marathon Valley, Opportunity explored the crater-form feature dubbed Spirit of St. Louis (SoSL) crater. This presentation describes the 430 to 1009 nm (VNIR) reflectance, measured by the rover's Pancam, of rock units present both at Spirit of St. Louis and within Marathon Valley.

Ultra-Rapid dUT1 Measurements on Japan-Fennoscandian Baselines - Application to 24-hour Sessions

NASA Technical Reports Server (NTRS)

Matsuzaka, Shigeru; Kurihara, Shinobu; Sekido, Mamoru; Hobiger, Thomas; Haas, Rudiger; Ritakari, Jouko; Wagner, Jan

2010-01-01

GSI, NICT, OSO, and MRO have been engaged in Ultra-rapid dUT1 experiments since 2007 aiming at the technological possibility of real-time dUT1 results using the e-VLBI technique. We have already successfully determined dUT1 in less than four minutes after the end of an experimental Intensive session in 2008, and at present we routinely get the results within 30 minutes for regular Intensives. In 2009 we applied the technique to 24-hour sessions and continuously obtained dUT1 values by processing and analyzing Tsukuba Onsala data in near real-time. It showed a detailed behavior of UT1 variations, which could be very valuable for scientific study as well as for precise prediction of UT1-UTC.

Windy Mars: A dynamic planet as seen by the HiRISE camera

USGS Publications Warehouse

Bridges, N.T.; Geissler, P.E.; McEwen, A.S.; Thomson, B.J.; Chuang, F.C.; Herkenhoff, K. E.; Keszthelyi, L.P.; Martinez-Alonso, S.

2007-01-01

With a dynamic atmosphere and a large supply of particulate material, the surface of Mars is heavily influenced by wind-driven, or aeolian, processes. The High Resolution Imaging Science Experiment (HiRISE) camera on the Mars Reconnaissance Orbiter (MRO) provides a new view of Martian geology, with the ability to see decimeter-size features. Current sand movement, and evidence for recent bedform development, is observed. Dunes and ripples generally exhibit complex surfaces down to the limits of resolution. Yardangs have diverse textures, with some being massive at HiRISE scale, others having horizontal and cross-cutting layers of variable character, and some exhibiting blocky and polygonal morphologies. "Reticulate" (fine polygonal texture) bedforms are ubiquitus in the thick mantle at the highest elevations. Copyright 2007 by the American Geophysical Union.

Decoding a Dark Splotch

NASA Image and Video Library

2017-10-09

Geologists aren't quite sure what to make of the dark splotch in the middle of this image from NASA's Mars Reconnaisance Orbiter (MRO) -- one of several similar dark splotches that extend east and west for over 100 kilometers. From measurements made in infrared, this and other dark splotches have what we call "high thermal inertia," meaning that it heats up and cools down slowly. Scientists use thermal inertia to assess how rocky, sandy, or dusty a place is. A higher thermal inertia than the surrounding area means it's less dusty. Wavy, banded patterns in the dark splotch (possibly due to cross bedding from sand dunes that once occupied the area) were lithified into sandstone, and then eroded away. These clues could help geologists figure out what's going on there. https://photojournal.jpl.nasa.gov/catalog/PIA22042

Spectral Modeling of the 0.4-2.5 μm Phobos CRISM dataset

NASA Astrophysics Data System (ADS)

Pajola, Maurizio; Roush, Ted; Dalle Ore, Cristina; Marzo, Giuseppe A.; Simioni, Emanuele

2017-04-01

We present the spectral modeling of the 0.4-2.5 μm MRO/CRISM Phobos dataset. After applying a statistical clustering technique, based on a K-means partitioning algorithm, we identified eight separate clusters in the Phobos CRISM data, extending the surface coverage beyond the previous analyses of Fraeman et al. (2012, 2014). Each resulting cluster is characterized by an average and its associated variability. We modeled these different spectra using a radiative transfer code based on the approach of Shkuratov et al. (1999). We used the optical constants of the model proposed by Pajola et al. (2013) in our effort, i.e. the Tagish Lake meteorite (TL) and the Mg-rich pyroxene glass (PM80). The Shkuratov model is used in an algorithm that iteratively, and simultaneously changes the relative abundance and grain sizes of the selected components to minimize the differences between the model and observations using a chi-squared criterion. The best-fitting models were achieved with a simple intimate mixture showing that the relative percentages of TL and PM80 vary between 80-20% and 95-5%, respectively, and grain sizes for TL are 12-14 μm and 20-22 μm for PM80. This work aims to return a detailed picture of the surface properties of Phobos identifying specific areas that may be of interest for future planetary exploration, as the proposed Japanese Mars Moon eXploration (MMX) sample return mission. Acknowledgements: We make use of the public NASA-Planetary Data System MRO-CRISM spectral data of Phobos. M.P. was supported for this research by an appointment to the National Aeronautics and Space Administration (NASA) Post-doctoral Program at the Ames Research Center administered by Universities Space Research Association (USRA) through a contract with NASA. References: Fraeman et al. 2012, J. Geophy. Res, E00J15, 10.1029/2012JE004137; Fraeman et al., 2014, Icarus, 229, 196-205, 10.1016/icarus.2013.11.021; Shkuratov, Y. et al. (1999), Icarus, 137, 235. Pajola et al., 2013, The Astrophysical Journal, 777:127, 10.1088/0004-637X/777/2/127.

Hints of Habitable Environments on Mars Challenge Our Studies of Mars-Analog Sites on Earth

NASA Technical Reports Server (NTRS)

desMarais, David J

2009-01-01

Life as we know it requires water with a chemical activity (alpha) >or approx.0.6 and sources of nutrients and useful energy. Some biota can survive even if favorable conditions occur only intermittently, but the minimum required frequency of occurrences is poorly understood. Recent discoveries have vindicated the Mars exploration strategy to follow the water. Mars Global Surveyor s Thermal Emission Spectrometer (TES) found coarse-grained hematite at Meridiani Planum. Opportunity rover confirmed this and also found evidence of ancient sulfate-rich playa lakes and near-surface groundwater. Elsewhere, TES found evidence of evaporitic halides in topographic depressions. But alpha might not have approached 0.6 in these evaporitic sulfate- and halide-bearing waters. Mars Express (MEX) and Mars Reconnaissance Orbiter (MRO) found extensive sulfate evaporites in Meridiani and Valles Marineris. MEX found phyllosilicates at several sites, most notably Mawrth Valles and Nili Fossae. MRO's CRISM near-IR mapper extended the known diversity and geographic distribution of phyllosilicates to include numerous Noachian craters. Phyllosilicates typically occur at the base of exposed ancient rock sections or in sediments in early Hesperian craters. It is uncertain whether the phyllosilicates developed in surface or subsurface aqueous environments and how long aqueous conditions persisted. Spirit rover found remarkably pure ferric sulfate, indicating oxidation and transport of Fe and S, perhaps in fumaroles or hot springs. Spirit also found opaline silica, consistent with hydrothermal activity. CRISM mapped extensive silica deposits in the Valles Marineris region, consistent with aqueous weathering and deposition. CRISM also found ultramafic rocks and magnesite at Nili Fossae, consistent with serpentinization, a process that can sustain habitable environments on Earth. The report of atmospheric methane implies subsurface aqueous conditions. A working hypothesis is that aqueous environments persisted in the near-subsurface for hundreds of millions of years and might exist even today. Studies of Mars-analog environments must better understand subsurface nonphotosynthetic ecosystems and their biosignatures in mafic and ultramafic terranes. Studies must determine minimum needs for water activity and energy and also establish survival limits when conditions that support active metabolism and propagation become progressively less frequent over time.

Surface Reflectance of Mars Observed by CRISM-MRO: 1. Multi-angle Approach for Retrieval of Surface Reflectance from CRISM Observations (mars-reco)

NASA Technical Reports Server (NTRS)

Ceamanos, Xavier; Doute, S.; Fernando, J.; Pinet, P.; Lyapustin, A.

2013-01-01

This article addresses the correction for aerosol effects in near-simultaneous multiangle observations acquired by the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) aboard the Mars Reconnaissance Orbiter. In the targeted mode, CRISM senses the surface of Mars using 11 viewing angles, which allow it to provide unique information on the scattering properties of surface materials. In order to retrieve these data, however, appropriate strategies must be used to compensate the signal sensed by CRISM for aerosol contribution. This correction is particularly challenging as the photometric curve of these suspended particles is often correlated with the also anisotropic photometric curve of materials at the surface. This article puts forward an innovative radiative transfer based method named Multi-angle Approach for Retrieval of Surface Reflectance from CRISM Observations (MARS-ReCO). The proposed method retrieves photometric curves of surface materials in reflectance units after removing aerosol contribution. MARS-ReCO represents a substantial improvement regarding previous techniques as it takes into consideration the anisotropy of the surface, thus providing more realistic surface products. Furthermore, MARS-ReCO is fast and provides error bars on the retrieved surface reflectance. The validity and accuracy of MARS-ReCO is explored in a sensitivity analysis based on realistic synthetic data. According to experiments, MARS-ReCO provides accurate results (up to 10 reflectance error) under favorable acquisition conditions. In the companion article, photometric properties of Martian materials are retrieved using MARS-ReCO and validated using in situ measurements acquired during the Mars Exploration Rovers mission.

Candidate Landing Site for the Mars Science Laboratory: Vernal Crater, S.W. ARabia Terra

NASA Technical Reports Server (NTRS)

Paris, K. N.; Allen, C. C.; Oehler, D. Z.

2007-01-01

In the fall of 2009, the Mars Science Laboratory (MSL) will be launched to Mars. The purpose of this mission is to assess biologic potential and geology and to investigate planetary processes of relevance to past habitability. MSL will be able to provide visual, chemical, radiation, and environmental data with its suite of instruments [1]. In order to be selected for the MSL landing site, certain engineering requirements must be met [1] and the area should contain geologic features suggestive of past habitability, so that the overriding science goal of the mission will be attained. There are a total of 33 proposed landing sites as of the first MSL Landing Site Workshop held in Pasadena, CA from May 31st to June 2nd, 2006 [1]. There will be an opportunity to gather high resolution visual and hyperspectral data on all proposed landing sites from the now-orbiting Mars Reconnaissance Orbiter (MRO) which entered martian orbit and began its main science phase in November of 2006 [2]. The data being gathered are from: the high resolution imaging science experiment (HiRISE), the context (CTX) camera and the compact reconnaissance imaging spectrometer (CRISM) onboard the spacecraft. The footprints of these instruments are centered on a single point, and each proposer must submit these coordinates, along with the coordinates of the proposed landing ellipse. Data from these instruments, along with new MOC images and THEMIS mosaics, will be used to enhance our understanding of the geologic and engineering parameters of each site.

