The Geology of Mercury: Results from the First Two MESSENGER Flybys of the Innermost Planet

Total Page：16

File Type：pdf, Size：1020Kb

The geology of Mercury: Results from the first two MESSENGER flybys of the innermost planet LOUISE M. PROCKTER1, SEAN C. SOLOMON2, JAMES W. HEAD3, THOMAS R. WATTERS4, SCOTT L. MURCHIE1, MARK S. ROBINSON5, CLARK R. CHAPMAN6, and RALPH McNUTT, JR1 1Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, U.S.A. 2Carnegie Institution of Washington, Washington, DC 20015, U.S.A. 3Brown University, Providence, RI 02912, U.S.A. 4National Air and Space Museum, Smithsonian Institution, Washington, DC 20560, U.S.A. 5Arizona State University, Tempe, AZ 85287, U.S.A. 6Southwest Research Institute, Boulder, CO 80302, U.S.A. In 2008 the MESSENGER spacecraft made two flybys of the planet Mercury, collecting a wealth of new near-global science data. These data included observations of approximately 50% of the planet that had not been viewed by the Mariner 10 spacecraft during its flybys in 1974-1975. Many of the new observations were focused on Mercury’s geology, including monochrome imaging at resolutions as high as 100 m/pixel, multispectral imaging in 11 filters at resolutions as high as 500 m/pixel, laser altimetry tracks extending over several thousands of kilometers, and high-resolution spectral measurements of several types of terrain. We present an overview of the first inferences on Mercury’s global geology from the MESSENGER observations. The new MESSENGER images and altimetry provide compelling evidence that volcanism was a widespread and protracted process on Mercury. MESSENGER observations show distinct spectral units as well as morphological evidence suggesting embayment and possibly pyroclastic eruptions. Preliminary measurements of impact crater size-frequency distributions suggest that plains material on Mercury’s surface ranges in age from a time shortly after the end of heavy impact bombardment to as young as perhaps 1 billion years ago. Image and laser altimeter data reveal details of Mercury’s global tectonic history, including confirmation that contractional features are the dominant global landform. Keywords: MESSENGER; Mercury; flyby; planetary geology. .

Copy Link

Recommended publications

Shallow Crustal Composition of Mercury As Revealed by Spectral Properties and Geological Units of Two Impact Craters
Planetary and Space Science 119 (2015) 250–263 Contents lists available at ScienceDirect Planetary and Space Science journal homepage: www.elsevier.com/locate/pss Shallow crustal composition of Mercury as revealed by spectral properties and geological units of two impact craters Piero D’Incecco a,n, Jörn Helbert a, Mario D’Amore a, Alessandro Maturilli a, James W. Head b, Rachel L. Klima c, Noam R. Izenberg c, William E. McClintock d, Harald Hiesinger e, Sabrina Ferrari a a Institute of Planetary Research, German Aerospace Center, Rutherfordstrasse 2, D-12489 Berlin, Germany b Department of Geological Sciences, Brown University, Providence, RI 02912, USA c The Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA d Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, CO 80303, USA e Westfälische Wilhelms-Universität Münster, Institut für Planetologie, Wilhelm-Klemm Str. 10, D-48149 Münster, Germany article info abstract Article history: We have performed a combined geological and spectral analysis of two impact craters on Mercury: the Received 5 March 2015 15 km diameter Waters crater (106°W; 9°S) and the 62.3 km diameter Kuiper crater (30°W; 11°S). Using Received in revised form the Mercury Dual Imaging System (MDIS) Narrow Angle Camera (NAC) dataset we deﬁned and mapped 9 October 2015 several units for each crater and for an external reference area far from any impact related deposits. For Accepted 12 October 2015 each of these units we extracted all spectra from the MESSENGER Atmosphere and Surface Composition Available online 24 October 2015 Spectrometer (MASCS) Visible-InfraRed Spectrograph (VIRS) applying a ﬁrst order photometric correc- Keywords: tion.
