CURRICULUM VITAE University of Idaho
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Cassini Update
Cassini Update Dr. Linda Spilker Cassini Project Scientist Outer Planets Assessment Group 22 February 2017 Sols%ce Mission Inclina%on Profile equator Saturn wrt Inclination 22 February 2017 LJS-3 Year 3 Key Flybys Since Aug. 2016 OPAG T124 – Titan flyby (1584 km) • November 13, 2016 • LAST Radio Science flyby • One of only two (cf. T106) ideal bistatic observations capturing Titan’s Northern Seas • First and only bistatic observation of Punga Mare • Western Kraken Mare not explored by RSS before T125 – Titan flyby (3158 km) • November 29, 2016 • LAST Optical Remote Sensing targeted flyby • VIMS high-resolution map of the North Pole looking for variations at and around the seas and lakes. • CIRS last opportunity for vertical profile determination of gases (e.g. water, aerosols) • UVIS limb viewing opportunity at the highest spatial resolution available outside of occultations 22 February 2017 4 Interior of Hexagon Turning “Less Blue” • Bluish to golden haze results from increased production of photochemical hazes as north pole approaches summer solstice. • Hexagon acts as a barrier that prevents haze particles outside hexagon from migrating inward. • 5 Refracting Atmosphere Saturn's• 22unlit February rings appear 2017 to bend as they pass behind the planet’s darkened limb due• 6 to refraction by Saturn's upper atmosphere. (Resolution 5 km/pixel) Dione Harbors A Subsurface Ocean Researchers at the Royal Observatory of Belgium reanalyzed Cassini RSS gravity data• 7 of Dione and predict a crust 100 km thick with a global ocean 10’s of km deep. Titan’s Summer Clouds Pose a Mystery Why would clouds on Titan be visible in VIMS images, but not in ISS images? ISS ISS VIMS High, thin cirrus clouds that are optically thicker than Titan’s atmospheric haze at longer VIMS wavelengths,• 22 February but optically 2017 thinner than the haze at shorter ISS wavelengths, could be• 8 detected by VIMS while simultaneously lost in the haze to ISS. -
Titan North Pole
. Melrhir Lacuna . Ngami Lacuna . Cardiel Lacus . Jerid Lacuna . Racetrack Lacuna . Uyuni Lacuna Vänern Freeman. Lanao . Lacus . Atacama Lacuna Lacus Lacus . Sevan Lacus Ohrid . Cayuga Lacus .Albano Lacus Lacus Logtak . .Junín Lacus . Lacus . Mweru Lacus . Prespa Lacus Eyre . Taupo Lacus . Van Lacus en Lacuna Suwa Lacus m Ypoa Lacus. lu . F Rukwa Lacus Winnipeg . Atitlán Lacus . Viedma Lacus . Rannoch Lacus Ihotry Lacus Lacus n .Phewa Lacus . o h . Chilwa Lacus i G Patos Maracaibo Lacus . Oneida Lacus Rombaken . Sinus Muzhwi Lacus Negra Lacus . Mývatn Lacus Sinus . Buada Lacus. Uvs Lacus Lagdo Lacus . Annecy Lacus . Dilolo Lacus Towada Lacus Dridzis Lacus . Vid Flumina Imogene Lacus . Arala Lacus Yessey Lacus Woytchugga Lacuna . Toba Lacus . .Olomega Lacus Zaza Lacus . Roca Lacus Müggel Buyan . Waikare Lacus . Insula Nicoya Rwegura Lacus . Quilotoa Lacus . Lacus . Tengiz Lacus Bralgu Ligeia Planctae Insulae Sinus Insulae Zub Lacus . Grasmere Lacus Puget XanthusSinus Flumen Hlawga Lacus . Mare Kokytos Flumina . Kutch Lacuna Mackay S Lithui Montes . a m Kivu Lacus Ginaz T Nakuru Lacuna Lacus Fogo Lacus . r . b e a tio v Niushe n i F Labyrinthus Wakasa z lum e i Letas Lacus na Sinus . Balaton Lacus Layrinthus F r e t u m . Karakul Lacus Ipyr Labyrinthus a Flu Xolotlán ay m . noh u en . a Lacus Sparrow Lacus p Moray A Okahu .Akema Lacus Sinus Sinus Trichonida .Brienz Lacus Meropis Insula . Lacus Qinghai Hawaiki . Insulae Onogoro Lacus Punga Insula Fundy Sinus Tumaco Synevyr Sinus . Mare Fagaloa Lacus Sinus Tunu s Saldanha u Sinus n Sinus i S a h c a v Trold Yojoa A . Lacus Neagh Kraken MareSinus Feia s Lacus u in Mayda S Lacus Insula Dingle Sinus Gamont Gen a Gabes Sinus . -
Mapping and Planetary Spatial Infrastructure Team