Formation and mantling ages of lobate debris aprons on Mars: Insights from categorized crater counts

NASA Astrophysics Data System (ADS)

Berman, Daniel C.; Crown, David A.; Joseph, Emily C. S.

2015-06-01

Lobate debris aprons in the Martian mid-latitudes offer important insights into the history of the Martian climate and the role of volatiles in Martian geologic activity. Here we present the results of counts of small impact craters, categorized by morphology, on debris aprons in the Deuteronilus Mensae region and the area east of Hellas basin. Mars Reconnaissance Orbiter (MRO) ConTeXt Camera (CTX) images were used to document crater populations on the apron surfaces. Each crater was assessed and categorized according to its morphological characteristics (fresh, degraded, or filled). Fresh and most degraded craters likely superpose recent mantling deposits, whereas filled craters contain mantling deposits and thus indicate a minimum formation age for the apron (i.e., the age since stabilization of the debris apron surface following some modification but prior to mantling). Size-frequency distributions (SFDs) were compiled using established methodologies and plotted to assess their fit to the isochrons. The range or ranges in crater diameter over which each distribution paralleled the isochrons was determined by visual inspection, and general age constraints were noted from SFDs for all craters on a given surface and from each morphological class. The diameter range of each SFD segment observed to parallel an isochron was then input into the Craterstats2 analysis tool to calculate specific age estimates. The aprons were assessed both individually and as regional populations, which improved interpretation of the results and demonstrated the value and limitations of both approaches. The categorized counts reveal three groups of ages: (a) filled impact craters at larger diameters (>~500 m) typically show the oldest ages, between ~300 Ma and 1 Ga, (b) smaller diameter filled and degraded craters reveal ages of resurfacing events between ~10 Ma and 300 Ma, and (c) fresh crater populations (<~100 m diameter) indicate mantling deposits of less than ~10 Ma in age. These results indicate that the lobate debris apron populations formed (or their surfaces became stable) in the Early to Middle Amazonian Epochs, and were subsequently subjected to complex degradation by erosion and sublimation and/or melting of contained ice, culminating in episodes of deposition of ice-rich mantles in the Late Amazonian Epoch.

Icy Layers in Craters

NASA Image and Video Library

2018-02-20

In this image from NASA's Mars Reconnaissance Rover (MRO) we can see the edge of a mound of ice in one of these mid-latitude craters. Some of it has already been removed, so we can see layering that used to be in the crater's interior. Scientists use ice deposits like these to figure out how the climate has changed on Mars. Another upside of recognizing this ice is that future astronauts will have plenty of drinking water. Scientists now realize that ice is very common on the Martian surface. It often fills up craters and valleys in the mid-latitudes in older climates, although when it's covered in dust it can be hard to recognize. Today the climate on Mars makes this ice unstable and some of it has evaporated away. https://photojournal.jpl.nasa.gov/catalog/PIA22255

Secondary Craters in Bas Relief

NASA Image and Video Library

2017-04-17

NASA's Mars Reconnaissance Orbiter (MRO) captured this region of Mars, sprayed with secondary craters from 10-kilometer Zunil Crater to the northwest. Secondary craters form from rocks ejected at high speed from the primary crater, which then impact the ground at sufficiently high speed to make huge numbers of much smaller craters over a large region. In this scene, however, the secondary crater ejecta has an unusual raised-relief appearance like bas-relief sculpture. How did that happen? One idea is that the region was covered with a layer of fine-grained materials like dust or pyroclastics about 1 to 2 meters thick when the Zunil impact occurred (about a million years ago), and the ejecta served to harden or otherwise protect the fine-grained layer from later erosion by the wind. https://photojournal.jpl.nasa.gov/catalog/PIA21591

MRO High Resolution Imaging Science Experiment (HiRISE): Instrument Development

NASA Technical Reports Server (NTRS)

Delamere, Alan; Becker, Ira; Bergstrom, Jim; Burkepile, Jon; Day, Joe; Dorn, David; Gallagher, Dennis; Hamp, Charlie; Lasco, Jeffrey; Meiers, Bill

2003-01-01

The primary functional requirement of the HiRISE imager is to allow identification of both predicted and unknown features on the surface of Mars to a much finer resolution and contrast than previously possible. This results in a camera with a very wide swath width, 6km at 300km altitude, and a high signal to noise ratio, >100:1. Generation of terrain maps, 30 cm vertical resolution, from stereo images requires very accurate geometric calibration. The project limitations of mass, cost and schedule make the development challenging. In addition, the spacecraft stability must not be a major limitation to image quality. The nominal orbit for the science phase of the mission is a 3pm orbit of 255 by 320 km with periapsis locked to the south pole. The track velocity is approximately 3,400 m/s.

Aerobraking Maneuver (ABM) Report Generator

NASA Technical Reports Server (NTRS)

Fisher, Forrest; Gladden, Roy; Khanampornpan, Teerapat

2008-01-01

abmREPORT Version 3.1 is a Perl script that extracts vital summarization information from the Mars Reconnaissance Orbiter (MRO) aerobraking ABM build process. This information facilitates sequence reviews, and provides a high-level summarization of the sequence for mission management. The script extracts information from the ENV, SSF, FRF, SCMFmax, and OPTG files and burn magnitude configuration files and presents them in a single, easy-to-check report that provides the majority of the parameters necessary for cross check and verification during the sequence review process. This means that needed information, formerly spread across a number of different files and each in a different format, is all available in this one application. This program is built on the capabilities developed in dragReport and then the scripts evolved as the two tools continued to be developed in parallel.

A Volcano of Mud or Lava?

NASA Image and Video Library

2018-06-11

This image from NASA's Mars Reconnaissance Orbiter (MRO) shows a hill with a central crater. Such features have been interpreted as both mud volcanoes (really a sedimentary structure) and as actual volcanoes (the erupting lava kind). They occur on the floor of Valles Marineris below a closed topographic contour that could have held a lake, and the compaction of wet sediments may have created mud volcanoes. The fracture pattern of the bright flow unit surrounding the hill resembles mud cracks. However, there have also been observations from the CRISM instrument interpreted as high-temperature minerals, suggesting actual volcanism, although not necessarily at this location. Fine layers in the hill are consistent with either volcanism or mud flows. Either way, this activity is relatively recent in geologic time and may mark habitable subsurface environments. https://photojournal.jpl.nasa.gov/catalog/PIA22514

Impact Craters on Mars: Natural 3D Exploration Probes of Geological Evolution

NASA Technical Reports Server (NTRS)

Garvin, James B.

2005-01-01

Introduction: The population of impact craters preserved on the surface of Mars offers fundamental constraints on the three- dimensional mechanical characteristics of the martian crust, its volatile abundance, and on the styles of erosion that have operated during essentially all epochs of martian geological history. On the basis of the present- day wealth of morphologic and geometric observations of impact landforms on Mars [ 1-31, an emerging understanding of the three-dimensional physical properties of the martian uppermost crust in space and time is at hand. In this summary, the current basis of understanding of the relatively non- degraded population of impact landforms on Mars is reviewed, and new Mars Global Surveyor (MGS)-based (MOLA) measurements of global geometric properties are summarized in the context of upcoming observations by Mars Reconnaissance Orbiter (MRO).

An Optimised System for Generating Multi-Resolution Dtms Using NASA Mro Datasets

NASA Astrophysics Data System (ADS)

Tao, Y.; Muller, J.-P.; Sidiropoulos, P.; Veitch-Michaelis, J.; Yershov, V.

2016-06-01

Within the EU FP-7 iMars project, a fully automated multi-resolution DTM processing chain, called Co-registration ASP-Gotcha Optimised (CASP-GO) has been developed, based on the open source NASA Ames Stereo Pipeline (ASP). CASP-GO includes tiepoint based multi-resolution image co-registration and an adaptive least squares correlation-based sub-pixel refinement method called Gotcha. The implemented system guarantees global geo-referencing compliance with respect to HRSC (and thence to MOLA), provides refined stereo matching completeness and accuracy based on the ASP normalised cross-correlation. We summarise issues discovered from experimenting with the use of the open-source ASP DTM processing chain and introduce our new working solutions. These issues include global co-registration accuracy, de-noising, dealing with failure in matching, matching confidence estimation, outlier definition and rejection scheme, various DTM artefacts, uncertainty estimation, and quality-efficiency trade-offs.

Inter-comparison of Methods for Extracting Subsurface Layers from SHARAD Radargrams over Martian polar regions

NASA Astrophysics Data System (ADS)

Xiong, S.; Muller, J.-P.; Carretero, R. C.

2017-09-01

Subsurface layers are preserved in the polar regions on Mars, representing a record of past climate changes on Mars. Orbital radar instruments, such as the Mars Advanced Radar for Subsurface and Ionosphere Sounding (MARSIS) onboard ESA Mars Express (MEX) and the SHAllow RADar (SHARAD) onboard the Mars Reconnaissance Orbiter (MRO), transmit radar signals to Mars and receive a set of return signals from these subsurface regions. Layering is a prominent subsurface feature, which has been revealed by both MARSIS and SHARAD radargrams over both polar regions on Mars. Automatic extraction of these subsurface layering is becoming increasingly important as there is now over ten years' of data archived. In this study, we investigate two different methods for extracting these subsurface layers from SHARAD data and compare the results against delineated layers derived manually to validate which methods is better for extracting these layers automatically.

Crustal thickness inversions from recent Mars Reconnaissance Orbiter gravity solutions

NASA Astrophysics Data System (ADS)

Neumann, Gregory; Zuber, Maria T.; Lemoine, Frank; Neumann, Gregory A.; Smith, David E.

Recent Mars Reconnaissance Orbiter gravity solutions from low-altitude tracking of MRO, together with previous spacecraft, have dramatically improved correlation with MOLA topography at spherical harmonic degrees up to 95. We present several updated models of crustal thickness. These models are calculated to fit the Bouguer potential anomaly following the assumptions in Neumann et al. 2004, with much weaker a priori constraints applied to the topographic corrections and the downward continuation to the martian mantle. These models are available via anonymous ftp to "ftp://lepftp.gsfc.nasa.gov/pub/exports/tharsis/marscrust3". The higher-resolution models improve on those we produced in 2004-2005. They are appropriate for modeling impacts as small as 300 km diameter, and for processes related to the hemispheric dichotomy boundary. We discuss in particular the assumption of quasi-uniform crustal density and its likely failure in volcanic regions.

