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Io in the Near Infrared: Near-Infrared Mapping Spectrometer (NIMS) Results from the Galileo Tlybys in 1999 and 2000 Rosaly M
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 106, NO. El2, PAGES 33,053-33,078, DECEMBER 25, 2001 Io in the near infrared: Near-Infrared Mapping Spectrometer (NIMS) results from the Galileo tlybys in 1999 and 2000 Rosaly M. C. Lopes,• L. W. Kamp,• S. Dout6,2 W. D. Smythe,• R. W. Carlson,• A. S. McEwen, 3 P. E. Geissler,3 S. W. Kieffer, 4 F. E. Leader, s A. G. Davies, • E. Barbinis,• R. Mehlman,s M. Segura,• J. Shirley,• and L. A. Soderblom6 Abstract. Galileo'sNear-Infrared Mapping Spectrometer(NIMS) observedIo duringthe spacecraft'sthree flybysin October 1999, November 1999, and February 2000. The observations,which are summarizedhere, were used to map the detailed thermal structure of activevolcanic regions and the surfacedistribution of SO2 and to investigatethe origin of a yet unidentified compoundshowing an absorptionfeature at ---1 •m. We present a summaryof the observationsand results,focusing on the distributionof thermal emission and of SO2 deposits.We find high eruption temperatures,consistent with ultramafic volcanism,at Pele. Such temperaturesmay be present at other hot spots,but the hottest areas may be too small for those temperaturesto be detected at the spatial resolutionof our observations.Loki is the site of frequent eruptions,and the low thermal emissionmay representlavas cooling on the caldera'ssurface or the coolingcrust of a lava lake. High- resolutionspectral observations of Emakong caldera show thermal emissionand SO2 within the same pixels,implying that patchesof SO2 frost and patchesof coolinglavas or sulfur flows are presentwithin a few kilometersfrom one another. Thermal maps of Prometheusand Amirani showthat these two hot spotsare characterizedby long lava flows.The thermal profilesof flows at both locationsare consistentwith insulatedflows, with the Amirani flow field havingmore breakoutsof fresh lava along its length. -
New Voyage to Rendezvous with a Small Asteroid Rotating with a Short Period
Hayabusa2 Extended Mission: New Voyage to Rendezvous with a Small Asteroid Rotating with a Short Period M. Hirabayashi1, Y. Mimasu2, N. Sakatani3, S. Watanabe4, Y. Tsuda2, T. Saiki2, S. Kikuchi2, T. Kouyama5, M. Yoshikawa2, S. Tanaka2, S. Nakazawa2, Y. Takei2, F. Terui2, H. Takeuchi2, A. Fujii2, T. Iwata2, K. Tsumura6, S. Matsuura7, Y. Shimaki2, S. Urakawa8, Y. Ishibashi9, S. Hasegawa2, M. Ishiguro10, D. Kuroda11, S. Okumura8, S. Sugita12, T. Okada2, S. Kameda3, S. Kamata13, A. Higuchi14, H. Senshu15, H. Noda16, K. Matsumoto16, R. Suetsugu17, T. Hirai15, K. Kitazato18, D. Farnocchia19, S.P. Naidu19, D.J. Tholen20, C.W. Hergenrother21, R.J. Whiteley22, N. A. Moskovitz23, P.A. Abell24, and the Hayabusa2 extended mission study group. 1Auburn University, Auburn, AL, USA ([email protected]) 2Japan Aerospace Exploration Agency, Kanagawa, Japan 3Rikkyo University, Tokyo, Japan 4Nagoya University, Aichi, Japan 5National Institute of Advanced Industrial Science and Technology, Tokyo, Japan 6Tokyo City University, Tokyo, Japan 7Kwansei Gakuin University, Hyogo, Japan 8Japan Spaceguard Association, Okayama, Japan 9Hosei University, Tokyo, Japan 10Seoul National University, Seoul, South Korea 11Kyoto University, Kyoto, Japan 12University of Tokyo, Tokyo, Japan 13Hokkaido University, Hokkaido, Japan 14University of Occupational and Environmental Health, Fukuoka, Japan 15Chiba Institute of Technology, Chiba, Japan 16National Astronomical Observatory of Japan, Iwate, Japan 17National Institute of Technology, Oshima College, Yamaguchi, Japan 18University of Aizu, Fukushima, Japan 19Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA 20University of Hawai’i, Manoa, HI, USA 21University of Arizona, Tucson, AZ, USA 22Asgard Research, Denver, CO, USA 23Lowell Observatory, Flagstaff, AZ, USA 24NASA Johnson Space Center, Houston, TX, USA 1 Highlights 1. -
