What Are the Bright Spots on Ceres?
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Impact Induced Heating of Occator Crater on Asteroid 1 Ceres
47th Lunar and Planetary Science Conference (2016) 2268.pdf IMPACT INDUCED HEATING OF OCCATOR CRATER ON ASTEROID 1 CERES. T. J. Bowling1, F. J. Ciesla1, S. Marchi2, B. C. Johnson3, T. M. Davison4, J. C. Castillo-Rogez5, M. C. De Sanctis6, C. A. Raymond5, and C. T. Russell7. 1University of Chicago, Chicago, IL ([email protected]), 2Southwest Research Institute, Boul- der, CO, 3Brown University, Providence, RI, 4Imperial College, London, UK, 5Jet Propulsion Laboratory, Caltech, Pasadena, CA, 6National Institute of Astrophysics, Rome, IT, 7University of California, Los Angeles, CA. Introduction: Dwarf planet Ceres, the current tar- H2O ice, although the inclusion of impurities may low- get of NASA’s Dawn mission and the inner solar sys- er the melting temperature considerably [16]. In both tem’s last remaining ‘wet protoplanet’, is thought to be simulations, the central peak is composed of material composed of a mixture of silicates and ices [1]. One of uplifted from considerable (15-30 km) pre-impact Ceres’ most intriguing features revealed by the Dawn depth. Because of its provenance, this material may spacecraft is the 92-km diameter crater Occator [2]. have been sheltered from heating and subsequent devo- This crater is expected to be 10s-100s Myr old and latilization from both previous impacts as well as the contains some of the highest albedo features on the Occator forming impact, and subsequently may be asteroid, which are possibly salt deposits [2]. Occa- more volatile rich than average for the crater. During tor’s longitude is also compatible with the putative the subsequent thermal evolution of the crater this un- source region for previously detected H2O outgassing altered, volatile rich material may be heated above the from Ceres [3], and may contain a diurnally periodic melting point of water by the conductive thermal pulse dust haze [2] driven by near surface volatile sublima- from the hot locus at the base of the central peak. -
Erosion of Volatiles by Micro-Meteoroid Bombardment On
Draft version April 27, 2021 Typeset using LATEX preprint style in AASTeX63 Erosion of volatiles by micro-meteoroid bombardment on Ceres, and comparison to the Moon and Mercury Petr Pokorny´ ,1, 2 Erwan Mazarico ,2 and Norbert Schorghofer 3 1The Catholic University of America, 620 Michigan Ave, NE Washington, DC 20064, USA 2Goddard Space Flight Center, 8800 Greenbelt Rd., Greenbelt, MD, 20771, USA 3Planetary Science Institute, Tucson, AZ 85719, USA (Received December 11, 2020; Revised March 15, 2021; Accepted March 16, 2021) Accepted to PSJ ABSTRACT (1) Ceres, the largest reservoir of water in the main-belt, was recently visited by the Dawn spacecraft that revealed several areas bearing H2O-ice features. Independent tele- scopic observations showed a water exosphere of currently unknown origin. We explore the effects of meteoroid impacts on Ceres considering the topography obtained from the Dawn mission using a widely-used micro-meteoroid model and ray-tracing tech- niques. Meteoroid populations with 0.01-2 mm diameters are considered. We analyze the short-term effects Ceres experiences during its current orbit as well as long-term effects over the entire precession cycle. We find the entire surface is subject to mete- oroid bombardment leaving no areas in permanent shadow with respect to meteoroid influx. The equatorial parts of Ceres produce 80% more ejecta than the polar regions due to the large impact velocity of long-period comets. Mass flux, energy flux, and ejecta production vary seasonally by a factor of 3{7 due to the inclined eccentric orbit. Compared to Mercury and the Moon, Ceres experiences significantly smaller effects of micro-meteoroid bombardment, with a total mass flux of 4:5 ± 1:2 × 10−17 kg m−2 s−1. -
NASA Spacecraft Nears Encounter with Dwarf Planet Ceres 4 March 2015