Mapping and Planetary Spatial Infrastructure Team INTRODUCTION SSB study on NASA PSD R&A Reorganization National Academy of Sciences, 13 May 2016 Jani Radebaugh, [email protected] Introducing the Mapping and Planetary Spatial Infrastructure Team • Mosaics, geologic maps, derived regional and global data products and associated geospatial infrastructure are integral to the success of the planetary science enterprise Introducing the Mapping and Planetary Spatial Infrastructure Team • Mosaics, geologic maps, derived regional and global data products and associated geospatial infrastructure are integral to the success of the planetary science enterprise Introducing the Mapping and Planetary Spatial Infrastructure Team • Mosaics, geologic maps, derived regional and global data products and associated geospatial infrastructure are integral to the success of the planetary science enterprise Introducing the Mapping and Planetary Spatial Infrastructure Team • Mosaics, geologic maps, derived regional and global data products and associated geospatial infrastructure are integral to the success of the planetary science enterprise Introducing the Mapping and Planetary Spatial Infrastructure Team • Mosaics, geologic maps, derived regional and global data products and associated geospatial infrastructure are integral to the success of the planetary science enterprise Introducing the Mapping and Planetary Spatial Infrastructure Team • Mosaics, geologic maps, derived regional and global data products and associated geospatial infrastructure are integral to the success of the planetary science enterprise Introducing the Mapping and Planetary Spatial Infrastructure Team • Mosaics, geologic maps, derived regional and global data products and associated geospatial infrastructure are integral to the success of the planetary science enterprise – Influence all phases of the mission lifecycle for science investigations and operations – Strategic needs must be anticipated and prioritized by the community – PSS recommended a “Cartography Research and Analysis Group” [CRAG] in Fall 2014. -
Catherinesaunders
The Utility of Robot Sensory Devices in a Collaborative Autonomic Environment Catherine Saunders, Roy Sterritt, George Wilkie School of Computing and Mathematics University of Ulster Northern Ireland [email protected], [email protected], [email protected] Abstract –-This paper proposes an Autonomic architecture that environment and relay meaningful information to each will enable mobile robots to self-manage and collaborate by other. using control loops to monitor their internal state and external environment. The Autonomic Computing MAPE-K control In this paper we discuss the sensor capabilities of the Dr loop is used to design a Robot Autonomic Element and a Robot X80-H platform that will be used for the research. A Mapping Autonomic Element; each can exchange data and collaborate to find an object located within a room. A review of design of the proposed system is included and explained. A the sensor capabilities of the X80-H mobile robot platform is brief literature review of robotic collaborative systems is undertaken with emphasis on how useful each sensor will be to also included. The Research Background section looks at the proposed research. A literature review of other projects why self-managing software systems are needed. that feature robot collaboration is also included. Keywords - autonomic computing; mobile robot; Dr Robot II. ROBOT SENSORY DEVICES X80-H; collaboration; MAPE-K This section gives an overview of the sensors that the Dr Robot X80-H is equipped with. We assess how reliable they are and how useful they will be for our research. We will be I. -
40Th Annual Meeting of the AAS Division for Planetary Sciences
40th Annual Meeting of the AAS Division for Planetary Sciences 10-15 October 2008 - Ithaca, New York, Statler Hotel, 130 Statler Drive, Ithaca, NY 14853 Friday, Saturday, Sunday, Monday, Tuesday, Wednesday, 10 October 11 October 12 October 13 October 14 October 15 October 8:00 Registration Park Atrium, Statler Hotel 8 am-4 pm Registration 8 am-noon 8:30- 1 Exoplanets I 20 Titan: Upper Atmosphere 50 Outer Planets II 59 Galilean Satellites 10:00 Statler Auditorium Statler Auditorium Statler Auditorium Statler Auditorium 2 Comets I 21 Planetary Rings: Theory 51 Mercury 60 Asteroid Composition DPS Members Meeting Statler Ballroom Statler Ballroom Statler Ballroom Statler Ballroom Statler Auditorium 3 Mars: Surface 22 MB Asteroids & Trojans 52 Asteroid Discovery & Orbits Uris Hall Uris Hall Uris Hall 10:00- Coffee Break Coffee Break Coffee Break Coffee Break Coffee Break 10:30 10:30- 4 Exoplanets II 23 Titan: Lower Atmosphere 34 Titan: Subsurface 53 Outer Planets III 61 Saturnian Satellites 12:00 Statler