The Pulse of the Volcano: Discovery of Episodic Activity at Prometheus on Io
Lunar and Planetary Science XXXIV (2003) 1455.pdf THE PULSE OF THE VOLCANO: DISCOVERY OF EPISODIC ACTIVITY AT PROMETHEUS ON IO. A. G. Da- vies. Jet Propulsion Laboratory-California Institute of Technology, ms 183-601, 4800 Oak Grove Drive, Pasadena, CA 91109-8099. (tel: 818-393-1775. email: [email protected]). Introduction: The temporal behaviour of thermal est e-corrected thermal emission during November 1997 output from a volcano yields valuable clues to the pro- (33 GW/µm), more than four times that seen in June cesses taking place at and beneath the surface. Galileo 1996 (orbit G1; see [3]) and Amirani showed its greatest Near Infrared Mapping Spectrometer (NIMS) data show thermal emission (up to May 1998) during May 1997 that the ionian volcanoes Prometheus and Amirani (orbit G8), nearly 100 GW/µm, nearly five times that have significant thermal emission in excess of non- seen during orbit G1. Including observations where e > volcanic background emission in every geometrically 60º, Amirani’s maximum observed 5 µm output is 291 appropriate NIMS observation. The 5 µm brightness of GW/µm (May 1998), and the Prometheus maximum is 54 these volcanoes shows considerable variation from GW/µm (May 1998). orbit to orbit. Prometheus in particular exhibits an epi- sodicity that yields valuable constraints to the mecha- x = time between peaks in months nisms of magma supply and eruption. This work is part 60 of an on-going study to chart and quantify the thermal 50 emission of Io’s volcanoes, determine mass eruption 9 rates, and note eruption style. -
POSTER SESSION I: CERES: MISSION RESULTS from DAWN 6:00 P.M
Lunar and Planetary Science XLVIII (2017) sess312.pdf Tuesday, March 21, 2017 [T312] POSTER SESSION I: CERES: MISSION RESULTS FROM DAWN 6: 00 p.m. Town Center Exhibit Area Russell C. T. Raymond C. A. De Sanctis M. C. Nathues A. Prettyman T. H. et al. POSTER LOCATION #171 Dawn at Ceres: What We Have Learned [#1269] A summary of the major discoveries and their implications at the close of the exploration of Ceres by Dawn. Ermakov A. I. Park R. S. Zuber M. T. Smith D. E. Fu R. R. et al. POSTER LOCATION #172 Regional Analysis of Ceres’ Gravity Anomalies [#1374] Put in geological and geomorphological context, the regional gravity anomalies give clues on the structure and evolution of Ceres’ crust. Nathues A. Platz T. Thangjam G. Hoffmann M. Mengel K. et al. POSTER LOCATION #173 Evolution of Occator Crater on (1) Ceres [#1385] We present recent results on the origin and evolution of the bright spots (Cerealia and Vinalia Faculae) at crater Occator on (1) Ceres. Buczkowski D. L. Scully J. E. C. Schenk P. M. Ruesch O. von der Gathen I. et al. POSTER LOCATION #174 Tectonic Analysis of Fracturing Associated with Occator Crater [#1488] The floor, walls, and ejecta of Occator Crater on Ceres are cut by multiple sets of linear and concentric fractures. We explore possible formation mechanisms. Pasckert J. H. Hiesinger H. Raymond C. A. Russell C. POSTER LOCATION #175 Degradation and Ejecta Mobility of Impact Craters on Ceres [#1377] We investigated the degradation and ejecta mobility of craters on Ceres, to investigate latitudinal variations, and to compare it with other planetary bodies. -
