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Planetary Sciences Community Meetings Calendar

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Organized by LPI/USRA *

December 2020

1-3	Refining Planetary Protection Requirements for Human Missions to Mars, Virtual  As part of planning for future space exploration, COSPAR (The Committee on Space Research) together with participating space agencies, is organizing an interdisciplinary meeting to consider next steps in Refining Planetary Protection Requirements for Human Missions to Mars. The objective for planetary protection is to avoid jeopardizing the conduct of scientific investigations of possible extraterrestrial life forms, precursors, and remnants and to protect the Earth from potential hazards posed by extra-terrestrial material on a spacecraft returning from an interplanetary mission. The next meeting on planetary protection for human missions is to be held virtually on December 1-3, 2020 from 10:30-1:30 EST each day. The meeting will focus on technologies and operations to control the contamination in- and outflow of crewed systems on the surface of Mars. The meeting is the latest in the workshop series on planetary protection for human missions to Mars, which first identified and then prioritized important knowledge gaps in science and technology areas. The latest report from these earlier workshops is posted under conference documents at this link: https://sma.nasa.gov/sma-disciplines/planetary-protection/ COSPAR meetings are open (to the capacity of the facilities) and members of the space science and engineering communities are particularly welcome to join in contributing to the important discussions to ensure integration of planetary protection considerations into future mission plans for human missions beyond Earth orbit. Please RSVP to [email protected] and to [email protected] by Nov. 27, 2020 to register.
3	Seminar Series: Extracting Secrets of the Solar System: Soluble Organic Analysis of Meteorites and Returned Samples (Jamie Cook, Goddard Space Flight Center), Virtual  Laboratory analysis of solar system materials, including meteorites and returned samples, provides important information about early solar system chemistry and the potential distribution of the ingredients necessary for life. Meteorites provide samples from diverse parent bodies, while samples returned by space missions represent materials from known parent bodies with the benefits of context and minimal contamination. Targeted laboratory analyses of these samples have identified a wide range of organic compounds, including soluble organics such as amino acids, carboxylic acids, aldehydes, ketones, sugars, nucleobases, hydrocarbons, and more, as well as insoluble macromolecular material. Amino acids are of particular interest to astrobiology because of the role they play in life on Earth. This talk will discuss how soluble organic compounds, especially amino acids, are analyzed in extraterrestrial materials, and how these analyses contribute to our understanding of the origin of life on Earth.
7-11	AGU Fall Meeting, San Francisco, California
10	Meteoritic Implications for the Galactic Environment of Solar System Formation (Emilie Dunham, University of California, Los Angeles), Virtual  The nature of the galactic environment in which our Sun and Solar System formed remains a mystery – did our Sun form in an active region of star formation, or in a quiescent part of the galaxy? The rate of star formation when and where the Sun formed is difficult to constrain using astronomical observations. I will present how we determined a precise star formation rate ~4.5 billion years ago in the vicinity of our nascent Solar System using a short-lived radionuclide (10Be) in ancient meteorite inclusions. We find that the majority of inclusions from a variety of chondrite types (CV3, CO3, CR2, and CH/CB) record a uniform initial 10Be/9Be = 7 × 10−4. These results indicate that our Sun likely formed in an active star forming region, such as a galactic spiral arm, with ~6–7 times higher star formation rate than at present. To R.S.V.P., visit https://rb.gy/fb5hxh.
17	Falling Sky: The Hadean and Archean Earth Asteroid Impact Flux (Simone Marchi, Southwest Research Institute), Virtual  In the aftermath of the giant collision resulting in the formation of the Moon, about 4.5 billion years ago, the Earth experienced a protracted time of bombardment by leftover planetesimals. In this talk I will present a bombardment model of the Hadean Earth (4.5-4.0 Ga) that has been calibrated using existing lunar and terrestrial data. We find that the surface of the Hadean Earth was widely reprocessed by impacts through mixing and burial by impact-generated melt. This model may explain the absence of early terrestrial rocks. Further, I will discuss the effects of collisions on the formation of impact-induced geochemical heterogeneities that could still persist in terrestrial mantle rocks. Finally, I will present a recent model for the Archean (4.0-2.5 Ga) impact flux, and discuss implications for the oxygenation history of Earth’s atmosphere. R.S.V.P.: https://rb.gy/oobmou