Mars Without Borders: Creating a Global Community with the HiTranslate Project

NASA Astrophysics Data System (ADS)

Spinoza, A.

2013-12-01

The HiTranslate Project by HiRISE (MRO) is the most unique outreach program for an active NASA mission. Utilizing social media, we have built up a network of volunteers across the world to translate captioned images into various languages to reach a global audience with limited-to-no English skills. The result is a volunteer group of over 150 people making over 1,000 translated HiRISE captions and counting. The HiTranslate Project has also created specific media channels for each of these audiences, including other languages not traditionally represented in American-led science outreach efforts, like Icelandic, Greek, Arabic and Hebrew. This session will outline results of the Project and how it is a model for other science-based outreach efforts that can build up a global audience and communicate more effectively with the general public to grow interest in science.

MARs Color Imager (MARCI) Daily Global Ozone Column Mapping from the Mars Reconnaissance Orbiter (MRO): A Survey of 2006-2010 Results

NASA Astrophysics Data System (ADS)

Clancy, R. T.; Wolff, M. J.; Malin, M. C.; Cantor, B. A.

2010-12-01

MARCI UV band imaging photometry within (260nm) and outside (320nm) the Hartley ozone band absorption supports daily global mapping of Mars ozone column abundances. Key retrieval issues include accurate UV radiometric calibrations, detailed specifications of surface and atmospheric background reflectance (surface albedo, atmospheric Raleigh and dust scattering/absorption), and simultaneous cloud retrievals. The implementation of accurate radiative transfer (RT) treatments of these processes has been accomplished (Wolff et al., 2010) such that daily global mapping retrievals for Mars ozone columns have been completed for the 2006-2010 period of MARCI global imaging. Ozone retrievals are most accurate for high column abundances associated with mid-to-high latitude regions during fall, winter, and spring seasons. We present a survey of these MARCI ozone column retrievals versus season, latitude, longitude, and year.

Mechanical Description of the Mars Climate Sounder Instrument

NASA Technical Reports Server (NTRS)

Jau, Bruno M.

2008-01-01

This paper introduces the Mars Climate Sounder (MCS) Instrument of the Mars Reconnaissance Orbiter (MRO) spacecraft. The instrument scans the Martian atmosphere almost continuously to systematically acquire weather and climate observations over time. Its primary components are an optical bench that houses dual telescopes with a total of nine channels for visible and infrared sensing, and a two axis gimbal that provides pointing capabilities. Both rotating joints consist of an integrated actuator with a hybrid planetary/harmonic transmission and a twist cap section that enables the electrical wiring to pass through the rotating joint. Micro stepping is used to reduce spacecraft disturbance torques to acceptable levels while driving the stepper motors. To ensure survivability over its four year life span, suitable mechanical components, lubrication, and an active temperature control system were incorporated. Some life test results and lessons learned are provided to serve as design guidelines for actuator parts and flex cables.

A case for ancient springs in Arabia Terra, Mars.

PubMed

Allen, Carlton C; Oehler, Dorothy Z

2008-12-01

Based on new image data from the High Resolution Imaging Science Experiment (HiRISE) on Mars Reconnaissance Orbiter (MRO), a case can be made that several structures in Vernal Crater, Arabia Terra are ancient springs. This interpretation is based on comprehensive geomorphologic analysis coupled with assessment of multiple hypotheses. The structures identified extend across several kilometers and are exceptional in that nothing with their detail and scale has been reported from Mars. The deposits are associated with an extensive fracture system that may have facilitated upward flow of warm fluids. Several additional spring-like features occur in Vernal Crater, and it is possible that these are part of a major province of spring activity. Since springs are environments where life could have evolved on Mars, where that life could have found refuge as the climate became colder and drier, and where signatures of that life may be preserved, Vernal Crater may be a site of major astrobiological importance.

Landing Site Dispersion Analysis and Statistical Assessment for the Mars Phoenix Lander

NASA Technical Reports Server (NTRS)

Bonfiglio, Eugene P.; Adams, Douglas; Craig, Lynn; Spencer, David A.; Strauss, William; Seelos, Frank P.; Seelos, Kimberly D.; Arvidson, Ray; Heet, Tabatha

2008-01-01

The Mars Phoenix Lander launched on August 4, 2007 and successfully landed on Mars 10 months later on May 25, 2008. Landing ellipse predicts and hazard maps were key in selecting safe surface targets for Phoenix. Hazard maps were based on terrain slopes, geomorphology maps and automated rock counts of MRO's High Resolution Imaging Science Experiment (HiRISE) images. The expected landing dispersion which led to the selection of Phoenix's surface target is discussed as well as the actual landing dispersion predicts determined during operations in the weeks, days, and hours before landing. A statistical assessment of these dispersions is performed, comparing the actual landing-safety probabilities to criteria levied by the project. Also discussed are applications for this statistical analysis which were used by the Phoenix project. These include using the statistical analysis used to verify the effectiveness of a pre-planned maneuver menu and calculating the probability of future maneuvers.

A New Strategy to Land Precisely on the Northern Plains of Mars

NASA Technical Reports Server (NTRS)

Cheng, Yang; Huertas, Andres

2010-01-01

During the Phoenix mission landing site selection process, the Mars Reconnaissance Orbiter (MRO) High Resolution Imaging Science Experiment (HiRISE) images revealed widely spread and dense rock fields in the northern plains. Automatic rock mapping and subsequent statistical analyses showed 30-90% CFA (cumulative fractional area) covered by rocks larger than 1 meter in dense rock fields around craters. Less dense rock fields had 5-30% rock coverage in terrain away from craters. Detectable meter-scale boulders were found nearly everywhere. These rocks present a risk to spacecraft safety during landing. However, they are the most salient topographic features in this region, and can be good landmarks for spacecraft localization during landing. In this paper we present a novel strategy that uses abundance of rocks in northern plains for spacecraft localization. The paper discusses this approach in three sections: a rock-based landmark terrain relative navigation (TRN) algorithm; the TRN algorithm feasibility; and conclusions.

Formations in Context (or, what is it?)

NASA Image and Video Library

2018-04-02

This image from NASA's Mars Reconnaissance Orbiter is a close-up of a trough, along with channels draining into the depression. Some HiRISE images show strange-looking formations. Sometimes it helps to look at Context Camera images to understand the circumstances of a scene -- like this cutout from CTX 033783_1509 -- which here shows an impact crater with a central peak, and a collapse depression with concentric troughs just north of that peak. On the floor of the trough is some grooved material that we typically see in middle latitude regions where there has been glacial flow. These depressions with concentric troughs exist elsewhere on Mars, and their origins remain a matter of debate. NB: The Context Camera is another instrument onboard MRO, and it has a larger viewing angle than HiRISE, but less resolution capability than our camera. https://photojournal.jpl.nasa.gov/catalog/PIA22348

The Case of the Martian Boulder Piles

NASA Image and Video Library

2018-03-05

This image from NASA's Mars Reconnaissance Orbiter (MRO) was originally meant to track the movement of sand dunes near the North Pole of Mars, but what's on the ground in between the dunes is just as interesting! The ground has parallel dark and light stripes from upper left to lower right in this area. In the dark stripes, we see piles of boulders at regular intervals. What organized these boulders into neatly-spaced piles? In the Arctic back on Earth, rocks can be organized by a process called "frost heave." With frost heave, repeatedly freezing and thawing of the ground can bring rocks to the surface and organize them into piles, stripes, or even circles. On Earth, one of these temperature cycles takes a year, but on Mars it might be connected to changes in the planet's orbit around the Sun that take much longer. https://photojournal.jpl.nasa.gov/catalog/PIA22334

Analyses of IR-Stealthy and Coated Surface Materials: A Comparison of LIBS and Reflectance Spectra and Their Application to Mars Surface Exploration

NASA Technical Reports Server (NTRS)

Wiens, R. C.; Kirkland, L. E.; McKay, C. P.; Cremers, D. A.; Thompson, J.; Maurice, S.; Pinet, P. C.

2004-01-01

Identification of non-silicate samples on Mars, such as carbonates, sulfates, nitrates, or evaporites in general, is important because of their association with aqueous processes and their potential as exobiology sites. Infrared (IR) and thermal emission (TE) spectroscopy have been considered the primary tools for remote identification of these minerals. This includes current and future orbital assets such as TES on MGS, THEMIS on Mars Odyssey, OMEGA on Mars Express, CRISM on MRO, and now the Mini-TES on the MER rovers. While reflectance and emission spectroscopy have clearly been the method of choice for these missions, the technique is not always successful in mineral identifications due to dust, surface weathering chemistry, coatings, or surface texture. Here we describe and show IR spectra of several such samples, and then report on the relative success of LIBS analyses in determining the rock type.

Model Estimates of Non-Hydrostatic Stresses in the Martian Crust and Mantle: 1—Two-Level Model

NASA Astrophysics Data System (ADS)

Gudkova, T. V.; Batov, A. V.; Zharkov, V. N.

2017-11-01

Regions of maximum shear and tension-compression stresses in the Martian interior have been revealed using two types of models: the elastic model and the model with an elastic lithosphere of varied thickness (150-500 km) positioned on a weak layer that has partially lost its elastic properties. The weakening is simulated by a ten-fold lower value of the shear modulus down to the core boundary. The numerical simulation applies Green's functions (load number method) with the step of 1 × 1 grade along latitude and longitude down to a depth of 1000 km. The boundary condition is the expansion of the latest data on Martian topography and the gravitational field (model MRO120D) in spherical harmonics up to the degree and order of 90 in relation to the reference surface that is assumed an equilibrium spheroid. The considered two-level compensation model assumes nonequilibrium relief and density anomalies at the crust-mantle boundary to be the sources of the anomalous gravitational field. Calculations are performed for two test models of Martian internal structure with the crust mean thicknesses of 50 to 100 km and mean density of 2900 kg/m3. Considerable tangential and simultaneously compressive stresses occur under the Tharsis region. The main regions of high shear and simultaneously extentional stresses are located in the Hellas region crust and in the lithosphere of the following regions: Argyre Planitia, Mare Acidalium, Arcadia Planitia and Valles Marineris. The zone of high maximum shear and extentional stresses has been found at the base of the lithosphere under the Olympus volcano and that under the Elysium rise.