Auditorium Statler Auditorium Statler Auditorium Statler Auditorium Statler Auditorium 5 Comets II 24 Planetary Rings: Physical 35 Outer Planets I 54 Laboratory Research 62 Venus Statler Ballroom Statler Ballroom Statler Ballroom Statler Ballroom Statler Ballroom 6 Mars: Atmosphere 25 Near Earth Asteroids 36 Icy Dwarf Planets 55 Asteroid Evolution Uris Hall Uris Hall Uris Hall Uris Hall 12:00- Lunch Lunch Lunch Lunch 1:30 Meet the IAU NSF Town Hall DPS Women Green Conferencing Yale/Princeton Rooms Yale/Princeton Rooms Yale/Princeton Rooms Yale/Princeton Rooms 1:30- 7 Special Session 37 Special Session 56 Special Session 2:30 Dynamical Classification 26 Prize Lectures Exoplanets Mission Highlights of Planetary Bodies Kuiper Prize: Statler Auditorium Statler Auditorium All talks in any given session Statler Auditorium Michael F. -
Transient Broad Specular Reflections from Titan's North Pole
Lunar and Planetary Science XLVIII (2017) 1519.pdf TRANSIENT BROAD SPECULAR REFLECTIONS FROM TITAN’S NORTH POLE Rajani Dhingra1, J. W. Barnes1, R. H. Brown2, B J. Buratti3, C. Sotin3, P. D. Nicholson4, K. H. Baines5, R. N. Clark6, J. M. Soderblom7, Ralph Jaumann8, Sebastien Rodriguez9 and Stéphane Le Mouélic10 1Dept. of Physics, University of Idaho, ID,USA, [email protected], 2Dept. of Planetary Sciences, University of Arizona, AZ, USA, 3JPL, Caltech, CA, USA, 4Cornell University, Astronomy Dept., NY, USA, 5Space Science & Engineering Center, University of Wisconsin- Madison, 1225 West Dayton St., WI, USA, 6Planetary Science Institute, Arizona, USA, 7Dept. of Earth, Atmospheric and Planetary Sciences, MIT, Cambridge, USA, 8Deutsches Zentrum für Luft- und Raumfahrt, 12489, Germany, 9Laboratoire AIM, Centre d’etude de Saclay, DAPNIA/Sap, Centre de lorme des Merisiers, 91191 Gif/Yvette, France, 10Laboratoire de Planetologie et Geodynamique, CNRS UMR6112, Universite de Nantes, France. Introduction: The recent Cassini VIMS (Visual and Infrared Mapping Spectrometer) T120 observation of Titan show extensive north polar surface features which might correspond to a broad, off-specular reflec- tion from a wet, rough, solid surface. The observation appears similar in spectral nature to previous specular reflection observations and also has the appropriate geometry. Figure 1 illustrates the geometry of specular reflection from Jingpo Lacus [1], waves from Punga Mare [2] and T120 observation of broad off-specular reflection from land surfaces. We observe specular reflections apart from the observation of broad specular reflection and extensive clouds in the T120 flyby. Our initial mapping shows that the off-specular re- flections occur only over land surfaces. -
Mapping and Planetary Spatial Infrastructure Team
Mapping and Planetary Spatial Infrastructure Team Report to the Planetary Science Subcommittee March 2016 Introducing the Mapping and Planetary Spatial Infrastructure Team • Mosaics, geologic maps, derived regional and global data products, and associated geospatial infrastructure are integral to the success of the planetary science enterprise – Influences all phases of the mission lifecycle for science investigations and operations – Strategic needs must be anticipated and prioritized by the community – PSS recommended a “Cartography Research and Analysis Group” [CRAG] in Fall 2014. • A team fulfilling this role now exists in the form of MAPSIT – MAPSIT succeeds former PCGMWG and assumes strategic planning role But wait, I thought we did this already? • No, we didn’t (really!) • From 1974 to 2012: – 1974: Lunar Photography and Cartography Committee (LPACC) – 1977: Lunar and Planetary Photography and Cartography Committee (LPPACC) – 1979: Planetary Cartography Working Group (PCWG) – Produced two 10-year plans and a supplement (at right) – 1994-2012: Planetary Cartography & Geologic Mapping Working Group (PCGMWG) • PCGMWG ceased “advisory” role in ~2011 • PCGMWG disbanded 2015 with end of PGG • Looming gap for NASA long-term strategic planning and prioritization activities until addressed by MAPSIT formation 3/9/2016 3 Enabling Planetary Science • Planetary Spatial Infrastructure is the technology, policies, standards, human resources, software tools, and related activities necessary to Geographic Information Science and Technology acquire, -
