7 CFR 318.13-16 - Regulated articles allowed interstate movement subject to specified conditions.

Code of Federal Regulations, 2013 CFR

2013-01-01

...(s) Additionalrequirements Hawaii Bananas 1 Musa spp Fruit (b)(1)(i), (b)(2)(ii) Litchi Litchi..., johnny-jump-ups, pansies, and violets Calendula spp Flower (b)(2)(iii) Pineapple 2 Ananas comosus Fruit... escuelentus Fruit (b)(3)(i) Pot marigold, johnny-jump-ups, pansies, and violets Calendula spp Flower (b)(2...

7 CFR 318.13-16 - Regulated articles allowed interstate movement subject to specified conditions.

Code of Federal Regulations, 2011 CFR

2011-01-01

...(s) Additionalrequirements Hawaii Bananas 1 Musa spp Fruit (b)(1)(i), (b)(2)(ii) Litchi Litchi..., johnny-jump-ups, pansies, and violets Calendula spp Flower (b)(2)(iii) Pineapple 2 Ananas comosus Fruit... escuelentus Fruit (b)(3)(i) Pot marigold, johnny-jump-ups, pansies, and violets Calendula spp Flower (b)(2...

7 CFR 318.13-16 - Regulated articles allowed interstate movement subject to specified conditions.

Code of Federal Regulations, 2014 CFR

2014-01-01

...(s) Additionalrequirements Hawaii Bananas 1 Musa spp Fruit (b)(1)(i), (b)(2)(ii) Litchi Litchi..., johnny-jump-ups, pansies, and violets Calendula spp Flower (b)(2)(iii) Pineapple 2 Ananas comosus Fruit... escuelentus Fruit (b)(3)(i) Pot marigold, johnny-jump-ups, pansies, and violets Calendula spp Flower (b)(2...

The Search for Meaning: How You Can Boost Kids' Reading Comprehension

ERIC Educational Resources Information Center

Grimes, Sharon

2004-01-01

A few years ago, most of the students at Lansdowne Elementary were struggling readers: while many could recognize words, half were unable to under stand the stories they'd just read. Not surprisingly, these kids weren't interested in books. The problem wasn't Why Johnnie Can't Read, but more specifically, Why Johnnie Can't Understand--and the…

"To See through Johnny and to See Johnny Through": The Guidance Movement in Interwar Australia

ERIC Educational Resources Information Center

Wright, Katie

2012-01-01

In the late 1920s and early 1930s, the guidance movement secured a foothold in the Australian educational landscape. Educators and psychologists looked to new initiatives in Britain and America in the hope that guidance programmes would provide solutions to a range of social, economic and educational problems: vocational guidance to help young…

7 CFR 318.13-16 - Regulated articles allowed interstate movement subject to specified conditions.

Code of Federal Regulations, 2010 CFR

2010-01-01

...(s) Additionalrequirements Hawaii Bananas 1 Musa spp Fruit (b)(1)(i), (b)(2)(ii) Pot marigold, johnny-jump-ups, pansies, and violets Calendula spp Flower (b)(2)(iii) Pineapple 2 Ananas comosus Fruit (b)(2... Fruit (b)(3)(i) Pot marigold, johnny-jump-ups, pansies, and violets Calendula spp Flower (b)(2)(iii) U.S...

Carbon associated nitrate (CAN) in the Ediacaran Johnnie Formation, Death Valley, California and links to the Shuram negative carbon isotope excursion

NASA Astrophysics Data System (ADS)

Dilles, Z. Y. G.; Prokopenko, M. G.; Bergmann, K.; Loyd, S. J.; Corsetti, F. A.; Berelson, W.; Gaines, R. R.

2014-12-01

Nitrogen, a major nutrient of marine primary production whose many redox states are linked through biological processes to O2, may afford better understanding of changes in post-Great Oxidation Event (GOE) environmental redox conditions. Using a novel approach to quantify nitrate content in carbonates, we identified a trend of CAN increase in the late-Proterozoic, including several distinct peaks within a carbonate succession of the Sonora province, Mexico, deposited ~630-500 Ma. The goal of the current study was to investigate CAN variability in the context of the global "Shuram" event, a large negative δ13C excursion expressed in Rainstorm member carbonates of the Johnnie Formation in Death Valley, CA. The lower Rainstorm Member "Johnnie Oolite", a time-transgressive, regionally extensive, shallow dolomitic oolite, was sampled. CAN concentrations ranged from 7.31 to 127.36 nmol/g, with higher values measured toward the base of the bed. This trend held at each sampled locality, along with a tendency towards decreasing CAN with larger magnitude negative δ13C excursions. Modern analog ooids formed in low-latitude marine environments lack CAN, consistent with their formation in low-nitrate waters of the euphotic zone characteristic of the modern ocean nitrogen cycling. In contrast, maximum values within the Johnnie oolite exceed by a factor of five to seven CAN measured in carbonates deposited below the main nitracline in the modern ocean, implying high nitrate content within shallow depositional environments. Johnnie oolite data, broadly consistent with the Sonora sequence findings, may indicate large perturbations in the Ediacaran nitrogen cycle immediately preceding the negative δ13C excursion. The implication of these findings for possible changes in the Ediacaran nitrogen, oxygen and carbon biogeochemical cycling will be further discussed.

Changing Course: Thurgood Marshall College Fund President Johnny Taylor Seeks New Partnerships and Avenues of Support for Public HBCUs

ERIC Educational Resources Information Center

Stuart, Reginald

2011-01-01

When veteran educator Dr. N. Joyce Payne handed the reins of the organization she founded, the Thurgood Marshall College Fund, to entertainment lawyer and board member Johnny Taylor, Taylor began pursuing a remake of the prestigious group that has turned it on its head in just a matter of months. Today, with just more than a year of leading the…

KENNEDY SPACE CENTER, FLA. - At the rollout of the One NASA initiative at KSC, Glenn Research Center Director Dr. Julian Earls embraces implementation team lead Johnny Stevenson while KSC Director Jim Kennedy (left) applauds. Earls gave a motivational speech during the luncheon held at the Visitor Complex Debus Conference Center. The event was held at the IMAX Theater® where NASA leaders discussed One NASA with selected employees. Explaining how their respective centers contribute to One NASA, along with Kennedy and Earls, were James Jennings, NASA’s associate deputy administrator for institutions and asset management; Ed Weiler, associate administrator for Space Science; Kevin Peterson, Dryden Flight Research Center director; incoming KSC Deputy Director Woodrow Whitlow; and implementation team lead Johnny Stevenson.

NASA Image and Video Library

2003-08-20

KENNEDY SPACE CENTER, FLA. - At the rollout of the One NASA initiative at KSC, Glenn Research Center Director Dr. Julian Earls embraces implementation team lead Johnny Stevenson while KSC Director Jim Kennedy (left) applauds. Earls gave a motivational speech during the luncheon held at the Visitor Complex Debus Conference Center. The event was held at the IMAX Theater® where NASA leaders discussed One NASA with selected employees. Explaining how their respective centers contribute to One NASA, along with Kennedy and Earls, were James Jennings, NASA’s associate deputy administrator for institutions and asset management; Ed Weiler, associate administrator for Space Science; Kevin Peterson, Dryden Flight Research Center director; incoming KSC Deputy Director Woodrow Whitlow; and implementation team lead Johnny Stevenson.

Warmed Winter Water Temperatures Alter Reproduction in Two Fish Species

NASA Astrophysics Data System (ADS)

Firkus, Tyler; Rahel, Frank J.; Bergman, Harold L.; Cherrington, Brian D.

2018-02-01

We examined the spawning success of Fathead Minnows ( Pimephales promelas) and Johnny Darters ( Etheostoma nigrum) exposed to elevated winter water temperatures typical of streams characterized by anthropogenic thermal inputs. When Fathead Minnows were exposed to temperature treatments of 12, 16, or 20 °C during the winter, spawning occurred at 16 and 20 °C but not 12 °C. Eggs were deposited over 9 weeks before winter spawning ceased. Fathead Minnows from the three winter temperature treatments were then exposed to a simulated spring transition. Spawning occurred at all three temperature treatments during the spring, but fish from the 16° and 20 °C treatment had delayed egg production indicating a latent effect of warm winter temperatures on spring spawning. mRNA analysis of the egg yolk protein vitellogenin showed elevated expression in female Fathead Minnows at 16 and 20 °C during winter spawning that decreased after winter spawning ceased, whereas Fathead Minnows at 12 °C maintained comparatively low expression during winter. Johnny Darters were exposed to 4 °C to represent winter temperatures in the absence of thermal inputs, and 12, 16, and 20 °C to represent varying degrees of winter thermal pollution. Johnny Darters spawned during winter at 12, 16, and 20 °C but not at 4 °C. Johnny Darters at 4 °C subsequently spawned following a simulated spring period while those at 12, 16, and 20 °C did not. Our results indicate elevated winter water temperatures common in effluent-dominated streams can promote out-of-season spawning and that vitellogenin expression is a useful indicator of spawning readiness for fish exposed to elevated winter temperatures.

Warmed Winter Water Temperatures Alter Reproduction in Two Fish Species.

PubMed

Firkus, Tyler; Rahel, Frank J; Bergman, Harold L; Cherrington, Brian D

2018-02-01

We examined the spawning success of Fathead Minnows (Pimephales promelas) and Johnny Darters (Etheostoma nigrum) exposed to elevated winter water temperatures typical of streams characterized by anthropogenic thermal inputs. When Fathead Minnows were exposed to temperature treatments of 12, 16, or 20 °C during the winter, spawning occurred at 16 and 20 °C but not 12 °C. Eggs were deposited over 9 weeks before winter spawning ceased. Fathead Minnows from the three winter temperature treatments were then exposed to a simulated spring transition. Spawning occurred at all three temperature treatments during the spring, but fish from the 16° and 20 °C treatment had delayed egg production indicating a latent effect of warm winter temperatures on spring spawning. mRNA analysis of the egg yolk protein vitellogenin showed elevated expression in female Fathead Minnows at 16 and 20 °C during winter spawning that decreased after winter spawning ceased, whereas Fathead Minnows at 12 °C maintained comparatively low expression during winter. Johnny Darters were exposed to 4 °C to represent winter temperatures in the absence of thermal inputs, and 12, 16, and 20 °C to represent varying degrees of winter thermal pollution. Johnny Darters spawned during winter at 12, 16, and 20 °C but not at 4 °C. Johnny Darters at 4 °C subsequently spawned following a simulated spring period while those at 12, 16, and 20 °C did not. Our results indicate elevated winter water temperatures common in effluent-dominated streams can promote out-of-season spawning and that vitellogenin expression is a useful indicator of spawning readiness for fish exposed to elevated winter temperatures.

Why Johnny Can't in: Sex Education

ERIC Educational Resources Information Center

Thompson, A. Gray

1971-01-01

Sex education in the schools is predicted to be the major educational issue in the 70's. It is concluded that total community involvement will eventually immobilize its politico-religious critics. (CP)

"Dear Teacher, Johnny Copied."

ERIC Educational Resources Information Center

Jackson, Louise A.; And Others

1987-01-01

Presents the problem of intentional or unintentional plagiarism on the part of young students, several possible causes for it, and offers ways teachers can help students avoid copying and understand the value of owning one's writing. (JC)

75 FR 13653 - Qualification of Drivers; Exemption Applications; Vision

Federal Register 2010, 2011, 2012, 2013, 2014

2010-03-22

... D. Bennett, Johnny W. Bradford Sr., Levi A. Brown, Charlie F. Cook, Clifford H. Dovel, Arthur L..., Steven L. Valley, Thomas E. Voyles, Jr., Darel G. Wagner, Bernard J. Wood. These exemptions are extended...

Television and Social Problems: A Case History.

ERIC Educational Resources Information Center

Willis, John

1978-01-01

Discusses two documentary television movies, "Johnny Go Home" and "Goodbye Longfellow Road," in terms of their resultant social change. Includes consideration of audience, time shown, and previous attitudes to provide evidence for his argument. (JEG)

Self-replicating machines in continuous space with virtual physics.

PubMed

Smith, Arnold; Turney, Peter; Ewaschuk, Robert

2003-01-01

JohnnyVon is an implementation of self-replicating machines in continuous two-dimensional space. Two types of particles drift about in a virtual liquid. The particles are automata with discrete internal states but continuous external relationships. Their internal states are governed by finite state machines, but their external relationships are governed by a simulated physics that includes Brownian motion, viscosity, and springlike attractive and repulsive forces. The particles can be assembled into patterns that can encode arbitrary strings of bits. We demonstrate that, if an arbitrary seed pattern is put in a soup of separate individual particles, the pattern will replicate by assembling the individual particles into copies of itself. We also show that, given sufficient time, a soup of separate individual particles will eventually spontaneously form self-replicating patterns. We discuss the implications of JohnnyVon for research in nanotechnology, theoretical biology, and artificial life.

Corrective Action Decision Document/Closure Report for Corrective Action Unit 374: Area 20 Schooner Unit Crater, Nevada National Security Site, Nevada with ROTC 1 and 2, Revision 0

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

Matthews, Patrick

Corrective Action Unit 374 comprises five corrective action sites (CASs): • 18-22-05, Drum • 18-22-06, Drums (20) • 18-22-08, Drum • 18-23-01, Danny Boy Contamination Area • 20-45-03, U-20u Crater (Schooner) The purpose of this Corrective Action Decision Document/Closure Report is to provide justification and documentation supporting the recommendation that no further corrective action is needed for CAU 374 based on the implementation of corrective actions. The corrective action of closure in place with administrative controls was implemented at CASs 18-23-01 and 20-45-03, and a corrective action of removing potential source material (PSM) was conducted at CAS 20-45-03. The othermore » CASs require no further action; however, best management practices of removing PSM and drums at CAS 18-22-06, and removing drums at CAS 18-22-08 were performed. Corrective action investigation (CAI) activities were performed from May 4 through October 6, 2010, as set forth in the Corrective Action Investigation Plan for Corrective Action Unit 374: Area 20 Schooner Unit Crater, Nevada Test Site, Nevada. The approach for the CAI was divided into two facets: investigating the primary release of radionuclides and investigating other releases (migration in washes and chemical releases). The purpose of the CAI was to fulfill data needs as defined during the data quality objective (DQO) process. The CAU 374 dataset of investigation results was evaluated based on the data quality indicator parameters. This evaluation demonstrated the dataset is acceptable for use in fulfilling the DQO data needs. Analytes detected during the CAI were evaluated against final action levels (FALs) established in this document. Radiological doses exceeding the FAL of 25 millirem per year were found to be present in the surface soil that was sampled. It is assumed that radionuclide levels present in subsurface media within the craters and ejecta fields (default contamination boundaries) at the Danny Boy and Schooner sites exceed the FAL. It is also assumed that PSM in the form of lead-acid batteries at Schooner exceeds the FAL. Therefore, corrective actions were undertaken that consist of removing PSM, where present, and implementing a use restriction and posting warning signs at the Danny Boy and Schooner sites. These use restrictions were recorded in the FFACO database; the U.S. Department of Energy, National Nuclear Security Administration Nevada Site Office (NNSA/NSO) Facility Information Management System; and the NNSA/NSO CAU/CAS files. Therefore, NNSA/NSO provides the following recommendations: • No further corrective actions are necessary for CAU 374. • A Notice of Completion to NNSA/NSO is requested from the Nevada Division of Environmental Protection for closure of CAU 374. • Corrective Action Unit 374 should be moved from Appendix III to Appendix IV of the FFACO.« less

Why Johnny Can Read...But Doesn't

ERIC Educational Resources Information Center

Landy, Sarah

1977-01-01

The article analyzes characteristics of readers vs. non-readers and environmental factors which influence reading patterns among Grade VII (age 12-13) students. The study is based on 573 students and includes data on frequency of reading and book subject preferences. (JAB)

Will Johnny See Daddy This Week?

ERIC Educational Resources Information Center

Stephens, Linda S.

1996-01-01

Examines the determinants of postdivorce contact between nonresidential fathers and their children after martial disruption and to evaluate the relative merit of three sociological perspectives on postdivorce contact: social parenting, marital-involvement parenting, and socioeconomic-advantaged parenting. Results suggest that fathers have limited…

Twentieth Century Books Influencing American Education

ERIC Educational Resources Information Center

McCaul, Robert L.

1977-01-01

Discusses: "Educational Psychology," Thorndike; "Medical Education," Flexner; "Democracy and Education," Dewey; "The Measurement of Intelligence," Terman; "Public Education," Cubberley; "The Thirty-Ninth Yearbook of the National Society for the Study of Education, Intelligence: Its Nature and Nurture;" and, "Why Johnny Can't Read," Flesch. (JM)

77 FR 15122 - Te-Moak Tribe of Western Shoshone- Ordinance Pursuant to United States Code, Legalizing and...

Federal Register 2010, 2011, 2012, 2013, 2014

2012-03-14

... alcoholic beverage business is seeking to be licensed. (e) No such license shall be transferred without the..., Chairman, Te-Moak Tribe of Western Shoshone ATTEST: /s/ Vera Johnny, Acting Recording Secretary Te-Moak...

Education Matters, April 2007

ERIC Educational Resources Information Center

Beckner, Gary, Ed.

2007-01-01

"Education Matters" is the monthly newsletter of the Association of American Educators (AAE), an organization dedicated to advancing the American teaching profession through personal growth, professional development, teacher advocacy and protection. This issue of the newsletter includes: (1) Johnny Can Write...If We Challenge Him (Bill…

Evidence for Mojave-Sonora megashear-Systematic left-lateral offset of Neoproterozoic to Lower Jurassic strata and facies, western United States and northwestern Mexico

USGS Publications Warehouse

Stewart, John H.

2005-01-01

Major successions as well as individual units of Neoproterozoic to Lower Jurassic strata and facies appear to be systematically offset left laterally from eastern California and western Nevada in the western United States to Sonora, Mexico. This pattern is most evident in units such as the "Johnnie oolite," a 1- to 2-m-thick oolite of the Neoproterozoic Rainstorm Member of the Johnnie Formation in the western United States and of the Clemente Formation in Sonora. The pattern is also evident in the Lower Cambrian Zabriskie Quartzite of the western United States and the correlative Proveedora Quartzite in Sonora. Matching of isopach lines of the Zabriskie Quartzite and Proveedora Quartzite suggests ???700-800 km of left-lateral offset. The offset pattern is also apparent in the distribution of distinctive lithologic types, unconformities, and fossil assemblages in other rocks ranging in age from Neoproterozoic to Early Jurassic. In the western United States, the distribution of facies in Neoproterozoic and Paleozoic strata indicates that the Cordilleran miogeocline trends north-south. A north-south trend is also suggested in Sonora, and if so is compatible with offset of the miogeocline but not with the ideas that the miogeocline wrapped around the continental margin and trends east-west in Sonora. An imperfect stratigraphic match of supposed offset segments along the megashear is apparent. Some units, such as the "Johnnie oolite" and Zabriskie-Proveedora, show almost perfect correspondence, but other units are significantly different. The differences seem to indicate that the indigenous succession of the western United States and offset segments in Mexico were not precisely side by side before offset but were separated by an area-now buried, eroded, or destroyed-that contained strata of intermediate facies. ?? 2005 Geological Society of America.

Operational Audit Model for a Small Not-for-Profit Organization.

DTIC Science & Technology

1980-06-01

is projected to lose only il0. Presently, they grow kiwi fruit, raspberries, olallieberries, asparagus, banana squash, acorn squash and zucchini...California 93940 0. LT Johnnie Johnson III 2 Procurement Division NTaval Supply Center Oakland, California 94617 7. Henry Flowers 2 Seventh Day

KENNEDY SPACE CENTER, FLA. - NASA leaders discuss the Agency’s One NASA initiative with selected employees at the KSC Visitor Complex IMAX Theater®. From left are KSC Director Jim Kennedy; James Jennings, NASA’s associate deputy administrator for institutions and asset management; Ed Weiler, associate administrator for Space Science; Kevin Peterson, Dryden Flight Research Center director; incoming KSC Deputy Director Woodrow Whitlow; and implementation team lead Johnny Stevenson. Glenn Research Center Director Dr. Julian Earls gave a motivational speech during the luncheon held at the Visitor Complex Debus Conference Center.