[Show full text]
Arxiv:2012.11628V3 [Astro-Ph.EP] 26 Jan 2021
manuscript submitted to JGR: Planets The Fundamental Connections Between the Solar System and Exoplanetary Science Stephen R. Kane1, Giada N. Arney2, Paul K. Byrne3, Paul A. Dalba1∗, Steven J. Desch4, Jonti Horner5, Noam R. Izenberg6, Kathleen E. Mandt6, Victoria S. Meadows7, Lynnae C. Quick8 1Department of Earth and Planetary Sciences, University of California, Riverside, CA 92521, USA 2Planetary Systems Laboratory, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA 3Planetary Research Group, Department of Marine, Earth, and Atmospheric Sciences, North Carolina State University, Raleigh, NC 27695, USA 4School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287, USA 5Centre for Astrophysics, University of Southern Queensland, Toowoomba, QLD 4350, Australia 6Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA 7Department of Astronomy, University of Washington, Seattle, WA 98195, USA 8Planetary Geology, Geophysics and Geochemistry Laboratory, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA Key Points: • Exoplanetary science is rapidly expanding towards characterization of atmospheres and interiors. • Planetary science has similarly undergone rapid expansion of understanding plan- etary processes and evolution. • Eﬀective studies of exoplanets require models and in-situ data derived from plan- etary science observations and exploration. arXiv:2012.11628v4 [astro-ph.EP] 8 Aug 2021 ∗NSF Astronomy and Astrophysics Postdoctoral Fellow Corresponding author: Stephen R. Kane, [email protected] {1{ manuscript submitted to JGR: Planets Abstract Over the past several decades, thousands of planets have been discovered outside of our Solar System. These planets exhibit enormous diversity, and their large numbers provide a statistical opportunity to place our Solar System within the broader context of planetary structure, atmospheres, architectures, formation, and evolution.
[Show full text]
Revisions to the Online Textbook Exploring the Planets (Explanet.Info): Mercury and Pluto
49th Lunar and Planetary Science Conference 2018 (LPI Contrib. No. 2083) 2724.pdf REVISIONS TO THE ONLINE TEXTBOOK EXPLORING THE PLANETS (EXPLANET.INFO): MERCURY AND PLUTO. B.C. Spilker1, E.H. Christiansen1, and J. Radebaugh1, 1Brigham Young University, De- partment of Geological Sciences, Provo, UT 84602. [email protected] Introduction: Exploring the Planets (http://ex- planet.info) [1] is a free online college textbook cover- ing the basic concepts of planetary science, and the character and evolution of the planetary bodies in the Solar System (including the planets, important moons, asteroids, and Kuiper Belt Objects). The latest edition (3rd edition) was published online in 2007 by Eric H Christiansen. Earlier paper editions were published by Prentice Hall in 1990 and 1995. Exploring the Planets approaches an introductory study of the solar system mainly through basic geolog- ical principles. Compared with other introductory plan- etary geology texts, such as Planetary Sciences by de Pater and Lissauer [2], Introduction to Planetary Sci- ence by Faure and Mensing [3], The New Solar System by Beatty, Petersen, and Chaikin [4] or Earth, Evolu- tion of a Habitable World by Lunine [5], this is the only book with a basic geology approach. It is intended to be used as a primary or supplementary source in in- troductory science courses (geology or astronomy ). Book Structure: Exploring the Planets is divided into three sections. The first section gives a broad over- view of the Solar System and an introduction to plane- tary science. This section helps the reader develop the geological background required to understand the pro- cesses that have shaped the planets, and to begin think- ing like a planetary scientist.
[Show full text]
Thomas Robert Watters
THOMAS ROBERT WATTERS Address: Center for Earth and Planetary Studies National Air and Space Museum Smithsonian Institution P. O. Box 37012, Washington, DC 20013-7012 Education: George Washington University, Ph.D., Geology (1981-1985). Bryn Mawr College, M.A., Geology (1977-1979). West Chester University, B.S. (magna cum laude), Earth Sciences (1973-1977). Experience: Senior Scientist, Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution (1998-present). Chairman, Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution (1989-1998). Research Geologist, Center for Earth and Planetary Studies, Smithsonian Institution, Planetary Geology and Tectonics, Structural Geology, Tectonophysics (1981-1989). Research Assistant, Department of Terrestrial Magnetism, Carnegie Institution of Washington, Chemical Analysis and Fission Track Studies of Meteorites (1980-1981). Research Fellowship, American Museum of Natural History, Electron Microprobe and Petrographic Study of Aubrites and Related Meteorites (1978-1980). Teaching Assistant, Bryn Mawr College (1977-1979), Physical and Historical Geology, Crystallography and Optical Crystallography. Undergraduate Assistant, West Chester University (1973-1977), Teaching Assistant in General and Advanced Astronomy, Physical and Historical Geology. Honors: William P. Phillips Memorial Scholarship (West Chester University); National Air and Space Museum Certificate of Award 1983, 1986, 1989, 1991, 1992, 2002, 2004; American Geophysical Union Editor's Citation for Excellence in Refereeing - Journal Geophysical Research-Planets, 1992; Smithsonian Exhibition Award - Earth Today: A Digital View of Our Dynamic Planet, 1999; Certificate of Appreciation, Geological Society of America, 2005, 2006; Elected to Fellowship in the Geological Society of America, 2007. The Johns Hopkins University Applied Physics Laboratory 2009 Publication Award - Outstanding Research Paper, “Return to Mercury: A Global Perspective on MESSENGER’s First Mercury Flyby (S.C.
