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DISR) on the Huygens Probe
Data Archive Users’ Guide for the Descent Imager and Spectral Radiometer (DISR) on the Huygens Probe By: The DISR Team 29 January 2013 Version 2.0 International Traffic in Arms Regulations (ITAR) disclosure... Evaluation by the Export Officer of the University of Arizona's Office for the Responsible Conduct of Research (ORCR) has deemed that this document is not subject to International Traffic in Arms Regulations (ITAR) control, and is not restricted by the Arms Export Control Act. It is suitable for public release, and its distribution is unlimited. DISR - C. See 29 January 2013 Index 1.0 Introduction & Science Objectives .................................................................................. 3 2.0 Instrument Description.................................................................................................... 4 3.0 Titan Descent Sequence & Divergences ...................................................................... 11 4.0 Archive Description....................................................................................................... 15 5.0 Data Calibration............................................................................................................ 19 5.1 General Information.................................................................................................. 19 5.2 Descent Cycles......................................................................................................... 20 5.3 Lamp Datasets ........................................................................................................ -
Echo Exoplanet Characterisation Observatory
Exp Astron (2012) 34:311–353 DOI 10.1007/s10686-012-9303-4 ORIGINAL ARTICLE EChO Exoplanet characterisation observatory G. Tinetti · J. P. Beaulieu · T. Henning · M. Meyer · G. Micela · I. Ribas · D. Stam · M. Swain · O. Krause · M. Ollivier · E. Pace · B. Swinyard · A. Aylward · R. van Boekel · A. Coradini · T. Encrenaz · I. Snellen · M. R. Zapatero-Osorio · J. Bouwman · J. Y-K. Cho · V. Coudé du Foresto · T. Guillot · M. Lopez-Morales · I. Mueller-Wodarg · E. Palle · F. Selsis · A. Sozzetti · P. A. R. Ade · N. Achilleos · A. Adriani · C. B. Agnor · C. Afonso · C. Allende Prieto · G. Bakos · R. J. Barber · M. Barlow · V. Batista · P. Bernath · B. Bézard · P. Bordé · L. R. Brown · A. Cassan · C. Cavarroc · A. Ciaravella · C. Cockell · A. Coustenis · C. Danielski · L. Decin · R. De Kok · O. Demangeon · P. Deroo · P. Doel · P. Drossart · L. N. Fletcher · M. Focardi · F. Forget · S. Fossey · P. Fouqué · J. Frith · M. Galand · P. Gaulme · J. I. González Hernández · O. Grasset · D. Grassi · J. L. Grenfell · M. J. Griffin · C. A. Griffith · U. Grözinger · M. Guedel · P. Guio · O. Hainaut · R. Hargreaves · P. H. Hauschildt · K. Heng · D. Heyrovsky · R. Hueso · P. Irwin · L. Kaltenegger · P. Kervella · D. Kipping · T. T. Koskinen · G. Kovács · A. La Barbera · H. Lammer · E. Lellouch · G. Leto · M. A. Lopez Valverde · M. Lopez-Puertas · C. Lovis · A. Maggio · J. P. Maillard · J. Maldonado Prado · J. B. Marquette · F. J. Martin-Torres · P. Maxted · S. Miller · S. Molinari · D. Montes · A. Moro-Martin · J. I. Moses · O. Mousis · N. Nguyen Tuong · R. -
In-System'' Fission-Events: an Insight Into Puzzles of Exoplanets and Stars?