NASA Image and Video Library

2003-08-20

KENNEDY SPACE CENTER, FLA. - NASA leaders discuss the Agency’s One NASA initiative with selected employees at the KSC Visitor Complex IMAX Theater®. From left are KSC Director Jim Kennedy; James Jennings, NASA’s associate deputy administrator for institutions and asset management; Ed Weiler, associate administrator for Space Science; Kevin Peterson, Dryden Flight Research Center director; incoming KSC Deputy Director Woodrow Whitlow; and implementation team lead Johnny Stevenson. Glenn Research Center Director Dr. Julian Earls gave a motivational speech during the luncheon held at the Visitor Complex Debus Conference Center.

Operations NOUGAT and WHETSTONE Events: HARD HAT, DANNY BOY, MARSHMALLOW, MUDPACK, WISHBONE, GUMDROP, DILUTED WATERS, and TINY TOT, 15 February 1962-17 June 1965.

DTIC Science & Technology

1984-01-31

were conducted to study weapons effects from 15 February 1962 to 17 June 1965. ,Four were shaft-type, three were tunnel- type, and one was a crater...Of the 194 nuclear device tests conducted, 161 were for weapons development or effects purposes, and 33 were safety ex- periments. An additional 22...testing on 25 April 1962 until the last atmospheric test on 4 November 1962, 40 weapons development and weapons effects tests were conducted as part of the

Schools for Cities: Urban Strategies. NEA Series on Design.

ERIC Educational Resources Information Center

Haar, Sharon, Ed.

This monograph presents papers from the 2000 Mayors' Institute on City Design and the public forum that followed it. Essays include: "Schools for Cities: Urban Strategies" (Sharon Haar); "Reenvisioning Schools; The Mayors' Questions" (Leah Ray); "Why Johnny Can't Walk to School" (Constance E. Beaumont); "Lessons…

Qualitative Data Analysis: A Methods Sourcebook. Third Edition

ERIC Educational Resources Information Center

Miles, Matthew B.; Huberman, A. Michael; Saldana, Johnny

2014-01-01

The Third Edition of Miles & Huberman's classic research methods text is updated and streamlined by Johnny Saldaña, author of "The Coding Manual for Qualitative Researchers." Several of the data display strategies from previous editions are now presented in re-envisioned and reorganized formats to enhance reader accessibility and…

76 FR 6142 - Agency Information Collection Activities; Submission for Office of Management and Budget Review...

Federal Register 2010, 2011, 2012, 2013, 2014

2011-02-03

... DEPARTMENT OF HEALTH AND HUMAN SERVICES Food and Drug Administration [Docket No. FDA-2010-N-0598... Drug Administration, HHS. ACTION: Notice. SUMMARY: The Food and Drug Administration (FDA) is announcing... CONTACT: Johnny Vilela, Office of Information Management, Food and Drug Administration, 1350 Piccard Dr...

Norm Abram of 'This Old House' visits KSC to film for show

NASA Technical Reports Server (NTRS)

2000-01-01

Steve Thomas (left) and Norm Abram (second from left), who are seen in the television series This Old House, talk with astronaut John Herrington (right). In the background is Johnny Johnson, media escort. Abram is at KSC to film an episode of This Old House.

Literature for Children and Adolescents.

ERIC Educational Resources Information Center

Matthews, Dorothy, Ed.

1978-01-01

The 11 articles in this publication discuss many topics regarding literature for children and adolescents, including the following: the major problems facing teachers and writers alike as they strive to communicate with the young; E.B. White's "Charlotte's Web"; two views of the American Revolution found in "Johnny Tremain" and "My Brother Sam Is…

Aliteracy: What Teachers Can Do to Keep Johnny Reading.

ERIC Educational Resources Information Center

Decker, Barbara Cooper

Aliteracy, the ability to read but the unwillingness to do so, is a growing problem in American society. Aliteracy crosses all socioeconomic levels, thereby allowing autocratic, charismatic leaders to influence thinking and decision-making. Social changes that have contributed to the problem of aliteracy include the influence of television on…

Why Johnny Can Be Average Today.

ERIC Educational Resources Information Center

Sturrock, Alan

1997-01-01

During a (hypothetical) phone interview with a university researcher, an elementary principal reminisced about a lifetime of reading groups with unmemorable names, medium-paced math problems, patchworked social studies/science lessons, and totally "average" IQ and batting scores. The researcher hung up at the mention of bell-curved assembly lines…

Johnny Can Write: Identifying the Epistemological Language of Undergraduate Writers

ERIC Educational Resources Information Center

Frye, Matthew Jay

2017-01-01

This dissertation examines the epistemological moves made by Washington State University undergraduates in their general education course writing and during two impromptu writing assessment exams administered by the WSU writing program. It builds from previous interview-based research on epistemological change (Perry, 1998; diSessa, 1993;…

How Johnny/Jane Writes: The Complex Word.

ERIC Educational Resources Information Center

Keller, Rodney D.

The process of getting a thought out of the mind and onto paper can be divided into five major categories: (1) discovering the word, (2) excavating the mythic word from the subconscious, (3) perceiving the word in the conscious, (4) verbalizing the expressed word, and (5) comprehending the unsaid word. When humans experience anything, their minds…

Freedom Road: Colonial Life

ERIC Educational Resources Information Center

Auerbach, Barbara

2010-01-01

While historical fiction by Jean Fritz as well as titles like Robert Lawson's "Ben and Me" (1939) or "Mr. Revere and I" (1954) and Esther Forbes's "Johnny Tremain" (1943) are widely known classics that bring this period to life, recent years have yielded a wealth of new offerings--many of which are accessible picture books or read-alouds. These…

To Click or Not to Click: That's the Question

ERIC Educational Resources Information Center

El-Rady, Johnny

2006-01-01

Classes of 100 students or more are not uncommon in higher education. With such large enrollments, it can be difficult for instructors to integrate active learning components to the traditional lecture format typically adopted in such large classes. To help address this problem, Johnny El-Rady discusses his use of an electronic classroom voting…

The Myth that College and Major Choice Decides Johnny's Future

ERIC Educational Resources Information Center

Dietz, Janis

2010-01-01

Though the importance of college is well recognized (Heckert & Wallace, 1998; Arney, Hardeback, Estrada & Permenter, 2006), there continues to be debate about whether a specific major or choice of college affects a person's future success as measured by position and/or compensation. As college costs have risen faster than income (Anonymous,…

Special Issue: Veterans in Higher Education--When Johnny and Jane Come Marching to Campus

ERIC Educational Resources Information Center

DiRamio, David; Jarvis, Kathryn

2011-01-01

This volume is intended to provide useful information about students with military experience who are attending college by blending the theoretical, practical, and empirical. The chapters contain theories, frameworks, facts, and ideas for consideration when approaching the subject of the newest generation of college students who have experienced…

Social Development of the Young Child: Why Can't Johnny Share?

ERIC Educational Resources Information Center

Bingham, B. Yvonne

There is growing concern that early childhood educators are not giving adequate attention to promoting their students' social development. This paper discusses the social developmental needs of young children, the importance of early intervention, and possible ways that early childhood educators can nurture healthy social skills through the school…

Why Can't Johnny Read? The Abell Report. Volume 23, No.7

ERIC Educational Resources Information Center

Jacobson, Joan

2010-01-01

Baltimore's school-based vision-screening program may be leaving thousands of children with uncorrected eyesight problems. Vision screening in public schools is essential for students to learn, especially when low-income children face a high rate of eyesight problems and have poor access to health care. Left undetected and uncorrected, vision…

Norm Abram of 'This Old House' visits KSC to film for show

NASA Technical Reports Server (NTRS)

2000-01-01

Astronaut John Herrington (right) shares a humorous moment with Steve Thomas (left) and Norm Abram (second from left), who are seen in the television series This Old House. In the background is Johnny Johnson, media escort. Abram is at KSC to film an episode of This Old House.

What Johnny Shouldn't Read: Textbook Censorship in America.

ERIC Educational Resources Information Center

DelFattore, Joan

This book discusses ways in which special-interest groups influence the content of textbooks used in public and private schools throughout the United States. The book focuses on recent federal lawsuits involving attempts to censor or ban reading, literature, science, and social studies textbooks. Recreating the story behind each lawsuit, the book…

What Johnny Can't Write: A University View of Freshman Writing Ability.

ERIC Educational Resources Information Center

Newkirk, Thomas R.; And Others

It is regularly claimed that the quality of writing done by college freshmen is declining. This study attempted, through the use of questionnaires and interviews, to determine what specific freshman writing problems English teaching assistants and English professors at the University of Texas viewed as most serious. Questionnaire results showed…

75 FR 73103 - Agency Information Collection Activities; Proposed Collection; Comment Request; Animal Drug User...

Federal Register 2010, 2011, 2012, 2013, 2014

2010-11-29

... are required to publish notice in the Federal Register concerning each proposed collection of... for public comment in response to the notice. This notice solicits comments on burden hours necessary... docket number found in brackets in the heading of this document. FOR FURTHER INFORMATION CONTACT: Johnny...

What Johnny Can't Read: "First Amendment Rights" in the Classroom.

ERIC Educational Resources Information Center

Orleans, Jeffrey H.

1981-01-01

Representative, delegated school governance by elected officials intrinsically vests curricular control in those officials. Because their offices are created so that the schools may be governed, they have authority to govern the schools--even especially--in the delicate and critical areas of deciding how and what the schools shall teach.…

Johnny Horizon Environmental Test Kit.

ERIC Educational Resources Information Center

Bentley, Richard; Bentley, William

Derived from tests presently used by state and federal agencies involved with pollution detection, this Environmental Test Kit contains materials and instructions for ten experiments. Each experiment is designed to test a different aspect of air and water, to find out whether or not the air and water in the tester's immediate area has been…

Jane and Johnny Love Math: Recognizing and Encouraging Mathematical Talent in Elementary Students; A Guidebook for Educators and Parents.

ERIC Educational Resources Information Center

Lupkowski, Ann E.; Assouline, Susan G.

This book is a guide for parents and teachers of mathematically talented elementary school students. Chapters and sections include: (1) "Overview"; (2) "Historical and Current Perspectives"; (3) "Making Informed Educational Decisions"; (4) "Diagnostic Testing Followed by Prescriptive Instruction: SMPY's DT to PI…

What Johnny Likes to Read Is Hard To Find in School.

ERIC Educational Resources Information Center

Worthy, Jo; Moorman, Megan; Turner, Margo

1999-01-01

Investigates reading preferences of an ethnically and economically diverse group of sixth-grade students from three middle schools. Shows that light materials (scary series books, comics, and magazines) top the list for every sub-group of students. Finds very limited availability of preferred materials in school; and shows that most students…

Grease Cowboy Fever; or, the making of Johnny T.

PubMed

Bradford, K

2002-01-01

Through a mix of theory, memoir and performance narrative, this chapter examines the making of drag persona Johnny T. as part of a king movement where the dominant cultural paradigm of gender is reconsidered and remastered. As seen in Grease, Saturday Night Fever and Urban Cowboy, pop culture icon John Travolta's particular blend of 50s greaser, faggy 70s disco, and 80s country masculinities are shown to be prime drag king conditions, particularly for a dyke who came of age during the 70s Travolta fever. While drawing from personal experience as a king, current trends in the king movement, and gender theory, this essay calls into question the lines between performing masculinity on and off the stage, inviting us to see both the work and play, the parody and realness, the struggle and liberation that make up the transgressive world of drag kinging and gender variance. Drawing upon gender theorists Judith Butler and Judith Halberstam, gender is exposed as a social construction both produced and performed, and as such, drag kinging is framed as an arena where gender is reconfigured.

Does Johnny's Reading Teacher Love to Read? How Teachers' Personal Reading Habits Affect Instructional Practices

ERIC Educational Resources Information Center

McKool, Sharon S.; Gespass, Suzanne

2009-01-01

This article investigates the relationship between teachers' personal reading habits and their instructional practices. Teachers responded to a questionnaire that revealed their attitudes toward reading, the amount of time they spent reading per day and the kind of literacy practices that they used in their classrooms. Results indicate: (1) while…

Gene banks pay big dividends to agriculture, the environment, and human welfare

Treesearch

R. C. Johnson

2008-01-01

Nearly a century after the pioneering American apple tree purveyor Johnny Appleseed traveled from town to town planting nurseries in the Midwestern United States, Frans Nicholas Meijer left his Netherlands home to pursue a similar vocation as an "agricultural explorer" for the US Department of Agriculture. Over the course of his career, Meijer, who...

Brown Country: Johnny Rodriguez

ERIC Educational Resources Information Center

Vargas, Deborah R.

2007-01-01

The year 1972 was part of a dynamic period of Chicano politics and cultural production in South Texas. A few years earlier, in the Crystal City Revolts, Tejanos had moved to gain control of city and school board positions, events that resulted in the creation of the Raza Unida Party in 1970. Nineteen seventy-two also marked the beginning of the…

Social Studies Losing out to Reading, Math

ERIC Educational Resources Information Center

Manzo, Kathleen Kennedy

2005-01-01

"Johnny" may be learning more about reading and mathematics, but he may have little time to study the discoveries of Columbus, the tenets of the U.S. Constitution, or the social and political causes of the Civil War. Those time-honored topics--as well as lesser-known events and figures throughout history--are fighting to maintain their…

Teachers Already Armed in Some Districts

ERIC Educational Resources Information Center

Shah, Nirvi

2013-01-01

Shooting instructor Johnny Price looked at the teachers lined up in front of him. Mr. Price, the owner of Big Iron Concealed Handgun Training in Waco, Texas, spent two days this month training teachers and staff members from the Clifton school district in all they need to know to earn licenses to carry weapons out of sight. There is no indication…

75 FR 79084 - Qualification of Drivers; Exemption Applications; Vision

Federal Register 2010, 2011, 2012, 2013, 2014

2010-12-17

....gpo.gov/2008/pdf/E8-785.pdf . FOR FURTHER INFORMATION CONTACT: Dr. Mary D. Gunnels, Director, Medical... are: Johnny Becerra John B. Ethridge Michael B. McClure Ross E. Burroughs Larry J. Folkerts Francis M. McMullin Lester W. Carter Paul W. Hunter Norman Mullins Christopher L. DePuy Ray P. Lenz David Triplett The...

ADVANCED MANUFACTURING TEAM

NASA Image and Video Library

2016-03-17

JOHNNIE CLARK, BRIAN WEST, AND ZACK JONES OF MSFC’S ADVANCED MANUFACTURING TEAM, WITH MSFC’S XLINE SELECTIVE LASER MELTING SYSTEM. CURRENTLY ONE OF THE LARGEST METAL 3D PRINTERS, THE XLINE AT MARSHALL IS BEING USED TO DEVELOP AND CERTIFY NICKEL ALLOY 718 MATERIAL PROPERTIES AND LARGE MANUFACTURING TECH DEMOS FOR THE RS25 ENGINE AND THE COMMERCIAL CREWED VEHICLE PROJECTS.

Schools and Communities as Partners. When Johnny Can't Read, Who Can Help?

ERIC Educational Resources Information Center

Educational Priorities Panel, New York, NY.

This study examines the extent to which the New York City public school system enables high-risk students to gain access to the kinds of programs and services most appropriate for them. The report is limited to programs in alternative settings, including those operated by the Board of Education and those operated under private nonprofit auspices.…

More than Meets the Ear: A Factor Analysis of Student Impressions of Television Talk Show Hosts.

ERIC Educational Resources Information Center

Walker, James R.

To identify the descriptors most frequently associated with four popular television talk show hosts and to isolate the fundamental dimensions of the images of those talk show hosts, a study surveyed 209 students from Memphis State University and the University of Arkansas (Little Rock) about their impressions of Johnny Carson, David Letterman,…

KENNEDY SPACE CENTER, FLA. - KSC Director Jim Kennedy (left) and incoming KSC Deputy Director Woodrow Whitlow talk about One NASA during the rollout of the Agency initiative at KSC. They were joined at the IMAX Theater® by other NASA leaders James Jennings, NASA’s associate deputy administrator for institutions and asset management; Ed Weiler, associate administrator for Space Science; Kevin Peterson, Dryden Flight Research Center director; and implementation team lead Johnny Stevenson to explain how their respective centers contribute to One NASA. Glenn Research Center Director Dr. Julian Earls gave a motivational speech during the luncheon held at the Visitor Complex Debus Conference Center.

NASA Image and Video Library

2003-08-20

KENNEDY SPACE CENTER, FLA. - KSC Director Jim Kennedy (left) and incoming KSC Deputy Director Woodrow Whitlow talk about One NASA during the rollout of the Agency initiative at KSC. They were joined at the IMAX Theater® by other NASA leaders James Jennings, NASA’s associate deputy administrator for institutions and asset management; Ed Weiler, associate administrator for Space Science; Kevin Peterson, Dryden Flight Research Center director; and implementation team lead Johnny Stevenson to explain how their respective centers contribute to One NASA. Glenn Research Center Director Dr. Julian Earls gave a motivational speech during the luncheon held at the Visitor Complex Debus Conference Center.

Don't Let Little Johnny Keep You from Your Money: A Critical Analysis of the Implementation of Neoliberal Accountability on an Elementary School

ERIC Educational Resources Information Center

Beach, Mary G.

2014-01-01

In this research study, the principal investigator used the methodology of auto-ethnography, interviews, and a critical perspective to analyze the effects of the implementation of high-stakes testing on educators and the classroom environment. In accessing reflective journals and interviews, the researcher gains insight into the dynamics of…

The Farrelly Brothers and Special Olympics Reach Out to Youth at a Favorite Venue--The Movies

ERIC Educational Resources Information Center

Exceptional Parent, 2005

2005-01-01

"The Ringer" is the new comedy produced by Bobby and Peter Farrelly, the writer-directors of such edgy fare as "Kingpin," "Stuck on You" and the blockbuster comedy "Something About Mary." "The Ringer" is a film about a guy named Stevie (played by Johnny Knoxville, the star of MTV's hit series "Jackass") who is pretending to have an intellectual…

Project Summary: Biology-Inspired Autonomous Control

DTIC Science & Technology

2011-02-01

AUTHOR( S ) 5d. PROJECT NUMBER 2304 Johnny H. Evers 5e. TASK NUMBER AM 5f. WORK UNIT NUMBER 08 7. PERFORMING...ORGANIZATION NAME( S ) AND ADDRESS(ES) Air Force Research Laboratory, Munitions Directorate 8. PERFORMING ORGANIZATION REPORT NUMBER AFRL/RWAV...101 West Eglin Blvd Eglin AFB, FL 32542-6810 AFRL-RW-EG-TP-2011-006 9. SPONSORING / MONITORING AGENCY NAME( S ) AND ADDRESS(ES

Why Johnny Struggles When Familiar Concepts Are Taken to a New Mathematical Domain: Towards a Polysemous Approach

ERIC Educational Resources Information Center

Kontorovich, Igor'

2018-01-01

This article is concerned with cognitive aspects of students' struggles in situations in which familiar concepts are reconsidered in a new mathematical domain. Examples of such cross-curricular concepts are divisibility in the domain of integers and in the domain of polynomials, multiplication in the domain of numbers and in the domain of vectors,…

Analysis of Photonic Networks for a Chip Multiprocessor Using Scientific Applications

DTIC Science & Technology

2009-05-01

Analysis of Photonic Networks for a Chip Multiprocessor Using Scientific Applications Gilbert Hendry†, Shoaib Kamil‡?, Aleksandr Biberman†, Johnnie...electronic networks -on-chip warrants investigating real application traces on functionally compa- rable photonic and electronic network designs. We... network can achieve 75× improvement in energy ef- ficiency for synthetic benchmarks and up to 37× improve- ment for real scientific applications

Celebrating the Faces of Literacy. The Twenty-Fourth Yearbook: A Peer Reviewed Publication of the College Reading Association, 2002. [Papers from the College Reading Association Conference, 2001].

ERIC Educational Resources Information Center

Linder, Patricia E., Ed.; Sampson, Mary Beth, Ed.; Dugan, Jo Ann R., Ed.; Brancato, Barrie, Ed.