[Show full text]
True Polar Wander of Mercury
Mercury: Current and Future Science 2018 (LPI Contrib. No. 2047) 6098.pdf TRUE POLAR WANDER OF MERCURY. J. T. Keane1 and I. Matsuyama2; 1California Institute of Technology, Pasadena, CA 91125, USA ([email protected]); 2Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA. Introduction: The spin of a planet is not constant to the Sun and subject to stronger tidal and rotational with time. Planetary spins evolve on a variety of time- forces. However, even with this corrected dynamical scales due to a variety of internal and external forces. oblateness, the required orbital configuration appears One process for changing the spin of a planet is true po- unreasonable−requiring semimajor axes <0.1 AU [5]. lar wander (TPW). TPW is the reorientation of the bulk An alternative explanation may be that a large fraction planet with respect to inertial space due to the redistri- of Mercury’s figure is a “thermal” figure, set Mercury’s bution of mass on or within the planet. The redistribu- close proximity to the Sun and its unique spin-orbit res- tion of mass alters the planet’s moments of inertia onance [7-8] (which are related to the planet’s spherical harmonic de- True Polar Wander of Mercury: While Mercury’s gree/order-2 gravity field). This process has been meas- impact basins and volcanic provinces cannot explain ured on the Earth, and inferred for a variety of solar sys- Mercury’s anomalous figure, they still have an im- tem bodies [1]. TPW can have significant consequences portant effect on planet’s moments of inertia and orien- for the climate, tectonics, and geophysics of a planet.
[Show full text]
The Planetary Geology Division of the Geological Society of America
The Planetary Geology Division of the Geological Society of America Volume 27, Number 1 March 2009 Message from the Chair on the latest MESSENGER mission results from Mercury and an impact cratering session to honor this year’s Gilbert award winner, the Louise M. Prockter indefatigable Bob Strom. The abstract deadline Applied Physics Laboratory, for the annual meeting will be August 11, and Johns Hopkins University we encourage you to consider submitting a paper. Abstract submittals will begin in April, but you can view the topical sessions now at As this year’s Chair it is my turn to thank you http://www.geosociety.org/meetings/2009/sessi all for your continued support of our Division, ons/topical.asp. whether through your membership dues, service as a judge for the Dwornik student Student papers are especially welcome, and award, or supporting us at our booth during last their authors can apply for one of our new year’s GSA Annual Meeting in Houston. The student awards to help offset travel costs (after Houston meeting was well attended, and we the meeting registration opens, look for capitalized on the location and the ties to information on the PGD website at human exploration that abound there. The http://www.geosociety.org/meetings/2009/sessi Planetary Geology Division historically has a ons/topical.asp.) significant number of topical sessions at the annual meeting, and it is a great opportunity to Despite the current economic uncertainties, I mix with terrestrial geologists, many of whom am happy to be writing this at a time when we are fascinated by what we do.