 

January 2021

7	Searching for Lunar Water with LunaH-Map: Tiny Interplanetary Spacecraft With Big Science and Exploration Goals (Craig Hardgrove, Arizona State University), Virtual  LunaH-Map is a new type of NASA planetary science mission manifested for launch on Space Launch System Artemis-1. Following in the footsteps of the MarCO cubesat's successful interplanetary mission, the LunaH-Map spacecraft is a miniaturized, shoebox-sized, interplanetary spacecraft that will use a small ion propulsion system to navigate into lunar orbit and a neutron spectrometer to map enrichments of hydrogen across the lunar South Pole. The maps produced by LunaH-Map will help constrain the amount of hydrogen within permanently shadowed regions, which will inform our understanding of sources and sinks for polar volatile deposits, as well as planning future lunar exploration missions. To R.S.V.P., visit http://ow.ly/JW5b50CZI4h
14	A Subterranean Hydrothermal System and Microbial Nursery Beneath the Floor of the Chicxulub Impact Crater (David A. Kring, Lunar and Planetary Institute), Virtual  An expedition sponsored by the International Ocean Discovery Program and International Continental Scientific Drilling Program recovered rock core from the peak ring of the ~180 km-diameter Chicxulub impact crater. Mineral assemblages in the core indicate the crater hosted a substantial and long-lived hydrothermal system. Furthermore, sulfur isotope compositions of pyrite framboids that precipitated in the hydrothermal system indicate it was inhabited by sulphate-reducing thermophilic organisms. The findings support the impact origin of life hypothesis, which posits prebiotic chemistry and the early evolution of life occurred in similar impact-generated systems during the Hadean on Earth and potentially in other planetary systems where similar hydrothermal systems are generated. To R.S.V.P., visit https://bit.ly/3ouPVuT
20-21	Lunar Surface Science Workshop *, Virtual Session 7: Space Biology  The Space Biology virtual session will inform the community about lunar surface science programmatic activities at NASA and solicit input from the community on the potential for new scientific research that could be enabled by Commercial Lunar Payload Services (CLPS) and human exploration on the Moon and the technologies needed to conduct the research investigations.
21	MSR Sample Caching Strategy Workshop, Virtual  In October 2020, NASA and ESA formalized a partnership to bring samples of Mars to Earth. One crucial piece of planning that will have a large impact on the potential number, nature, and diversity of returned samples, and thus on the science that can be performed on the samples, is the caching strategy for the samples collected by the rover Perseverance. The delivery of cached samples to the Sample Retrieval Lander (SRL)is possible via transport by two pathways: 1) retrieval of samples cached on the Mars surface by the Sample Fetch Rover (SFR) and then transport to the Sample Retrieval Lander; and/or 2) delivery of samples retained on Perseverance to the SRL. Thus, there are multiple options for caching. The samples can be cached in one or more depots on the surface of Mars, and the Perseverance rover itself can carry a cache, allowing one or both of the above pathways to be utilized. Which strategies are actually implemented will depend on the nature and perceived value of each sample, the diversity of the samples at a depot, landing site accessibility for SRL, the capabilities of Perseverance and Sample Fetch Rover, lifetime projections for Perseverance and SFR, and the projected risk of rover survivability and trafficability of the terrain encountered. Potential scenarios may include acquiring duplicate samples as well as where, when, and how many depots are established. We solicit your participation in a four-hour workshop on January 21, 2021 (8am-12pm PST) to consider the strategy for establishing the caches on Mars. Key discussion points wil include: • What are the minimum attributes of a cache that warrants sample return? • What should be the strategy for duplicate sampling? • What approach(es) will offer the best balance between minimizing risk and maximizing the scientific value of the samples to be returned? The workshop will present a review of relevant material, and a forum for community discussion on possible viable scenarios for a sample caching strategy. More detailed information will be forthcoming. Please let us know of your interest so we can properly scope the meeting by filling out the Indication of Interest form at https://forms.gle/gf4rxQ1BjFqdVe9BA. Gerhard Kminek and Michael Meyer on behalf of the Caching Strategy Steering Committee (CSSC).