The College Reading Association believes and values literacy education for all as one way to protect people's freedoms. This 24th Yearbook celebrates the varied "faces" of literacy. The yearbook contains the following special articles: (Presidential Address) "What Is Johnny Reading? A Research Update" (Maria Valerie Gold);…

Pathogenesis of Salmonellosis: Salmonella Exotoxins

DTIC Science & Technology

1982-03-08

of Salmonella enteritidis , which included 9630 serotype newport, 9136 serotype newport, 10016 serotype javiana, and 8832, serotype javiana were also...supplied by Dr. T. Huber. Additionally, four clinical isolates of Salmonella enteritidis , which included 986 serotype typhimurium, 2000 serotype...77Z7I AD _ REPORT NUMBER 3 0 Pathogenesis of Salmonellosis: Salmonella Exotoxins Annual Progress Report (9/1/79-8/31/80) M Johnny W. Peterson, Ph.D

Pathogenesis of Salmonellosis: Salmonella Exotoxins

DTIC Science & Technology

1982-03-08

membrane-as3ociated enterotowin produced by S. enteritidis and by S. typhimurium ; however they could find no similarities between their Salmonella ...AD. . 0 REPORT NUJMBER 1 Pathogenesis of Salmoneiliosis: Salmonella Exotoxins Annual Progress Report (12/1/77-9/1/78) Johnny W. Peterson. Ph.D. March...TYPE OF REPORT & PERIOD COVEREOD",- Uathogenesis of ,Salmonellosils: Salmonella Annual Progress Report Exotoxins 12/T/77 9/1/78 C. PERFORMCNG ORG

Fallout from Nuclear Cratering Shot DANNY BOY. I. Radiochemical Analysis and Some Physical Observations on Selected Samples

DTIC Science & Technology

1980-02-01

radiochemical procedures described in Appendix A. All results were reported in terms of the number of u035 thermal- neutron fissions which would have produced...Ca, Mg, Al, Si, and Fe, expressed both as elements and as oxides . The last column shows the sum of the oxides . The deviation of t~pse values from 100...4.4 Cs13 6 12.9 0.0537 0.006 9.71 y 10’ 7.14 y i0ř 5.9 Ba140 12.79 0.0542 6.3 Ce 3.5 0.0213 6.0 6Ce 52 o.OQ h 6 6.1 a. For ther-a!- neutron fission

System Design for Navy Occupational Standards Development

DTIC Science & Technology

2014-07-01

including, Mr. Thomas Crain, Deputy Director, Workforce Classifications Department, LCDR Juan Carrasco, Michele Jackson, and Johnny Powell. David...and Carrasco, Juan ; Navy Job Analysis Management Project Description, NAVMAC, January 2010. 34  Lists of validated tasks, sorted by Functional...34 runat="server"> <div> <rsweb:ReportViewer ID="ReportViewerSample" runat="server" Font -Names="Verdana" Font -Size=Ŝpt

Recognizing the Face of Johnny, Suzy, and Me: Insensitivity to the Spacing Among Features at 4 Years of Age

ERIC Educational Resources Information Center

Mondloch, Catherine J.; Leis, Anishka; Maurer, Daphne

2006-01-01

Four-year-olds were tested for their ability to use differences in the spacing among features to recognize familiar faces. They were given a storybook depicting multiple views of 2 children. They returned to the laboratory 2 weeks later and used a "magic wand" to play a computer game that tested their ability to recognize the familiarized faces…

New Advances in Molecular Therapy for Muscle Repair after Diseases and Injuries

DTIC Science & Technology

2009-04-01

broader scientific community . Investigator: Johnny Huard - 9 - Project # 1 Progress Report The use of suramin to improve muscle healing after...black arrow ) in grey matter indicated small neuron and axon communication . Project # 5 Final Report Inhibiting cell death and promoting muscle...potential to treat muscle wasting induced by cancer. We anticipate that these results can be generalized to the treatment of other genetic and acquired

Life Cycle Assessment for Chemical Agent Resistant Coating.

DTIC Science & Technology

1996-09-01

994) document to develop HVs from 1 to 2.5. The final equivalency factor for a chemical was based on the formula: Equivalency Factor = (toxicity HV...applicable to the development of processes/procedures and their implementation, likely would fit better with a true LCA- based design exercise for a product...Johnny Springer, Jr., National Risk Management Research Laboratory, Office of Research and Development , U.S. Environmental Protection Agency

Pathogenesis of Salmonellosis: Salmonella Exotoxins

DTIC Science & Technology

1982-03-08

Newport; Sal. 9633 - serotype Newport; and Sal. 9186 - serotype Newport. Salmonella enteritidis serotype typhimurium strain 2000 was obtained from...7054 Table 1I CULTURE MEDIA SURVEY Salmonella enteritidis Salmonella typhimurium serotype Javiana #10016 SRlI Culture Media C H 0 Cell Factor C H 0 Cell...C r AD REPORT NUMBER 2 0 Pathogenesis of Salmonellosis: Salmonella Exotoxins Annual Progress Report (9/1/78-9/1/79) Johnny W. Peterson, Ph.D. March 8

KENNEDY SPACE CENTER, FLA. - NASA’s Ed Weiler, associate administrator for Space Science, speaks to employees and guests during the rollout at KSC of the Agency initiative One NASA . The event was held at the IMAX Theater®. Explaining how their respective centers contribute to One NASA, along with Weiler, were KSC Director Jim Kennedy; James Jennings, NASA’s associate deputy administrator for institutions and asset management; Kevin Peterson, Dryden Flight Research Center director; incoming KSC Deputy Director Woodrow Whitlow; and implementation team lead Johnny Stevenson. Glenn Research Center Director Dr. Julian Earls gave a motivational speech during the luncheon held at the Visitor Complex Debus Conference Center.

NASA Image and Video Library

2003-08-20

KENNEDY SPACE CENTER, FLA. - NASA’s Ed Weiler, associate administrator for Space Science, speaks to employees and guests during the rollout at KSC of the Agency initiative One NASA . The event was held at the IMAX Theater®. Explaining how their respective centers contribute to One NASA, along with Weiler, were KSC Director Jim Kennedy; James Jennings, NASA’s associate deputy administrator for institutions and asset management; Kevin Peterson, Dryden Flight Research Center director; incoming KSC Deputy Director Woodrow Whitlow; and implementation team lead Johnny Stevenson. Glenn Research Center Director Dr. Julian Earls gave a motivational speech during the luncheon held at the Visitor Complex Debus Conference Center.

Physical properties of root cementum: Part 16. Comparisons of root resorption and resorption craters after the application of light and heavy continuous and controlled orthodontic forces for 4, 8, and 12 weeks.

PubMed

Paetyangkul, Anchalee; Türk, Tamer; Elekdağ-Türk, Selma; Jones, Allan S; Petocz, Peter; Cheng, Lam L; Darendeliler, M Ali

2011-03-01

Orthodontic force duration can affect the severity of root resorption. The aim of this clinical study was to investigate the amounts of root resorption volumetrically after the application of controlled light and heavy forces in the buccal direction for 4, 8, and 12 weeks. The sample consisted of 54 maxillary first premolars in 36 patients (mean age, 14.9 years; 21 girls, 15 boys) who required first premolar extractions as part of their orthodontic treatment. The teeth were allocated into 3 groups that varied in the duration of force application: 4, 8, or 12 weeks. The right or left first premolars were randomly selected to receive 2 levels of forces. A light buccally directed orthodontic force of 25 g was applied to the experimental tooth on 1 side, while a heavy orthodontic force of 225 g was applied on the contralateral premolar. At the end of the experimental period, the teeth were extracted and scanned with the microcomputed-tomography x-ray system. Resorption crater analysis was performed with specially designed software for direct volumetric measurements. Significant differences in the extent of root resorption were found between 4, 8, and 12 weeks of force application (P <0.001), with substantially more severe resorption in the longer force duration groups. The light force produced significantly less root resorption than did the heavy force. After 4, 8, or 12 weeks of buccally directed orthodontic forces applied on the maxillary first premolars, the volumes of root resorption craters were found to be related to the duration and the magnitude of the forces. Copyright © 2011 American Association of Orthodontists. Published by Mosby, Inc. All rights reserved.

MSFC Annual Day of Remembrance ceremony

NASA Image and Video Library

2018-01-25

Johnny Stephenson, Director of the Office of Strategic Analysis and Communications, addresses guests and employees at the Marshall Space Flight Center’s annual “Day of Remembrance” honoring those astronauts who have passed away. Looking on, from left, are Rick Burt, Marshall Safety and Mission Assurance Directorate director; Marshall Center Director Todd May; and former NASA astronauts retired Army Brig. Gen. Robert Stewart; former Marshall Deputy Director Jan Davis; and Robert "Hoot" Gibson.

Organizing Chaos: Restructuring Counter-Piracy Forces Off the Coast of Somalia

DTIC Science & Technology

2011-05-04

the Maersk Alabama cargo ship. Prior to these attacks, most Americans were likely to associate a pirate with Hollywood’s mascara-wearing Johnny Depp...However, the approach to countering Somali pirates is disorganized. The international community attempts to achieve unity of effort by relying heavily...conducting counter-piracy as ―a good model not only for the Gulf of Aden and the Somali bases, but also for future such endeavors.‖ 12 Mr. Countryman

KENNEDY SPACE CENTER, FLA. - KSC Director Jim Kennedy and Glenn Research Center Director Dr. Julian Earls share the stage during the rollout of the One NASA initiative at KSC. Earls gave a motivational speech during the luncheon held at the Visitor Complex Debus Conference Center. The event was held at the IMAX Theater® where NASA leaders discussed One NASA with selected employees. Explaining how their respective centers contribute to One NASA, along with Kennedy and Earls, were James Jennings, NASA’s associate deputy administrator for institutions and asset management; Ed Weiler, associate administrator for Space Science; Kevin Peterson, Dryden Flight Research Center director; incoming KSC Deputy Director Woodrow Whitlow; and implementation team lead Johnny Stevenson.

NASA Image and Video Library

2003-08-20

KENNEDY SPACE CENTER, FLA. - KSC Director Jim Kennedy and Glenn Research Center Director Dr. Julian Earls share the stage during the rollout of the One NASA initiative at KSC. Earls gave a motivational speech during the luncheon held at the Visitor Complex Debus Conference Center. The event was held at the IMAX Theater® where NASA leaders discussed One NASA with selected employees. Explaining how their respective centers contribute to One NASA, along with Kennedy and Earls, were James Jennings, NASA’s associate deputy administrator for institutions and asset management; Ed Weiler, associate administrator for Space Science; Kevin Peterson, Dryden Flight Research Center director; incoming KSC Deputy Director Woodrow Whitlow; and implementation team lead Johnny Stevenson.

KENNEDY SPACE CENTER, FLA. - Dryden Flight Research Center Director Kevin Peterson talks about One NASA during the rollout of the Agency initiative at KSC. The event was held at the IMAX Theater® where NASA leaders discussed One NASA with selected employees. Explaining how their respective centers contribute to One NASA, along with Peterson, were KSC Director Jim Kennedy, James Jennings, NASA’s associate deputy administrator for institutions and asset management; Ed Weiler, associate administrator for Space Science; Kevin Peterson, Dryden Flight Research Center director; incoming KSC Deputy Director Woodrow Whitlow; and implementation team lead Johnny Stevenson. Glenn Research Center Director Dr. Julian Earls gave a motivational speech during the luncheon held at the Visitor Complex Debus Conference Center.

NASA Image and Video Library

2003-08-20

KENNEDY SPACE CENTER, FLA. - Dryden Flight Research Center Director Kevin Peterson talks about One NASA during the rollout of the Agency initiative at KSC. The event was held at the IMAX Theater® where NASA leaders discussed One NASA with selected employees. Explaining how their respective centers contribute to One NASA, along with Peterson, were KSC Director Jim Kennedy, James Jennings, NASA’s associate deputy administrator for institutions and asset management; Ed Weiler, associate administrator for Space Science; Kevin Peterson, Dryden Flight Research Center director; incoming KSC Deputy Director Woodrow Whitlow; and implementation team lead Johnny Stevenson. Glenn Research Center Director Dr. Julian Earls gave a motivational speech during the luncheon held at the Visitor Complex Debus Conference Center.

KENNEDY SPACE CENTER, FLA. - KSC’s incoming Deputy Director Woodrow Whitlow speaks to employees and guests during the rollout at KSC of the Agency initiative One NASA . The event was held at the IMAX Theater® where NASA leaders discussed One NASA with selected employees. Explaining how their respective centers contribute to One NASA, along with Whitlow, were KSC Director Jim Kennedy; James Jennings, NASA’s associate deputy administrator for institutions and asset management; Ed Weiler, associate administrator for Space Science; Kevin Peterson, Dryden Flight Research Center director; and implementation team lead Johnny Stevenson. Glenn Research Center Director Dr. Julian Earls gave a motivational speech during the luncheon held at the Visitor Complex Debus Conference Center.

NASA Image and Video Library

2003-08-20

KENNEDY SPACE CENTER, FLA. - KSC’s incoming Deputy Director Woodrow Whitlow speaks to employees and guests during the rollout at KSC of the Agency initiative One NASA . The event was held at the IMAX Theater® where NASA leaders discussed One NASA with selected employees. Explaining how their respective centers contribute to One NASA, along with Whitlow, were KSC Director Jim Kennedy; James Jennings, NASA’s associate deputy administrator for institutions and asset management; Ed Weiler, associate administrator for Space Science; Kevin Peterson, Dryden Flight Research Center director; and implementation team lead Johnny Stevenson. Glenn Research Center Director Dr. Julian Earls gave a motivational speech during the luncheon held at the Visitor Complex Debus Conference Center.

Minutes of the Explosives Safety Seminar (24th) Held in St. Louis, Missouri on 28-30 August 1990. Volume 2

DTIC Science & Technology

1990-08-30

else were not! 20 2017 6 Unlike the preparation and limits determination phases of the site planning process, QDS determination is neither math...Inst. of Mining & Tech, Socorro, NM i CONNELL, Malcolm Property Svcs Agency, Croydon, UK COOK, Johnnie, L. Red River Army Depot, Texarkana , TX 75507...Head, MD 20640 SCHNEIDER, Bruce A. New Mexico Engr Rsch Inst., Albq., NM 87131 SCHOOLER, James S. Red River Army Depot, Texarkana , TX 75507 SCHULTEN

Section 14 Detailed Project Report, Emergency Shoreline Protection, Portersville Bay Mobile County, Alabama

DTIC Science & Technology

1990-05-01

MOBILE COUNTY, ALABAMA MAY 1990 FT~~f f r’ep l c sl m 0 F UNCLASSIFIED SECURITY CLASSIFICATION OF THIS PAGE rw’hen Dat. Entered) REPOT DCUMNTATON...1990 Portersville Bay, Mobile County, Ala. 6. PERFORMING ORG. REPORT NUMBER 7. AUJTHOR(*) 8. CONTRACT OR GRANT NUMBER(*.) Johnny L. Grandison 9. PE...RFORMING ORGANIZATION NAME AND ADDRESS 10. PROGRAM1 ELEMENT, PROJECT, TASK U.S. Army En(7ineer District, Mobile AREA& ORK UNIT NUMBERS Plan Develop

Responses to Nitroprusside Following Hemorrhage in Anesthetized Pigs

DTIC Science & Technology

1991-08-01

well as SPC Bharatkumar Gandhi and SPC Johnny Singson. We also thank Mary Thomas for her secretarial assistance and Charles E. Wade, Ph.D., for his...anesthesia and operation in the head-up position. Anesth Analg 1977; 56:391-394. 9. Larsen R, Teichmann J, Hilfiker 0, Busse C, Sonntag H. Nitroprusside...JN, Burke LP. Nitroprusside. Ann Intern Med 1979; 91:752-757. O’Benar et al .-- Page 26 OFFICIAI. DISTRIBUTION I.IST (’o mmander US Army Medical

"Launch Your Business with NASA" conference in Decatur, Alabama.

NASA Image and Video Library

2017-10-18

The Morgan County Economic Development Association and the City of Decatur, in Partnership with the NASA/Marshall Space Flight Center (MSFC), hosted a business forum on, How to Launch Your Business with NASA, Wednesday, October 18, 2017, at the Alabama Center for the Arts in downtown Decatur, AL. The event was open to all businesses allowed them to connect with Senior NASA representatives and their prime contractors. The program guided businesses through the process of working with NASA as a supplier, subcontractor, and/or a service provider. The Marshall Space Flight Center’s projected procurement budget in FY 2018 is approximately $2.2 billion and numerous procurement opportunities are available for small business participation each fiscal year. The program included Todd May, Director of Marshall Space Flight Center; Johnny Stephenson, Director of Marshall Space Flight Center’s Office of Strategic Analysis and Communication; David Brock, Small Business Specialist with Marshall Space Flight Center; and Lynn Garrison, Small Business Specialist Technical Advisor with Marshall Space Flight Center. Additionally, there was a prime contractor panel consisting of representatives from five NASA prime contractors. The event included a dedicated networking session with those prime contractors. The “Launch Your Business With NASA” event provides those in attendance the opportunity to network with key Marshall Space Flight Center procurement and technical personnel, and representatives of several major Marshall Space Flight Center prime contractors.Arts.. OSAC Director Johnny Stephenson talks about Marshall's Mission areas to audience

Corrective Action Investigation Plan for Corrective Action Unit 374: Area 20 Schooner Unit Crater Nevada Test Site, Nevada, Revision 0

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

Patrick Matthews

Corrective Action Unit 374 is located in Areas 18 and 20 of the Nevada Test Site, which is approximately 65 miles northwest of Las Vegas, Nevada. Corrective Action Unit 374 comprises the five corrective action sites (CASs) listed below: • 18-22-05, Drum • 18-22-06, Drums (20) • 18-22-08, Drum • 18-23-01, Danny Boy Contamination Area • 20-45-03, U-20u Crater (Schooner) These sites are being investigated because existing information on the nature and extent of potential contamination is insufficient to evaluate and recommend corrective action alternatives (CAAs). Additional information will be obtained by conducting a corrective action investigation before evaluating CAAsmore » and selecting the appropriate corrective action for each CAS. The results of the field investigation will support a defensible evaluation of viable CAAs that will be presented in the Corrective Action Decision Document. The sites will be investigated based on the data quality objectives (DQOs) developed on October 20, 2009, by representatives of the Nevada Division of Environmental Protection and the U.S. Department of Energy (DOE), National Nuclear Security Administration Nevada Site Office. The DQO process was used to identify and define the type, amount, and quality of data needed to develop and evaluate appropriate corrective actions for CAU 374.« less

Knowledge, Skills, Abilities, and Other Characteristics for Remotely Piloted Aircraft Pilots and Operators

DTIC Science & Technology

2011-10-19

Editor Dr. Gregory Manley HQ AFPC/DSYX, Dr. Lisa Mills AF/A1PF, Dr. Paul DiTullio HQ Af/A1PFA, Kenneth Schwartz HQ AFPC/DSYX, Johnny Weissmuller HQ...B ru s k ie w ic z e t a l. , 2 0 0 7 : A V O , M P O C h a p p e ll e e t a l. , 2 0 1 0 : M P O C h a p p e ll e e t a l. , 2 0 1 1

Secondary Craters

NASA Image and Video Library

2016-12-21

This image of a southern mid-latitude crater was intended to investigate the lineated material on the crater floor. At the higher resolution of HiRISE, the image reveals a landscape peppered by small impact craters. These craters range from about 30 meters in diameter down to the resolution limit (about 2 meter diameter in this image acquired by averaging 2x2 picture elements). Such dense clusters of small craters are frequently formed by secondary craters, caused by the impact of material that was excavated and ejected from the surface of Mars during the creation of a larger nearby crater by the impact of a comet or an asteroid. Secondary impact craters are both interesting and vexing. They are interesting because they show the trajectories of the material that was ejected from the primary impact with the greatest speeds, typically material from near the surface of the blast zone. Secondary craters are often found along the traces of crater rays, linear features that extend radially from fresh impact craters and can reach many crater diameters in length. Secondary craters can be useful when crater rays are visible and the small craters can be associated with a particular primary impact crater. They can be used to constrain the age of the surface where they fell, since the surface must be older than the impact event. The age of the crater can be approximately estimated from the probability of an impact that produced a crater of such a size within a given area of Mars over a given time period. But these secondary craters can also be perplexing when no crater rays are preserved and a source crater is not easily identifiable, as is the case here. The impact that formed these secondary craters took place long enough ago that their association with a particular crater has been erased. They do not appear along the trace of a crater ray that is still apparent in visible or thermal infrared observations. These secondary craters complicate the task of estimating the age of the lineated material on the crater floor. It is necessary to distinguish secondary craters from the primary impacts that we rely upon to estimate the ages of Martian surfaces. The large number of small craters clustered together here is typical of crater rays elsewhere on Mars and suggests that these are indeed, secondary impact craters. http://photojournal.jpl.nasa.gov/catalog/PIA14450

Degradation studies of Martian impact craters

NASA Technical Reports Server (NTRS)

Barlow, N. G.