The Optimization of Trained and Untrained Image Classification Algorithms for Use on Large Spatial Datasets

NASA Technical Reports Server (NTRS)

Kocurek, Michael J.

2005-01-01

The HARVIST project seeks to automatically provide an accurate, interactive interface to predict crop yield over the entire United States. In order to accomplish this goal, large images must be quickly and automatically classified by crop type. Current trained and untrained classification algorithms, while accurate, are highly inefficient when operating on large datasets. This project sought to develop new variants of two standard trained and untrained classification algorithms that are optimized to take advantage of the spatial nature of image data. The first algorithm, harvist-cluster, utilizes divide-and-conquer techniques to precluster an image in the hopes of increasing overall clustering speed. The second algorithm, harvistSVM, utilizes support vector machines (SVMs), a type of trained classifier. It seeks to increase classification speed by applying a "meta-SVM" to a quick (but inaccurate) SVM to approximate a slower, yet more accurate, SVM. Speedups were achieved by tuning the algorithm to quickly identify when the quick SVM was incorrect, and then reclassifying low-confidence pixels as necessary. Comparing the classification speeds of both algorithms to known baselines showed a slight speedup for large values of k (the number of clusters) for harvist-cluster, and a significant speedup for harvistSVM. Future work aims to automate the parameter tuning process required for harvistSVM, and further improve classification accuracy and speed. Additionally, this research will move documents created in Canvas into ArcGIS. The launch of the Mars Reconnaissance Orbiter (MRO) will provide a wealth of image data such as global maps of Martian weather and high resolution global images of Mars. The ability to store this new data in a georeferenced format will support future Mars missions by providing data for landing site selection and the search for water on Mars.

The Niagara Falls of Mars

NASA Image and Video Library

2017-06-26

Various researchers are often pre-occupied with the quest for flowing water on Mars. However, this image from NASA's Mars Reconnaissance Orbiter (MRO), shows one of the many examples from Mars where lava (when it was molten) behaved in a similar fashion to liquid water. The northern rim of a 30-kilometer diameter crater situated in the western part of the Tharsis volcanic province is shown. The image shows that a lava flow coming from the north-northeast surrounded the crater rim, and rose to such levels that it breached the crater rim at four locations to produce spectacular multi-level lava falls (one in the northwest and three in the north). These lava "falls" cascaded down the wall and terraces of the crater to produce a quasi-circular flow deposit. It seems that the flows were insufficient to fill or even cover the pre-existing deposits of the crater floor. This is evidenced by the darker-toned lavas that overlie the older, and possibly dustier, lighter-toned deposits on the crater floor. This image covers the three falls in the north-central region of the crater wall. The lava flows and falls are distinct as they are rougher than the original features that are smooth and knobby. In a close-up image the rough-textured lava flow to the north has breached the crater wall at a narrow point, where it then cascades downwards, fanning out and draping the steeper slopes of the wall in the process. Image scale is 54.5 centimeters (21.5 inches) per pixel (with 2 x 2 binning); objects on the order of 164 centimeters (64.6 inches) across are resolved.] North is up. https://photojournal.jpl.nasa.gov/catalog/PIA21763

Inflated flows on Daedalia Planum (Mars)? Clues from a comparative analysis with the Payen volcanic complex (Argentina)

NASA Astrophysics Data System (ADS)

Giacomini, L.; Massironi, M.; Martellato, E.; Pasquarè, G.; Frigeri, A.; Cremonese, G.

2009-05-01

Inflation is an emplacement process of lava flows, where a thin visco-elastic layer, produced at an early stage, is later inflated by an underlying fluid core. The core remains hot and fluid for extended period of time due to the thermal-shield effect of the surface visco-elastic crust. Plentiful and widespread morphological fingerprints of inflation like tumuli and lava rises are found on the Payen volcanic complex (Argentina), where pahoehoe lava flows extend over the relatively flat surface of the Pampean foreland and reach at least 180 km in length. The morphology of the Argentinean Payen flows were compared with lava flows on Daedalia Planum (Mars), using Thermal Emission Imaging System (THEMIS), Mars Orbiter Laser Altimeter (MOLA), Mars Orbiter Camera (MOC), Mars Reconnaissance Orbiter (MRO)/High-Resolution Imaging Science Experiment (HiRISE). THEMIS images were used to map the main geological units of Daedalia Planum and determine their stratigraphic relationships. MOLA data were used to investigate the topographic surface over which the flows propagated and assess the thickness of lava flows. Finally, MOC and MRO/HIRISE images were used to identify inflations fingerprints and assess the cratering age of the Daedalia Planum' s youngest flow unit which were found to predate the caldera formation on top of the Arsia Mons. The identification of similar inflation features between the Daedalia Planum and the Payen lava fields suggests that moderate and long lasting effusion rates coupled with very efficient spreading processes could have cyclically occurred in the Arsia Mons volcano during its eruptive history. Consequently the effusion rates and rheological proprieties of Daedalia lava flows, which do not take into account the inflation process, can be overestimated. These findings raise some doubts about the effusion rates and lava rheological properties calculated on Martian flows and recommends that these should be used with caution if applied on flows not checked with high-resolution images and potentially affected by inflation. Further HiRISE data acquisition will permit additional analysis of the flow surfaces and will allow more accurate estimates of effusion rates and rheological properties of the lava flows on Mars particularly if this data is acquired under a favourable illumination.

Geologic investigation of layered mound of Henry Crater, Mars: Implications for history of ancient hydrological activities in the region

NASA Astrophysics Data System (ADS)

Sarkar, Samarpita; Sinha, Rishitosh Kumar; Banerjee, Debabrata; Vijayan, S.

2016-07-01

Craters around the Schiaparelli Basin (sim460 km diameter; 2.71^circS 16.77^circE) on Mars are distributed in a unique combination that includes infilled craters with mound on their floors. The mounds have preserved intriguing layers in stratigraphy that has exposed pristine sets of geomorphic and geochemical signatures bearing strong implications towards understanding geological history of Mars. With a view to avail the maximum scientific benefit from this unique geological assemblage on Mars, we have carried out remote analysis of stratigraphy of layers exposed over Henry crater's (sim150 km diameter; 10.79^circN 23.45^circE) mound (rising sim2km from floor) to infer the origin and episodes of geological events occurred in the region. Henry crater is situated approximately 500 km northeast of Schiaparelli Basin. Using crater counting technique the age of the topmost surface of the crater mound is found to be sim3.64 Ga since the exposure of this strata post complete infilling. The stratigraphy of consistent and conformable layers in the crater interior acts as a proxy of the long-lived event of sediment deposition in a rather quiescent condition. Distinct layering can be traced across the crater from the mound to the crater wall across the floor. Evidence for differential erosion of deposited materials, wherein local geological setup developed in the different parts of the crater interior is preserved. Using MRO HiRISE & CTX images, distinct spatial distribution of morphological features distributed in stratigraphy is observed that reveals the dominant geological agents behind their formation, viz. temporal hydrological and eolian processes. The morphological features were aided with an understanding of the composition of the exposed sedimentary succession. MRO CRISM based mineralogical investigation reveals diagnostic signature of the hydrated sulfate mineral Kieserite. Based on the thermodynamic properties of Kieserite and apparent lack of desiccation cracks in the scale of observation, it is inferred that the water level inside the crater did not experience fluctuation. Rather on systematic compilation of the mineralogical and morphological data, it is inferred that the mound formation process was gradual and can be correlated with the water level inside the crater at various stages during the recession stage.

Opportunistic MSPA Demonstration #1: Final Report

NASA Astrophysics Data System (ADS)

Abraham, D. S.; Finley, S. G.; Heckman, D. P.; Lay, N. E.; Lush, C. M.; MacNeal, B. E.

2015-02-01

The Opportunistic Multiple Spacecraft Per Antenna (OMSPA) concept seeks to provide smallsat missions with a low-attributed-aperture-fee technique for obtaining routine downlink in a manner that is very low cost to the Deep Space Network (DSN). Unlike traditional MSPA in which the number of spacecraft that can be supported is limited by the number of available receivers, OMSPA makes use of a digital recorder at each station that is capable of capturing IF signals from every spacecraft in the antenna beam within the frequency bands of interest. When smallsat missions see one or more opportunities to intercept the traditionally scheduled antenna beam of a "host" spacecraft, they can transmit open loop during those opportunities. Via a secure Internet site, the smallsat mission operators can then retrieve relevant portions of the digital recording for subsequent demodulation and decoding or subscribe to a service that does it for them. The demonstration discussed in this article was intended to provide prospective smallsat users and the DSN, as the prospective service provider, with demonstrable proof that the OMSPA concept is, in fact, an operationally viable means for obtaining routine downlink telemetry. To do this, the demonstration began by treating Mars Odyssey as a "smallsat" and Mars Reconnaissance Orbiter (MRO) as the "host" spacecraft. Using a specially created Beam Intercept Planning System (BIPS) and a DSN 7-Day Schedule Cross-Comparison (7-DSC) tool, opportunities were identified when Mars Odyssey would be transmitting while in MRO's ground antenna beam. Existing Very Long Baseline Interferometry (VLBI) Science Receivers (VSRs) were used to record the Mars Odyssey downlink telemetry during these opportunities. The recordings were played back to a secure server outside the Flight Operations Network firewall, but inside the JPL firewall. The demonstration team's signal processing personnel retrieved the recordings from this secure server and downloaded them to a workstation containing an OMSPA Software Demodulator (OSD) tool that was developed to demodulate and decode the Mars Odyssey signal. Validation of the recovered data was then accomplished by comparing the transfer frames obtained through OMSPA with those recovered via Mars Odyssey's formally scheduled downlink. The demonstration successfully achieved its intended purpose. All of the above steps were accomplished within an operationally viable timeframe, with at least 99.95 percent of the transfer frames being successfully recovered from each demonstration recording.

