DOCSLIB.ORG

Ios Hot Spots in the Nearinfrared Detected by LEISA During the New Horizons Flyby

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Ios Hot Spots in the Nearinfrared Detected by LEISA During the New Horizons Flyby PUBLICATIONS Journal of Geophysical Research: Planets RESEARCH ARTICLE Io’s hot spots in the near-infrared detected by LEISA 10.1002/2014JE004670 during the New Horizons flyby Key Points: Constantine C. C. Tsang1, Julie A. Rathbun2, John R. Spencer1, Brigette E. Hesman3, and Oleg Abramov4 • Io’s nightside near-infrared thermal emissions mapped 1Department of Space Studies, Southwest Research Institute, Boulder, Colorado, USA, 2Department of Physics, University of • A total of 36 hot spots detected, 4 new 3 hot spots Redlands, Redlands, California, USA, Department of Astronomy, University of Maryland, College Park, Maryland, USA, 4 • Global coverage on the nightside Astrogeology Science Center, United States Geological Survey, Flagstaff, Arizona, USA Abstract The New Horizons spacecraft flew past Jupiter and its moons in February and March 2007. The Correspondence to: flyby provided one of the most comprehensive inventories of Io’s active plumes and hot spots yet taken, C. C. C. Tsang, [email protected] including the large 350 km high eruption of Tvashtar. Among the suite of instruments active during the flyby was the Linear Etalon Infrared Spectral Array (LEISA), a near-infrared imaging spectrometer covering the spectral range 1.25 to 2.5 μm. We have identified 37 distinct hot spots on Io in the nine LEISA spectral Citation: fl fi Tsang, C. C. C., J. A. Rathbun, J. R. Spencer, imagecubestakenduringthe yby. We describe the thermal emissions from these volcanoes and t B. E. Hesman, and O. Abramov (2014), single-component blackbody curves to the hot spot spectra to derive eruption temperatures, areas, and Io’s hot spots in the near-infrared power output for the hot spots with sufficient signal-to-noise. Of these, 11 hot spots were seen by LEISA more detected by LEISA during the New Horizons flyby, J. Geophys. Res. Planets, than once, and East Girru showed short-term variability over a few days, also seen by other New Horizons 119, 2222–2238 doi:10.1002/ instruments. This work presents a comprehensive look at the global distribution of Io’s volcanism at the time of 2014JE004670. the flyby. From these measurements, we estimate the global power output of high-temperature (>550 K) volcanism on Io to be ~8 TW. This work provides the first short-wavelength near-infrared survey with global Received 19 MAY 2014 Accepted 17 SEP 2014 coverage at all longitudes on the nightside of Io without sunlight contamination at these wavelengths. A major Accepted article online 19 SEP 2014 conclusion from this study is that 90% of all the volcanoes observed in the New Horizons LEISA near-infrared Published online 16 OCT 2014 data in 2007 were also observed during the Galileo epoch, suggesting these are all long-lived hot spots. 1. Introduction Since the discovery of active volcanism on Io in 1979 by the Voyager 1 spacecraft [Pearl et al., 1979], Io has been extensively observed and studied in an attempt to understand the source and the driving mechanisms of its widespread volcanism. Numerous studies of Ionian volcanoes have focused on their spatial distribution [Williams et al., 2011; Veeder et al., 2012], physical characteristics such as temperature and emitted areas [e.g., Allen et al., 2013], temporal variability [e.g., Davies and Ennis, 2011; Rathbun and Spencer, 2010], eruption style [e.g., Davies et al., 2006], and emitted power [e.g., Davies, 2003]. The Galileo spacecraft notably provided the most detailed snapshot of these volcanoes over 20 orbits between 1996 and 2001. Continued long-term ground-based observations of Io’svolcanism,ateverimproving spatial resolutions, especially in the near-infrared [e.g., Marchis et al., 2005], can provide the ability to study the temporal variability of hot spots over decadal timescales [e.g., Rathbun and Spencer, 2006]. However, only a few ground-based observatories have the ability to spatially resolve more than a few of the brightest individual hot spots at all Io longitudes. In this study, we present estimates of temperatures, emitting areas, and powers of 17 volcanoes, from a total of some 37 detected volcanoes observed at all longitudes, from the New Horizons flyby of Io in 2007. By doing so, we provide a rare instantaneous homogeneous inventory of the global distribution of high-temperature Io volcanism, as the flyby covered all longitude ranges on Io. 2. New Horizon LEISA Observations The New Horizons spacecraft was launched in January 2006 and will arrive at Pluto in 2015. One of the instruments on board is Ralph, which consists of two subsystems, MVIC, the Multispectral Visible Imaging Camera and LEISA, the Linear Etalon Infrared Spectral Array. The analysis of the MVIC data on Io’s hot spots during the New Horizons flyby of Io is presented in Rathbun et al. [2014]. Here we present the LEISA observations from that same flyby. LEISA covers the wavelength region between 1.25 and 2.5 μm, at spectral resolving powers of ~240, with a higher-resolving power segment (R ~ 540) covering 2.1 to 2.25 μm. Both TSANG ET AL. ©2014. American Geophysical Union. All Rights Reserved. 