universe Review “In-System” Fission-Events: An Insight into Puzzles of Exoplanets and Stars? Elizabeth P. Tito 1,* and Vadim I. Pavlov 2,* 1 Scientific Advisory Group, Pasadena, CA 91125, USA 2 Faculté des Sciences et Technologies, Université de Lille, F-59000 Lille, France * Correspondence: [email protected] (E.P.T.); [email protected] (V.I.P.) Abstract: In expansion of our recent proposal that the solar system’s evolution occurred in two stages—during the first stage, the gaseous giants formed (via disk instability), and, during the second stage (caused by an encounter with a particular stellar-object leading to “in-system” fission- driven nucleogenesis), the terrestrial planets formed (via accretion)—we emphasize here that the mechanism of formation of such stellar-objects is generally universal and therefore encounters of such objects with stellar-systems may have occurred elsewhere across galaxies. If so, their aftereffects may perhaps be observed as puzzling features in the spectra of individual stars (such as idiosyncratic chemical enrichments) and/or in the structures of exoplanetary systems (such as unusually high planet densities or short orbital periods). This paper reviews and reinterprets astronomical data within the “fission-events framework”. Classification of stellar systems as “pristine” or “impacted” is offered. Keywords: exoplanets; stellar chemical compositions; nuclear fission; origin and evolution Citation: Tito, E.P.; Pavlov, V.I. “In-System” Fission-Events: An 1. Introduction Insight into Puzzles of Exoplanets As facilities and techniques for astronomical observations and analyses continue to and Stars?. Universe 2021, 7, 118. expand and gain in resolution power, their results provide increasingly detailed information https://doi.org/10.3390/universe about stellar systems, in particular, about the chemical compositions of stellar atmospheres 7050118 and structures of exoplanets. -
Mineralogy of Super-Earth Planets
This article was originally published in Treatise on Geophysics, Second Edition, published by Elsevier, and the attached copy is provided by Elsevier for the author's benefit and for the benefit of the author's institution, for non-commercial research and educational use including without limitation use in instruction at your institution, sending it to specific colleagues who you know, and providing a copy to your institution’s administrator. All other uses, reproduction and distribution, including without limitation commercial reprints, selling or licensing copies or access, or posting on open internet sites, your personal or institution’s website or repository, are prohibited. For exceptions, permission may be sought for such use through Elsevier's permissions site at: http://www.elsevier.com/locate/permissionusematerial Duffy T., Madhusudhan N. and Lee K.K.M Mineralogy of Super-Earth Planets. In: Gerald Schubert (editor-in-chief) Treatise on Geophysics, 2nd edition, Vol 2. Oxford: Elsevier; 2015. p. 149-178. Author's personal copy 2.07 Mineralogy of Super-Earth Planets T Duffy, Princeton University, Princeton, NJ, USA N Madhusudhan, University of Cambridge, Cambridge, UK KKM Lee, Yale University, New Haven, CT, USA ã 2015 Elsevier B.V. All rights reserved. 2.07.1 Introduction 149 2.07.2 Overview of Super-Earths 150 2.07.2.1 What Is a Super-Earth? 150 2.07.2.2 Observations of Super-Earths 151 2.07.2.3 Interior Structure and Mass–Radius Relationships 151 2.07.2.4 Selected Super-Earths 154 2.07.2.5 Super-Earth Atmospheres 155 2.07.3 Theoretical -
Terrestrial Planets
Terrestrial Planets First ever ‘whole Earth’ picture from deep space, taken by Bill Anders on Apollo 8 Apollo 8 crew, Bill Anders centre: The Earth is just a planet courtesy Nasa 1- 4 from the Sun Image courtesy: http://commons.wikimedia.org/wiki/Image:Terrestrial_planet_size_comparisons_edit.jpg Mercury, Venus, Earth and Mars are four astonishingly different planets Mercury and Venus have only been seen in any detail within the last 30 years Mercury in sight Courtesy NASA (Mariner 10) Mercury is visible only soon after the setting sun or shortly before dawn the Mariner 10 probe (1974/75) is the source of most information about Mercury – Messenger, launched 2004, first flypast in 2008 and orbit Mercury in 2011. ESA’s BepiColombo, to be launched in 2013 Mercury Mercury is like the Earth inside