1991-01-01

The amount of obliteration suffered by Martian impact craters is quantified by comparing measurable attributes of the current crater shape to those values expected for a fresh crater of identical size. Crater diameters are measured from profiles obtained using photoclinometry across the structure. The relationship between the diameter of a fresh crater and a crater depth, floor width, rim height, central peak height, etc. was determined by empirical studies performed on fresh Martian impact craters. We utilized the changes in crater depth and rim height to judge the degree of obliteration suffered by Martian impact craters.

The Global Contribution of Secondary Craters on the Icy Satellites

NASA Astrophysics Data System (ADS)

Hoogenboom, T.; Johnson, K. E.; Schenk, P.

2014-12-01

At present, surface ages of bodies in the Outer Solar System are determined only from crater size-frequency distributions (a method dependent on an understanding of the projectile populations responsible for impact craters in these planetary systems). To derive accurate ages using impact craters, the impactor population must be understood. Impact craters in the Outer Solar System can be primary, secondary or sesquinary. The contribution of secondary craters to the overall population has recently become a "topic of interest." Our objective is to better understand the contribution of dispersed secondary craters to the small crater populations, and ultimately that of small comets to the projectile flux on icy satellites in general. We measure the diameters of obvious secondary craters (determined by e.g. irregular crater shape, small size, clustering) formed by all primary craters on Ganymede for which we have sufficiently high resolution data to map secondary craters. Primary craters mapped range from approximately 40 km to 210 km. Image resolution ranges from 45 to 440 m/pixel. Bright terrain on Ganymede is our primary focus. These resurfaced terrains have relatively low crater densities and serve as a basis for characterizing secondary populations as a function of primary size on an icy body for the first time. Although focusing on Ganymede, we also investigate secondary crater size, frequency, distribution, and formation, as well as secondary crater chain formation on icy satellites throughout the Saturnian and Jovian systems principally Rhea. We compare our results to similar studies of secondary cratering on the Moon and Mercury. Using Galileo and Voyager data, we have identified approximately 3,400 secondary craters on Ganymede. In some cases, we measured crater density as a function of distance from a primary crater. Because of the limitations of the Galileo data, it is necessary to extrapolate from small data sets to the global population of secondary craters. Nonetheless, we confirm that secondary craters on Ganymede have narrow size-frequency distributions and that they correlate with primary crater diameter. From these data we will evaluate the contribution of secondary craters over a range of crater diameters.

Evidence for self-secondary cratering of Copernican-age continuous ejecta deposits on the Moon

NASA Astrophysics Data System (ADS)

Zanetti, M.; Stadermann, A.; Jolliff, B.; Hiesinger, H.; van der Bogert, C. H.; Plescia, J.

2017-12-01

Crater size-frequency distributions on the ejecta blankets of Aristarchus and Tycho Craters are highly variable, resulting in apparent absolute model age differences despite ejecta being emplaced in a geologic instant. Crater populations on impact melt ponds are a factor of 4 less than on the ejecta, and crater density increases with distance from the parent crater rim. Although target material properties may affect crater diameters and in turn crater size-frequency distribution (CSFD) results, they cannot completely reconcile crater density and population differences observed within the ejecta blanket. We infer from the data that self-secondary cratering, the formation of impact craters immediately following the emplacement of the continuous ejecta blanket by ejecta from the parent crater, contributed to the population of small craters (< 300 m diameter) on ejecta blankets and must be taken into account if small craters and small count areas are to be used for relative and absolute model age determinations on the Moon. Our results indicate that the cumulative number of craters larger than 1 km in diameter per unit area, N(1), on the continuous ejecta blanket at Tycho Crater, ranges between 2.17 × 10-5 and 1.0 × 10-4, with impact melt ponds most accurately reflecting the primary crater flux (N(1) = 3.4 × 10-5). Using the cratering flux recorded on Tycho impact melt deposits calibrated to accepted exposure age (109 ± 1.5 Ma) as ground truth, and using similar crater distribution analyses on impact melt at Aristarchus Crater, we infer the age of Aristarchus Crater to be ∼280 Ma. The broader implications of this work suggest that the measured cratering rate on ejecta blankets throughout the Solar System may be overestimated, and caution should be exercised when using small crater diameters (i.e. < 300 m on the Moon) for absolute model age determination.

Moon-Mercury: Relative preservation states of secondary craters

USGS Publications Warehouse

Scott, D.H.

1977-01-01

Geologic mapping of the Kuiper quadrangle of Mercury and other geologic studies of the planet indicate that secondary craters are much better preserved than those on the moon around primary craters of similar size and morphology. Among the oldest recognized secondary craters on the moon associated with craters 100 km across or less are those of Posidonius, Atlas and Plato; these craters have been dated as middle to late Imbrian in age. Many craters on Mercury with dimensions, morphologies and superposed crater densities similar to these lunar craters have fields and clusters of fresher appearing secondary craters. The apparent differences between secondary-crater morphology and parent crater may be due in part to: (1) rapid isostatic adjustment of the parent crater; (2) different impact fluxes between the two planets; and (or) (3) to the greater concentration of Mercurian secondaries around impact areas, thereby accentuating crater forms. Another factor which may contribute to the better state of preservation of Mercurian secondaries relative to the moon is the difference in crater ejecta velocities on both bodies. These velocities have been calculated for fields of secondary craters at about equal ranges from lunar and Mercurian parent craters. Results show that ejection velocities of material producing most of the secondary craters are rather low (<1 km/s) but velocities on Mercury are about 50% greater than those on the moon for equivalent ranges. Higher velocities may produce morphologically enhanced secondary craters which may account for their better preservation with time. ?? 1977.

Geology of five small Australian impact craters

USGS Publications Warehouse

Shoemaker, E.M.; Macdonald, F.A.; Shoemaker, C.S.

2005-01-01

Here we present detailed geological maps and cross-sections of Liverpool, Wolfe Creek, Boxhole, Veevers and Dalgaranga craters. Liverpool crater and Wolfe Creek Meteorite Crater are classic bowlshaped, Barringer-type craters, Liverpool was likely formed during the Neoproterozoic and was filled and covered with sediments soon thereafter. In the Cenozoic, this cover was exhumed exposing the crater's brecciated wall rocks. Wolfe Creek Meteorite Crater displays many striking features, including well-bedded ejecta units, crater-floor faults and sinkholes, a ringed aeromagnetic anomaly, rim-skirting dunes, and numerous iron-rich shale balls. Boxhole Meteorite Crater, Veevers Meteorite Crater and Dalgaranga crater are smaller, Odessa-type craters without fully developed, steep, overturned rims. Boxhole and Dalgaranga craters are developed in highly follated Precambrian basement rocks with a veneer of Holocene colluvium. The pre-existing structure at these two sites complicates structural analyses of the craters, and may have influenced target deformation during impact. Veevers Meteorite Crater is formed in Cenozoic laterites, and is one of the best-preserved impact craters on Earth. The craters discussed herein were formed in different target materials, ranging from crystalline rocks to loosely consolidated sediments, containing evidence that the impactors struck at an array of angles and velocities. This facilitates a comparative study of the influence of these factors on the structural and topographic form of small impact craters. ?? Geological Society of Australia.

Lunar Cratering Chronology: Calibrating Degree of Freshness of Craters to Absolute Ages

NASA Astrophysics Data System (ADS)

Trang, D.; Gillis-Davis, J.; Boyce, J. M.

2013-12-01

The use of impact craters to age-date surfaces of and/or geomorphological features on planetary bodies is a decades old practice. Various dating techniques use different aspects of impact craters in order to determine ages. One approach is based on the degree of freshness of primary-impact craters. This method examines the degradation state of craters through visual inspection of seven criteria: polygonality, crater ray, continuous ejecta, rim crest sharpness, satellite craters, radial channels, and terraces. These criteria are used to rank craters in order of age from 0.0 (oldest) to 7.0 (youngest). However, the relative decimal scale used in this technique has not been tied to a classification of absolute ages. In this work, we calibrate the degree of freshness to absolute ages through crater counting. We link the degree of freshness to absolute ages through crater counting of fifteen craters with diameters ranging from 5-22 km and degree of freshness from 6.3 to 2.5. We use the Terrain Camera data set on Kaguya to count craters on the continuous ejecta of each crater in our sample suite. Specifically, we divide the crater's ejecta blanket into quarters and count craters between the rim of the main crater out to one crater radii from the rim for two of the four sections. From these crater counts, we are able to estimate the absolute model age of each main crater using the Craterstats2 tool in ArcGIS. Next, we compare the degree of freshness for the crater count-derived age of our main craters to obtain a linear inverse relation that links these two metrics. So far, for craters with degree of freshness from 6.3 to 5.0, the linear regression has an R2 value of 0.7, which corresponds to a relative uncertainty of ×230 million years. At this point, this tool that links degree of freshness to absolute ages cannot be used with craters <8km because this class of crater degrades quicker than larger craters. A graphical solution exists for correcting the degree of freshness for craters <8 km in diameter. We convert this graphical solution to a single function of two independent variables, observed degree of freshness and crater diameter. This function, which results in a corrected degree of freshness is found through a curve-fitting routine and corrects the degree of freshness for craters <8 km in diameter. As a result, we are able to derive absolute ages from the degree of freshness of craters with diameters from about ≤20 km down to a 1 km in diameter with a precision of ×230 million years.

Craters on Crater

NASA Image and Video Library

2006-10-10

Several craters were formed on the rim of this large crater. The movement of material downhill toward the floor of the large crater has formed interesting patterns on the floors of the smaller craters

Using THEMIS thermal infrared observations of rays from Corinto crater to study secondary crater formation on Mars

NASA Astrophysics Data System (ADS)

Williams, J. P.

2017-12-01

Corinto crater (16.95°N, 141.72°E), a 13.8 km diameter crater in Elysium Planitia, displays dramatic rays in Mars Odyssey's Thermal Emission Imaging System (THEMIS) nighttime infrared imagery where high concentrations of secondary craters have altered the thermophysical properties of the martian surface. The THEMIS observations provide a record of secondary crater formation in the region and ray segments are identified up to 2000 km ( 145 crater radii) distance [1][2]. Secondary craters are likely to have the largest influence on model surfaces ages between 0.1 to a few Myr as there is the potential for one or two sizeable craters to project secondary craters onto those surfaces and thus alter the crater size-frequency distribution (CSFD) with an instantaneous spike in crater production [3]. Corinto crater is estimated to be less than a few Ma [4] placing the formation of its secondaries within this formative time period. Secondary craters superposed on relatively young impact craters that predate Corinto provide observations of the secondary crater populations. Crater counts at 520 and 660 km distance from Corinto (38 and 48 crater radii respectively), were conducted. Higher crater densities were observed within ray segments, however secondary craters still influenced the CSFD where ray segments were not apparent, resulting in steepening in the CSFD. Randomness analysis confirms an increase in clustering as diameters decrease suggesting an increasing fraction of secondary craters at smaller diameters, both within the ray and outside. The counts demonstrate that even at nearly 50 crater radii, Corinto secondaries still influence the observed CSFD, even outside of any obvious rays. Crater populations used to derive model ages on many geologically young regions on Mars, such as glacial and periglacial landforms related to obliquity excursions that occur on 106 - 107 yr cycles, should be used cautiously and analyzed for any evidence, either morphologic or statistical, for secondary cratering that may potentially influence the derived age. [1] Williams et al. (2017) MAPS, in press. [2] Bloom et al. (2014) Mars 8th, #1289. [3] Hartmann and Daubar (2017), MAPS, 52, 493- 510. [4] Hundal et al. (2017), LPSC, #1726.

A global catalogue of Ceres impact craters ≥ 1 km and preliminary analysis

NASA Astrophysics Data System (ADS)

Gou, Sheng; Yue, Zongyu; Di, Kaichang; Liu, Zhaoqin

2018-03-01

The orbital data products of Ceres, including global LAMO image mosaic and global HAMO DTM with a resolution of 35 m/pixel and 135 m/pixel respectively, are utilized in this research to create a global catalogue of impact craters with diameter ≥ 1 km, and their morphometric parameters are calculated. Statistics shows: (1) There are 29,219 craters in the catalogue, and the craters have a various morphologies, e.g., polygonal crater, floor fractured crater, complex crater with central peak, etc.; (2) The identifiable smallest crater size is extended to 1 km and the crater numbers have been updated when compared with the crater catalogue (D ≥ 20 km) released by the Dawn Science Team; (3) The d/D ratios for fresh simple craters, obviously degraded simple crater and polygonal simple crater are 0.11 ± 0.04, 0.05 ± 0.04 and 0.14 ± 0.02 respectively. (4) The d/D ratios for non-polygonal complex crater and polygonal complex crater are 0.08 ± 0.04 and 0.09 ± 0.03. The global crater catalogue created in this work can be further applied to many other scientific researches, such as comparing d/D with other bodies, inferring subsurface properties, determining surface age, and estimating average erosion rate.

Crater Mound Formation by Wind Erosion on Mars

NASA Astrophysics Data System (ADS)

Steele, L. J.; Kite, E. S.; Michaels, T. I.

2018-01-01

Most of Mars' ancient sedimentary rocks by volume are in wind-eroded sedimentary mounds within impact craters and canyons, but the connections between mound form and wind erosion are unclear. We perform mesoscale simulations of different crater and mound morphologies to understand the formation of sedimentary mounds. As crater depth increases, slope winds produce increased erosion near the base of the crater wall, forming mounds. Peak erosion rates occur when the crater depth is ˜2 km. Mound evolution depends on the size of the host crater. In smaller craters mounds preferentially erode at the top, becoming more squat, while in larger craters mounds become steeper sided. This agrees with observations where smaller craters tend to have proportionally shorter mounds and larger craters have mounds encircled by moats. If a large-scale sedimentary layer blankets a crater, then as the layer recedes across the crater it will erode more toward the edges of the crater, resulting in a crescent-shaped moat. When a 160 km diameter mound-hosting crater is subject to a prevailing wind, the surface wind stress is stronger on the leeward side than on the windward side. This results in the center of the mound appearing to "march upwind" over time and forming a "bat-wing" shape, as is observed for Mount Sharp in Gale crater.

Rock spatial densities on the rims of the Tycho secondary craters in Mare Nectaris

NASA Astrophysics Data System (ADS)

Basilevsky, A. T.; Michael, G. G.; Kozlova, N. A.

2018-04-01

The aim of this work is to check whether the technique of estimation of age of small lunar craters based on spatial density of rock boulders on their rims described in Basilevsky et al. (2013, 2015b) and Li et al. (2017) for the craters < 1 km in diameter is applicable to the larger craters. The work presents the rock counts on the rims of four craters having diameters 1000, 1100, 1240 and 1400 m located in Mare Nectaris. These craters are secondaries of the primary crater Tycho, whose age was found to be 109 ± 4 Ma (Stoffler and Ryder, 2001) so this may be taken as the age of the four craters, too. Using the dependence of the rock spatial densities at the crater rims on the crater age for the case of mare craters (Li et al., 2017) our measured rock densities correspond to ages from ∼100 to 130 Ma. These estimates are reasonably close to the given age of the primary crater Tycho. This, in turn, suggests that this technique of crater age estimation is applicable to craters up to ∼1.5 km in diameter. For the four considered craters we also measured their depth/diameter ratios and the maximum angles of the crater inner slopes. For the considered craters it was found that with increasing crater diameter, the depth/diameter ratios and maximum angles of internal slopes increase, but the values of these parameters for specific craters may deviate significantly from the general trends. The deviations probably result from some dissimilarities in the primary crater geometries, that may be due to crater to crater differences in characteristics of impactors (e.g., in their bulk densities) and/or differences in the mechanical properties of the target. It may be possible to find secondaries of crater Tycho in the South pole area and, if so, they may be studied to check the specifics and rates of the rock boulder degradation in the lunar polar environment.

Successive Formation of Impact Craters

NASA Image and Video Library

2012-02-16

This image from NASA Dawn spacecraft shows two overlapping impact craters on asteroid Vesta. The rims of the craters are both reasonably fresh but the larger crater must be older because the smaller crater cuts across the larger crater rim.

The self-secondary crater population of the Hokusai crater on Mercury

NASA Astrophysics Data System (ADS)

Xiao, Zhiyong; Prieur, Nils C.; Werner, Stephanie C.

2016-07-01

Whether or not self-secondaries dominate small crater populations on continuous ejecta deposits and floors of fresh impact craters has long been a controversy. This issue potentially affects the age determination technique using crater statistics. Here the self-secondary crater population on the continuous ejecta deposits of the Hokusai crater on Mercury is unambiguously recognized. Superposition relationships show that this population was emplaced after both the ballistic sedimentation of excavation flows and the subsequent veneering of impact melt, but it predated the settlement and solidification of melt pools on the crater floor. Fragments that formed self-secondaries were launched via impact spallation with large angles. Complex craters on the Moon, Mercury, and Mars probably all have formed self-secondaries populations. Dating young craters using crater statistics on their continuous ejecta deposits can be misleading. Impact melt pools are less affected by self-secondaries. Overprint by subsequent crater populations with time reduces the predominance of self-secondaries.

KSC-04PD-0726

NASA Technical Reports Server (NTRS)

2004-01-01

KENNEDY SPACE CENTER, FLA. -- At Oscar Patterson Elementary Magnet School in Panama City, Fla., Center Director Jim Kennedy (far left) stands with (left to right) Bay County school board members Johnny Brock and Thelma Rohan, astronaut Sam Durrance and Panama City Commissioner Johnathon Wilson. Kennedy and Durrance and other NASA officials were at the school to share Americas new vision for space exploration with the next generation of explorers. Kennedy is talking with students about our destiny as explorers, NASAs stepping stone approach to exploring Earth, the Moon, Mars and beyond, how space impacts our lives, and how people and machines rely on each other in space.

Interior and Ejecta Morphologies of Impact Craters on Ganymede

NASA Astrophysics Data System (ADS)

Barlow, Nadine G.; Klaybor, K.; Katz-Wigmore, J.

2006-09-01

We are utilizing Galileo SSI imagery of Ganymede to classify impact crater interior and ejecta morphologies. Although we are in the early stages of compiling our Catalog of Impact Craters on Ganymede, some interesting trends are beginning to emerge. Few craters display obvious ejecta morphologies, but 68 craters are classified as single layer ejecta and 3 as double layer ejecta. We see no obvious correlation of layered ejecta morphologies with terrain or latitude. All layered ejecta craters have diameters between 10 and 40 km. Sinuosity ("lobateness") and ejecta extent ("ejecta mobility ratio") of Ganymede layered ejecta craters are lower than for martian layered ejecta craters. This suggests less mobility of ejecta materials on Ganymede, perhaps due to the colder temperatures. Interior structures being investigated include central domes, peaks, and pits. 57 dome craters, 212 central peak craters, and 313 central pit craters have been identified. Central domes occur in 50-100 km diameter craters while peaks are found in craters between 20 and 50 km and central pit craters range between 29 and 74 km in diameter. The Galileo Regio region displays higher concentrations of central dome and central pit craters than other regions we have investigated. 67% of central pit craters studied to date are small pits, where the ratio of pit diameter to crater diameter is <0.2. Craters containing the three interior structures preferentially occur on darker terrain units, suggesting that an ice-silicate composition is more conducive to interior feature formation than pure ice alone. Results of this study have important implications not only for the formation of specific interior and ejecta morphologies on Ganymede but also for analogous features associated with Martian impact craters. This research is funded through NASA Outer Planets Research Program Award #NNG05G116G to N. G. Barlow.