Identifying Surface Changes on HRSC Images of the Mars South Polar Residual CAP (sprc)

NASA Astrophysics Data System (ADS)

Putri, Alfiah Rizky Diana; Sidiropoulos, Panagiotis; Muller, Jan-Peter

2016-06-01

The surface of Mars has been an object of interest for planetary research since the launch of Mariner 4 in 1964. Since then different cameras such as the Viking Visual Imaging Subsystem (VIS), Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC), and Mars Reconnaissance Orbiter (MRO) Context Camera (CTX) and High Resolution Imaging Science Experiment (HiRISE) have been imaging its surface at ever higher resolution. The High Resolution Stereo Camera (HRSC) on board of the European Space Agency (ESA) Mars Express, has been imaging the Martian surface, since 25th December 2003 until the present-day. HRSC has covered 100 % of the surface of Mars, about 70 % of the surface with panchromatic images at 10-20 m/pixel, and about 98 % at better than 100 m/pixel (Neukum et. al., 2004), including the polar regions of Mars. The Mars polar regions have been studied intensively recently by analysing images taken by the Mars Express and MRO missions (Plaut et al., 2007). The South Polar Residual Cap (SPRC) does not change very much in volume overall but there are numerous examples of dynamic phenomena associated with seasonal changes in the atmosphere. In particular, we can examine the time variation of layers of solid carbon dioxide and water ice with dust deposition (Bibring, 2004), spider-like channels (Piqueux et al., 2003) and so-called Swiss Cheese Terrain (Titus et al., 2004). Because of seasonal changes each Martian year, due to the sublimation and deposition of water and CO2 ice on the Martian south polar region, clearly identifiable surface changes occur in otherwise permanently icy region. In this research, good quality HRSC images of the Mars South Polar region are processed based on previous identification as the optimal coverage of clear surfaces (Campbell et al., 2015). HRSC images of the Martian South Pole are categorized in terms of quality, time, and location to find overlapping areas, processed into high quality Digital Terrain Models (DTMs) and Orthorectified Images (ORIs) and projected into polar stereographic projection using DLR (Deutsches Zentrum für Luft- und Raumfahrt; German Aerospace Center)'s VICAR and GIS software with modifications developed by Kim & Muller (2009). Surface changes are identified in the Mars SPRC region and analysed based on their appearance in the HRSC images.

MRO Mars Color Imager (MARCI) Investigation Primary Mission Results

NASA Astrophysics Data System (ADS)

Edgett, K. S.; Cantor, B. A.; Malin, M. C.; Science; Operations Teams, M.

2008-12-01

The Mars Reconnaissance Orbiter (MRO) Mars Color Imager (MARCI) investigation was designed to recover the wide angle camera science objectives of the Mars Climate Orbiter MARCI which was destroyed upon arrival at Mars in 1999 and extend the daily meteorological coverage of the Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) wide angle investigation that was systematically conducted from March 1999 to October 2006. MARCI consists of two wide angle cameras, each with a 180° field of view. The first acquires data in 5 visible wavelength channels (420, 550, 600, 650, 720 nm), the second in 2 UV channels (260, 320 nm). Data have been acquired daily, except during spacecraft upsets, since 24 September 2006. From the MRO 250 to 315 km altitude orbit, inclined 93 degrees, visible wavelength images usually have a pixel scale of about 1 km at nadir and the UV data are at about 8 km per pixel. Data are obtained during every orbit on the day side of the planet from terminator to terminator. These provide a nearly continuous record of meteorological events and changes in surface frost and albedo patterns that span more than 1 martian year and extend the daily global record of such events documented by the MGS MOC. For a few weeks in September and October 2006, both camera systems operated simultaneously, providing views of weather events at about 1400 local time (MOC) and an hour later at about 1500 (MARCI). The continuous meteorological record, now spanning more than 5 Mars years, shows very repeatable weather from year to year with cloud and dust-raising events occurring in the same regions within about 2 weeks of their prior occurrence in previous years. This provides a measure of predictability ideal for assessing future landing sites, orbiter aerobraking plans, and conditions to be encountered by the current landed spacecraft on Mars. However, less predictable are planet-encircling dust events. MOC observed one in 2001, the next was observed by MARCI in 2007. These occurred at different times of year. While popularly known as global dust storms, the nomenclature is misleading, as in each case a storm did not raise dust nor saltate sand on a global basis. Instead, multiple regional storms created a dust haze which obscured much of the martian surface from viewpoints above the lower atmosphere, but in each case the dust opacity was never so high that one could not determine where dust was being raised and where it was not. Within weeks of the end of the 2001 and 2007 global dust events, martian weather returned to its normal, repeatable pattern, with one exception: occasionally thereafter, dust storms were observed in regions where dust-raising had not been seen in the previous years. In these cases, winds capable of raising dust likely occurred at that location every year, but only became visible following a planet-encircling dust event and deposition of dust on a surface that previously did not have sufficient dust to raise. Other MARCI results center on seasonal monitoring of water vapor in the atmosphere, particularly by taking advantage of the anti-correlation between ozone (observable using the UV channels) and water vapor. Owing to their higher spatial resolution than the MOC daily global coverage, details of seasonal polar cap retreat became more apparent, as with these data it is now possible to separate surface frost from ground-hugging fog which forms along the retreating cap edge. MARCI images and meteorological observations are posted weekly on the Internet for public consumption, and the data are archived every 6 months with the NASA Planetary Data System.

[Positron emission tomographic evaluations on hemodynamics and glucose metabolism of brain tumors and perifocal edematous tissues].

PubMed

Mizukawa, N; Hino, A; Imahori, Y; Tenjin, H; Yano, I; Yoshino, E; Hirakawa, K; Yamashita, M; Oki, F; Nakahashi, H

1989-03-01

Blood flow and glucose metabolism of the tumors and perifocal edematous tissues were evaluated using positron emission tomography (PET). Thirty-one brain tumor cases were investigated 12 non glial tumors (9 meningiomas and 3 metastatic tumors) and 19 gliomas (these were classified in 5 astrocytomas, 7 anaplastic astrocytomas and 7 glioblastomas, according to the malignancy). The diagnosis were confirmed pathologically in 30 cases. Cerebral blood flow (CBF), cerebral metabolic rate for oxygen (CMRO2), oxygen extraction fraction (OEF) and cerebral blood volume (CBV) were measured by O-15 labeled gases inhalation methods. Cerebral metabolic rate for glucose (CMFglu) were measured by F-18 Deoxyglucose intravenous injection method and calculated by Hutchins's formula. The rate constant (ks) and lumped constant (LC) used in this study were the same as those published by Phelps et al. in 1979. The blood flow and glucose metabolic rates of tumors were measured by the same methods. The results were as follows: 1) Meningiomas showed very high blood flow and blood volume with a wide range. The OEF and metabolic rate for glucose (MRglu) values were very low. 2) Metastatic tumors showed the low values of blood flow, metabolic rate for oxygen (MRO2) and OEF. 3) The blood flow and MRglu values on gliomas were varied with no significant differences between the three subgroups. On the other hands, as the malignancy of the glioma increased, a statistically significant increase in blood volume and a decrease in OEF were noted. 4) The OEF values from the various types of tumors studied were significantly lower than those obtained from the normal tissue.(ABSTRACT TRUNCATED AT 250 WORDS)

Particle Size of CO2 Condensates in Mars Atmosphere Revealed by Climate Sounder and Laser Ranging Observations

NASA Astrophysics Data System (ADS)

Hu, Renyu

Current-generation Mars Climate Sounder (MCS) onboard the Mars Reconnaissance Orbiter (MRO) offers extensive coverage of the latitudinal and seasonal distribution of CO_2 condensation in Mars’s atmosphere. The atmospheric temperature profiles measured by MCS reveal that the thickness of CO_2 condensation layer reaches a maximum of 10-15 km (north) or ˜20 km (south) during the middle of winter. There is a shrinking of the CO_2 condensation layer from L_S ˜270(°) to ˜300(°) in 2007, probably related to a planet-encircling dust storm. We integrate the condensation area and the condensation occurrence rate synthesized from the MCS observations to estimate cumulative masses of CO2 condensates deposited onto the northern and southern seasonal polar caps. The mass loading of CO_2 condensate particles, when condensation occurs, can be independently inferred from the detections of reflective clouds by the Mars Orbiter Laser Altimetry (MOLA) onboard the Mars Global Surveyor (MGS). Therefore, we approximate the precipitation flux by the particle settling flux, which is estimated using the impulse responses of MOLA filter channels. With our approach, the total atmospheric condensation mass can be estimated from these observational data sets, with average particle size as the only free parameter. By comparison with the seasonal polar cap masses inferred from the time-varying gravity of Mars, our estimates indicate that the average condensate particle radius is 8 - 22 mum in the northern hemisphere and 4 - 13 mum in the southern hemisphere. This multi-instrument data analysis provides new constraints on modeling the microphysics of CO_2 clouds on Mars.

Atypical pit craters on Mars: new insights from THEMIS, CTX and HiRISE observations

USGS Publications Warehouse

Cushing, Glen; Okubo, Chris H.; Titus, Timothy N.

2015-01-01

More than 100 pit craters in the Tharsis region of Mars exhibit morphologies, diameters and thermal behaviors that diverge from the much larger bowl-shaped pit craters that occur in most regions across Mars. These Atypical Pit Craters (APCs) generally have sharp and distinct rims, vertical or overhanging walls that extend down to their floors, surface diameters of ~50-350 m, and high depth-to-diameter (d/D) ratios that are usually greater than 0.3 (which is an upper-range value for impacts and bowl-shaped pit craters), and can exceed values of 1.8. Observations by the Mars Odyssey THermal Emission Imaging System (THEMIS) show that APC floor temperatures are warmer at night, and fluctuate with much lower diurnal amplitudes than nearby surfaces or adjacent bowl-shaped pit craters. Kīlauea volcano, Hawai'i, hosts pit craters that formed through subsurface collapse into active volcanic dikes, resulting in pits that can appear morphologically analogous to either APCs or bowl-shaped pit craters. Partially-drained dikes are sometimes exposed within the lower walls and floors of these terrestrial APC analogs and can form extensive cave systems with unique microclimates. Similar caves in martian pit craters are of great interest for astrobiology. This study uses new observations by the Mars Reconnaissance Orbiter (MRO) High Resolution Imaging Science Experiment (HiRISE) and Context Camera (CTX) to refine previous work where seven APCs were described from lower-resolution THEMIS visible-wavelength (VIS) observations. Here, we identify locations of 115 APCs, map their distribution across the Tharsis region, characterize their internal morphologies with high-resolution observations, and discuss possible formation mechanisms.

Ultraviolet dust aerosol properties as observed by MARCI

NASA Astrophysics Data System (ADS)

Wolff, Michael J.; Todd Clancy, R.; Goguen, Jay D.; Malin, Michael C.; Cantor, Bruce A.