and the Moon outside Mercury has had a cooling and bombardment history similar to the moon It appears as cratered lava with scarps Its rocks are Earth-like Mariner 10 image Messenger images ↑ Double-ringed crater – a Mercury feature courtesy: http://messenger.jhuapl.edu/gallery/sciencePhotos/pics/S trom02.jpg ← Courtesy: http://messenger.jhuapl.edu/gal lery/sciencePhotos/pics/EN010 8828161M.jpg Messenger image Courtesy: http://messenger.jhuapl.edu/gallery/sciencePhotos/pics/Prockter06.jpg Mercury Close-up Mercury’s topography was formed under stronger gravity than on the Moon The Caloris basin is an impact crater ~1400 km across, beneath which is thought to be a dense mass 2 Mercury’s rotation period is exactly /3 of its orbital period -
1 the Martian Near Surface
The Martian Near Surface Environment: Analysis of Antarctic Soils and Laboratory Experiments on Putative Martian Organics Item Type text; Electronic Dissertation Authors Archer, Paul Douglas Publisher The University of Arizona. Rights Copyright © is held by the author. Digital access to this material is made possible by the University Libraries, University of Arizona. Further transmission, reproduction or presentation (such as public display or performance) of protected items is prohibited except with permission of the author. Download date 07/10/2021 13:24:53 Link to Item http://hdl.handle.net/10150/195892 1 THE MARTIAN NEAR SURFACE ENVIRONMENT: ANALYSIS OF ANTARCTIC SOILS AND LABORATORY EXPERIMENTS ON PUTATIVE MARTIAN ORGANICS by Paul Douglas Archer, Jr. _____________________ A Dissertation Submitted to the Faculty of the DEPARTMENT OF PLANETARY SCIENCES In Partial Fulfillment of the Requirements For the Degree of DOCTOR OF PHILOSOPHY In the Graduate College THE UNIVERSITY OF ARIZONA 2010 2 THE UNIVERSITY OF ARIZONA GRADUATE COLLEGE As members of the Dissertation Committee, we certify that we have read the dissertation prepared by Paul Douglas Archer, Jr. entitled The Martian Near Surface Environment: Analysis of Antarctic Soils and Laboratory Experiments on Putative Martian Organics and recommend that it be accepted as fulfilling the dissertation requirement for the Degree of Doctor of Philosophy _______________________________________________________________________ Date: April 22, 2010 Peter H. Smith _______________________________________________________________________ -
Phoenix Mission to Mars Will Search for Climate Clues 22 May 2008
Phoenix mission to Mars will search for climate clues 22 May 2008 On May 25, 2008, approaching 5 p.m. PDT, NASA Phoenix will touch down in Green Valley with the scientists will be wondering: Just how green is their aid of a parachute, retro rockets and three strong valley? That's because at that time the Phoenix legs with shock absorbing footpads to slow it Mars Mission space vehicle will be touching down down. on its three legs to make a soft landing onto the northern Mars terrain called Green Valley. That's sol (a Martian day) zero. Of course, no valley is actually green on the Red "We'll know within two hours of landing if Phoenix Planet. The place got its name after analysis of landed nominally," said Arvidson. "It will land, images from Mars Reconnaissance Orbiter's deploy its solar panels, take a picture and then go HiRISE instrument. HiRISE can image rocks on to bed." Mars as small as roughly a yard and a half across. Green is the color that that landing site selection The next day, Sol 1, begins a crucial period of team used to represent the fewest number of rocks operations for the mission. Arvidson said, "We'll be in an area, corresponding to a desirable place to checking out the instruments and begin robotic arm land. Thus, "green valley," a relatively rock-less operations within about a week, if everything goes region, is a "sweet spot" where the Phoenix well, and collect soil and ice samples over the spacecraft will land. -
Phoenix–Thefirst Marsscout Mission