Simultaneous impact and lunar craters

NASA Technical Reports Server (NTRS)

Oberbeck, V. R.

1972-01-01

The existence of large terrestrial impact crater doublets and crater doublets that have been inferred to be impact craters on Mars suggests that simultaneous impact of two or more bodies can occur at nearly the same point on planetary surfaces. An experimental study of simultaneous impact of two projectiles near one another shows that doublet craters with ridges perpendicular to the bilateral axis of symmetry result when separation between impact points relative to individual crater diameter is large. When separation is progressively less, elliptical craters with central ridges and peaks, and circular craters with deep round bottoms are produced. These craters are similar in structure to many of the large lunar craters. Results suggest that the simultaneous impact of meteoroids near one another may be an important mechanism for the production of central peaks in large lunar craters.

Volatile-rich Crater Interior Deposits on Mars: An Energy Balance Model of Modification

NASA Technical Reports Server (NTRS)

Russell, Patrick S.; Head, James W.; Hecht, Michael H.

2003-01-01

Several craters on Mars are partially filled by material emplaced by post-impact processes. Populations of such craters include those in the circumsouth polar cap region, in Arabia Terra, associated with the Medusae Fossae Formation, and in the northern lowlands proximal to the north polar cap. In this study, crater fill material refers to an interior mound, generally separated from the interior walls of the crater by a trough that may be continuous along the crater s circumference (i.e. a ring-shaped trough), or may only partially contact the crater walls (i.e. a crescent-shaped trough). The fill deposit is frequently off-center from the crater center and may be asymmetric, (i.e. not circular) in plan view shape. Here we test the hypothesis that asymmetries in volatile fill shape, profile, and center-location within a crater result from asymmetries in local energy balance within the crater due mainly to variation of solar insolation and radiative effects of the crater walls over the crater interior. We first focus on Korolev crater in the northern lowlands. We can then apply this model to other craters in different regions. If asymmetry in morphology and location of crater fill are consistent with radiative-dominated asymmetries in energy budget within the crater, then 1) the volatile-rich composition of the fill is supported (this process should not be effective at shaping volcanic or sedimentary deposits), and 2) the dominant factor determining the observed shape of volatile-rich crater fill is the local radiative energy budget within the crater (and erosive processes such as eolian deflation are not necessary).

Crater dimensions from apollo data and supplemental sources

USGS Publications Warehouse

Pike, R.J.

1976-01-01

A catalog of crater dimensions that were compiled mostly from the new Apollo-based Lunar Topographic Orthophotomaps is presented in its entirety. Values of crater diameter, depth, rim height, flank width, circularity, and floor diameter (where applicable) are tabulated for a sample of 484 craters on the Moon and 22 craters on Earth. Systematic techniques of mensuration are detailed. The lunar craters range in size from 400 m to 300 km across and include primary impact craters of the main sequence, secondary impact craters, craterlets atop domes and cones, and dark-halo craters. The terrestrial craters are between 10 m and 22.5 km in diameter and were formed by meteorite impact. ?? 1976 D. Reidel Publishing Company.

Methods of Estimating Initial Crater Depths on Icy Satellites using Stereo Topography

NASA Astrophysics Data System (ADS)

Persaud, D. M.; Phillips, C. B.

2014-12-01

Stereo topography, combined with models of viscous relaxation of impact craters, allows for the study of the rheology and thermal history of icy satellites. An important step in calculating relaxation of craters is determining the initial depths of craters before viscous relaxation. Two methods for estimating initial crater depths on the icy satellites of Saturn have been previously discussed. White and Schenk (2013) present the craters of Iapetus as relatively unrelaxed in modeling the relaxation of craters of Rhea. Phillips et al. (2013) assume that Herschel crater on Saturn's satellite Mimas is unrelaxed in relaxation calculations and models of Rhea and Dione. In the second method, the depth of Herschel crater is scaled based on the different crater diameters and the difference in surface gravity on the large moons to predict the initial crater depths for Rhea and Dione. In the first method, since Iapetus is of similar size to Dione and Rhea, no gravity scaling is necessary; craters of similar size on Iapetus were chosen and their depths measured to determine the appropriate initial crater depths for Rhea. We test these methods by first extracting topographic profiles of impact craters on Iapetus from digital elevation models (DEMs) constructed from stereo images from the Cassini ISS instrument. We determined depths from these profiles and used them to calculate initial crater depths and relaxation percentages for Rhea and Dione craters using the methods described above. We first assumed that craters on Iapetus were relaxed, and compared the results to previously calculated relaxation percentages for Rhea and Dione relative to Herschel crater (with appropriate scaling for gravity and crater diameter). We then tested the assumption that craters on Iapetus were unrelaxed and used our new measurements of crater depth to determine relaxation percentages for Dione and Rhea. We will present results and conclusions from both methods and discuss their efficacy for determining initial crater depth. References: Phillips, C.B., et al. (2013). Lunar Planet Sci. XLIV, abstract 2766. White, O.L., and P.L. Schenk. Icarus 23, 699-709, 2013. This work was supported by the NASA Outer Planets Research Program grant NNX10AQ09G and by the NSF REU Program.

Elevation and igneous crater modification on Venus: Implications for magmatic volatile content

NASA Technical Reports Server (NTRS)

Wichman, R. W.

1993-01-01

Although most impact craters on Venus preserve nearly pristine crater rim and ejecta features, a small number of craters have been identified showing clear evidence of either igneous intrusion emplacement (floor-fracturing) beneath the crater floor or of volcanically embayed exterior ejecta deposits. Since the volcanically embayed craters consistently occur at higher elevations than the identified floor-fractured craters, this report proposes that igneous crater modification on Venus is elevation dependent. This report describes how regional variations in magmatic neutral buoyancy could produce such elevation dependent crater modification and considers the implications for typical magmatic volatile contents on Venus.

Size-Frequency Distribution of Small Lunar Craters: Widening with Degradation and Crater Lifetime

NASA Astrophysics Data System (ADS)

Ivanov, B. A.

2018-01-01

The review and new measurements are presented for depth/diameter ratio and slope angle evolution during small ( D < 1 km) lunar impact craters aging (degradation). Comparative analysis of available data on the areal cratering density and on the crater degradation state for selected craters, dated with returned Apollo samples, in the first approximation confirms Neukum's chronological model. The uncertainty of crater retention age due to crater degradational widening is estimated. The collected and analyzed data are discussed to be used in the future updating of mechanical models for lunar crater aging.

Physical properties of lunar craters

NASA Astrophysics Data System (ADS)

Joshi, Maitri P.; Bhatt, Kushal P.; Jain, Rajmal

2017-02-01

The surface of the Moon is highly cratered due to impacts of meteorites, asteroids, comets and other celestial objects. The origin, size, structure, age and composition vary among craters. We study a total of 339 craters observed by the Lunar Reconnaissance Orbiter Camera (LROC). Out of these 339 craters, 214 craters are known (named craters included in the IAU Gazetteer of Planetary Nomenclature) and 125 craters are unknown (craters that are not named and objects that are absent in the IAU Gazetteer). We employ images taken by LROC at the North and South Poles and near side of the Moon. We report for the first time the study of unknown craters, while we also review the study of known craters conducted earlier by previous researchers. Our study is focused on measurements of diameter, depth, latitude and longitude of each crater for both known and unknown craters. The diameter measurements are based on considering the Moon to be a spherical body. The LROC website also provides a plot which enables us to measure the depth and diameter. We found that out of 214 known craters, 161 craters follow a linear relationship between depth (d) and diameter (D), but 53 craters do not follow this linear relationship. We study physical dimensions of these 53 craters and found that either the depth does not change significantly with diameter or the depths are extremely high relative to diameter (conical). Similarly, out of 125 unknown craters, 78 craters follow the linear relationship between depth (d) and diameter (D) but 47 craters do not follow the linear relationship. We propose that the craters following the scaling law of depth and diameter, also popularly known as the linear relationship between d and D, are formed by the impact of meteorites having heavy metals with larger dimension, while those with larger diameter but less depth are formed by meteorites/celestial objects having low density material but larger diameter. The craters with very high depth and with very small diameter are perhaps formed by the impact of meteorites that have very high density but small diameter with a conical shape. Based on analysis of the data selected for the current investigation, we further found that out of 339 craters, 100 (29.5%) craters exist near the equator, 131 (38.6%) are in the northern hemisphere and 108 (31.80%) are in the southern hemisphere. This suggests the Moon is heavily cratered at higher latitudes and near the equatorial zone.

Geomorphology of crater and basin deposits - Emplacement of the Fra Mauro formation

NASA Technical Reports Server (NTRS)

Morrison, R. H.; Oberbeck, V. R.

1975-01-01

Characteristics of continuous deposits near lunar craters larger than about 1 km wide are considered, and it is concluded that (1) concentric dunes, radial ridges, and braided lineations result from deposition of the collision products of ejecta from adjacent pairs of similarly oriented secondary-crater chains and are, therefore, concentrations of secondary-crater ejecta; (2) intracrater ridges are produced within preexisting craters surrounding a fresh primary crater by ricocheting and focusing of secondary-crater ejecta from the preexisting craters' walls; and (3) secondary cratering has produced many of the structures of the continuous deposits of relatively small lunar craters and is the dominant process for emplacement of most of the radial facies of the continuous deposits of large lunar craters and basins. The percentages of Imbrium ejecta in deposits and the nature of Imbrium sculpturing are investigated.

Cratering on Ceres: Implications for its crust and evolution

USGS Publications Warehouse

Hiesinger, H.; Marchi, S.; Schmedemann, N.; Schenk, P.; Pasckert, J. H.; Neesemann, A.; O'Brien, D. P.; Kneissl, T.; Ermakov, A.; Fu, R.R.; Bland, M. T.; Nathues, A.; Platz, T.; Williams, D.A.; Jaumann, R.; Castillo-Rogez, J. C.; Ruesch, O.; Schmidt, B.; Park, R.S.; Preusker, F.; Buczkowski, D.L.; Russell, C.T.; Raymond, C.A.

2016-01-01

Thermochemical models have predicted that Ceres, is to some extent, differentiated and should have an icy crust with few or no impact craters. We present observations by the Dawn spacecraft that reveal a heavily cratered surface, a heterogeneous crater distribution, and an apparent absence of large craters. The morphology of some impact craters is consistent with ice in the subsurface, which might have favored relaxation, yet large unrelaxed craters are also present. Numerous craters exhibit polygonal shapes, terraces, flowlike features, slumping, smooth deposits, and bright spots. Crater morphology and simple-to-complex crater transition diameters indicate that the crust of Ceres is neither purely icy nor rocky. By dating a smooth region associated with the Kerwan crater, we determined absolute model ages (AMAs) of 550 million and 720 million years, depending on the applied chronology model.

Centrifuge impact cratering experiment 5

NASA Technical Reports Server (NTRS)

1984-01-01

Transient crates motions, cratering flow fields, crates dynamics, determining impact conditions from total crater welt, centrifuge quarter-space cratering, and impact cratering mechanics research is documented.

Geomorphology and Geology of the Southwestern Margaritifer Sinus and Argyre Regions of Mars. Part 4: Flow Ejecta Crater Distribution

NASA Technical Reports Server (NTRS)

Parker, T. J.; Pieri, D. C.

1985-01-01

Flow ejecta craters - craters surrounded by lobate ejecta blankets - are found throughout the study area. The ratio of the crater's diameter to that of the flow ejecta in this region is approximately 40 to 45%. Flow ejecta craters are dominantly sharply defined craters, with slightly degraded craters being somewhat less common. This is probably indicative of the ejecta's relatively low resistence to weathering and susceptibility to burial. Flow ejecta craters here seem to occur within a narrow range of crater sizes - the smallest being about 4km in diameter and the largest being about 27km in diameter. Ejecta blankets of craters at 4km are easily seen and those of smaller craters are simply not seen even in images with better than average resolution for the region. This may be due to the depth of excavation of small impacting bodies being insufficient to reach volatile-rich material. Flow ejecta craters above 24km are rare, and those craters above 27km do not display flow ejecta blankets. This may be a result of an excavation depth so great that the volatile content of the ejecta is insufficient to form a fluid ejecta blanket. The geomorphic/geologic unit appears also to play an important role in the formation of flow ejecta craters. Given the typical size range for the occurrence of flow ejecta craters for most units, it can be seen that the percentage of flow ejecta craters to the total number of craters within this size range varies significantly from one unit to the next. The wide variance in flow ejecta crater density over this relatively small geographical area argues strongly for a lithologic control of their distribution.

Spatial distribution of impact craters on Deimos

NASA Astrophysics Data System (ADS)

Hirata, Naoyuki

2017-05-01

Deimos, one of the Martian moons, has numerous impact craters. However, it is unclear whether crater saturation has been reached on this satellite. To address this issue, we apply a statistical test known as nearest-neighbor analysis to analyze the crater distribution of Deimos. When a planetary surface such as the Moon is saturated with impact craters, the spatial distribution of craters is generally changed from random to more ordered. We measured impact craters on Deimos from Viking and HiRISE images and found (1) that the power law of the size-frequency distribution of the craters is approximately -1.7, which is significantly shallower than those of potential impactors, and (2) that the spatial distribution of craters over 30 m in diameter cannot be statistically distinguished from completely random distribution, which indicates that the surface of Deimos is inconsistent with a surface saturated with impact craters. Although a crater size-frequency distribution curve with a slope of -2 is generally interpreted as indicating saturation equilibrium, it is here proposed that two competing mechanisms, seismic shaking and ejecta emplacement, have played a major role in erasing craters on Deimos and are therefore responsible for the shallow slope of this curve. The observed crater density may have reached steady state owing to the obliterations induced by the two competing mechanisms. Such an occurrence indicates that the surface is saturated with impact craters despite the random distribution of craters on Deimos. Therefore, this work proposes that the age determined by the current craters on Deimos reflects neither the age of Deimos itself nor that of the formation of the large concavity centered at its south pole because craters should be removed by later impacts. However, a few of the largest craters on Deimos may be indicative of the age of the south pole event.

Cratering history of Miranda: Implications for geologic processes

USGS Publications Warehouse

Plescia, J.B.

1988-01-01

Miranda's surface is divisible into cratered terrain and coronae. The cratered terrain is the most heavily cratered of the terrains and presumably is the oldest. The frequency of craters in the cratered terrain is variable and related to position on the satellite. The coronae are also variably cratered. Elsinore and Arden Coronae have similar crater frequencies and may have formed simultaneously. They are of intermediate agompared to the cratered terrain and to Inverness Corona, which is the youngest major terrain. Graben formation appears to have occured both before and after the formation of the coronae reflecting periods of global expansion. Miranda's surfaces are, in general, the least cratered and therefore inferred to be the youngest within the Uranian system. ?? 1988.

Impact craters on Venus: An overview from Magellan observations

NASA Technical Reports Server (NTRS)

Schaber, G. G.; Strom, R. G.; Moore, H. J.; Soderblom, L. A.; Kirk, R. L.; Chadwick, D. J.; Dawson, D. D.; Gaddis, L. R.; Boyce, J. M.; Russell, J.

1992-01-01

Magellan has revealed an ensemble of impact craters on Venus that is unique in many important ways. We have compiled a database describing 842 craters on 89 percent of the planet's surface mapped through orbit 2578 (the craters range in diameter from 1.5 to 280 km). We have studied the distribution, size-frequency, morphology, and geology of these craters both in aggregate and, for some craters, in more detail. We have found the following: (1) the spatial distribution of craters is highly uniform; (2) the size-density distribution of craters with diameters greater than or equal to 35 km is consistent with a 'production' population having a surprisingly young age of about 0.5 Ga (based on the estimated population of Venus-crossing asteroids); (3) the spectrum of crater modification differs greatly from that on other planets--62 percent of all craters are pristine, only 4 percent volcanically embayed, and the remainder affected by tectonism, but none are severely and progressively depleted based on size-density distribution extrapolated from larger craters; (4) large craters have a progression of morphologies generally similar to those on other planets, but small craters are typically irregular or multiple rather than bowl shaped; (5) diffuse radar-bright or -dark features surround some craters, and about 370 similar diffuse 'splotches' with no central crater are observed whose size-density distribution is similar to that of small craters; and (6) other features unique to Venus include radar-bright or -dark parabolic arcs opening westward and extensive outflows originating in crater ejecta.

Tabular comparisons of the Flynn Creek impact crater, United States, Steinheim impact crater, Germany and Snowball explosion crater, Canada

NASA Technical Reports Server (NTRS)

Roddy, D. J.

1977-01-01

A tabular outline of comparative data is presented for 340 basic dimensional, morphological, and structural parameters and related aspects for three craters of the flat-floored, central uplift type, two of which are natural terrestrial impact craters and one is a large-scale experimental explosion crater. The three craters are part of a general class, in terms of their morphology and structural deformation that is represented on each of the terrestrial planets including the moon. One of the considered craters, the Flynn Creek Crater, was formed by a hypervelocity impact event approximately 360 m.y. ago in what is now north central Tennessee. The impacting body appears to have been a carbonaceous chondrite or a cometary mass. The second crater, the Steinheim Crater, was formed by an impact event approximately 14.7 m.y. ago in what is now southwestern Germany. The Snowball Crater was formed by the detonation of a 500-ton TNT hemisphere on flat-lying, unconsolidated alluvium in Alberta, Canada.

Experimental simulation of impact cratering on icy satellites

NASA Technical Reports Server (NTRS)

Greeley, R.; Fink, J. H.; Gault, D. E.; Guest, J. E.

1982-01-01

Cratering processes on icy satellites were simulated in a series of 102 laboratory impact experiments involving a wide range of target materials. For impacts into homogeneous clay slurries with impact energies ranging from five million to ten billion ergs, target yield strengths ranged from 100 to 38 Pa, and apparent viscosities ranged from 8 to 200 Pa s. Bowl-shaped craters, flat-floored craters, central peak craters with high or little relief, and craters with no relief were observed. Crater diameters increased steadily as energies were raised. A similar sequence was seen for experiment in which impact energy was held constant but target viscosity and strength progressively decreases. The experiments suggest that the physical properties of the target media relative to the gravitationally induced stresses determined the final crater morphology. Crater palimpsests could form by prompt collapse of large central peak craters formed in low target strength materials. Ages estimated from crater size-frequency distributions that include these large craters may give values that are too high.

Terrace width variations in complex Mercurian craters and the transient strength of cratered Mercurian and lunar crust

NASA Technical Reports Server (NTRS)

Leith, Andrew C.; Mckinnon, William B.

1991-01-01

The effective cohesion of the cratered region during crater collapse is determined via the widths of slump terraces of complex craters. Terrace widths are measured for complex craters on Mercury; these generally increase outward toward the rim for a given crater, and the width of the outermost major terrace is generally an increasing function of crater diameter. The terrace widths on Mercury and a gravity-driven slump model are used to estimate the strength of the cratered region immediately after impact (about 1-2 MPa). A comparison with the previous study of lunar complex craters by Pearce and Melosh (1986) indicates that the transient strength of cratered Mercurian crust is no greater than that of the moon. The strength estimates vary only slightly with the geometric model used to restore the outermost major terrace to its precollapse configuration and are consistent with independent strength estimates from the simple-to-complex crater depth/diameter transition.

Craters on Earth, Moon, and Mars: Multivariate classification and mode of origin

USGS Publications Warehouse

Pike, R.J.

1974-01-01

Testing extraterrestrial craters and candidate terrestrial analogs for morphologic similitude is treated as a problem in numerical taxonomy. According to a principal-components solution and a cluster analysis, 402 representative craters on the Earth, the Moon, and Mars divide into two major classes of contrasting shapes and modes of origin. Craters of net accumulation of material (cratered lunar domes, Martian "calderas," and all terrestrial volcanoes except maars and tuff rings) group apart from craters of excavation (terrestrial meteorite impact and experimental explosion craters, typical Martian craters, and all other lunar craters). Maars and tuff rings belong to neither group but are transitional. The classification criteria are four independent attributes of topographic geometry derived from seven descriptive variables by the principal-components transformation. Morphometric differences between crater bowl and raised rim constitute the strongest of the four components. Although single topographic variables cannot confidently predict the genesis of individual extraterrestrial craters, multivariate statistical models constructed from several variables can distinguish consistently between large impact craters and volcanoes. ?? 1974.