NASA spacecraft nears encounter with dwarf planet Ceres 4 March 2015 of 590 miles (950 kilometers), makes a full rotation every nine hours, and NASA is hoping for a wealth of data once the spacecraft's orbit begins. "Dawn is about to make history," said Robert Mase, project manager for the Dawn mission at NASA JPL in Pasadena, California. "Our team is ready and eager to find out what Ceres has in store for us." Experts will be looking for signs of geologic activity, via changes in these bright spots, or other features on Ceres' surface over time. The latest images came from Dawn when it was 25,000 miles (40,000 kilometers) away on February 25. This image was taken by NASA's Dawn spacecraft of dwarf planet Ceres on February 19, 2015 from a The celestial body was first spotted by Sicilian distance of nearly 29,000 miles astronomer Father Giuseppe Piazzi in 1801. "Ceres was initially classified as a planet and later called an asteroid. In recognition of its planet-like A NASA spacecraft called Dawn is about to qualities, Ceres was designated a dwarf planet in become the first mission to orbit a dwarf planet 2006, along with Pluto and Eris," NASA said. when it slips into orbit Friday around Ceres, the most massive body in the asteroid belt. Ceres is named after the Roman goddess of agriculture and harvests. The mission aims to shed light on the origins of the solar system 4.5 billion years ago, from its "rough The spacecraft on its way to circle it was launched and tumble environment of the main asteroid belt in September 2007. -
Comparative Kbology: Using Surface Spectra of Triton
COMPARATIVE KBOLOGY: USING SURFACE SPECTRA OF TRITON, PLUTO, AND CHARON TO INVESTIGATE ATMOSPHERIC, SURFACE, AND INTERIOR PROCESSES ON KUIPER BELT OBJECTS by BRYAN JASON HOLLER B.S., Astronomy (High Honors), University of Maryland, College Park, 2012 B.S., Physics, University of Maryland, College Park, 2012 M.S., Astronomy, University of Colorado, 2015 A thesis submitted to the Faculty of the Graduate School of the University of Colorado in partial fulfillment of the requirement for the degree of Doctor of Philosophy Department of Astrophysical and Planetary Sciences 2016 This thesis entitled: Comparative KBOlogy: Using spectra of Triton, Pluto, and Charon to investigate atmospheric, surface, and interior processes on KBOs written by Bryan Jason Holler has been approved for the Department of Astrophysical and Planetary Sciences Dr. Leslie Young Dr. Fran Bagenal Date The final copy of this thesis has been examined by the signatories, and we find that both the content and the form meet acceptable presentation standards of scholarly work in the above mentioned discipline. ii ABSTRACT Holler, Bryan Jason (Ph.D., Astrophysical and Planetary Sciences) Comparative KBOlogy: Using spectra of Triton, Pluto, and Charon to investigate atmospheric, surface, and interior processes on KBOs Thesis directed by Dr. Leslie Young This thesis presents analyses of the surface compositions of the icy outer Solar System objects Triton, Pluto, and Charon. Pluto and its satellite Charon are Kuiper Belt Objects (KBOs) while Triton, the largest of Neptune’s satellites, is a former member of the KBO population. Near-infrared spectra of Triton and Pluto were obtained over the previous 10+ years with the SpeX instrument at the IRTF and of Charon in Summer 2015 with the OSIRIS instrument at Keck. -
New Animation Takes a Colorful Flight Over Ceres 29 January 2016
New animation takes a colorful flight over Ceres 29 January 2016 "The simulated overflight shows the wide range of crater shapes that we have encountered on Ceres. The viewer can observe the sheer walls of the crater Occator, and also Dantu and Yalode, where the craters are a lot flatter," said Ralf Jaumann, a Dawn mission scientist at DLR. Dawn is the first mission to visit Ceres, the largest object in the main asteroid belt between Mars and Jupiter. After orbiting asteroid Vesta for 14 months in 2011 and 2012, Dawn arrived at Ceres in March 2015. The spacecraft is currently in its final and lowest mapping orbit, at about 240 miles (385 Occator Crater (57 miles, 92 kilometers) on Ceres, home kilometers) from the surface. of the brightest spots on the dwarf planet, in a simulated view using Dawn images. Credit: NASA/JPL- Caltech/UCLA/MPS/DLR/IDA Provided by NASA A colorful new animation shows a simulated flight over the surface of dwarf planet Ceres, based on images from NASA's Dawn spacecraft. The movie shows Ceres in enhanced color, which helps to highlight subtle differences in the appearance of surface materials. Scientists believe areas with shades of blue contain younger, fresher material, including flows, pits and cracks. The animated flight over Ceres emphasizes the most prominent craters, such as Occator, and the tall, conical mountain Ahuna Mons. Features on Ceres are named for earthly agricultural spirits, deities and festivals. The movie was produced by members of Dawn's framing camera team at the German Aerospace Center, DLR, using images from Dawn's high- altitude mapping orbit. -