Phoenix – The First Mars Scout Mission Barry Goldstein Jet Propulsion Laboratory, California Institute of Technology Pasadena CA [email protected] Robert Shotwell Jet Propulsion Laboratory, California Institute of Technology [email protected] Abstract —1 2As the first of the new Mars Scouts missions, 4) Characterize the history of water, ice, and the polar the Phoenix project was select ed by NASA in August of climate. Determine the past and present biological potential 2003. Four years later, almost to the day, Phoenix was of the surface and subsurface environments. launched from Cape Canaveral Air Station and successfully injected into an interplanetary trajectory on its way to Mars. TABLE OF CONTENTS On May 25, 2008 Phoenix conducted the first successful 1. INTRODUCTION ..................................................... 1 powered decent on Mars in over 30 years. This paper will 2. DEVELOPMENT PHASE ACTIVITIES ..................... 3 highlight some of the key changes since the 2008 IEEE 3. ENTRY DESCENT & LANDING MATURITY .......... 11 paper of the same name, as well as performance through 4. CONCLUSION ....................................................... 18 cruise, landing at the north pole of Mars and some of the REFERENCES ........................................................... 19 preliminary results of the surface mission. BIOGRAPHIES .......................................................... 20 Phoenix “Follows the water” responding directly to the recently published data from Dr. William Boynton, PI (and 1. INTRODUCTION Phoenix co-I) of the Mars Odyssey Gamma Ray Spectrometer (GRS). GRS data indicate extremely large The first of a new series of highly ambitious missions to quantities of water ice (up to 50% by mass) within the upper explore Mars, Phoenix was selected in August 2003 to 50 cm of the northern polar regolith. -
Camera on Mars Orbiter Snaps Phoenix During Landing 27 May 2008
Camera on Mars Orbiter Snaps Phoenix During Landing 27 May 2008 information that it was in good health after its first night on Mars, and the Phoenix team sent the spacecraft its to-do list for the day. "We can see cracks in the troughs that make us think the ice is still modifying the surface," said Phoenix Principal Investigator Peter Smith of the University of Arizona, Tucson. "We see fresh cracks. Cracks can't be old. They would fill in." Camera pointing for the image from HiRISE used navigational information about Phoenix updated on landing day. The camera team and Phoenix team would not know until the image was sent to Earth whether it had actually caught Phoenix. "We saw a few other bright spots in the image first, but when we saw the parachute and the lander with the cords connecting them, there was no question," said HiRISE Principal Investigator Alfred McEwen, also of the University of Arizona. NASA's Mars Phoenix Lander can be seen parachuting "I'm floored. I'm absolutely floored," said Phoenix down to Mars, in this image captured by the High Project Manager Barry Goldstein of NASA's Jet Resolution Imaging Science Experiment camera on Propulsion Laboratory, Pasadena, Calif. A team NASA's Mars Reconnaissance Orbiter. Image credit: analyzing what can be learned from the Phoenix NASA/JPL-Calech/University of Arizona descent through the Martian atmosphere will use the image to reconstruct events. HiRISE usually points downward. For this image, A telescopic camera in orbit around Mars caught a the pointing was at 62 degrees, nearly two-thirds of view of NASA's Phoenix Mars Lander suspended the way from straight down to horizontal. -
From Dust to Dust: Protoplanetary Disk Accretion, Hot Jupiter Climates, and the Evaporation of Rocky Planets
UC Berkeley UC Berkeley Electronic Theses and Dissertations Title From Dust to Dust: Protoplanetary Disk Accretion, Hot Jupiter Climates, and the Evaporation of Rocky Planets Permalink https://escholarship.org/uc/item/9jq3136f Author Perez-Becker, Daniel Alonso Publication Date 2013 Peer reviewed|Thesis/dissertation eScholarship.org Powered by the California Digital Library University of California From Dust to Dust: Protoplanetary Disk Accretion, Hot Jupiter Climates, and the Evaporation of Rocky Planets By Daniel Alonso Perez-Becker A dissertation submitted in partial satisfaction of the requirements for the degree of Doctor of Philosophy in Physics in the Graduate Division of the University of California, Berkeley Committee in charge: Professor Eugene Chiang, Co-chair Professor Christopher McKee, Co-chair Professor Eliot Quataert Professor Geoffrey Marcy Fall 2013 From Dust to Dust: Protoplanetary Disk Accretion, Hot Jupiter Climates, and the Evaporation of Rocky Planets Copyright 2013 by Daniel Alonso Perez-Becker 1 Abstract From Dust to Dust: Protoplanetary