2010-07-01

Observations by the Mars Color Imager (MARCI) on board the Mars Reconnaissance Orbiter (MRO) in two ultraviolet (UV, Bands 6 and 7; 258 nm, and 320 nm, respectively) and one visible (Band 1, 436 nm) channels of the 2007 planet encircling dust storm are combined with those made by the two Mars Exploration Rovers (MERs) to better characterize the single scattering albedo (ω0) of martian dust aerosols. Exploiting the low contrast of the surface in the UV (and blue) as well as the reduced importance of surface reflectance under very dusty conditions, we utilize the sampling of photometric angles by the MARCI cross-track geometry to synthesize an analog of the classical Emergence Phase Function (EPF). This so-called "pseudo-EPF", used in conjunction with the "ground-truth" measurements provided by the MERs, is able to effectively isolate the effects of the dust ω0. The motivation for this approach is the elimination of a significant portion of the type of uncertainty involved in many previous radiative transfer analyses. Furthermore, we produce a self-consistent set of complex refractive indices (m=n+ik) through our use of an explicit microphysical representation of the aerosol scattering properties. Because of uncertainty in the exact size of the dust particles during the epoch of the observations, we consider two effective particle radii (reff) to cover the range anticipated from the literature: 1.6 and 1.8 μm. The resulting set of model-data comparisons, ω0, and m are presented along with an assessment of potential sources of error and uncertainty. Analysis of the Band 1 results is limited to ω0 as a "proof-of-concept" for our approach through a comparison to contemporaneous CRISM EPF results at 440 nm. The derived ω0 are: assuming reff=1.6μm-0.619-0.626,0.648, and 0.765, for Bands 6, 7, and 1, respectively; for reff=1.8μm-0.625-0.635,0.653,0.769, for the same band order. For either reff case, the total estimated error is 0.022, 0.019, and 0.010, again for Bands 6, 7, and 1. We briefly discuss our retrievals, including the asymmetry parameter ( g) associated with our model phase functions, within the context of previous efforts, with an emphasis on the improved precision of our results compared to those in the literature. We also suggest several applications of our results, including an extension of the dust climatological record using MARCI Band 7 pseudo-EPFs outside of 2007 global dust event. Initial work on this particular application using a sample of 135 pseudo-EPFs near the MERs suggests that optical depth retrievals with a precision in the range 0.2-0.4 may be possible under moderate loading conditions (i.e., τ < 1.5).

Structural properties of medium-range order in CuNiZr alloy

NASA Astrophysics Data System (ADS)

Gao, Tinghong; Hu, Xuechen; Xie, Quan; Li, Yidan; Ren, Lei

2017-10-01

The evolution characteristics of icosahedral clusters during the rapid solidification of Cu50Ni10Zr40 alloy at cooling rate of 1011 K s-1 are investigated based on molecular dynamics simulations. The structural properties of the short-range order and medium-range order of Cu50Ni10Zr40 alloy are analyzed by several structural characterization methods. The results reveal that the icosahedral clusters are the dominant short-range order structure, and that they assemble themselves into medium-range order by interpenetrating connections. The different morphologies of medium-range order are found in the system and include chain, triangle, tetrahedral, and their combination structures. The tetrahedral morphologies of medium-range order have excellent structural stability with decreasing temperature. The Zr atoms are favorable to form longer chains, while the Cu atoms are favorable to form shorter chains in the system. Those chains interlocked with each other to improve the structural stability.

Positional short-range order in the nematic phase of n BABAs

NASA Astrophysics Data System (ADS)

Usha Deniz, K.; Pepy, G.; Parette, G.; Keller, P.

1991-10-01

The positional short-range order, SRO ⊥, perpendicular to the nematic director n̂ has been studied in the fibre-type nematics, nBABAs, by neutron diffraction. SRO ⊥ is found to be dependent on other types of nematic short-range order but not on the orientational long-range order.

Modeling Mars Cyclogenesis and Frontal Waves: Seasonal Variations and Implications on Dust Activity

NASA Technical Reports Server (NTRS)

Hollingsworth, J. L.; Kahre, M. A.

2014-01-01

Between late autumn through early spring,middle and high latitudes onMars exhibit strong equator-to-polemean temperature contrasts (i.e., "baroclinicity"). Data collected during the Viking era and observations from both the Mars Global Surveyor (MGS) and Mars Reconnaissance Orbiter (MRO) indicate that such strong baroclinicity supports vigorous, large-scale eastward traveling weather systems (i.e., transient synoptic period waves) [1, 2]. For a rapidly rotating, differentially heated, shallow atmosphere such as on Earth and Mars, these large-scale, extratropical weather disturbances are critical components of the global circulation. The wave-like disturbances serve as agents in the transport of heat and momentum between low and high latitudes of the planet. Through cyclonic/anticyclonic winds, intense shear deformations, contractions-dilatations in temperature and density, and sharp perturbations amongst atmospheric tracers (i.e., dust, volatiles (e.g., water vapor) and condensates (e.g., water-ice cloud particles)), Mars' extratropical weather systems have significant sub-synoptic scale ramifications by supporting atmospheric frontal waves (Fig. 1).

Selecting A Landing Site Of Astrobiological Interest For Mars Landers And Sample Return Missions

NASA Astrophysics Data System (ADS)

Wills, Danielle; Monaghan, E.; Foing, B.

2008-09-01

The landscape of Mars, despite its apparent hostility to life, is riddled with geological and mineralogical signs of past or present hydrological activity. As such, it is a key target for astrobiological exploration. The aim of this work is to combine data and studies to select top priority landing locations for in-situ landers and sample return missions to Mars. We report in particular on science and technical criteria and our data analysis for sites of astrobiological interest. This includes information from previous missions (such as Mars Express, MGS, Odyssey, MRO and MER rovers) on mineralogical composition, geomorphology, evidence from past water history from imaging and spectroscopic data, and existence of in-situ prior information from landers and rovers (concerning evidence for volatiles, organics and habitability conditions). We discuss key mission objectives, and consider the accessibility of chosen locations. We describe what additional measurements are needed, and outline the technical and scientific operations requirements of in-situ landers and sample return missions to Mars.

Extratropical Cyclogenesis and Frontal Waves on Mars: Influences on Dust, Weather and the Planet's climate

NASA Technical Reports Server (NTRS)

Hollingsworth, J. L.; Kahre, Melinda A.

2012-01-01

Between late autumn and early spring, middle and high latitudes on Mars exhibit strong equatortopole mean temperature contrasts (i.e., "baroclinicity"). Data collected during the Viking era and observations from both the Mars Global Surveyor (MGS) and Mars Reconnaissance Orbiter (MRO) indicate that this strong baroclinicity supports vigorous, large-scale eastward traveling weather systems (i.e., transient synoptic periodwaves) [1,2]. For a rapidly rotating, differentially heated, shallow atmosphere such as on Earth and Mars, these large-scale, extratropical weather disturbances are critical components of the global circulation. The wavelike disturbances act as agents in the transport of heat and momentum between low and high latitudes of the planet. Through cyclonic/anticyclonic winds, intense shear deformations, contractions-dilatations in temperature and density, and sharp perturbations amongst atmospheric tracers (i.e., dust, volatiles (e.g., water vapor) and condensates (e.g., water-ice cloud particles)), Mars extratropical weather systems have significant subsynoptic scale ramifications by supporting atmospheric frontal waves (Fig. 1).

Influence of Fault-Controlled Topography on Fluvio-Deltaic Sedimentary Systems in Eberswalde Crater, Mars

NASA Technical Reports Server (NTRS)

Rice, Melissa S.; Gupta, Sanjeev; Bell, James F., III; Warner, Nicholas H.

2011-01-01

Eberswalde crater was selected as a candidate landing site for the Mars Science Laboratory (MSL) mission based on the presence of a fan-shaped sedimentary deposit interpreted as a delta. We have identified and mapped five other candidate fluvio -deltaic systems in the crater, using images and digital terrain models (DTMs) derived from the Mars Reconnaissance Orbiter (MRO) High Resolution Imaging Science Experiment (HiRISE) and Context Camera (CTX). All of these systems consist of the same three stratigraphic units: (1) an upper layered unit, conformable with (2) a subpolygonally fractured unit, unconformably overlying (3) a pitted unit. We have also mapped a system of NNE-trending scarps interpreted as dip-slip faults that pre-date the fluvial -lacustrine deposits. The post-impact regional faulting may have generated the large-scale topography within the crater, which consists of a Western Basin, an Eastern Basin, and a central high. This topography subsequently provided depositional sinks for sediment entering the crater and controlled the geomorphic pattern of delta development.

Internal Characteristics of Phobos and Deimos from Spectral Properties and Density: Relationship to Landforms and Comparison with Asteroids

NASA Technical Reports Server (NTRS)

Murchie, S. L.; Fraeman, A. A.; Arvidson, R. E.; Rivkin, A. S.; Morris, R. V.

2013-01-01

Compositional interpretations of new spectral measurements of Phobos and Deimos from Mars Express/OMEGA and MRO/CRISM and density measurements from encounters by multiple spacecraft support refined estimates of the moons' porosity and internal structure. Phobos' estimated macroporosity of 12-20% is consistent with a fractured but coherent interior; Deimos' estimated macroporosity of 23-44% is more consistent with a loosely consolidated interior. These internal differences are reflected in differences in surface morphology: Phobos exhibits a globally coherent pattern of grooves, whereas Deimos has a surface dominated instead by fragmental debris. Comparison with other asteroids .110 km in diameter shows that this correspondence between landforms and inferred internal structure is part of a pervasive pattern: asteroids interpreted to have coherent interiors exhibit pervasive, organized ridge or groove systems, whereas loosely consolidated asteroids have landforms dominated by fragmental debris and/or retain craters >1.3 body radii in diameter suggesting a porous, compressible interior.

Assessing Spectral Evidence of Aqueous Activity in Two Putative Martian Paleolakes

NASA Technical Reports Server (NTRS)

Roush, Ted L.; Marzo, Giuseppe A.; Fonti, Sergio; Orofino, Vicenzo; Blanco, Armando; Gross, Christoph; Wendt, Lorenz

2011-01-01

We evaluate the evidence for the presence of mineral spectral signatures indicative of the past presence of water at two putative paleolakes on Mars using observations by the Mars Reconnaissance Orbiter (MRO) Compact Reconnaissance Image Spectrometer for Mars (CRISM). CRISM spectra of both sites are consistent with laboratory spectra of Mg-rich phyllosilicates. Our analysis represents the first detailed evaluation of these locations. The spatial occurrence and association with topographic features within the craters is distinctly different for the two sites. The occurrence of these minerals supports the conclusion that water was once active in the areas sampled by these craters. The distribution of the phyllosilicates in Luqa does not provide distinctive evidence for the presence of a previous standing body of water and is consistent with either impact emplacement or post-impact alteration. For Cankuzo, the phyllosilicate distribution provides evidence of a layer in the crater wall indicative of aqueous activity, but does not require a paleolake.