The Evolution of Occator Crater and Its Faculae Revealed by Highest Resolution Observations of Ceres
50th Lunar and Planetary Science Conference 2019 (LPI Contrib. No. 2132) 1619.pdf THE EVOLUTION OF OCCATOR CRATER AND ITS FACULAE REVEALED BY HIGHEST RESOLUTION OBSERVATIONS OF CERES. J.E.C. Scully1, P.M. Schenk2, D.A. Williams3, D.L. Buczkowski4, J.H. Pasckert5, K.D. Duarte6, V.N. Romero6, M.M. Sori7, M. Landis8, L.C. Quick9, B.E. Schmidt6, C.A. Raymond1, J.C. Castillo-Rogez1, C.T. Russell10, 1Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA, 2LPI, Houston, TX, USA, 3ASU, Tempe, AZ, USA, 4JHU-APL, Laurel, MD, USA, 5Institute für Planetologie, WWU Mün- ster, Germany, 6Georgia Institute of Technology, Atlanta, GA, USA, 7LPI, Tucson, AZ, USA, 8PSI, Tucson, AZ, USA, 9National Air & Space Museum, Smithsonian Institution, Washington DC, USA, 10UCLA, Los Angeles, CA, USA. Introduction: The Dawn mission explored Ceres, interior before solidifying [6,9]. It is apparent from the the largest object in the asteroid belt, from 2015-2018 XM2 data that the lobate material coats almost the entire [1]. Occator crater (92 km diameter) contains enigmatic crater interior. While the large, thick sheet (label a in interior bright regions, named Cerealia Facula and Vi- figure) and smaller, isolated, pond-like deposits of lo- nalia Faculae. The faculae are six times brighter than bate material were observed in pre-XM2 data, the thin- Ceres’ average [2], are mostly sodium carbonate [3] and ner veneer of lobate material that coats the majority of are only a few millions of years old [4]. the terraces and the crater floor is only clearly visible in Previous Work: A special issue of Icarus sought to the XM2 images (label b in figure). -
Nasa Planetary Mission Concept Study: Assessing Dwarf Planet Ceres’ Past and Present Habitability Potential
NASA PLANETARY MISSION CONCEPT STUDY: ASSESSING DWARF PLANET CERES’ PAST AND PRESENT HABITABILITY POTENTIAL. J. C. Castillo-Rogez1, M. T. Bland2, D. L. Buczkowski3, A. R. Hen- drix4, K. E. Miller5, T. H. Prettyman4, L.C. Quick6, J. E. C. Scully1, Y. Sekine7, M. M. Sori8,9, T. Titus2, D. A. Wil- liams10, H. Yano11, M. Zolensky12, C. A. Raymond1, J. Brophy1, W. Frazier1, G. Lantoine1, B. G. Lee1, M. S. Kelley13, 1Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA. 2United States Geological Sur- vey, Flagstaff, AZ. 3John Hopkins University, Applied Physics Laboratory, Laurel, MD. 4Planetary Science Institute. 5Southwest Research Institute, San Antonio, TX. 6NASA Goddard Space Flight Center, Greenbelt, MD. 7Earth-Life Science Institute, Tokyo Institute of Technology, Tokyo, Japan. 8Lunar and Planetary Laboratory, University of Ari- zona, Tucson, AZ. 9Purdue University, West Lafayette, IN. 10School of Earth and Space Exploration, Arizona State University, Phoenix, AZ. 11Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Kana- gawa, Japan. 12Astromaterials Research and Exploration Science, NASA Johnson Space Center, Houston, TX. 13NASA Headquarters, Washington, DC. Email: [email protected]. Introduction: The Dawn mission revolutionized ical evolution. While the latter goal does not directly re- our understanding of Ceres during the same decade that late to ROW, it addresses the place of Ceres in the early has also witnessed the rise of ocean worlds as a research solar system and its potential connection to other large and exploration focus. We will report progress on the dwarf planets. Planetary Mission Concept Study (PMCS) on the future Future exploration of Ceres would reveal the de- exploration of Ceres under the New Frontiers or Flag- gree to which liquid water and other environmental fac- ship program that was selected for NASA funding in tors may have combined to make this dwarf planet a October 2019. -
Mineralogy of the Occator Quadrangle