Application of high explosion cratering data to planetary problems

NASA Technical Reports Server (NTRS)

Oberbeck, V. R.

1977-01-01

The present paper deals with the conditions of explosion or nuclear cratering required to simulate impact crater formation. Some planetary problems associated with three different aspects of crater formation are discussed, and solutions based on high-explosion data are proposed. Structures of impact craters and some selected explosion craters formed in layered media are examined and are related to the structure of lunar basins. The mode of ejection of material from impact craters is identified using explosion analogs. The ejection mode is shown to have important implications for the origin of material in crater and basin deposits. Equally important are the populations of secondary craters on lunar and planetary surfaces.

Paradigm lost: Venus crater depths and the role of gravity in crater modification

NASA Technical Reports Server (NTRS)

Sharpton, Virgil L.

1992-01-01

Previous to Magellan, a convincing case had been assembled that predicted that complex impact craters on Venus were considerably shallower than their counterparts on Mars, Mercury, the Moon, and perhaps even Earth. This was fueled primarily by the morphometric observation that, for a given diameter (D), crater depth (d) seems to scale inversely with surface gravity for the other planets in the inner solar system. The unpredicted depth of fresh impact craters on Venus argues against a simple inverse relationship between surface gravity and crater depth. Factors that could contribute to deep craters on Venus include (1) more efficient excavation on Venus, possibly reflecting rheological effects of the hot venusian environment; (2) more melting and efficient removal of melt from the crater cavity; and (3) enhanced ejection of material out of the crater, possibly as a result of entrainment in an atmosphere set in motion by the passage of the projectile. The broader issue raised by the venusian crater depths is whether surface gravity is the predominant influence on crater depths on any planet. While inverse gravity scaling of crater depths has been a useful paradigm in planetary cratering, the venusian data do not support this model and the terrestrial data are equivocal at best. The hypothesis that planetary gravity is the primary influence over crater depths and the paradigm that terrestrial craters are shallow should be reevaluated.

Martian Low-Aspect-Ratio Layered Ejecta (LARLE) craters: Distribution, characteristics, and relationship to pedestal craters

NASA Astrophysics Data System (ADS)

Barlow, Nadine G.; Boyce, Joseph M.; Cornwall, Carin

2014-09-01

Low-Aspect-Ratio Layered Ejecta (LARLE) craters are a unique landform found on Mars. LARLE craters are characterized by a crater and normal layered ejecta pattern surrounded by an extensive but thin outer deposit which terminates in a sinuous, almost flame-like morphology. We have conducted a survey to identify all LARLE craters ⩾1-km-diameter within the ±75° latitude zone and to determine their morphologic and morphometric characteristics. The survey reveals 140 LARLE craters, with the majority (91%) located poleward of 40°S and 35°N and all occurring within thick mantles of fine-grained deposits which are likely ice-rich. LARLE craters range in diameter from the cut-off limit of 1 km up to 12.2 km, with 83% being smaller than 5 km. The radius of the outer LARLE deposit displays a linear trend with the crater radius and is greatest at higher polar latitudes. The LARLE deposit ranges in length between 2.56 and 14.81 crater radii in average extent, with maximum length extending up to 21.4 crater radii. The LARLE layer is very sinuous, with lobateness values ranging between 1.45 and 4.35. LARLE craters display a number of characteristics in common with pedestal craters and we propose that pedestal craters are eroded versions of LARLE craters. The distribution and characteristics of the LARLE craters lead us to propose that impact excavation into ice-rich fine-grained deposits produces a dusty base surge cloud (like those produced by explosion craters) that deposits dust and ice particles to create the LARLE layers. Salts emplaced by upward migration of water through the LARLE deposit produce a surficial duricrust layer which protects the deposit from immediate removal by eolian processes.

Morphometry of impact craters on Mercury from MESSENGER altimetry and imaging

NASA Astrophysics Data System (ADS)

Susorney, Hannah C. M.; Barnouin, Olivier S.; Ernst, Carolyn M.; Johnson, Catherine L.

2016-06-01

Data acquired by the Mercury Laser Altimeter and the Mercury Dual Imaging System on the MESSENGER spacecraft in orbit about Mercury provide a means to measure the geometry of many of the impact craters in Mercury's northern hemisphere in detail for the first time. The combination of topographic and imaging data permit a systematic evaluation of impact crater morphometry on Mercury, a new calculation of the diameter Dt at which craters transition with increasing diameter from simple to complex forms, and an exploration of the role of target properties and impact velocity on final crater size and shape. Measurements of impact crater depth on Mercury confirm results from previous studies, with the exception that the depths of large complex craters are typically shallower at a given diameter than reported from Mariner 10 data. Secondary craters on Mercury are generally shallower than primary craters of the same diameter. No significant differences are observed between the depths of craters within heavily cratered terrain and those of craters within smooth plains. The morphological attributes of craters that reflect the transition from simple to complex craters do not appear at the same diameter; instead flat floors first appear with increasing diameter in craters at the smallest diameters, followed with increasing diameter by reduced crater depth and rim height, and then collapse and terracing of crater walls. Differences reported by others in Dt between Mercury and Mars (despite the similar surface gravitational acceleration on the two bodies) are confirmed in this study. The variations in Dt between Mercury and Mars cannot be adequately attributed to differences in either surface properties or mean projectile velocity.

Variations in interior morphology of 15-20 km lunar craters - Implications for a major subsurface discontinuity

NASA Technical Reports Server (NTRS)

De Hon, R. A.

1980-01-01

Craters vary in morphology as a function of crater diameter, age, and mode of origin. This study concentrates on the morphology of young lunar impact craters within a limited size range. Elimination of morphologic variations generally attributed to crater size or age leaves a small population which should nearly reflect the varying properties of the lunar substrate. The sample consists of 17 craters 15-20 km in diameter with both simple and complex morphologies. While depth/diameter ratios do not obviously differ between mare and highland subsets, apparent depth, rim height, and profile data do differ distinctly. Highland craters tend to be deep, simple, and bowl-shaped. Mare craters tend to be shallow and flat-floored. Rim heights of complex mare craters are typically greater than those of simple craters. Differences of highland and mare crater morphologies are attributed to variations in the thickness of the lunar megaregolith. Highland craters in this size range do not penetrate the megaregolith. The depth and morphology of complex craters are controlled by the discontinuity at the transition from highly brecciated megaregolith to more coherent crystalline material of the upper crust.

Relative depths of simple craters and the nature of the lunar regolith

NASA Astrophysics Data System (ADS)

Stopar, Julie D.; Robinson, Mark S.; Barnouin, Olivier S.; McEwen, Alfred S.; Speyerer, Emerson J.; Henriksen, Megan R.; Sutton, Sarah S.

2017-12-01

We assessed the morphologies of more than 930 simple impact craters (diameters 40 m-10 km) on the Moon using digital terrain models (DTMs) of a variety of terrains in order to characterize the variability of fresh crater morphology as a function of crater diameter. From Lunar Reconnaissance Orbiter Camera (LROC) Narrow Angle Camera (NAC) DTMs, we determined depth-to-diameter (d/D) ratios for an extremely fresh set of these craters with diameters less than 400 m and found that their d/D ratios range from 0.11 to 0.17. Using both NAC and Kaguya Terrain Camera DTMs, we also determined the d/D ratios for the set of fresh simple craters larger than 400 m in diameter. The d/D ratios of these larger craters are typically near 0.21, as expected of gravity-dominated crater excavation. Fresh craters less than ∼400 m in diameter, on the other hand, exhibit significantly lower d/D ratios. Various possible factors affect the morphologies and relative depths (d/D ratios) of small strength-dominated craters, including impactor and target properties (e.g., effective strength, strength contrasts, porosity, pre-existing weaknesses), impact angle and velocity, and degradation state. While impact conditions resulting from secondary impacts can also affect crater morphologies, we found that d/D ratio alone was not a unique discriminator of small secondary craters. To investigate the relative influences of degradation and target properties on the d/D ratios of small strength-dominated craters, we examined a subset of fresh craters located on the geologically young rim deposits of Tycho crater. These craters are deeper and steeper than other craters of similar diameter and degradation state, consistent with their relative freshness and formation in the relatively coherent, melt-rich deposits in this region. The d/D ratios of globally distributed small craters of similar degradation state and size range, on the other hand, are relatively shallow with lower average wall slopes, consistent with crater excavation in a weak or poorly cohesive layer. The widespread predominance of these small, shallow craters is consistent with the pervasive, poorly cohesive upper regolith.

Marine-target craters on Mars? An assessment study

USGS Publications Warehouse

Ormo, J.; Dohm, J.M.; Ferris, J.C.; Lepinette, A.; Fairen, A.G.

2004-01-01

Observations of impact craters on Earth show that a water column at the target strongly influences lithology and morphology of the resultant crater. The degree of influence varies with the target water depth and impactor diameter. Morphological features detectable in satellite imagery include a concentric shape with an inner crater inset within a shallower outer crater, which is cut by gullies excavated by the resurge of water. In this study, we show that if oceans, large seas, and lakes existed on Mars for periods of time, marine-target craters must have formed. We make an assessment of the minimum and maximum amounts of such craters based on published data on water depths, extent, and duration of putative oceans within "contacts 1 and 2," cratering rate during the different oceanic phases, and computer modeling of minimum impactor diameters required to form long-lasting craters in the seafloor of the oceans. We also discuss the influence of erosion and sedimentation on the preservation and exposure of the craters. For an ocean within the smaller "contact 2" with a duration of 100,000 yr and the low present crater formation rate, only ???1-2 detectable marine-target craters would have formed. In a maximum estimate with a duration of 0.8 Gyr, as many as 1400 craters may have formed. An ocean within the larger "contact 1-Meridiani," with a duration of 100,000 yr, would not have received any seafloor craters despite the higher crater formation rate estimated before 3.5 Gyr. On the other hand, with a maximum duration of 0.8 Gyr, about 160 seafloor craters may have formed. However, terrestrial examples show that most marine-target craters may be covered by thick sediments. Ground penetrating radar surveys planned for the ESA Mars Express and NASA 2005 missions may reveal buried craters, though it is uncertain if the resolution will allow the detection of diagnostic features of marine-target craters. The implications regarding the discovery of marine-target craters on Mars is not without significance, as such discoveries would help address the ongoing debate of whether large water bodies occupied the northern plains of Mars and would help constrain future paleoclimatic reconstructions. ?? Meteoritical Society, 2004.

Occurrence and mechanisms of impact melt emplacement at small lunar craters

NASA Astrophysics Data System (ADS)

Stopar, Julie D.; Hawke, B. Ray; Robinson, Mark S.; Denevi, Brett W.; Giguere, Thomas A.; Koeber, Steven D.

2014-11-01

Using observations from the Lunar Reconnaissance Orbiter Camera (LROC), we assess the frequency and occurrence of impact melt at simple craters less than 5 km in diameter. Nine-hundred-and-fifty fresh, randomly distributed impact craters were identified for study based on their maturity, albedo, and preservation state. The occurrence, frequency, and distribution of impact melt deposits associated with these craters, particularly ponded melt and lobate flows, are diagnostic of melt emplacement mechanisms. Like larger craters, those smaller than a few kilometers in diameter often exhibit ponded melt on the crater floor as well as lobate flows near the crater rim crest. The morphologies of these deposits suggest gravity-driven flow while the melt was molten. Impact melt deposits emplaced as veneers and ;sprays;, thin layers of ejecta that drape other crater materials, indicate deposition late in the cratering process; the deposits of fine sprays are particularly sensitive to degradation. Exterior melt deposits found near the rims of a few dozen craters are distributed asymmetrically around the crater and are rare at craters less than 2 km in diameter. Pre-existing topography plays a role in the occurrence and distribution of these melt deposits, particularly for craters smaller than 1 km in diameter, but does not account for all observed asymmetries in impact melt distribution. The observed relative abundance and frequency of ponded melt and flows in and around simple lunar craters increases with crater diameter, as was previously predicted from models. However, impact melt deposits are found more commonly at simple lunar craters (i.e., those less than a few kilometers in diameter) than previously expected. Ponded melt deposits are observed in roughly 15% of fresh craters smaller than 300 m in diameter and 80% of fresh craters between 600 m and 5 km in diameter. Furthermore, melt deposits are observed at roughly twice as many non-mare craters than at mare craters. We infer that the distributions and occurrences of impact melt are strongly influenced by impact velocity and angle, target porosity, pre-existing topography, and degradation. Additionally, areally small and volumetrically thin melt deposits are sensitive to mixing with solid debris and/or burial during the modification stage of impact cratering as well as post-cratering degradation. Thus, the production of melt at craters less than ∼800 m in diameter is likely greater than inferred from the present occurrence of melt deposits, which is rapidly affected by ongoing degradation processes.

Apollo 12 Mission image - High oblique view of crater Copernicus and Carpathian Mt. range

NASA Image and Video Library

1969-11-19

AS12-47-6876 (November 1969) --- An Apollo 12 high-oblique view of the lunar nearside looking northeast toward the crater Copernicus (in center near horizon), as photographed from lunar orbit. The shaded crater in the foreground is Reinhold. Reinhold B is the crater next to Reinhold which as the small crater in the center of it. Also, visible is the keyhole-shaped crater Fauth near the crater Copernicus.

An assessment of crater erosional histories on the Earth and Mars using digital terrain models.

NASA Astrophysics Data System (ADS)

Paul, R. L.; Muller, J.-P.; Murray, J. B.

The research will examine quantitatively the geomorphology of both Terrestrial and Martian craters. The erosional and sub-surface processes will be investigated to understand how these affect a crater's morphology. For example, the Barringer crater in Arizona has an unusual shape. The Earth has a very high percentage of water both in the atmosphere as clouds or rain and under the surface. The presence of water will therefore affect a crater's formation and its subsequent erosional modification. On Mars there is little or no water present currently, though recent observations suggest there may be near-surface ice in some areas. How do craters formed in the Martian environment therefore differ from Terrestrial ones? How has the structure of Martian craters changed in areas of possible fluvial activity? How does the surface material affect crater formation? How does the Earth's fluvial activity affect a crater's evolution? At present, four measurements of circularity have been used to describe a crater (Murray & Guest, 1972). These parameters will be re-examined to see how effectively they describe Terrestrial and Martian craters using high resolution DTMs which were not available at the time of the original study. The model described by Forsberg-Taylor et al. 2004, and others will also be applied to results obtained from the chosen craters to assess how effectively these craters are described. Both hypsometric curves and hydrological analysis will be used to assess crater evolution. A suitable criterion for the selection of Terrestrial and Martian craters is essential for this type of research. Terrestrial craters have been selected in arid or semi-arid terrain with crater diameters larger than one kilometre. Craters less than five million years old would be ideal. However, this was too restrictive and so a variety of crater ages have had to be used. Eight terrestrial craters have been selected in arid or semi-arid areas for study, using the Earth Impact Database and ICEDS. These are: Barringer, Arizona, U.S.A; Goat Paddock, West Australia; Ouarkziz, Algeria; Roter Kamm, Namibia; Talemzane, Algeria; Tenoumer, Mauritania; Tswaing, South Africa 1 and Upheaval Dome, Utah, U.S.A. Comparable Martian craters are in the process of being chosen using the USGS PIGWAD database and the Morphological Catalogue of the Craters of Mars. Digital Terrain Models of each crater using SRTM DEMs and data from the recent Mars Express HRSC will be used at various resolutions (30m upwards) to provide three dimensional models to assess the capabilities of measuring erosional effects. There is also available ASTER DEMs and ASTER Level 1A for terrestrial craters and MOLA tracks for Martian craters. Both laboratory and theoretical models of crater shape and erosion features will provide a better understanding of the processes observed. This will enable us to develop a better explanation of why craters are the shape they are. References. Barlow N., 1987, Crater Size-Frequency Distribution and a Revised Martian Relative Chronology, Icarus, 75, 285-305. Barlow, N., 1995, The degradation of impact craters in Maja Valles and Arabia Mars, Journal GeoPhys. Res., 100, 23307-23316. Earth Impact Database http://www.unb.ca/passc/ImpactDatabase/ Earth PIGWAD database http://webgis.wr.usgs.gov/website/mars%5Fcrater%5Fhtml/viewer.htm ICEDS http://iceds.ge.ucl.ac.uk/ Morphology Catalogue of the Craters of Mars http://selena.sai.msu.ru/Home/Mars_Cat/Mars_Cat.htm Murray J.B, Guest J.E, 1970, Circularities of craters and related structures on Earth and Moon, Modern Geology, 1, 149-159. Forsberg-Taylor N., Howard A.D., 2004, Crater degradation in the Martian Highlands: Morphometric Analysis of the Sinus Sabaeus region and simulation modelling suggest fluvial processes, Journal GeoPhys Res., 109, E05002. 2

Small Rayed Crater Ejecta Retention Age Calculated from Current Crater Production Rates on Mars

NASA Technical Reports Server (NTRS)

Calef, F. J. III; Herrick, R. R.; Sharpton, V. L.

2011-01-01

Ejecta from impact craters, while extant, records erosive and depositional processes on their surfaces. Estimating ejecta retention age (Eret), the time span when ejecta remains recognizable around a crater, can be applied to estimate the timescale that surface processes operate on, thereby obtaining a history of geologic activity. However, the abundance of sub-kilometer diameter (D) craters identifiable in high resolution Mars imagery has led to questions of accuracy in absolute crater dating and hence ejecta retention ages (Eret). This research calculates the maximum Eret for small rayed impact craters (SRC) on Mars using estimates of the Martian impactor flux adjusted for meteorite ablation losses in the atmosphere. In addition, we utilize the diameter-distance relationship of secondary cratering to adjust crater counts in the vicinity of the large primary crater Zunil.

Regional variations in degradation and density of Martian craters.

NASA Technical Reports Server (NTRS)

Mcgill, G. E.; Wise, D. U.

1972-01-01

Martian craters visible on Mariner 6 and 7 imagery show a spectrum of topographic types from very fresh to highly degraded. A method of numerical scoring of rim, wall, and floor is proposed to yield a degradation number to classify each crater. Plots of degradation class vs density of large craters are similar for all four regions studied, whereas similar plots for small craters show marked differences between regions. The data suggest general continuity of crater formation and degradation, along with locally sporadic formation and/or degradation of the smallest craters classified. Deucalionis Regio, with an excess of fresh, small craters, experienced an episode of small crater formation (or nondegradation) most recently; Margaritifer Sinus was similarly disturbed at some more remote time. Meridiani Sinus and Hellespontus-Noachis show little or no sign of excess fresh, small craters.

Rampart craters on Ganymede: Their implications for fluidized ejecta emplacement

NASA Astrophysics Data System (ADS)

Boyce, Joseph; Barlow, Nadine; Mouginis-Mark, Peter; Stewart, Sarah

2010-04-01

Some fresh impact craters on Ganymede have the overall ejecta morphology similar to Martian double-layer ejecta (DLE), with the exception of the crater Nergal that is most like Martian single layer ejecta (SLE) craters (as is the terrestrial crater Lonar). Similar craters also have been identified on Europa, but no outer ejecta layer has been found on these craters. The morphometry of these craters suggests that the types of layered ejecta craters identified by Barlow et al. (2000) are fundamental. In addition, the mere existence of these craters on Ganymede and Europa suggests that an atmosphere is not required for ejecta fluidization, nor can ejecta fluidization be explained by the flow of dry ejecta. Moreover, the absence of fluidized ejecta on other icy bodies suggests that abundant volatiles in the target also may not be the sole cause of ejecta fluidization. The restriction of these craters to the grooved terrain of Ganymede and the concentration of Martian DLE craters on the northern lowlands suggests that these terrains may share key characteristics that control the development of the ejecta of these craters. In addition, average ejecta mobility (EM) ratios indicate that the ejecta of these bodies are self-similar with crater size, but are systematically smaller on Ganymede and Europa. This may be due to the effects of the abundant ice in the crusts of these satellites that results in increased ejection angle causing ejecta to impact closer to the crater and with lower horizontal velocity.

Impact Craters: Size-Dependent Degration Rates

NASA Astrophysics Data System (ADS)

Ravi, S.; Mahanti, P.; Meyer, H. M.; Robinson, M. S.