Icarus 316 (2018) 63–83
Icarus 316 (2018) 63–83 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus The Ac-5 (Fejokoo) quadrangle of Ceres: Geologic map and geomorphological evidence for ground ice me diate d surface processes ∗ Kynan H.G. Hughson a, , C.T. Russell a, D.A. Williams b, D.L. Buczkowski c, S.C. Mest d, J.H. Pasckert e, J.E.C. Scully f, J.-P. Combe g, T. Platz d,h, O. Ruesch i, F. Preusker j, R. Jaumann j, A. Nass j, T. Roatsch j, A. Nathues h, M. Schaefer h, B.E. Schmidt k, H.T. Chilton k, A. Ermakov f, S. Singh g, L.A. McFadden i, C.A. Raymond f a Department of Earth, Planetary, and Space Sciences, University of California Los Angeles, 595 Charles E. Young Drive East, Los Angeles, CA 90095, USA b School of Earth and Space Exploration, Arizona State University, PO Box 871404, Tempe, AZ 85287-1404, USA c Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Rd, Laurel, MD 20723, USA d Planetary Science Institute, 1700 E Fort Lowell Rd # 106, Tucson, AZ 85719, USA e University of Münster, Schlossplatz 2, 48149 Münster, Germany f Jet Propulsion Laboratory, 4800 Oak Grove Dr, Pasadena, CA 91109, USA g Bear Fight Institute, 22 Fiddler’s Rd, Winthrop, WA 98862, USA h Max Planck Institute for Solar System Research, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany i NASA Goddard Space Flight Center, 8800 Greenbelt Rd, Greenbelt, MD 20771, USA j German Aerospace Center (DLR), Friedrichstraße 171, 10117 Berlin, Germany k School of Earth ans Atmospheric Sciences, Georgia Institute of Technology, 311 Ferst Dr, Atlanta, GA 30318, USA a r t i c l e i n f o a b s t r a c t Article history: NASA’s Dawn spacecraft arrived at Ceres on March 6, 2015, and has been studying the dwarf planet Received 10 August 2016 through a series of successively lower orbits. -
Ceres Survey Atlas Derived from Dawn Framing Camera Images
Planetary and Space Science ∎ (∎∎∎∎) ∎∎∎–∎∎∎ Contents lists available at ScienceDirect Planetary and Space Science journal homepage: www.elsevier.com/locate/pss Ceres Survey Atlas derived from Dawn Framing Camera images Th. Roatsch a,n, E. Kersten a, K.-D. Matz a, F. Preusker a, F. Scholten a, R. Jaumann a, C.A. Raymond b, C.T. Russell c a Institute of Planetary Research, German Aerospace Center (DLR), Berlin, Germany b Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA c Institute of Geophysics, UCLA, Los Angeles, CA, USA article info abstract Article history: The Dawn Framing Camera (FC) acquired almost 900 clear filter images of Ceres with a resolution of Received 10 November 2015 about 400 m/pixels during the seven cycles in the Survey orbit in June 2015. We ortho-rectified 42 Received in revised form images from the third cycle and produced a global, high-resolution, controlled mosaic of Ceres. This 26 November 2015 global mosaic is the basis for a high-resolution Ceres atlas that consists of 3 tiles mapped at a scale of Accepted 16 December 2015 1:2,000,000. The nomenclature used in this atlas was proposed by the Dawn team and was approved by the International Astronomical Union (IAU). The whole atlas is available to the public through the Dawn Keywords: GIS web page [http://dawn_gis.dlr.de/atlas]. Dawn & 2015 Elsevier Ltd. All rights reserved. Ceres Dwarf planets Planetary mapping 1. Introduction followed by the radiometric calibration of the images (Schröder et al., 2013,2014). The Dawn mission has mapped Ceres during the Survey orbit The next step towards the cartographic products is to ortho- phase from an altitude of 4424 km (Russell and Raymond, 2011)in rectify the images to the proper scale and map projection type. -