Shuttle Repair Tools Automate Vehicle Maintenance

NASA Technical Reports Server (NTRS)

2013-01-01

Successfully building, flying, and maintaining the space shuttles was an immensely complex job that required a high level of detailed, precise engineering. After each shuttle landed, it entered a maintenance, repair, and overhaul (MRO) phase. Each system was thoroughly checked and tested, and worn or damaged parts replaced, before the shuttle was rolled out for its next mission. During the MRO period, workers needed to record exactly what needed replacing and why, as well as follow precise guidelines and procedures in making their repairs. That meant traceability, and with it lots of paperwork. In 2007, the number of reports generated during electrical system repairs was getting out of hand-placing among the top three systems in terms of paperwork volume. Repair specialists at Kennedy Space Center were unhappy spending so much time at a desk and so little time actually working on the shuttle. "Engineers weren't spending their time doing technical work," says Joseph Schuh, an electrical engineer at Kennedy. "Instead, they were busy with repetitive, time-consuming processes that, while important in their own right, provided a low return on time invested." The strain of such inefficiency was bad enough that slow electrical repairs jeopardized rollout on several occasions. Knowing there had to be a way to streamline operations, Kennedy asked Martin Belson, a project manager with 30 years experience as an aerospace contractor, to co-lead a team in developing software that would reduce the effort required to document shuttle repairs. The result was System Maintenance Automated Repair Tasks (SMART) software. SMART is a tool for aggregating and applying information on every aspect of repairs, from procedures and instructions to a vehicle s troubleshooting history. Drawing on that data, SMART largely automates the processes of generating repair instructions and post-repair paperwork. In the case of the space shuttle, this meant that SMART had 30 years worth of operations that it could apply to ongoing maintenance work. According to Schuh, "SMART standardized and streamlined many shuttle repair processes, saving time and money while increasing safety and the quality of repairs." Maintenance technicians and engineers now had a tool that kept them in the field, and because SMART is capable of continually evolving, each time an engineer put it to use, it would enrich the Agency-wide knowledge base. "If an engineer sees something in the work environment that they could improve, a repair process or a procedure, SMART can incorporate that data for use in future operations," says Belson.

Reconnaissance Imaging Spectrometer for Mars CRISM Data Analysis

NASA Astrophysics Data System (ADS)

Frink, K.; Hayden, D.; Lecompte, D.

2009-05-01

The Compact Reconnaissance Imaging Spectrometer for Mars CRISM (CRISM) carried aboard the Mars Reconnaissance Orbiter (MRO), is the first visible-infrared spectrometer to fly on a NASA Mars mission. CRISM scientists are using the instrument to look for the residue of minerals that form in the presence of water: the 'fingerprints' left by evaporated hot springs, thermal vents, lakes or ponds. With unprecedented clarity, CRISM is mapping regions on the Martian surface at scales as small as 60 feet (about 18 meters) across, when the spacecraft is 186 miles (300 kilometers) above the planet. CRISM is reading 544 'colors' in reflected sunlight to detect certain minerals on the surface, including signature traces of past water. CRISM alone will generate more than 10 terabytes of data, enough to fill more than 15,000 compact discs. Given that quantity of data being returned by MRO-CRISM, this project partners with Johns Hopkins University (JHU) Applied Physics Laboratory (APL) scientists of the CRISM team to assist in the data analysis process. The CRISM operations team has prototyped and will provide the necessary software analysis tools. In addition, the CRISM operations team will provide reduced data volume representations of the data as PNG files, accessible via a web interface without recourse to specialized user tools. The web interface allows me to recommend repeating certain of the CRISM observations as survey results indicate, and to enter notes on the features present in the images. After analysis of a small percentage of CRISM observations, APL scientists concluded that their efforts would be greatly facilitated by adding a preliminary survey to evaluate the overall characteristics and quality of the CRISM data. The first-look should increase the efficiency and speed of their data analysis efforts. This project provides first-look assessments of the data quality while noting features of interest likely to need further study or additional CRISM observations. The project includes looking at CRISM images to determine if any were corrupted by transient environmental or instrumental perturbations or whether the Martian surface was obscured by haze, clouds, dust or dust storms preventing further study. In such cases, the project report will recommend conducting additional observations of a specific site. The project will also identify images containing interesting features that are candidates for more detailed investigation. For example, images of rock outcrops with evidence of water-containing minerals may be quickly recognized and marked for special treatment. In many cases, the project will be the first eyes on the data coming down from the spacecraft.

Initial results from radio occultation measurements with the Mars Reconnaissance Orbiter: A nocturnal mixed layer in the tropics and comparisons with polar profiles from the Mars Climate Sounder

NASA Astrophysics Data System (ADS)

Hinson, David P.; Asmar, Sami W.; Kahan, Daniel S.; Akopian, Varoujan; Haberle, Robert M.; Spiga, Aymeric; Schofield, John T.; Kleinböhl, Armin; Abdou, Wedad A.; Lewis, Stephen R.; Paik, Meegyeong; Maalouf, Sami G.

2014-11-01

The Mars Reconnaissance Orbiter (MRO) performs radio occultation (RO) measurements on selected orbits, generally once per day. We have retrieved atmospheric profiles from two subsets of data, yielding a variety of new results that illustrate the scientific value of the observations. One set of measurements sounded the tropics in northern summer at a local time ∼1 h before sunrise. Some of these profiles contain an unexpected layer of neutral stability with a depth of ∼4 km and a pressure at its upper boundary of ∼160 Pa. The mixed layer is bounded above by a temperature inversion and below by another strong inversion adjacent to the surface. This type of structure is observed near Gale Crater, in the Tharsis region, and at a few other locations, whereas profiles in Amazonis Planitia and Elysium Planitia show no sign of a detached mixed layer with an overlying inversion. We supplemented the measurements with numerical simulations by the NASA Ames Mars General Circulation Model, which demonstrate that water ice clouds can generate this distinctive type of temperature structure through their influence on radiative transfer at infrared wavelengths. In particular, the simulations predict the presence of a nocturnal cloud layer in the Tharsis region at a pressure of ∼150 Pa (∼10 km above the surface), and the nighttime radiative cooling at cloud level is sufficient to produce a temperature inversion above the cloud as well as convective instability below the cloud, consistent with the observations. The second set of measurements sounded mid-to-high northern latitudes in spring, when carefully coordinated observations by the MRO Mars Climate Sounder (MCS) are also available. The differences between the RO and MCS temperature profiles are generally consistent with the expected performance of the two instruments. Within this set of 21 comparisons the average temperature difference is less than 1 K where the aerosol opacities are smaller than 10-3km-1 , at pressures of 10-50 Pa, whereas it increases to ∼2 K where the aerosol opacities exceed this threshold, at pressures of 50-300 Pa. The standard deviation of the temperature difference is ∼2 K, independent of pressure. The second set of RO measurements also provides unique information about the stability of the annual CO2 cycle and the dynamics near the edge of the seasonal CO2 ice cap.

Atmospheric Science using CRISM EPF Sequences

NASA Astrophysics Data System (ADS)

Wolff, M. J.; Clancy, R. T.; Arvidson, R.; Smith, M. D.; Murchie, S. L.; McGuire, P. C.

2006-12-01

Near the end of September 2006, the MRO/CRISM (Compact Reconnaissance Imaging Spectrometer for Mars; Murchie et al., 2006, JGR, in press.) will acquire its first observations of Mars. MRO's Primary Science Phase beginning in early November. One of CRISM's investigations is characterization of seasonal variations in dust and ice aerosols and trace gases using a systematic, global grid of hyperspectral measurements of emission phase functions (EPFs) acquired repetitively throughout the Martian year. EPFs will also be obtained as part of each of approximately 5000 "targeted" observations of surface geologic features. EPF measurements allow accurate determination of column abundances of water vapor, CO, dust and ice aerosols, and their seasonal variations (e.g., Clancy et al., 2003, 108(E9), 5098). EPFs are measured using eleven superimposed images within which the slit field-of-view is swept across a target point on the Martian surface. When EPFs are taken as part of a global grid, 10x spatial pixel binning will be used in all of the images, providing data at 150-200 m/pixel. In the targeted observations, the central image will be obtained at either full resolution or with 2x binning (15-38 m/pixel). In all cases, hyperspectral data (545 wavelengths) will be taken during each of the 11 superimposed scans. There are two types of global EPF grids, one with better temporal sampling and one with better spatial sampling of the atmosphere. The "atmospheric monitoring campaign" consists one Martian day of pole-to-pole EPF's every ~9°\\ of solar longitude (Ls). There is sufficient time for 8 EPFs in an orbit, one approximately every 22°\\ of latitude. Alternate orbits (projected onto the planet) are offset in latitude by about 11°\\ north or south to increase latitudinal resolution. Longitude spacing between the orbits is about 27°. The "seasonal change campaign" occurs approximately every ~36°\\ of Ls. A grid similar to that executed during the atmospheric monitoring campaign is taken on 3 non-contiguous days over about 2 weeks, to provide a higher spatial density grid (longitude spacing about 10°) to monitor seasonal changes in surface material spectral properties, especially absorption and desorption of H2O. Every 3 orbits projected on the planet, the EPFs are offset by 0°, +8°, and -8°\\ north or south to increase latitudinal resolution. Our presentation will discuss several aspects of the atmospheric analyses (optical depths, radiative properties, radiative transfer methodology) to be performed using the early-mission EPFs, with the primary focus being those EPFs planned for the end of September.