Icarus 318 (2019) 205–211 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Mineralogy of the Occator quadrangle ∗ A. Longobardo a, , E. Palomba a,b, F.G. Carrozzo a, A. Galiano a, M.C. De Sanctis a, K. Stephan c, F. Tosi a, A. Raponi a, M. Ciarniello a, F. Zambon a, A. Frigeri a, E. Ammannito d, C.A. Raymond e, C.T. Russell f a INAF-IAPS, via Fosso del Cavaliere 100, I-00133 Rome, Italy b ASI-ASDC, via del Politecnico snc, I-00133 Rome, Italy c Institute for Planetary Research, Deutsches Zentrum fur Luft- und Raumfahrt (DLR), D-12489 Berlin, Germany d ASI-URS, via del Politecnico snc, I-00133 Rome, Italy e California Institute of Technology, JPL, 91109 Pasadena, CA, USA f UCLA, Los Angeles, CA 90095, USA a r t i c l e i n f o a b s t r a c t Article history: We present an analysis of the areal distribution of spectral parameters derived from the VIR imaging Received 28 April 2017 spectrometer on board NASA/Dawn spacecraft. Specifically we studied the Occator quadrangle of Ceres, Revised 11 September 2017 which is bounded by latitudes 22 °S to 22 °N and longitudes 214 °E to 288 °E, as part of the overall study Accepted 18 September 2017 of Ceres’ surface composition reported in this special publication. The spectral parameters used are the Available online 22 September 2017 photometrically corrected reflectance at 1.2 μm, the infrared spectral slope (1.1–1.9 μm), and depths of Keywords: the absorption bands at 2.7 μm and 3.1 μm that are ascribed to hydrated and ammoniated materials, Asteroid ceres respectively. -
Ceres: Astrobiological Target and Possible Ocean World
ASTROBIOLOGY Volume 20 Number 2, 2020 Research Article ª Mary Ann Liebert, Inc. DOI: 10.1089/ast.2018.1999 Ceres: Astrobiological Target and Possible Ocean World Julie C. Castillo-Rogez,1 Marc Neveu,2,3 Jennifer E.C. Scully,1 Christopher H. House,4 Lynnae C. Quick,2 Alexis Bouquet,5 Kelly Miller,6 Michael Bland,7 Maria Cristina De Sanctis,8 Anton Ermakov,1 Amanda R. Hendrix,9 Thomas H. Prettyman,9 Carol A. Raymond,1 Christopher T. Russell,10 Brent E. Sherwood,11 and Edward Young10 Abstract Ceres, the most water-rich body in the inner solar system after Earth, has recently been recognized to have astrobiological importance. Chemical and physical measurements obtained by the Dawn mission enabled the quantification of key parameters, which helped to constrain the habitability of the inner solar system’s only dwarf planet. The surface chemistry and internal structure of Ceres testify to a protracted history of reactions between liquid water, rock, and likely organic compounds. We review the clues on chemical composition, temperature, and prospects for long-term occurrence of liquid and chemical gradients. Comparisons with giant planet satellites indicate similarities both from a chemical evolution standpoint and in the physical mechanisms driving Ceres’ internal evolution. Key Words: Ceres—Ocean world—Astrobiology—Dawn mission. Astro- biology 20, xxx–xxx. 1. Introduction these bodies, that is, their potential to produce and maintain an environment favorable to life. The purpose of this article arge water-rich bodies, such as the icy moons, are is to assess Ceres’ habitability potential along the same lines Lbelieved to have hosted deep oceans for at least part of and use observational constraints returned by the Dawn their histories and possibly until present (e.g., Consolmagno mission and theoretical considerations. -
The Formation and Evolution of the Bright Faculae in Occator Crater on Ceres
The Formation And Evolution Of The Bright Faculae In Occator Crater On Ceres Jennifer SCULLY1#+, Debra BUCZKOWSKI2, Paul SCHENK3, Adrian NEESEMANN4, Carol RAYMOND5, Christopher RUSSELL6, Michael BLAND7, Julie CASTILLO-ROGEZ5, Lynnae QUICK8, Ottaviano RUESCH9, Britney SCHMIDT10 1 JPL/Caltech, United States, 2 Johns Hopkins University, United States, 3 Universities Space Research Association, United States, 4 Freie Universitaet Berlin, Germany, 5 California Institute of Technology, United States, 6 University of California, Los Angeles, United States, 7 United States Geological Survey, United States, 8 Planetary Science Institute, United States, 9 NASA Goddard Space Flight Center/Oak Ridge Associated Universities, United States, 10 Georgia Institute of Technology, United States #Corresponding author: [email protected] +Presenter Ceres is a 940-km-diameter dwarf planet, located in the main asteroid belt. Since 2015, NASA’s Dawn spacecraft has orbited Ceres, and observed bright regions on the mostly dark surface. The brightest regions are in the 92-km-diameter Occator crater, which are approximately seven times brighter than average Ceres, as defined by their single scattering albedo (Russell et al., 2016; Li et al., 2016). The central bright region in Occator crater, called the Cerealia Facula, is located in a ~9 km wide and ~700 m deep central pit (e.g. Schenk et al., 2016). There are also bright regions in the eastern floor of Occator crater, called the Vinalia Faculae. Geologic mapping reveals that the faculae belong to a type of geologic material that is unique on Ceres, and that they are associated with the central pit and fractures in the floor of Occator crater (Scully et al., 2017; Buczkowski et al., 2017). -