Appendix 1: Io's Hot Spots Rosaly M
Appendix 1: Io's hot spots Rosaly M. C. Lopes,Jani Radebaugh,Melissa Meiner,Jason Perry,and Franck Marchis Detections of plumes and hot spots by Galileo, Voyager, HST, and ground-based observations. Notes and sources . (N) NICMOS hot spots detected by Goguen etal . (1998). (D) Hot spots detected by C. Dumas etal . in 1997 and/or 1998 (pers. commun.). Keck are hot spots detected by de Pater etal . (2004) and Marchis etal . (2001) from the Keck telescope using Adaptive Optics. (V, G, C) indicate Voyager, Galileo,orCassini detection. Other ground-based hot spots detected by Spencer etal . (1997a). Galileo PPR detections from Spencer etal . (2000) and Rathbun etal . (2004). Galileo SSIdetections of hot spots, plumes, and surface changes from McEwen etal . (1998, 2000), Geissler etal . (1999, 2004), Kezthelyi etal. (2001), and Turtle etal . (2004). Galileo NIMS detections prior to orbit C30 from Lopes-Gautier etal . (1997, 1999, 2000), Lopes etal . (2001, 2004), and Williams etal . (2004). Locations of surface features are approximate center of caldera or feature. References de Pater, I., F. Marchis, B. A. Macintosh, H. G. Rose, D. Le Mignant, J. R. Graham, and A. G. Davies. 2004. Keck AO observations of Io in and out of eclipse. Icarus, 169, 250±263. 308 Appendix 1: Io's hot spots Goguen, J., A. Lubenow, and A. Storrs. 1998. HST NICMOS images of Io in Jupiter's shadow. Bull. Am. Astron. Assoc., 30, 1120. Geissler, P. E., A. S. McEwen, L. Keszthelyi, R. Lopes-Gautier, J. Granahan, and D. P. Simonelli. 1999. Global color variations on Io. Icarus, 140(2), 265±281. -
March 21–25, 2016
FORTY-SEVENTH LUNAR AND PLANETARY SCIENCE CONFERENCE PROGRAM OF TECHNICAL SESSIONS MARCH 21–25, 2016 The Woodlands Waterway Marriott Hotel and Convention Center The Woodlands, Texas INSTITUTIONAL SUPPORT Universities Space Research Association Lunar and Planetary Institute National Aeronautics and Space Administration CONFERENCE CO-CHAIRS Stephen Mackwell, Lunar and Planetary Institute Eileen Stansbery, NASA Johnson Space Center PROGRAM COMMITTEE CHAIRS David Draper, NASA Johnson Space Center Walter Kiefer, Lunar and Planetary Institute PROGRAM COMMITTEE P. Doug Archer, NASA Johnson Space Center Nicolas LeCorvec, Lunar and Planetary Institute Katherine Bermingham, University of Maryland Yo Matsubara, Smithsonian Institute Janice Bishop, SETI and NASA Ames Research Center Francis McCubbin, NASA Johnson Space Center Jeremy Boyce, University of California, Los Angeles Andrew Needham, Carnegie Institution of Washington Lisa Danielson, NASA Johnson Space Center Lan-Anh Nguyen, NASA Johnson Space Center Deepak Dhingra, University of Idaho Paul Niles, NASA Johnson Space Center Stephen Elardo, Carnegie Institution of Washington Dorothy Oehler, NASA Johnson Space Center Marc Fries, NASA Johnson Space Center D. Alex Patthoff, Jet Propulsion Laboratory Cyrena Goodrich, Lunar and Planetary Institute Elizabeth Rampe, Aerodyne Industries, Jacobs JETS at John Gruener, NASA Johnson Space Center NASA Johnson Space Center Justin Hagerty, U.S. Geological Survey Carol Raymond, Jet Propulsion Laboratory Lindsay Hays, Jet Propulsion Laboratory Paul Schenk, -
Oxo Crater on (1) Ceres: Geological History and the Role of Water-Ice