Disk Accretion, Hot Jupiter Climates, and the Evaporation of Rocky Planets by Daniel Alonso Perez-Becker Doctor of Philosophy in Physics University of California, Berkeley Professor Eugene Chiang, Co-chair Professor Christopher McKee, Co-chair This dissertation is composed of three independent projects in astrophysics concerning phenomena that are concurrent with the birth, life, and death of planets. In Chapters 1 & 2, we study surface layer accretion in protoplanetary disks driven stellar X-ray and far-ultraviolet (FUV) radiation. In Chapter 3, we identify the dynamical mechanisms that control atmospheric heat redistribution on hot Jupiters. Finally, in Chapter 4, we characterize the death of low-mass, short-period rocky planets by their evaporation into a dusty wind. -
Space Optics Contributions by the College of Optical Sciences Over the Past 50 Years
Invited Paper Space optics contributions by the College of Optical Sciences over the past 50 years James B. Breckinridge*a and Peter Smithb aGraduate Aeronautical Laboratory, M/S 150-50 Firestone, Caltech, 1200 E. California Blvd. , Pasadena, CA., 91125; bLunar and Planetary Laboratory, University of Arizona, Tucson, AZ. 85721 ABSTRACT We present a review of the contributions by students, staff, faculty and alumni to the Nation’s space program over the past 50 years. The balloon polariscope led the way to future space optics missions. The missions Pioneer Venus (large probe solar flux radiometer), Pioneer 10/11 (imaging photopolarimeter) to Jupiter and Saturn, Hubble Space Telescope (HST), and next generation large aperture space telescopes are discussed. Keywords: Pioneer 10/11, Imaging, Photopolarimetry, Pioneer Venus, Jupiter, Saturn, Venus, Radiometry, balloon polariscope and space telescopes 1. INTRODUCTION The successful development of rocket engines during WW2 inspired the image of space telescopes and the exploration of the solar system. The May 29, 1944 issue of Life Magazine (p. 78) shows the first science based drawings of what a man walking on a planetary surface might see. Made by Chesley Bonestell these images inspired generations of astronomers, geologists and the general public. In 1946 Professor Lyman Spitzer of Princeton University proposed the construction of a space telescope for astrophysics. Thus were planted the seeds of modern space telescopes for planetary science and astrophysics. The Optical Science Center was founded only 6 years after the Russians orbited Sputnik. In the fall of 1958 President Eisenhower established the civilian space agency: National Aeronautics and Space Agency (NASA). -
Arxiv:1711.02098V2 [Astro-Ph.EP] 13 Jan 2018
Draft version January 16, 2018 Typeset using LATEX twocolumn style in AASTeX61 SIMULATED JWST/NIRISS TRANSIT SPECTROSCOPY OF ANTICIPATED TESS PLANETS COMPARED TO SELECT DISCOVERIES FROM SPACE-BASED AND GROUND-BASED SURVEYS Dana R. Louie,1 Drake Deming,1, 2 Loic Albert,3 L. G. Bouma,4 Jacob Bean,5, 2 and Mercedes Lopez-Morales6, 2 1Department of Astronomy, University of Maryland, College Park, MD 20742, USA 2TESS Atmospheric Characterization Working Group 3Institut de recherche sur les exoplanetes (iREx), Universite de Montreal, Montreal, Quebec, Canada 4Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08540, USA 5Department of Astronomy and Astrophysics, University of Chicago, IL 60637, USA 6Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA Submitted to PASP ABSTRACT The Transiting Exoplanet Survey Satellite (TESS) will embark in 2018 on a 2-year wide-field survey mission, discov- ering over a thousand terrestrial, super-Earth and sub-Neptune-sized exoplanets (Rpl ≤ 4R⊕) potentially suitable for follow-up observations using the James Webb Space Telescope (JWST). This work aims to understand the suitability of anticipated TESS planet discoveries for atmospheric characterization by JWST's Near InfraRed Imager and Slitless Spectrograph (NIRISS) by employing a simulation tool to estimate the signal-to-noise (S/N) achievable in transmission spectroscopy. We applied this tool to Monte Carlo predictions of the TESS expected planet yield and then compared the S/N for anticipated TESS discoveries to our estimates of S/N for 18 known exoplanets. We analyzed the sensitivity of our results to planetary composition, cloud cover, and presence of an observational noise floor.