2017-12-01

From superposition relations, Shoemaker and Hackman (1) devised the lunar geologic timescale with Copernican and Eratosthenian as the most recent periods. Classifying craters into the two periods is key to understanding impactor flux and regolith maturation rates over the last 3 Ga. Both Copernican and Eratosthenian craters exhibit crisp morphologies (sharp rims, steep slopes), however, only the former exhibit high reflectance rays and ejecta (1). Based on the Optical Maturity Parameter (OMAT; 2), Grier et al. (3) classified 50 fresh craters (D >20 km) into 3 categories - young (OMAT >0.22), intermediate, and old (OMAT <0.16). In our previous work, Copernican craters (D > 10) were identified (4) from a catalogue of 11,875 craters (5). In this work; we compare two size ranges (D: 5 km - 10 km and 10 km to 15 km) of 177 Copernican craters based on the average OMAT, measured near the crater rim (3). OMAT is measured at the crater rim (as opposed to further away from the crater) to minimize the influence of spatial variation of OMAT (6) in our investigation. We found that OMAT values are typically lower for smaller craters (5km < D < 10km) in comparison to larger craters (10km < D < 15km). However, when compared against morphological freshness (as determined by d/D for simpler craters), the smaller craters were fresher (higher d/D value). Since the OMAT value decreases with age, craters with higher d/D value (morphologically fresher) should have higher OMAT, but this is not the case. We propose that quicker loss of OMAT (over time) for smaller craters compared to decrease in d/D with crater ageing, is responsible for the observed decreased OMAT for smaller craters. (1) Shoemaker and Hackman, 1962 (2) Lucey et al., 2000 (3) Grier et al., 2001 (4) Ravi et al., 2016 (5) Reinhold et al., 2015 (6) Mahanti et al., 2016

Ancient fluvial processes in the equatorial highlands of Mars

NASA Technical Reports Server (NTRS)

Craddock, Robert A.; Maxwell, Ted A.

1991-01-01

Martian highland craters typically lack ejecta deposits, have no noticeable rim, and are flat floored. In addition, crater size frequency distribution curves show that highland craters have depleted populations less than 20 km in diameter. A variety of processes have been suggested to explain these observations including deposition of aeolian or volcanic materials up to the crater rim crests, thermal creep, terrain softening, and mass wasting. However, none of these processes adequately explains both the crater morphology and population distribution. In order to explain both the Martian highland crater morphology and population distribution, a fluvial process is proposed which is capable of removing the loose crater rim material. The resulting effect is to decrease the crater diameter, thereby causing the population curves to bendover. The eroded material is redistributed, burying or partially burying smaller diameter craters before complete erosion. This material may also be deposited into local topographic lows, creating the depositional basins observed. A fluvial process explains both sets of observations: crater morphology and crater population distribution curves.

Multivariate analyses of crater parameters and the classification of craters

NASA Technical Reports Server (NTRS)

Siegal, B. S.; Griffiths, J. C.

1974-01-01

Multivariate analyses were performed on certain linear dimensions of six genetic types of craters. A total of 320 craters, consisting of laboratory fluidization craters, craters formed by chemical and nuclear explosives, terrestrial maars and other volcanic craters, and terrestrial meteorite impact craters, authenticated and probable, were analyzed in the first data set in terms of their mean rim crest diameter, mean interior relief, rim height, and mean exterior rim width. The second data set contained an additional 91 terrestrial craters of which 19 were of experimental percussive impact and 28 of volcanic collapse origin, and which was analyzed in terms of mean rim crest diameter, mean interior relief, and rim height. Principal component analyses were performed on the six genetic types of craters. Ninety per cent of the variation in the variables can be accounted for by two components. Ninety-nine per cent of the variation in the craters formed by chemical and nuclear explosives is explained by the first component alone.

Phobos - Surface density of impact craters

NASA Technical Reports Server (NTRS)

Thomas, P.; Veverka, J.

1977-01-01

Revised crater counts for Phobos are presented which are based on uniform Mariner 9 imagery and Duxbury's (1974) map of the satellite. The contiguous portion of the satellite's surface on which all craters down to the limiting resolution of 0.2 to 0.3 km in diameter would be expected to be identified is delineated and found to contain 87 identifiable craters larger than 0.2 km in diameter. Analysis of the crater size distribution shows that the surface appears to be saturated for craters exceeding 1 km in diameter but the crater counts definitely fall below the saturation curve for smaller craters. Reasons for this fall-off are considered, and it is noted that too few craters are visible in Mariner 9 images of Deimos to permit meaningful crater counts on that satellite's surface. It is concluded that, contrary to a previous assertion, the surfaces of Phobos and Deimos are not known to be saturated with craters larger than 0.2 km in diameter.

On the usefulness of optical maturity for relative age classification of fresh craters

NASA Astrophysics Data System (ADS)

Ravi, S.; Meyer, H. M.; Mahanti, P.; Robinson, M. S.

2016-12-01

Copernican and Eratosthenian craters represent the two most recent geologic periods in the lunar timescale, and their characterization is essential for understanding impact crater flux over the last 3 Gy. Craters from both periods exhibit crisp morphologies, but Copernican craters are 'rayed craters' per Wilhelms (1) classification scheme. Distinguishing compositional from maturity rays is possible using compositional estimates and the optical maturity parameter (OMAT; 2). From OMAT estimates, Grier et al. (3) classified 50 fresh craters (diameter (D) > 20 km) into young (OMAT > 0.22), intermediate, and old (OMAT < 0.16) classes. In this work we analyze morphology and optical maturity for a population of 12,000 craters (D> 10 km; 60 to investigate the applicability of OMAT for relative age classification among Copernican craters. Craters obtained from (4,5) were initially classified based on crispness of morphology (LROC WAC observations (6)) and then were then analyzed based on OMAT values averaged from rim out to one crater radius (n=2000). We found that typically craters larger than Copernicus (D = 95 km) were had lower OMAT values than Copernicus (OMAT = 0.17) except for Vavilov, Pythagorus, Fizeau and Moretus which had OMAT > 0.17. These large craters are clearly affected by rays from small, nearby craters. We estimate that at least 250 craters (D > 10 km; OMAT > 0.22) on the Moon are Copernican (> 2% of all craters analyzed) and of these at least 100 are as optically immature (or more so) than Tycho crater (OMAT >= 0.24). A calibration curve (OMAT vs Absolute Model Age) obtained for craters with known ages showed that OMAT <=0.15 displays little change with AMA and are thus unsuitable for estimating relative ages. Normalization by crater size was found to reduce the uncertainty associated with the relation between AMA and OMAT. 1) Wilhelms (1987), The Geologic History of the Moon, USGS, pp. 1348. 2) Lucey et al (2000), JGR, 105, 20377-20386. 3) Grier et al. (2001), JGR, 106, 847-862. 4) Povilaitis et al. (2013), NLSI, Session 5B. 5) Head et al. (2010), Science, 239, 1504-1506. 6) Boyd et al. (2013), AGU, P13B-1744.

Gully formation in terrestrial simple craters: Meteor Crater, USA and Lonar Crater, India

NASA Astrophysics Data System (ADS)

Kumar, P.; Head, J. W.; Kring, D. A.

2007-12-01

Geomorphic features such as gullies, valley networks, and channels on Mars have been used as a proxy to understand the climate and landscape evolution of Mars. Terrestrial analogues provide significant insight as to how the various exogenic and endogenic processes might contribute to the evolution of these martian landscapes. We describe here a terrestrial example from Meteor Crater, which shows a spectacular development of gullies throughout the inner wall in response to rainwater precipitation, snow melting and groundwater discharge. As liquid water has been envisaged as one of the important agents of landscape sculpturing, Meteor Crater remains a useful landmark, where planetary geologists can learn some lessons. We also show here how the lithology and structural framework of this crater controls the gully distribution. Like many martian impact craters, it was emplaced in layered sedimentary rocks with an exceptionally well-developed centripetal drainage pattern consisting of individual alcoves, channels and fans. Some of the gullies originate from the rim crest and others from the middle crater wall, where a lithologic transition occurs. Deeply incised alcoves are well-developed on the soft sandstones of the Coconino Formation exposed on the middle crater wall, beneath overlying dolomite. In general, the gully locations are along crater wall radial fractures and faults, which are favorable locales of groundwater flow and discharge; these structural discontinuities are also the locales where the surface runoff from rain precipitation and snow melting can preferentially flow, causing degradation. Like martian craters, channels are well developed on the talus deposits and alluvial fans on the periphery of the crater floor. In addition, lake sediments on the crater floor provide significant evidence of a past pluvial climate, when groundwater seeped from springs on the crater wall. Caves exposed on the lower crater level may point to percolation of surface runoff and selective discharge through fractures on the crater wall. Similar relationships are seen at Lonar Crater, India. Although these hydrological processes continue at Meteor Crater today, conditions at the crater are much more arid than they were soon after impact, reflecting a climatic shift similar in direction to that inferred for Mars.

Impact craters on Titan

USGS Publications Warehouse

Wood, Charles A.; Lorenz, Ralph; Kirk, Randy; Lopes, Rosaly; Mitchell, Karl; Stofan, Ellen; ,

2010-01-01

Five certain impact craters and 44 additional nearly certain and probable ones have been identified on the 22% of Titan's surface imaged by Cassini's high-resolution radar through December 2007. The certain craters have morphologies similar to impact craters on rocky planets, as well as two with radar bright, jagged rims. The less certain craters often appear to be eroded versions of the certain ones. Titan's craters are modified by a variety of processes including fluvial erosion, mass wasting, burial by dunes and submergence in seas, but there is no compelling evidence of isostatic adjustments as on other icy moons, nor draping by thick atmospheric deposits. The paucity of craters implies that Titan's surface is quite young, but the modeled age depends on which published crater production rate is assumed. Using the model of Artemieva and Lunine (2005) suggests that craters with diameters smaller than about 35 km are younger than 200 million years old, and larger craters are older. Craters are not distributed uniformly; Xanadu has a crater density 2-9 times greater than the rest of Titan, and the density on equatorial dune areas is much lower than average. There is a small excess of craters on the leading hemisphere, and craters are deficient in the north polar region compared to the rest of the world. The youthful age of Titan overall, and the various erosional states of its likely impact craters, demonstrate that dynamic processes have destroyed most of the early history of the moon, and that multiple processes continue to strongly modify its surface. The existence of 24 possible impact craters with diameters less than 20 km appears consistent with the Ivanov, Basilevsky and Neukum (1997) model of the effectiveness of Titan's atmosphere in destroying most but not all small projectiles.

Impact craters on Titan

USGS Publications Warehouse

Wood, C.A.; Lorenz, R.; Kirk, R.; Lopes, R.; Mitchell, Ken; Stofan, E.

2010-01-01

Five certain impact craters and 44 additional nearly certain and probable ones have been identified on the 22% of Titan's surface imaged by Cassini's high-resolution radar through December 2007. The certain craters have morphologies similar to impact craters on rocky planets, as well as two with radar bright, jagged rims. The less certain craters often appear to be eroded versions of the certain ones. Titan's craters are modified by a variety of processes including fluvial erosion, mass wasting, burial by dunes and submergence in seas, but there is no compelling evidence of isostatic adjustments as on other icy moons, nor draping by thick atmospheric deposits. The paucity of craters implies that Titan's surface is quite young, but the modeled age depends on which published crater production rate is assumed. Using the model of Artemieva and Lunine (2005) suggests that craters with diameters smaller than about 35 km are younger than 200 million years old, and larger craters are older. Craters are not distributed uniformly; Xanadu has a crater density 2-9 times greater than the rest of Titan, and the density on equatorial dune areas is much lower than average. There is a small excess of craters on the leading hemisphere, and craters are deficient in the north polar region compared to the rest of the world. The youthful age of Titan overall, and the various erosional states of its likely impact craters, demonstrate that dynamic processes have destroyed most of the early history of the moon, and that multiple processes continue to strongly modify its surface. The existence of 24 possible impact craters with diameters less than 20 km appears consistent with the Ivanov, Basilevsky and Neukum (1997) model of the effectiveness of Titan's atmosphere in destroying most but not all small projectiles. ?? 2009 Elsevier Inc.

An investigation of the cratering-induced motions occurring during the formation of bowl-shaped craters. [using high explosive charges as the cratering source

NASA Technical Reports Server (NTRS)

Piekutowski, A. J.

1980-01-01

The effects of the dynamic processes which occur during crater formation were examined using small hemispherical high-explosive charges detonated in a tank which had one wall constructed of a thick piece of clear plexiglas. Crater formation and the motions of numerous tracer particles installed in the cratering medium at the medium-wall interface were viewed through the wall of this quarter-space tank and recorded with high-speed cameras. Subsequent study and analysis of particle motions and events recorded on the film provide data needed to develop a time-sequence description of the formation of a bowl-shaped crater. Tables show the dimensions of craters produced in a quarter-space tank compared with dimensions of craters produced in normal half-space tanks. Crater growth rate summaries are also tabulated.

The Lord of the Rings - Deep Learning Craters on the Moon and Other Bodies

NASA Astrophysics Data System (ADS)

Silburt, Ari; Ali-Dib, Mohamad; Zhu, Chenchong; Jackson, Alan; Valencia, Diana; Kissin, Yevgeni; Tamayo, Daniel; Menou, Kristen

2018-01-01

Crater detection has traditionally been done via manual inspection of images, leading to statistically significant disagreements between scientists for the Moon's crater distribution. In addition, there are millions of uncategorized craters on the Moon and other Solar System bodies that will never be classified by humans due to the time required to manually detect craters. I will show that a deep learning model trained on the near-side of the Moon can successfully reproduce the crater distribution on the far-side, as well as detect thousands of small, new craters that were previously uncharacterized. In addition, this Moon-trained model can be transferred to accurately classify craters on Mercury. It is therefore likely that this model can be extended to classify craters on all Solar System bodies with Digital Elevation Maps. This will facilitate, for the first time ever, a systematic, accurate, and reproducible study of the crater records throughout the Solar System.

Ceres and the terrestrial planets impact cratering record

NASA Astrophysics Data System (ADS)

Strom, R. G.; Marchi, S.; Malhotra, R.

2018-03-01

Dwarf planet Ceres, the largest object in the Main Asteroid Belt, has a surface that exhibits a range of crater densities for a crater diameter range of 5-300 km. In all areas the shape of the craters' size-frequency distribution is very similar to those of the most ancient heavily cratered surfaces on the terrestrial planets. The most heavily cratered terrain on Ceres covers ∼15% of its surface and has a crater density similar to the highest crater density on <1% of the lunar highlands. This region of higher crater density on Ceres probably records the high impact rate at early times and indicates that the other 85% of Ceres was partly resurfaced after the Late Heavy Bombardment (LHB) at ∼4 Ga. The Ceres cratering record strongly indicates that the period of Late Heavy Bombardment originated from an impactor population whose size-frequency distribution resembles that of the Main Belt Asteroids.

A proposed origin for palimpsests and anomalous pit craters on Ganymede and Callisto

NASA Technical Reports Server (NTRS)

Croft, S. K.

1983-01-01

The hypothesis that palimpsests and anomalous pit craters are essentially pristine crater forms derived from high-velocity impacts and/or impacts into an ice crust with preimpact temperatures near melting is explored. The observational data are briefly reviewed, and an impact model is proposed for the direct formation of a palimpsest from an impact when the modification flow which produces the final crater is dominated by 'wet' fluid flow, as opposed to the 'dry' granular flow which produces normal craters. Conditions of 'wet' modification occur when the volume of impact melt remaining in the transient crater attains a volume comparable to the transient crater. The normal crater-palimpsest transition is found to occur for sufficiently large impacts or sufficiently fast impactors. The range of crater diameters and morphological characteristics inferred from the impact model is consistent with the observed characteristics of palimpsests and anomalous pit craters.

A first-order model for impact crater degradation on Venus

NASA Technical Reports Server (NTRS)

Izenberg, Noam R.; Arvidson, Raymond E.; Phillips, Roger J.

1993-01-01

A first-order impact crater aging model is presented based on observations of the global crater population of Venus. The total population consists of 879 craters found over the approximately 98 percent of the planet that has been mapped by the Magellan spacecraft during the first three cycles of its mission. The model is based upon three primary aspects of venusian impact craters: (1) extended ejecta deposits (EED's); (2) crater rims and continuous ejecta deposits; and (3) crater interiors and floors.

Martian Central Pit Craters

NASA Technical Reports Server (NTRS)

Hillman, E.; Barlow, N. G.

2005-01-01

Impact craters containing central pits are rare on the terrestrial planets but common on icy bodies. Mars is the exception among the terrestrial planets, where central pits are seen on crater floors ( floor pits ) as well as on top of central peaks ( summit pits ). Wood et al. [1] proposed that degassing of subsurface volatiles during crater formation produced central pits. Croft [2] argued instead that central pits might form during the impact of volatile-rich comets. Although central pits are seen in impact craters on icy moons such as Ganymede, they do show some significant differences from their martian counterparts: (a) only floor pits are seen on Ganymede, and (b) central pits begin to occur at crater diameters where the peak ring interior morphology begins to appear in terrestrial planet craters [3]. A study of craters containing central pits was conducted by Barlow and Bradley [4] using Viking imagery. They found that 28% of craters displaying an interior morphology on Mars contain central pits. Diameters of craters containing central pits ranged from 16 to 64 km. Barlow and Bradley noted that summit pit craters tended to be smaller than craters containing floor pits. They also noted a correlation of central pit craters with the proposed rings of large impact basins. They argued that basin ring formation fractured the martian crust and allowed subsurface volatiles to concentrate in these locations. They favored the model that degassing of the substrate during crater formation was responsible for central pit formation due to the preferential location of central pit craters along these basin rings.

Why do complex impact craters have elevated crater rims?

NASA Astrophysics Data System (ADS)

Kenkmann, Thomas; Sturm, Sebastian; Krueger, Tim

2014-05-01

Most of the complex impact craters on the Moon and on Mars have elevated crater rims like their simple counterparts. The raised rim of simple craters is the result of (i) the deposition of a coherent proximal ejecta blanket at the edge of the transient cavity (overturned flap) and (ii) a structural uplift of the pre-impact surface near the transient cavity rim during the excavation stage of cratering [1]. The latter occurs either by plastic thickening or localized buckling of target rocks, as well as by the emplacement of interthrust wedges [2] or by the injection of dike material. Ejecta and the structural uplift contribute equally to the total elevation of simple crater rims. The cause of elevated crater rims of large complex craters [3] is less obvious, but still, the rim height scales with the final crater diameter. Depending on crater size, gravity, and target rheology, the final crater rim of complex craters can be situated up to 1.5-2.0 transient crater radii distance from the crater center. Here the thickness of the ejecta blanket is only a fraction of that occurring at the rim of simple craters, e.g. [4], and thus cannot account for a strong elevation. Likewise, plastic thickening including dike injection of the underlying target may not play a significant role at this distance any more. We started to systematically investigate the structural uplift and ejecta thickness along the rim of complex impact craters to understand the cause of their elevation. Our studies of two lunar craters (Bessel, 16 km diameter and Euler, 28 km diameter) [5] and one unnamed complex martian crater (16 km diameter) [6] showed that the structural uplift at the final crater rim makes 56-67% of the total rim elevation while the ejecta thickness contributes 33-44%. Thus with increasing distance from the transient cavity rim, the structural uplift seems to dominate. As dike injection and plastic thickening are unlikely at such a distance from the transient cavity, we propose that reverse faulting induced by radially outward directed maximum stresses during the excavation flow may be responsible for the elevation of complex crater rims. This hypothesis is tested at terrestrial craters whose apparent crater rims are often confined by circumferential faults [7]. References:[1] Shoemaker, E. M. (1963) The Solar System, 4, 301-336. [2] Poelchau M.H. et al. (2009), JGR, 114, E01006. [3] Settle, M., and Head, J.W., (1977), Icarus, 31, 123. [4] McGetchin, T. R., et al., (1973), EPSL, 20, 226.[5] Krüger T. et al. (2014), LPSC 45, #1834. [6] Sturm, S. et al. (2014), LPSC 45, 1801. [7] Turtle, E. et al. (2005), GSA-SP. 384, 1.

Low-velocity impact craters in ice and ice-saturated sand with implications for Martian crater count ages.