The Astronomical Journal, 154:84 (13pp), 2017 September https://doi.org/10.3847/1538-3881/aa7a04 © 2017. The American Astronomical Society. All rights reserved. Oxo Crater on (1) Ceres: Geological History and the Role of Water-ice A. Nathues1, T. Platz1, M. Hoffmann1, G. Thangjam1, E. A. Cloutis2, D. M. Applin2, L. Le Corre1,3, V. Reddy1,4, K. Mengel5, S. Protopapa6, D. Takir7, F. Preusker8, B. E. Schmidt9, and C. T. Russell10 1 Max Planck Institute for Solar System Research, Justus-von-Liebig-Weg 3, D-37077 Goettingen, Germany; [email protected] 2 University of Winnipeg, Winnipeg, MB R3B 2E9, Canada 3 Planetary Science Institute, 1700 East Fort Lowell Rd, Suite 106, Tucson, AZ 85719-2395, USA 4 Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA 5 IELF, TU Clausthal, Adolph-Roemer-Straße 2A, D-38678 Clausthal-Zellerfeld, Germany 6 University of Maryland, Department of Astronomy, College Park, MD 20742, USA 7 SETI Institute, Mountain View, CA 94043, USA 8 German Aerospace Center (DLR), Institute of Planetary Research, D-12489 Berlin, Germany 9 Georgia Institute of Technology, Atlanta, GA, USA 10 Institute of Geophysics and Planetary Physics, Dept. of Earth, Planetary and Space Sciences, University of California Los Angeles, Los Angeles, CA, USA Received 2017 March 1; revised 2017 June 14; accepted 2017 June 14; published 2017 August 4 Abstract Dwarf planet Ceres (∅∼940 km) is the largest object in the main asteroid belt. Investigations suggest that Ceres is a thermally evolved, volatile-rich body with potential geological activity, a body that was never completely molten, but one that possibly partially differentiated into a rocky core and an ice-rich mantle, and may contain remnant internal liquid water. -
THE PLANETARY REPORT JUNE SOLSTICE 2016 VOLUME 36, NUMBER 2 Planetary.Org
THE PLANETARY REPORT JUNE SOLSTICE 2016 VOLUME 36, NUMBER 2 planetary.org ILLUMINATING CERES DAWN SHEDS NEW LIGHT ON AN ENIGMATIC WORLD BREAKTHROUGH STARSHOT C LIGHTSAIL 2 TEST C MEMBERSHIP UPGRADES SNAPSHOTS FROM SPACE EMILY STEWART LAKDAWALLA blogs at planetary.org/blog. Black Sands of Mars ON SOL 1192 (December 13, 2015), Curiosity approached the side of Namib, a Faccin and Marco Bonora Image: NASA/JPL/MSSS/Elisabetta massive barchan sand dune. Namib belongs to a field of currently active dark basaltic sand dunes that form a long barrier between the rover and the tantalizing rocks of Mount Sharp. This view, processed by Elisabetta Bonora and Marco Faccin, features wind-carved yardangs (crests or ridges ) of Mount Sharp in the background. After taking this set of photos, Curiosity went on to sample sand from the dune, and it is now working its way through a gap in the dune field on the way to the mountain. —Emily Stewart Lakdawalla SEE MORE AMATEUR-PROCESSED SPACE IMAGES planetary.org/amateur SEE MORE EVERY DAY! planetary.org/blogs 2 THE PLANETARY REPORT C JUNE SOLSTICE 2016 CONTENTS JUNE SOLSTICE 2016 COVER STORY Unveiling Ceres 6 Simone Marchi on why Ceres is a scientific treasure chest for Dawn. Pathway to the Stars Looking back at years of Society-led solar sail 10 development as Breakthrough Starshot is announced. Life, the Universe, and Everything 13 Planetary Radio in Death Valley. ADVOCATING FOR SPACE Partisan Peril 18 Casey Dreier looks at the U.S. President’s impact on space policy and legislation. DEVELOPMENTS IN SPACE SCIENCE Update on LightSail 2 20 Bruce Betts details the progress we’ve made in the year since LightSail 1 launched. -
AEOLIAN GEOLOGY of the MARS PATHFINDER SITE. Ronald