[Show full text]
Terrestrial Planets (Bennett Et Al
Earth and the Geology of the Terrestrial Planets (Bennett et al. Ch. 9) Major Ideas In This Chapter ● Terrestrial planets looked (largely) the same when they were formed. Differences due to geological processes. ● Geological activity is driven by internal heat ● Planetary size plays a large role in retaining heat ● Distance from the Sun, rotation affects erosion ● Crater density can indicate surface age ● Earth has a unique geology Terrestrial Planets ● Compared to Jovian planets: – Smaller size/mass – Large “core” to atmosphere ratio – Higher density – Closer to Sun and closer together – Warmer – Few or no moons – No rings (NASA) Planetary Surfaces and Interiors ● Terrestrial planets + Moon were similar when young – Subjected to heavy bombardment – Differences due to processes that occurred after formation ● Understanding the surface features: planetary geology ● Processes in the interior drive activity at the surface Your book uses “terrestrial worlds” to refer to the terrestrial planets + the Moon. (from Bennett et al.) (from Bennett et al.) How Do We Learn About Planetary Interiors? ● Average density determinations ● Local gravity variations as measured with artificial satellites ● Magnetic fields: molten core/convection ● Lava flow: internal composition ● Earthquakes: internal structure Earthquakes: Seismic Waves ● Earthquakes generate vibrations – Typical wavelength ~ several km – Reconstruct interior ● Two types of waves: – P-waves: compressional waves – S-waves: shear waves ● S-waves cannot pass through liquid (from Bennett et
[Show full text]
Iac-09-A3.6.2 the Messenger Mission: Results from The
IAC-09-A3.6.2 THE MESSENGER MISSION: RESULTS FROM THE FIRST TWO MERCURY FLYBYS Ralph L. McNutt, Jr.1, Sean C. Solomon2, Peter D. Bedini3, Eric J. Finnegan4, David G. Grant5, and the MESSENGER Team 1The Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Road, M/S MP3-E128, Laurel, MD 20723 U.S.A. [email protected] 443-778-5435, Fax: 443-778-0386 2Department of Terrestrial Magnetism, Carnegie Institution of Washington, 5241 Broad Branch Road, N.W., Washington, DC 20015 U.S.A. [email protected] 202-478-8850, Fax: 202-478-8821 3The Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Road, M/S 23-282, Laurel, MD 20723 U.S.A. [email protected] 443-778-4642, Fax: 443-778-5295 4The Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Road, M/S 23-282, Laurel, MD 20723 U.S.A. [email protected] 443-778-1712, Fax: 443-778-6635 5The Johns Hopkins University Applied Physics Laboratory, 11100 Johns Hopkins Road, M/S 4-283, Laurel, MD 20723 U.S.A. [email protected] 443-778-5297, Fax: 443-778-5295 ABSTRACT NASA’s MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft is well into its voyage to initiate a new era in our understanding of the innermost planet. During 2008 MESSENGER flew by Mercury twice and completed the initial spacecraft reconnaissance of the planet begun 34 years earlier by Mariner 10. MESSENGER observations have illuminated how the 1500-km- diameter Caloris basin was a focus for magmatic and deformational activity.
[Show full text]
1 the Planets Mercury and Venus 2 the Geology of Mercury
General Astronomy (29:61) Fall 2012 Lecture 34 Notes, November 26, 2012 1 The Planets Mercury and Venus 1.0.1 Just the facts, Ma'am . Here are the fundamental numbers on these planets (also available in Table A.3. • Mercury, radius = 0.383 R⊕, mass = 0.0553 M⊕; orbital properties: a = 0.387 AU, = 0.2056 • Venus, radius = 0.950 R⊕, mass = 0.815 M⊕; orbital properties: a = 0.723 AU, = 0.0068 Last time, we described how the comparable, and commensurable orbital and rotational period of Mercury are responsible for an odd nature of the day on Mercury. 2 The Geology of Mercury Our knowledge of Mercury is being enormously expanded by the Messenger space- craft, which arrived in orbit around Mercury early in March of 2011. There are two ways in which Messenger is providing huge amounts of new data. 1. High resolution pictures of the surface of Mercury are being taken from in orbit. 2. An instrument on Messenger uses x-ray fluorescence to determine the chemical composition of the surface of Mercury. Natural x-rays from the Sun excite atoms on the surface of Mercury. When these items radiative de-excite, the give off other x-rays which are spectral lines of elements. Different elements have different spectral lines, even in the x-ray. The results of observations with this x-ray spectrometer have recently been an- nounced. It has been found that the chemical composition of smooth plains is differ- ent from more heavily cratered surroundings. This is interpreted as evidence that the magma that produced these features came from two different sources in the interior of Mercury.
[Show full text]
Mercury Stereo Topography: Construction of Regional Topographic Maps Derived from Mariner 10 Images
Lunar and Planetary Science XXXVIII (2007) 2155.pdf MERCURY STEREO TOPOGRAPHY: CONSTRUCTION OF REGIONAL TOPOGRAPHIC MAPS DERIVED FROM MARINER 10 IMAGES. S. L. Andre1 and T. R. Watters1, 1Center for Earth and Planetary Studies, National Air and Space Museum, Smithsonian Institution, Washington, D.C. 20013-7012, [email protected]. Introduction: Much of our current understanding DEM is selected during the error analysis process for of geology of Mercury is based on data obtained from each individual stereo pair, and thus the DEM gener- Mariner 10. This Mariner 10 view has provided the ated from the stereo pair with the smallest error is se- framework for the scientific issues and questions to be lected to be the core DEM and is used to “anchor” the addressed by future missions to Mercury (in particular other neighboring DEMs. Regional products were con- the MESSENGER mission [1]). Critical to unraveling structed by hand-laying each pair on the main mosaic. the geologic evolution is knowledge of the topography In SMTK, the quality of the point matching in a stereo of Mercury. The overlap and lighting conditions be- pair is estimated using the error in the adaptive least tween the first and second Mariner 10 flybys are fa- squares routine for each matched point. SMTK then vorable for stereo, but little stereo analysis was done at translates the error for the matched points into a height the time of the mission [2]. More recent improvements accuracy for each point within the DEM. We conser- in the control network and SPICE information for the vatively choose the highest error within the DEM to Mariner 10 mission [3] have allowed for recent stereo represent the overall height error.