(Preprint) AAS 18-416 PRELIMINARY INTERPLANETARY MISSION
(Preprint) AAS 18-416 PRELIMINARY INTERPLANETARY MISSION DESIGN AND NAVIGATION FOR THE DRAGONFLY NEW FRONTIERS MISSION CONCEPT Christopher J. Scott,∗ Martin T. Ozimek,∗ Douglas S. Adams,y Ralph D. Lorenz,z Shyam Bhaskaran,x Rodica Ionasescu,{ Mark Jesick,{ and Frank E. Laipert{ Dragonfly is one of two mission concepts selected in December 2017 to advance into Phase A of NASA’s New Frontiers competition. Dragonfly would address the Ocean Worlds mis- sion theme by investigating Titan’s habitability and prebiotic chemistry and searching for evidence of chemical biosignatures of past (or extant) life. A rotorcraft lander, Dragonfly would capitalize on Titan’s dense atmosphere to enable mobility and sample materials from a variety of geologic settings. This paper describes Dragonfly’s baseline mission design giv- ing a complete picture of the inherent tradespace and outlines the design process from launch to atmospheric entry. INTRODUCTION Hosting the moons Titan and Enceladus, the Saturnian system contains at least two unique destinations that have been classified as ocean worlds. Titan, the second largest moon in the solar system behind Ganymede and the only planetary satellite with a significant atmosphere, is larger than the planet Mercury at 5,150 km (3,200 miles) in diameter. Its atmosphere, approximately 10 times the column mass of Earth’s, is composed of 95% nitrogen, 5% methane, 0.1% hydrogen along with trace amounts of organics.1 Titan’s atmosphere may resemble that of the Earth before biological processes began modifying its composition. Similar to the hydrological cycle on Earth, Titan’s methane evaporates into clouds, rains, and flows over the surface to fill lakes and seas, and subsequently evaporates back into the atmosphere. -
NEWSLETTER Comets: Visitors from The
P LANETARY S CIENCE I NSTITUTE NEWSLETTER SPRING 2006 Vol. 7, No. 1 Comets: Visitors from the Early Solar System by Beatrice Mueller This is a great time to be a cometary scientist. We have had three successful spacecraft encounters in the past few years: Deep Space 1 flew by comet 19P/Borrelly in September 2001; Stardust flew through the dust coma of comet 81P/Wild 2 col- lecting samples in January, 2004, and delivering them success- fully to Earth in January, 2006; and, most recently, Deep Impact (the mission, not the movie) hit comet 9P/Tempel 1 in July, 2005. We have also had two “naked-eye” comets in the middle of the nineties: comets Hale-Bopp and Hyakutake, both discov- ered by amateurs. Although I am not on the science teams of these spacecraft mis- sions, I was, and still am, involved with ground-based support observations doing additional scientific research. Only a few specific, but important, science questions can be answered at the time of the actual short-lived spacecraft flybys and much impor- tant research is accomplished long after these exciting events. I am working currently on the rotation state of comet 10P/ Tempel 2. Ignacio Ferrin and I (Mueller & Ferrin 1996, Icarus) observed this comet in 1994 and compared the derived rotation period with a previous pass and found a small change in the rota- Raw CCD R-filter image of the main component of comet tion period. Numerical simulations by Nalin Samarasinha (PSI & 73P/Schwassmann-Wachmann 3 (small white object). Note the National Optical Astronomy Observatory [NOAO]) show the extension and fuzziness of the comet and the narrow tail. -
Enceladus Life Finder: the Search for Life in a Habitable Moon
Geophysical Research Abstracts Vol. 17, EGU2015-14923, 2015 EGU General Assembly 2015 © Author(s) 2015. CC Attribution 3.0 License. Enceladus life finder: the search for life in a habitable moon. Jonathan Lunine (1), Hunter Waite (2), Frank Postberg (3), Linda Spilker (4), and Karla Clark (4) (1) Center for Radiophysics and Space Research, Cornell University, Ithaca ([email protected]), (2) Southwest Research Institute,San Antonio, ( [email protected]), (3) U. Stuttgart, Stuttgart, ([email protected]), (4) Jet Propulsion Laboratory, Pasadena CA 91125, ( [email protected]) Is there life elsewhere in the solar system? Guided by the principle that we can most easily recognize life as we know it—life that requires liquid water—Enceladus is particularly attractive