21	A Tale of Lunar Water (Casey Honniball, Goddard Space Flight Center), Virtual  For decades the lunar surface was believed to be anhydrous, however, reports by three independent spacecraft in 2009 changed this view when they detected a 3 µm hydration band on the Moon. The 3 µm absorption band is attributed to hydroxyl (OH) and possibly molecular water (H2O). The band exhibits variations with lunar time of day, temperature, soil maturity, and composition that has been interpreted as variations in water concentrations. Data from an infrared spectrometer, the Moon Mineralogy Mapper (M3) onboard the Chandrayaan-1 spacecraft, is widely used to study the 3 µm band, its spectral range, however, only covers half the hydration band. Due to the limited wavelength range of M3, variations of hydration has been called into question. To investigate the validity of variations in the 3 µm band we used the Spex infrared cross-dispersed spectrograph at the NASA InfraRed Telescope Facility (IRTF) at Maunakea Observatory in Hawaiʻi. Our improved data showed that the variation in hydration is real. But is hydroxyl or water responsible for the variations? Distinction between OH and H2O from spacecraft measurements at 3 µm is difficult due to their similar spectral properties. We have developed a new approach for unambiguous detection of the water molecule on the sunlit lunar surface. At 6.07 µm the fundamental H-O-H bend of H2O is exhibited and is strictly due to H2O without contribution by OH. The only current observatory capable of 6 µm observations of the Moon at 6 µm is the Stratospheric Observatory For Infrared Astronomy (SOFIA). Using data from SOFIA we report the first direct detection of the water molecule on the sunlit lunar surface. To R.S.V.P., visit Https://rb.gy/7z77ll
26-27	24th Meeting of the NASA Small Bodies Assessment Group (SBAG) *, Virtual  The Small Bodies Assessment Group (SBAG) was established by NASA in March 2008 to identify scientific priorities and opportunities for the exploration of asteroids, comets, interplanetary dust, small satellites, and Trans-Neptunian Objects.
27	MEPAG Virtual Meeting #11, Virtual  The next virtual meeting (VM11) of the Mars Exploration Program Analysis Group (MEPAG), is scheduled for Wednesday, January 27th, 2021, from 10:00 am-2:00 pm PST, 1:00 – 5:00 p.m. EST. Agenda items are expected to include updates about recent MEPAG, Mars Exploration Program, and Mars Sample Return Program activities, as well as presentations from Jim Watzin and Eric Ianson on Mars Ice Mapper and a discussion led by Scott Hubbard on Humans to Mars activities. The VM11 agenda and 2nd Information Circular will be shared in early January on the MEPAG meeting website (https://mepag.jpl.nasa.gov/meetings.cfm). WebEx connectivity information will be included in the 2nd Information Circular. This meeting is open to all members of the Mars science community including our international colleagues, and we look forward to your participation.
28	Regional Atmospheric Dynamics of Water in Valles Marineris, Mars (Cecilia W.S. Leung, Jet Propulsion Laboratory), Virtual  Water vapor in the planetary boundary layer is substantially influenced by local topographic gradients. Using a mesoscale atmospheric model, we investigate the convergence of regional moist air masses that forces asymmetries between the day-night concentrations of water in the canyon system. I will discuss the conditions under which water ice fogs may form inside Valles Marineris, and the implications for deliquescence and brines that may result from an atmospheric reservoir. To R.S.V.P., visit https://rb.gy/mql0ye