[Show full text]
Terrestrial Worlds
Terrestrial Worlds Orin Harris and Greg Anderson Department of Physics & Astronomy Northeastern Illinois University Spring 2021 c 2012-2021 G. Anderson., O. Harris Universe: Past, Present & Future – slide 1 / 84 Outline Terrestrial Interiors Magnetic Fields Geologic Processes Terrestrial Worlds Terrestrial Atmospheres Review c 2012-2021 G. Anderson., O. Harris Universe: Past, Present & Future – slide 2 / 84 Terrestrial Planets c 2012-2021 G. Anderson., O. Harris Universe: Past, Present & Future – slide 3 / 84 Outline Terrestrial Planets Terrestrial Planets Terrestrial Interiors Sources of Evidence Onion article Planetary Densities S and P Waves Terrestrial Interiors S and P Waves Differentiation Interiors of Terrestrial Plants Q: Differentiation Q: Planetary Cores Earth’s Interior Sources of Internal Heat Earth Heat Evolution Heat Transfer Q: Cooling Volume to Surface Ratio Q: Cooling Planets c 2012-2021 G. Anderson., O. Harris Universe: Past, Present & Future – slide 5 / 84 Q: Rank Sources of Evidence How do we know what is inside? • Average density • Earthquakes • Magnetic fields • Lava flows • Local gravity variations c 2012-2021 G. Anderson., O. Harris Universe: Past, Present & Future – slide 6 / 84 Planetary Densities (ρ = M/V ) 5.52 5.43 5.24 5.0 4.0 3.92 ) 3 3.0 2.0 Density (g/cm 1.0 Mercury Venus Earth Mars Saturn Uranus Neptune tNOs 0.0 Asteroids Jupiter c 2012-2021 G. Anderson., O. Harris Universe: Past, Present & Future – slide 8 / 84 Differentiation • Gravity pulls high-density material to the center. • Lower-density material “floats” to the surface. • Material ends up sorted by density. least dense denser densest c 2012-2021G.Anderson.,O.Harris Universe:Past,Present&Future – slide 11 / 84 Interiors of Terrestrial Plants Earth Venus Mars Mercury Moon Core Mantle Crust highest density medium density lowest density c 2012-2021G.Anderson.,O.Harris Universe:Past,Present&Future – slide 12 / 84 Q: Differentiation What is necessary for differentiation to occur in a planet? A) It must have metal and rock in it.
[Show full text]
Geology of the Moon Geology of Mercury
Geology of the Moon • Smooth, dark lunar maria are less heavily cratered than lunar highlands • Maria were made by flood of runny lava • Wrinkles arise from cooling and contraction of lava flood • heavily cratered, no atmosphere (too small), geologically inactive Geology of Mercury • A mixture of heavily cratered and smooth regions like the Moon • Smooth regions are likely ancient lava flows • Tectonics: Long cliffs indicate that Mercury shrank early in its history • No atmosphere (too small), geologically dead 1 Geology of Mars • mountains & canyons • Valles Marineris • volcanoes • thin atmosphere (CO2) • no plate tectonics • evidence for water erosion Cratering on Mars • Amount of cratering differs greatly across surface • Many early craters have been erased 2 Volcanism on Mars • Mars has many large shield volcanoes • Olympus Mons is largest volcano in solar system Tectonics on Mars • System of valleys known as Valles Marineris thought to originate from tectonics 3 Dry Riverbeds? • Close-up photos of Mars show what appear to be dried- up riverbeds • Details of some craters suggest they were once filled with water • Mars rovers have found rocks that appear to have formed in water Water on Mars? • Some craters have frozen water exposed for short period • There is evidence for (frozen) water within 1 meter under the surface • this underground water may be all over the planet 4 Ancient Water on Mars • Liquid water can not exist on Mars today. • temperatures below freezing • air pressure too low • Dry river channels in southern highlands • heavily cratered terrain (> 3 billion years old) • Some surface features are eroded. • implies running water, rain • crater lakes • Mars was warm & wet over 3 billion years ago.
[Show full text]