because liquid water from its deep interior is actively erupting into space, making sampling of the interior straightforward. The Cassini Saturn Orbiter has provided the motivation. In particular, at high resolution, spatial coincidences between individual geysers and small-scale hot spots revealed the liquid reservoir supplying the eruptions to be not in the near-surface but deeper within the moon [1], putting on a firm foundation the principle that sampling the plume allows us to know the composition of the ocean. Sensitive gravity and topography measurements established the location and dimensions of that reservoir: ∼ 35 km beneath the SPT ice shell and extending out to at least 50 degrees latitude, implying an interior ocean large enough to have been stable over geologic time [2]. The Cassini ion neutral mass spectrometer (INMS) discovered organic and nitrogen-bearing molecules in the plume vapour, and the Cosmic Dust Analyser (CDA) detected salts in the plume icy grains, arguing strongly for ocean water being in con-tact with a rocky core [3], [4]. -
The Science Case for a Titan Flagship-Class Orbiter with Probes (White Paper for the NRC Decadal Survey for Planetary Science and Astrobiology) Conor A
The Science Case for a Titan Flagship-class Orbiter with Probes (White paper for the NRC Decadal Survey for Planetary Science and Astrobiology) Conor A. Nixon, James Abshire, Andrew Ashton, Jason W. Barnes, Nathalie Carrasco, Mathieu Choukroun, Athena Coustenis, Louis-Alexandre Couston, Niklas Edberg, Alexander Gagnon, et al. To cite this version: Conor A. Nixon, James Abshire, Andrew Ashton, Jason W. Barnes, Nathalie Carrasco, et al.. The Science Case for a Titan Flagship-class Orbiter with Probes (White paper for the NRC Decadal Survey for Planetary Science and Astrobiology). 2020. hal-03085250 HAL Id: hal-03085250 https://hal.archives-ouvertes.fr/hal-03085250 Preprint submitted on 21 Dec 2020 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. The Science Case for a Titan Flagship-class Orbiter with Probes Authors: Conor A. Nixon, NASA Goddard Space Flight Center, USA Planetary Systems Laboratory, 8800 Greenbelt Road, Greenbelt, MD 20771 (301) 286-6757 [email protected] James Abshire, University oF Maryland, USA Andrew Ashton, Woods Hole Oceanographic Institution, USA Jason W. Barnes, University oF Idaho, USA Nathalie Carrasco, Université Paris-Saclay, France, Mathieu Choukroun, Jet Propulsion Laboratory, Caltech, USA Athena Coustenis, Paris Observatory, CNRS, PSL, France Louis-Alexandre Couston, British Antarctic Survey, UK Niklas Edberg, Swedish Institute oF Space Physics, Sweden Alexander Gagnon, University oF Washington, USA Jason D. -
NAI Icy Satellites Environments Focus Group
Discussion with NAI Icy Satellites Environments Focus Group NASA Outer Planets Assessment Group William B McKinnon, Chair Washington University Sept 8, 2010 1 What is OPAG? The Outer Planets Assessment Group (OPAG) was established by NASA in late 2004 to identify scientific priorities and pathways for solar system exploration beyond the asteroid belt. The group consists of an ~15-person steering committee which actively solicits input from the scientific community and reports its findings to NASAʼs Planetary Science Division and the Planetary Science Subcommittee of NASAʼs Advisory Council." !It is OPAG's goal that its findings represent the broad consensus of the scientific community. OPAG holds meeting semiannually, each attended by ~100 scientists. The meetings consist of a broad range of presentations from NASA HQ representatives, mission PIs, individual scientists, and technology researchers. Meetings often include breakout sessions where scientists work in small groups to prioritize scientific questions and mission requirements at specific destinations (e.g., Europa, Titan, giant planets, midsize icy satellites such as Enceladus). Community input is solicited at the meetings and through the OPAG email list containing over 500 members." 2 Outer Planets Assessement Group Steering Committee William McKinnon, Washington University (Chair, 2009- )" Torrence Johnson*, Jet Propulsion Laboratory" Fran Bagenal, University of Colorado (Chair, 2004-2009)" Bill Kurth, University of Iowa" Sushil Atreya, University of Michigan" Ralph Lorenz, JHU/APL"