HiRISE: The People's Camera

NASA Astrophysics Data System (ADS)

McEwen, A. S.; Eliason, E.; Gulick, V. C.; Spinoza, Y.; Beyer, R. A.; HiRISE Team

2010-12-01

The High Resolution Imaging Science Experiment (HiRISE) camera, orbiting Mars since 2006 on the Mars Reconnaissance Orbiter (MRO), has returned more than 17,000 large images with scales as small as 25 cm/pixel. From it’s beginning, the HiRISE team has followed “The People’s Camera” concept, with rapid release of useful images, explanations, and tools, and facilitating public image suggestions. The camera includes 14 CCDs, each read out into 2 data channels, so compressed images are returned from MRO as 28 long (up to 120,000 line) images that are 1024 pixels wide (or binned 2x2 to 512 pixels, etc.). This raw data is very difficult to use, especially for the public. At the HiRISE operations center the raw data are calibrated and processed into a series of B&W and color products, including browse images and JPEG2000-compressed images and tools to make it easy for everyone to explore these enormous images (see http://hirise.lpl.arizona.edu/). Automated pipelines do all of this processing, so we can keep up with the high data rate; images go directly to the format of the Planetary Data System (PDS). After students visually check each image product for errors, they are fully released just 1 month after receipt; captioned images (written by science team members) may be released sooner. These processed HiRISE images have been incorporated into tools such as Google Mars and World Wide Telescope for even greater accessibility. 51 Digital Terrain Models derived from HiRISE stereo pairs have been released, resulting in some spectacular flyover movies produced by members of the public and viewed up to 50,000 times according to YouTube. Public targeting began in 2007 via NASA Quest (http://marsoweb.nas.nasa.gov/HiRISE/quest/) and more than 200 images have been acquired, mostly by students and educators. At the beginning of 2010 we released HiWish (http://www.uahirise.org/hiwish/), opening HiRISE targeting to anyone in the world with Internet access, and already more than 100 public suggestions have been acquired. HiRISE has proven very popular with the public and science community. For example, a Google search on “HiRISE Mars” returns 626,000 results. We've participated in well over a two dozen presentations, specifically talking to middle and high-schoolers about HiRISE. Our images and captions have been featured in high-quality print magazines such as "National Geographic, Ciel et Espace, and Sky and Telescope.

An Avoidance Model for Short-Range Order Induced by Soft Repulsions in Systems of Rigid Rods

NASA Astrophysics Data System (ADS)

Han, Jining; Herzfeld, Judith

1996-03-01

The effects of soft repulsions on hard particle systems are calculated using an avoidance model which improves upon the simple mean field approximation. Avoidance reduces, but does not eliminate, the energy due to soft repulsions. On the other hand, it also reduces the configurational entropy. Under suitable conditions, this simple trade-off yields a free energy that is lower than the mean field value. In these cases, the variationally determined avoidance gives an estimate for the short-range positional order induced by soft repulsions. The results indicate little short-range order for isotropically oriented rods. However, for parallel rods, short-range order increases to significant levels as the particle axial ratio increases. The implications for long- range positional ordering are also discussed. In particular, avoidance may explain the smectic ordering of tobacco mosaic virus at volume fractions lower than those necessary for smectic ordering of hard particles.

Short range smectic order driving long range nematic order: Example of cuprates

DOE Office of Scientific and Technical Information (OSTI.GOV)

Markiewicz, R. S.; Lorenzana, J.; Seibold, G.

We present a model for describing the combined presence of nematic and ‘smectic’ or stripe-like orders seen in recent scanning tunneling microscopy (STM) experiments on cuprates. The smectic order is treated as an electronic charge density wave with an associated Peierls distortion or a ‘Pomeranchuk wave’. This primary order is restricted to nanoscale domains by disorder effects, while the secondary coupling to strain generates the nematic order with a considerably longer range. Lastly, a variety of experimental results are shown to be consistent with our theoretical predictions.

Short range smectic order driving long range nematic order: Example of cuprates

DOE PAGES

Markiewicz, R. S.; Lorenzana, J.; Seibold, G.; ...

2016-01-27

We present a model for describing the combined presence of nematic and ‘smectic’ or stripe-like orders seen in recent scanning tunneling microscopy (STM) experiments on cuprates. The smectic order is treated as an electronic charge density wave with an associated Peierls distortion or a ‘Pomeranchuk wave’. This primary order is restricted to nanoscale domains by disorder effects, while the secondary coupling to strain generates the nematic order with a considerably longer range. Lastly, a variety of experimental results are shown to be consistent with our theoretical predictions.

Magnetism and atomic short-range order in Ni-Rh alloys

NASA Astrophysics Data System (ADS)

Carnegie, D. W., Jr.; Claus, H.

1984-07-01

Low-field ac susceptibility measurements of Ni-Rh samples of various concentrations are presented. Giant effects of the metallurgical state on the magnetic ordering temperature are associated with changes in the degree of atomic short-range order. By careful control of this degree of short-range order, it is possible to demonstrate the existence of a spin-glass state in Ni-Rh alloys.

Research Center Renaming Will Honor Senator Domenici

NASA Astrophysics Data System (ADS)

2008-05-01

New Mexico Tech and the National Radio Astronomy Observatory (NRAO) will rename the observatory's research center on the New Mexico Tech campus to honor retiring U.S. Senator Pete V. Domenici in a ceremony on May 30. The building that serves as the scientific, technical, and administrative center for the Very Large Array (VLA) and Very Long Baseline Array (VLBA) radio telescopes will be named the "Pete V. Domenici Science Operations Center." The building previously was known simply as the "Array Operations Center." Sen. Pete V. Domenici Sen. Pete V. Domenici "The new name recognizes the strong and effective support for science that has been a hallmark of Senator Domenici's long career in public service," said Dr. Fred Lo, NRAO Director. New Mexico Tech President Daniel H. Lopez said Sen. Domenici has always been a supporter of science and research in Socorro and throughout the state. "He's been a statesman for New Mexico, the nation -- and without exaggeration -- for the world," Lopez said. "Anyone with that track record deserves this recognition." Van Romero, Tech vice president of research and economic development, has served as the university's main lobbyist in Washington, D.C., for more than a decade. He said Sen. Domenici has always been receptive to new ideas and willing to take risks. "Over the years, Sen. Domenici has always had time to listen to our needs and goals," Romero said. "He has served as a champion of New Mexico Tech's causes and we owe him a debt of gratitude for all his efforts over the decades." Originally dedicated in 1988, the center houses offices and laboratories that support VLA and VLBA operations. The center also supports work on the VLA modernization project and on the international Atacama Large Millimeter/submillimeter Array (ALMA) project. Work on ALMA at the Socorro center and at the ALMA Test Facility at the VLA site west of Socorro has focused on developing and testing equipment to be deployed at the ALMA site in Chile's Atacama Desert. The research facility, part of the National Science Foundation-funded NRAO, was located on the NM Tech campus through a joint Federal-State effort spearheaded by Domenici. "Senator Domenici has worked hard over the years to support research both at New Mexico Tech and at the NRAO, and our facility on the New Mexico Tech campus is a symbol of that support. It's highly appropriate to name it after him," said Dr. Ethan Schreier, President of Associated Universities Inc., which operates the NRAO for the National Science Foundation. Senator Domenici helped make New Mexico Tech's Magdalena Ridge Observatory (MRO) a reality and provided essential support for NRAO's VLA and VLBA. MRO is one of the world's most technologically-advanced optical observatories. The VLA is the most scientifically-productive ground-based telescope in the history of astronomy. "Both these facilities will advance the frontiers of 21st-Century astrophysics, and keep our state and its research community in the forefront of science worldwide," said Dr. Robert Dickman, NRAO's Director for New Mexico Operations. Domenici also was instrumental in bringing the International Law Enforcement Academy -- another New Mexico Tech division -- to Roswell. During the Reagan Administration, Domenici sponsored the legislation that allowed the university to use the "M" Mountain range for research and testing. Lopez said the U.S. Department of the Interior would not let the university conduct testing on the range. A high level bureaucrat told Laurence Lattman, then the president of Tech, that it "would take an act of Congress" for Tech to have unlimited access to the land. Domenici sponsored the legislation -- signed by Reagan -- that gave Tech access to the land. Over the years, Domenici's support has helped Tech launch the homeland security training program in Playas, the EarthScope research and other anti-terrorism training programs. "All these projects benefit New Mexico Tech," Lopez said. "But these programs also benefit the nation. Senator Domenici has always been careful to make sure that federal money went to programs that benefit the entire nation." The National Radio Astronomy Observatory is a facility of the National Science Foundation, operated under cooperative agreement by Associated Universities, Inc.

Buried CO2 Ice traces in South Polar Layered Deposits of Mars detected by radar sounder

NASA Astrophysics Data System (ADS)

Castaldo, L.; Mège, D.; Orosei, R.; Séjourné, A.

2014-12-01

SHARAD (SHAllow RADar) is the subsurface sounding radar provided by the Italian Space Agency (ASI) as a facility instrument to NASA's 2005 Mars Reconnaissance Orbiter (MRO). The Reduced Data Record of SHARAD data covering the area of the South Polar Layered Deposits (SPLD), has been used. The elaboration and interpretation of the data, aimed to estimate electromagnetic properties of surface layers, has been performed in terms of permittivity. The theory of electromagnetic scattering from fractal surfaces, and the estimation of geometric parameters from topographic data by Mars Orbiter Laser Altimeter (MOLA) which was one of five instruments on board the Mars Global Surveyor (MGS) spacecraft, has been used. A deep analysis of inversion has been made on all Mars and extended to the South Polar Caps in order to extract the area with a permittivity constant of CO2 ice. Several corrections have been applied to the data, moreover the calibration of the signal requires the determination of a constant that takes into account the power gain due to the radar system and the surface in order to compensate the power losses due to the orbitographic phenomena. The determination of regions with high probability of buried CO2 ice in the first layer of the Martian surface, is obtained extracting the real part of the permittivity constant of the CO2 ice (~2), estimated by other means. The permittivity of CO2ice is extracted from the Global Permittivity Map of Mars using the global standard deviation of itself as following: ɛCO2ice=ɛCO2ice+ Σ (1)where Σ=±std(ɛMapMars)/2Figure 1(a) shows the south polar areas where the values of the permittivity point to the possibility of a CO2 ice layer. Figure 1(b) is the corresponding geologic map. The comparison between the two maps indicates that the area with probable buried CO2 overlaps Hesperian and Amazonian polar units (Hp, Hesperian plains-forming deposits marked by narrow sinuous, anabranching ridges and irregular depressions, and Apu, Amazonian layered plateaus). From this analysis, the south polar cap could be covered by a thin frozen carbon dioxide coating. The perennial south polar cap is probably made of frozen carbon dioxide ca. 8 meters thick.