Dramatic Clips: the Mystery Bright Spots on Ceres in the Astroid Belt
Dramatic Clips: The Mystery Bright Spots On Ceres in the Astroid Belt By Washington's Blog Theme: Science and Medicine Global Research, May 16, 2015 Washington's Blog NASA’s Dawn spacecraft flew by thedwarf planet Ceres this week. Located between Mars and Jupiter, Ceres is the largest object in the asteroid belt. Dawn took some stunning pictures. NASA’s Jet Propulsion Laboratory made an animation from the images: Then ZLD zeroed in on the bright spots so we could get a good look: | 1 Scientists are still trying to figure out what’s causing the bright spots … theories being floated are ice, salt, etc. What do you think the bright spots are: Ice? Salt? Alien disco party? Death Star being powered up? Update: The new flyby images are making scientists lean towards plain oldwater ice (as opposed to nastier frozen substances which have been found on other planets). The original source of this article is Washington's Blog Copyright © Washington's Blog, Washington's Blog, 2015 Comment on Global Research Articles on our Facebook page Become a Member of Global Research Articles by: Washington's Blog Disclaimer: The contents of this article are of sole responsibility of the author(s). The Centre for Research on Globalization will not be responsible for any inaccurate or incorrect statement in this article. The Centre of Research on Globalization grants permission to cross-post Global Research articles on community internet sites as long the source and copyright are acknowledged together with a hyperlink to the original Global Research article. For publication of Global Research articles in print or other forms including commercial internet sites, contact: [email protected] www.globalresearch.ca contains copyrighted material the use of which has not always been specifically authorized by the copyright owner. -
Comparative Kbology: Using Surface Spectra of Triton, Pluto, and Charon
COMPARATIVE KBOLOGY: USING SURFACE SPECTRA OF TRITON, PLUTO, AND CHARON TO INVESTIGATE ATMOSPHERIC, SURFACE, AND INTERIOR PROCESSES ON KUIPER BELT OBJECTS by BRYAN JASON HOLLER B.S., Astronomy (High Honors), University of Maryland, College Park, 2012 B.S., Physics, University of Maryland, College Park, 2012 M.S., Astronomy, University of Colorado, 2015 A thesis submitted to the Faculty of the Graduate School of the University of Colorado in partial fulfillment of the requirement for the degree of Doctor of Philosophy Department of Astrophysical and Planetary Sciences 2016 This thesis entitled: Comparative KBOlogy: Using spectra of Triton, Pluto, and Charon to investigate atmospheric, surface, and interior processes on KBOs written by Bryan Jason Holler has been approved for the Department of Astrophysical and Planetary Sciences Dr. Leslie Young Dr. Fran Bagenal Date The final copy of this thesis has been examined by the signatories, and we find that both the content and the form meet acceptable presentation standards of scholarly work in the above mentioned discipline. ii ABSTRACT Holler, Bryan Jason (Ph.D., Astrophysical and Planetary Sciences) Comparative KBOlogy: Using spectra of Triton, Pluto, and Charon to investigate atmospheric, surface, and interior processes on KBOs Thesis directed by Dr. Leslie Young This thesis presents analyses of the surface compositions of the icy outer Solar System objects Triton, Pluto, and Charon. Pluto and its satellite Charon are Kuiper Belt Objects (KBOs) while Triton, the largest of Neptune’s satellites, is a former member of the KBO population. Near-infrared spectra of Triton and Pluto were obtained over the previous 10+ years with the SpeX instrument at the IRTF and of Charon in Summer 2015 with the OSIRIS instrument at Keck.