AEOLIAN GEOLOGY OF THE MARS PATHFINDER SITE. Ronald Greeley, Michael Kraft, Gregory Wilson (Arizona State University); Robert Sullivan (Cornell University); Ruslan Kuzmin (Vernadsky Institute, Russian Academy of Sciences); Michael Malin (Malin Space Science Systems); Nathan Bridges, Kenneth Herkenhoff, Matthew Golombek (Jet Propulsion Laboratory); Peter Smith (University of Arizona). Introduction wind tails, 2) drift deposits, 3) ripplelike deposits, duneforms of several types, and 4) material on the The Mars Pathfinder landing site contains abun- tops of some rocks and spacecraft components, dant features attributed to aeolian, or wind, proc- presumably settled from atmospheric suspension. esses. These include wind tails, drift deposits, duneforms of various types, ripplelike features, Wind-tails are found in association with many and ventifacts (the first seen on Mars). Many of rocks. Typically they taper to a point away from these features are consistent with formation in- the rock in the inferred downwind direction (at volving sand-size particles. Although some fea- the time of their formation). They range in length tures, such as the barchan dunes, could develop from a cm to nearly a meter and are bright red. from saltating sand-size aggregates of finer Drift deposits are also bright red, but occur as grains, the discovery of ventifact flutes cut in patches, only some of which are associated with rocks strongly suggests that at least some of the rocks. Wind- tails and drift deposits have a grains are crystalline, rather than aggregates. Ex- sculpted appearance and are similar to those seen cluding the ventifacts, the orientations of the at the Viking lander sites (3). wind-related features correlate well with the ori- entations of bright wind streaks seen on Viking Dunelike structures occur as transverse, bar- Orbiter images in the general area. -
Fracture Geometry and Statistics of Ceres' Floor Fractures
1 Fracture Geometry and Statistics of Ceres’ Floor Fractures 2 3 K. Krohn1, D. L. Buczkowski2, I. von der Gathen1, R. Jaumann1,3, F. Schulzeck1, K. Stephan1, R. 4 Wagner1, J. E. C. Scully4, C. A. Raymond4, C. T. Russell5 5 6 1Institute of Planetary Research, German Aerospace Center, Berlin, Germany; 2Johns Hopkins 7 University Applied Physics Laboratory, Laurel, MD, USA; 3Freie Universiät Berlin, Germany; 8 4NASA JPL, California Institute of Technology, Pasadena, California, USA; 5UCLA, Institute of 9 Geophysics, Los Angeles, CA, USA 10 11 Corresponding author: Katrin Krohn, [email protected], Rutherfordstraße 2, 12489 Berlin, Germany 12 13 Keywords: Ceres, dwarf planet, floor fractured craters 14 15 16 Highlights: 17 18 We measured 2336 fractures in thirteen floor-fractured craters (FFC) on Ceres. 19 20 Floor-fractured craters on Ceres share similarities with FFCs on other planetary bodies 21 especially those on the Moon and Mars. 22 23 On Ceres some floor-fractured craters are impact-driven; other appear to be related to cooling- 24 melting processes, outgassing and/or tectonics such as doming of the subsurface. 25 26 Fracture studies point out brittle surface materials. 27 28 29 30 Abstract 31 32 Floor-fractured craters are one of the most distinct features on Ceres. Most of the fractures are located 33 on the crater floors. The floor-fractures are concentric, radial or polygonal and share similarities with 34 Class 1 and 4 floor-fractured craters (FFC) on the Moon (e.g., Buczkowski et al., 2018; Schultz, 1976) 35 In total we measured 2336 fractures in thirteen craters.