 

February 2021

3-5	Mercury Exploration Assessment Group (MExAG) *, Virtual  This will be the first meeting of the newly chartered MExAG. The agenda will include an overview of NASA programs, ongoing science of the innermost planet, updates on ongoing and concepts for future spacecraft missions, and initiation of the development of a goals document for the future of Mercury science and exploration.
9-11	OPAG Meeting *, Virtual  The next Outer Planets Assessment Group (OPAG) meeting will be delivered virtually on February 9–11, 2021. The focus of this meeting will be on aspects of the Decadal Survey that are relevant to OPAG. Status reports will be requested from the Decadal Survey co-chairs and panel chairs. The meeting agenda will be posted at a later date. Invited presenters are required to upload a presentation file two weeks prior to the start of the meeting, using the USRA meeting portal. Detailed instructions will be forthcoming.
11	Potassium isotope anomalies in meteorites inherited from the protosolar molecular cloud (Yaray Ku, Harvard University), Virtual  Potassium (K) and other moderately volatile elements are depleted in many solar system bodies relative to CI chondrites, which closely match the composition of the Sun. These depletions and associated isotopic fractionations were initially believed to result from thermal processing in the protoplanetary disk, but so far, no correlation between the K depletion and its isotopic composition has been found. In this talk, I will present our high-precision K isotope data correlated with other neutron-rich nuclides (e.g., 64Ni and 54Cr), suggesting the observed 41K variations of a nucleosynthetic origin. In addition, I will present new K isotope data from individual chondrules and matrix analysis during this talk. Our data support that K isotope anomalies are inherited from an isotopically heterogeneous protosolar molecular cloud, and were preserved in bulk primitive meteorites. To R.S.V.P., visit https://rb.gy/jtztzn.
22-26	Habitable Worlds, Virtual  The Nexus for Exoplanet System Science (NExSS), a NASA research coordination network devoted to the study of habitability and detectability of life on exoplanets, is pleased to announce a virtual workshop on Habitable Worlds 2021. This workshop will generate input from the astronomical community during October 2020, culminating in a synchronous online meeting the week of 22-26 February 2021. The goal of the workshop is to identify opportunities and obstacles to cross-disciplinary collaboration on the questions of what makes planets habitable, and life on them detectable.
24-25	Lunar Surface Science Workshop *, Virtual Session 8: Structuring Real-Time Science Support of Artemis Crewed Operations  When astronauts walked on the Moon during the Apollo program, scientists were embedded in the Flight Control Team (FCT). These scientists populated a science backroom, and they were responsible for helping direct science activities, including sampling, instrument deployment, and other exploration tasks. In this way, the science backroom was critical in maximizing the productivity of the Apollo missions. Part of the reason for their success was that the scientists were able to work closely with the flight controllers, astronauts, and other critical members of the Apollo Program before, during, and after the missions. In the same way, scientists will work with Artemis Program flight controllers, flight directors, astronauts, and spaceflight engineers to achieve mission success and maximize scientific productivity by ensuring that the Artemis lunar surface missions effectively and efficiently accomplish high-priority science objectives.
25	The End-Cretaceous Planktic Foraminifera Crisis Linked to Ocean Acidification? (Jahnavi Punekar Dept. of Earth Sciences Jahnavi Punekar, IIT Bombay), Virtual  The Cretaceous-Palaeogene boundary event (K-Pg; ~66 Ma) is well known for the demise of >70% life on Earth, including the non-avian dinosaurs. It is one of the BIG FIVE mass extinctions of the Phanerozoic, the only one linked with two triggers- the Chicxulub impact (Yucatan peninsula, Mexico) and Deccan volcanism (India). Recent high-precision U-Pb ages constrain Deccan volcanism between ~66.3 Ma and ~65.6 Ma1. Mercury chemostratigraphy coupled with planktic foraminifera biostratigraphy have enabled unprecedented correlation of the timing, tempo and extent of the end-Cretaceous faunal, climatic and environmental perturbations with Deccan eruptions2. In the main Deccan province (India), the K-Pg boundary is now inferred to be at the top of the Poladpur Formation - a likely catastrophic high-volume eruptive event that lasted <100 kyr1. Proximal K-Pg sequences in the Krishna-Godavari basin intertrappeans (India) document >90% planktic foraminifera species going extinct in response to correlative lava megaflows3. The distal western Tethyan sites reveal a “poor-carbonate-preservation” interval4 with high planktic test fragmentation, increased abundance of opportunist taxa (Guembelitria spp.) and intraspecific dwarfing immediately preceding the K-Pg boundary. Experimental validation of preservation-based proxies lends support to this end-Cretaceous acidification hypothesis. Coeval bulk-rock low magnetic susceptibility and peak mercury signals firmly tie this acidification to ongoing Deccan volcanism5. The biological, taphonomic and geochemical evidence strongly support an ocean acidification interval that persisted for <52 kyr (~2 precession cycles) prior to the K-Pg boundary. The age, duration and nature of this acidification event are better explained by recurrent pulses of Deccan volcanism than the geologically instantaneous Chicxulub impact. To R.S.V.P., visit https://rb.gy/lgjqst.

 

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