USGS Publications Warehouse

Croft, S.K.; Kieffer, S.W.; Ahrens, T.J.

1979-01-01

We produced a series of decimeter-sized impact craters in blocks of ice near 0oC and -70oC and in ice-saturated sand near -70oC as a preliminary investigation of cratering in materials analogous to those found on Mars and the outer solar satellites. Crater diameters in the ice-saturated sand were 2 times larger than craters in the same energy and velocity range in competent blocks of granite, basalt and cement. Craters in ice were c.3 times larger. Martian impact crater energy versus diameter scaling may thus be a function of latitude. -from Authors

Experimental Simulations of Large-Scale Collisions

NASA Technical Reports Server (NTRS)

Housen, Kevin R.

2002-01-01

This report summarizes research on the effects of target porosity on the mechanics of impact cratering. Impact experiments conducted on a centrifuge provide direct simulations of large-scale cratering on porous asteroids. The experiments show that large craters in porous materials form mostly by compaction, with essentially no deposition of material into the ejecta blanket that is a signature of cratering in less-porous materials. The ratio of ejecta mass to crater mass is shown to decrease with increasing crater size or target porosity. These results are consistent with the observation that large closely-packed craters on asteroid Mathilde appear to have formed without degradation to earlier craters.

Shallow and deep fresh impact craters in Hesperia Planum, Mars

NASA Technical Reports Server (NTRS)

Mouginis-Mark, Peter J.; Hayashi, Joan N.

1993-01-01

The depths of 109 impact craters about 2-16 km in diameter, located on the ridged plains materials of Hesperia Planum, Mars, have been measured from their shadow lengths using digital Viking Orbiter images (orbit numbers 417S-419S) and the PICS computer software. On the basis of their pristine morphology (very fresh lobate ejecta blankets, well preserved rim crests, and lack of superposed impact craters), 57 of these craters have been selected for detailed analysis of their spatial distribution and geometry. We find that south of 30 deg S, craters less than 6.0 km in diameter are markedly shallower than similar-sized craters equatorward of this latitude. No comparable relationship is observed for morphologically fresh craters greater than 6.0 km diameter. We also find that two populations exist for older craters less than 6.0 km diameter. When craters that lack ejecta blankets are grouped on the basis of depth/diameter ratio, the deeper craters also typically lie equatorward of 30 S. We interpret the spatial variation in crater depth/diameter ratios as most likely due to a poleward increase in volatiles within the top 400 m of the surface at the times these craters were formed.

Lunar and Venusian radar bright rings

NASA Technical Reports Server (NTRS)

Thompson, T. W.; Saunders, R. S.; Weissman, D. E.

1986-01-01

Twenty-one lunar craters have radar bright ring appearances which are analogous to eleven complete ring features in the earth-based 12.5 cm observations of Venus. Radar ring diameters and widths for the lunar and Venusian features overlap for sizes from 45 to 100 km. Radar bright areas for the lunar craters are associated with the slopes of the inner and outer rim walls, while level crater floors and level ejecta fields beyond the raised portion of the rim have average radar backscatter. It is proposed that the radar bright areas of the Venusian rings are also associated with the slopes on the rims of craters. The lunar craters have evolved to radar bright rings via mass wasting of crater rim walls and via post-impact flooding of crater floors. Aeolian deposits of fine-grained material on Venusian crater floors may produce radar scattering effects similar to lunar crater floor flooding. These Venusian aeolian deposits may preferentially cover blocky crater floors producing a radar bright ring appearance. It is proposed that the Venusian features with complete bright ring appearances and sizes less than 100 km are impact craters. They have the same sizes as lunar craters and could have evolved to radar bright rings via analogous surface processes.

The Explorer's Guide to Impact Craters

NASA Technical Reports Server (NTRS)

Chuang, F.; Pierazzo, E.; Osinski, G.

2005-01-01

Impact cratering is a fundamental geologic process of our solar system. It competes with other processes, such as plate tectonics, volcanism, fluvial, glacial and eolian activity, in shaping the surfaces of planetary bodies. In some cases, like the Moon and Mercury, impact craters are the dominant landform. On other planetary bodies impact craters are being continuously erased by the action of other geological processes, like volcanism on Io, erosion and plate tectonics on the Earth, tectonic and volcanic resurfacing on Venus, or ancient erosion periods on Mars. The study of crater populations is one of the principal tools for understanding the geologic history of a planetary surface. Among the general public, impact cratering has drawn wide attention through its portrayal in several Hollywood movies. Questions that are raised after watching these movies include: How do scientists learn about impact cratering? , and What information do impact craters provide in understanding the evolution of a planetary surface? Fundamental approaches used by scientists to learn about impact cratering include field work at known terrestrial craters, remote sensing studies of craters on various solid surfaces of solar system bodies, and theoretical and laboratory studies using the known physics of impact cratering.

The phanerozoic impact cratering rate: Evidence from the farside of the Moon

USGS Publications Warehouse

McEwen, A.S.; Moore, Johnnie N.; Shoemaker, E.M.

1997-01-01

The relatively recent (< 1 b.y.) flux of asteroids and comets forming large craters on the Earth and Moon may be accurately recorded by craters with bright rays on the Moon's farside. Many previously unknown farside rayed craters are clearly distinguished in the low-phase-angle images returned by the Clementine spacecraft. Some large rayed craters on the lunar nearside are probably significantly older than 1 Ga; rays remain visible over the maria due to compositional contrasts long after soils have reached optical maturity. Most of the farside crust has a more homogeneous composition and only immature rays are visible. The size-frequency distribution of farside rayed craters is similar to that measured for Eratosthenian craters (up to 3.2 b.y.) at diameters larger than 15 km. The areal density of farside rayed craters matches that of a corrected tabulation of nearside Copernican craters. Hence the presence of bright rays due to immature soils around large craters provides a consistent time-stratigraphic basis for defining the base of the Copernican System. The density of large craters less than ???3.2 b.y. old is ???3.2 times higher than that of large farside rayed craters alone. This observation can be interpreted in two ways: (1) the average cratering rate has been constant over the past 3.2 b.y. and the base of the Copernican is ???1 Ga, or (2) the cratering rate has increased in recent geologic time and the base of the Copernican is less than 1 Ga. We favor the latter interpretation because the rays of Copernicus (800-850 m.y. old) appear to be very close to optical maturity, suggesting that the average Copernican cratering rate was ???35% higher than the average Eratosthenian rate. Other lines of evidence for an increase in the Phanerozoic (545 Ga) cratering rate are (1) the densities of small craters superimposed on Copernicus and Apollo landing sites, (2) the rates estimated from well-dated terrestrial craters (??? 120 m.y.) and from present-day astronomical observations, and (3) the Proterozoic rate suggested by the crater record of Australia. The hypothesis most consistent with several key observations is that the cratering rate has increased by ???2x during the past ???300 m.y. Copyright 1997 by the American Geophysical Union.

Styles of crater gradation in Southern Ismenius Lacus, Mars

NASA Technical Reports Server (NTRS)

Grant, J. A.; Schultz, P. H.

1991-01-01

Preserved morphology around selected impact craters together with results from study of long term gradational evolution are used to assess processes responsible for crater modification in southern Ismenius Lacus. Results are compared with the gradational styles of selected terrestrial craters. Although most craters in the region display complex primary morphologies, some first order comparisons with the gradational styles around simple terrestrial craters may be valid. Nearly complete high resolution coverage provides a basis for studying morphologic features at scales comparable to those observed in LANDSAT TM images of terrestrial craters. It is concluded that the relative importance of gradational processes differs around the terrestrial and Martian craters considered here: Martian rimless morphologies are produced by mass wasting, eolian deposition/erosion, and limited fluvial incisement resulting in downwasting and significant backwasting of crater walls.

Crater Age and Hydrogen Content in Lunar Regolith from LEND Neutron Data

NASA Astrophysics Data System (ADS)

Sanin, Anton; Starr, Richard; Litvak, Maxim; Petro, Noah; Mitrofanov, Igor

2017-04-01

We are presenting an analysis of Lunar Exploration Neutron Detector (LEND) epithermal neutron count rates for a large set of mid-latitude craters. Epithermal neutron count rates for crater interiors measured by the LEND Sensor for Epithermal Neutrons (SETN) were compared to crater exteriors for 322 craters. An increase in relative count rate at about 9-sigma confidence level was found, consistent with a lower hydrogen content. A smaller subset of 31 craters, all located near three Copernican era craters, Jackson, Tycho, and Necho, also shows a significant increase in Optical Maturity parameter implying an immature regolith. The increase in SETN count rate for these craters is greater than the increase for the full set of craters by more than a factor of two.

Crater Age and Hydrogen Content in Lunar Regolith from LEND Neutron Data

NASA Technical Reports Server (NTRS)

Starr, Richard D.; Litvak, Maxim L.; Petro, Noah E.; Mitrofanov, Igor G.; Boynton, William V.; Chin, Gordon; Livengood, Timothy A.; McClanahan, Timothy P.; Sanin, Anton B.; Sagdeev, Roald Z.;

Crater gradation in Gusev crater and Meridiani Planum, Mars

NASA Astrophysics Data System (ADS)

Grant, J. A.; Arvidson, R. E.; Crumpler, L. S.; Golombek, M. P.; Hahn, B.; Haldemann, A. F. C.; Li, R.; Soderblom, L. A.; Squyres, S. W.; Wright, S. P.; Watters, W. A.

2006-01-01

The Mars Exploration Rovers investigated numerous craters in Gusev crater and Meridiani Planum during the first ~400 sols of their missions. Craters vary in size and preservation state but are mostly due to secondary impacts at Gusev and primary impacts at Meridiani. Craters at both locations are modified primarily by eolian erosion and infilling and lack evidence for modification by aqueous processes. Effects of gradation on crater form are dependent on size, local lithology, slopes, and availability of mobile sediments. At Gusev, impacts into basaltic rubble create shallow craters and ejecta composed of resistant rocks. Ejecta initially experience eolian stripping, which becomes weathering-limited as lags develop on ejecta surfaces and sediments are trapped within craters. Subsequent eolian gradation depends on the slow production of fines by weathering and impacts and is accompanied by minor mass wasting. At Meridiani the sulfate-rich bedrock is more susceptible to eolian erosion, and exposed crater rims, walls, and ejecta are eroded, while lower interiors and low-relief surfaces are increasingly infilled and buried by mostly basaltic sediments. Eolian processes outpace early mass wasting, often produce meters of erosion, and mantle some surfaces. Some small craters were likely completely eroded/buried. Craters >100 m in diameter on the Hesperian-aged floor of Gusev are generally more pristine than on the Amazonian-aged Meridiani plains. This conclusion contradicts interpretations from orbital views, which do not readily distinguish crater gradation state at Meridiani and reveal apparently subdued crater forms at Gusev that may suggest more gradation than has occurred.

Moon-Mercury: Large impact structures, isostasy and average crustal viscosity

USGS Publications Warehouse

Schaber, G.G.; Boyce, J.M.; Trask, N.J.

1977-01-01

Thirty-five craters and basins larger than 200 km in diameter are recognized on the imaged portion (45%) of Mercury. If the unimaged portion of the planet is similarly cratered, a total of 78 such impact features may be present. Sixty-two craters and basins 200 km in diameter are recognized on the moon, a body with only half the cross-sectional area of Mercury. If surface areas are considered, however, Mercury is cratered only 70% as densely as the moon. The density of impact craters with diameters greater than 400 km on Mercury is only 30% of that on the moon, and for craters with diameters between 400 and 700 km, the density on Mercury is only 21% of the lunar crater density. The size-frequency distribution curve for the large Mercurian craters follows the same cumulative -2 slope as the lunar curve but lies well below the 10% surface saturation level characteristic of the lunar curve. This is taken as evidence that the old heavily cratered terrain on Mercury is, at least presently, not in a state of cratering equilibrium. The reduced density of large craters and basins on Mercury relative to the moon could be either a function of the crater-production rates on these bodies or an effect of different crustal histories. Resurfacing of the planet after the basin-forming period is ruled out by the presence of 54 craters and basins 100 km in diameter and larger (on the imaged portion of Mercury) that have either well-defined or poorly-defined secondary-crater fields. Total isostatic compensation of impact craters ???800 km in diameter indicates that the average viscosity of the Mercurian crust over the past 4+ aeons was the same as that for the moon (???1026.5 P). This calculated viscosity and the distribution of large craters and basins suggest that either the very early crustal viscosity on Mercury was less than that of the moon and the present viscosity greater, or the differences in large crater populations on the two bodies is indeed the result of variations in rates of crater production. ?? 1977.

Modeling turbulent flows in the atmospheric boundary layer of Mars: application to Gale crater, Mars, landing site of the Curiosity rover

NASA Astrophysics Data System (ADS)

Anderson, William; Day, Kenzie; Kocurek, Gary

2016-11-01

Mars is a dry planet with a thin atmosphere. Aeolian processes - wind-driven mobilization of sediment and dust - are the exclusive mode of landscape variability on Mars. Craters are common topographic features on the surface of Mars, and many craters on Mars contain a prominent central mound (NASA's Curiosity rover was landed in Gale crater). Using density-normalized large-eddy simulations, we have modeled turbulent flows over crater-like topographies that feature a central mound. We have also run one simulation of flow over a digital elevation map of Gale crater. Resultant datasets suggest a deflationary mechanism wherein vortices shed from the upwind crater rim are realigned to conform to the crater profile via stretching and tilting. This was accomplished using three-dimensional datasets (momentum and vorticity) retrieved from LES. As a result, helical vortices occupy the inner region of the crater and, therefore, are primarily responsible for aeolian morphodynamics in the crater. We have also used the immersed-boundary method body force distribution to compute the aerodynamic surface stress on the crater. These results suggest that secondary flows - originating from flow separation at the crater - have played an important role in shaping landscape features observed in craters (including the dune fields observed on Mars, many of which are actively evolving). None.

Modeling turbulent flows in the atmospheric boundary layer of Mars: application to Gale crater, Mars, landing site of the Curiosity rover

NASA Astrophysics Data System (ADS)

Anderson, William

2017-04-01

Mars is a dry planet with a thin atmosphere. Aeolian processes - wind-driven mobilization of sediment and dust - are the exclusive mode of landscape variability on Mars. Craters are common topographic features on the surface of Mars, and many craters on Mars contain a prominent central mound (NASA's Curiosity rover was landed in Gale crater). Using density-normalized large-eddy simulations, we have modeled turbulent flows over crater-like topographies that feature a central mound. We have also run one simulation of flow over a digital elevation map of Gale crater. Resultant datasets suggest a deflationary mechanism wherein vortices shed from the upwind crater rim are realigned to conform to the crater profile via stretching and tilting. This was accomplished using three-dimensional datasets (momentum and vorticity) retrieved from LES. As a result, helical vortices occupy the inner region of the crater and, therefore, are primarily responsible for aeolian morphodynamics in the crater. We have also used the immersed-boundary method body force distribution to compute the aerodynamic surface stress on the crater. These results suggest that secondary flows - originating from flow separation at the crater - have played an important role in shaping landscape features observed in craters (including the dune fields observed on Mars, many of which are actively evolving).

What Dominates a Craters Size, the Largest Single Explosion of the Formation Process or the Cumulative Energy of Many? Results of Multiblast Crater Evolution Experiments

NASA Astrophysics Data System (ADS)

Sonder, I.; Graettinger, A. H.; Valentine, G. A.

2015-12-01

Craters of explosive volcanic eruptions are products of many explosions. Such craters are different than products of single events such as meteorite impacts or those produced by military testing because they typically result from multiple, rather than single, explosions. We analyzed the evolution of experimental craters that were created by several detonations of chemical explosives in layered aggregates. A method to calculate an effective explosion depth for non-flat topography (e.g. for explosions below existing craters) is derived, showing how multi-blast crater sizes differ from the single blast case. It is shown that sizes of natural caters (radii, volumes) are not characteristic of the number of explosions, and therefore not characteristic for the total acting energy, that formed a crater. Also the crater size is not simply related to the largest explosion in a sequence, but depends upon that explosion and the energy of that single blast and on the cumulative energy of all blasts that formed the crater. The two energies can be combined to form an effective number of explosions that is characteristic for the crater evolution. The multi-blast crater size evolution implies that it is not correct to estimate explosion energy of volcanic events from crater size using previously published relationships that were derived for single blast cases.

Lonar Lake, India: An impact Crater in basalt

USGS Publications Warehouse

Fredriksson, K.; Dube, A.; Milton, D.J.; Balasundaram, M.S.

1973-01-01

Discovery of shock-metamorphosed material establishes the impact origin of Lonar Crater. Coarse breccia with shatter coning and microbreccia with moderately shocked fragments containing maskelynite were found in drill holes through the crater floor. Trenches on the rim yield strongly shocked fragments in which plagioclase has melted and vesiculated, and bombs and spherules of homogeneous rock melt. As the only known terrestrial impact crater in basalt, Lonar Crater provides unique opportunities for comparison with lunar craters. In particular, microbreccias and glass spherules from Lonar Crater have close analogs among the Apollo specimens.

Cratering on Mars. I - Cratering and obliteration history. II Implications for future cratering studies from Mariner 4 reanalysis

NASA Technical Reports Server (NTRS)

Chapman, C. R.

1974-01-01

It is pointed out that Mars is especially well adapted to statistical studies of crater morphologies for deciphering its geological history. A framework for understanding planetary geomorphological histories from the diameter-frequency relations of different morphological classes of craters described by Chapmam et al. (1970) is extended in order to understand Martian cratering, erosional, and depositional history. The cratering-obliteration history derived is compared with global interpretations considered by Hartman (1973) and Soderblom et al. (1974). An idealized dust-filling model is employed.

Impact Craters of Venus with D Greater Than 5 km Classified Based on Degree of Preservation of the Associated Radar-Dark Deposits

NASA Technical Reports Server (NTRS)

Basilevsky, A. T.; Head, J. W.; Setyaeva, I. V.

2003-01-01

This is a further continuation of work, which studied craters greater than or equal to 30 km in diameter. That work subdivided craters based on character of the associated radar dark deposits. It was suggested and then confirmed that the most pristine deposits of that sort are radar-dark parabolas. Non-parabolic radar-dark halos represent the next stage of the deposit evolution and then with time they disappear. So presence and character of crater-associated dark deposit can be used for estimates of the crater age and then for dating other features. Previous work classified craters into: 1) craters with dark parabola (DP), 2) with clear dark halo (CH), 3) with faint halo (FH) and 4) with no dark halo (NH). It was found that abundances of craters superposed on regional plains (whose mean age is close to the planet mean surface age T) and belonging to DP, CH, FH and NH classes were correspondingly 15, 30, 30 and 25%. From that it was concluded that DP craters are not older than 0.1-0.15T; CH craters formed during the time interval from approx. 0.5T until 0.1-0.15T ago, and the FH and NH craters formed prior to approx. 0.5T ago. It was shown that the DP, CH, FH and NH percentages show only slight apparent dependence on the crater geographic latitudes and no noticeable dependence on the crater size. The present study analyzes a much larger population (all D greater than or equal to 5 km craters) to investigate better the latitude effect and to study if within this larger crater population the size effect exists.

Evidence for rapid topographic evolution and crater degradation on Mercury from simple crater morphometry

NASA Astrophysics Data System (ADS)

Fassett, Caleb I.; Crowley, Malinda C.; Leight, Clarissa; Dyar, M. Darby; Minton, David A.; Hirabayashi, Masatoshi; Thomson, Bradley J.; Watters, Wesley A.

2017-06-01

Examining the topography of impact craters and their evolution with time is useful for assessing how fast planetary surfaces evolve. Here, new measurements of depth/diameter (d/D) ratios for 204 craters of 2.5 to 5 km in diameter superposed on Mercury's smooth plains are reported. The median d/D is 0.13, much lower than expected for newly formed simple craters ( 0.21). In comparison, lunar craters that postdate the maria are much less modified, and the median crater in the same size range has a d/D ratio that is nearly indistinguishable from the fresh value. This difference in crater degradation is remarkable given that Mercury's smooth plains and the lunar maria likely have ages that are comparable, if not identical. Applying a topographic diffusion model, these results imply that crater degradation is faster by a factor of approximately two on Mercury than on the Moon, suggesting more rapid landform evolution on Mercury at all scales.