2222 Journal of Geophysical Research: Planets 10.1002/2014JE004670 segments share the same detector array. Each row on the detector is sensitive to a particular wavelength. The target is scanned across the rows, resulting in a 256 × 256 × N (spatial [x], spatial + spectral [y + λ], temporal [t]) pixel image cube with a 62 μrad per pixel field of view, where N is depends on the scan rate and duration of each scan. For the Io observations, N = 356 temporal frames. These cubes can be rectified to produce conventional x, y, λ spatial/spectral image cubes, though we did not do this for the present analysis. In this work, we only use the lower resolution 1.25–2.5 μm segment due to the wider spectral sample [Reuter et al., 2008]. New Horizons flew by Io in February 2007, with closest approach occurring on 28 February at a range of 2.26 million km, with LEISA observations ranging from this closest approach to a distance of 3.04 million km. Other remote sensing observations of Io including monochromatic and color images [Spencer et al., 2007; Rathbun et al., 2014] and ultraviolet spectra [Retherford et al., 2007] were taken. Initial analysis of the detected hot spots and temperatures from LEISA was presented in Spenceretal.[2007].LEISAtooka total of nine spectral image cubes in the near-infrared, presented here in full. Io was observed at solar phase angles ranging from 36° to 120°, some when Io was in eclipse (Table 1). 2.1. Data Calibration We use Level 2 calibrated data taken from NASA’s Planetary Data System (PDS). The Level 2 data include the observed radiances and wavelengths at each pixel, and the ephemeris required to interpret the data. Further detail can be found in Reuter et al. [2008]. The PDS calibration is inaccurate, and the LEISA spectra presented in Spenceretal. [2007, hereinafter referred to as S07] used a different method of arriving at the radiometric calibration that does not provide the best possible calibration for fluxes.Wehavetherefore improved the radiometric calibration for this work. An accurate radiometric calibration is important because any uncertainty in the absolute radiances can lead to uncertainty in the derived area of hot spots, while wavelength-dependent changes in the radiance lead to changes in the derived temperatures. To better determine the absolute radiances, we compared LEISA spectra taken from the standard star Vega, between 2001 and 2006 during cruise, with its well characterized 1–2.5 μm spectra from other works [Castelli and Kurucz, 1994]. The LEISA spectrum of Vega was divided by the standard Vega spectrum to produce a wavelength-dependent calibration correction. This was done three separate times during annual checkout (ACO) observations 2 (18 October 2008), 4 (24 June 2010), and 6 (1 June 2012). The average of these spectra was used as the final conversion (Figure 1), which we applied to all Level 2 (L2) radiometric values from the PDS. 2.2. Data Reduction We extract hot spot spectra in each observation using the following procedure. We take the spectral image cube (x, y + λ, t) and adjust for the motion of Io along the time (t) dimension. We then coadd the registered (x, y + λ) frames to produce a color composite image to maximize the signal-to-noise ratio (SNR) in order to identify the locations of the hot spots. We produce image composites (Figures 3–9) using approximately 100 frames in total per observation, with frames between approximately 1.7–1.9 μmfor blue, 1.9–2.2 μm for green, and 2.2–2.4 μm for red. The contrast is stretched to highlight the hot spots on the nightside of Io, saturating the dayside. We calculate the pixel positions of each hot spot relative to a bright reference hot spot such as Tvashtar or East Girru such that the bright reference hot spot can be tracked in each of the individual spectral frames. We do this because faint hot spots are difficult to observe and track at individual frames, particularly at shorter wavelengths. The tracking of the bright reference offset hot spot is usually done by manually stepping through each spectral frame and identifying the bright reference hot spot. This is difficult to do with an automatic algorithm because of confusion from “hot” pixels caused by cosmic rays or instrument noise. The positions of each hot spot are accurate to a pixel. As described below, this precision is sufficient to identify these hot spots, but not to determine if these hot spots have moved in location since Galileo observations. Observations by the Long-Range Reconnaissance Imager (LORRI) and MVIC instruments of Io’s hot spot in a companion work [Rathbun et al., 2014] were able to distinguish spatial movement of volcanic features.
Load more

Recommended publications
  • 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.
    [Show full text]
  • 1783-84 Laki Eruption, Iceland
    1783-84 Laki eruption, Iceland Eruption History and Atmospheric Effects Thor Thordarson Faculty of Earth sciences, University of Iceland 12/8/2017 1 Atmospheric Effects of the 1783-84 Laki Eruption in Iceland Outline . Volcano-Climate interactions - background Laki eruption . Eruption history . Sulfur release and aerosol loading . Plume transport and aerosol dispersal . Environmental and climatic effects 12/8/2017. Concluding Remarks 2 Santorini, 1628 BC Tambora, 1815 Etna, 44 BC Lakagígar, 1783 Toba, 71,000 BP Famous Volcanic Eruptions Krakatau, 1883 Pinatubo, 1991 El Chichón, 1982 Agung, 1963 St. Helens, 1980 Major volcanic eruptions of the past 250 years Volcano Year VEI d.v.i/Emax IVI Lakagígar [Laki craters], Iceland 1783 4 2300 0.19 Unknown (El Chichón?) 1809 0.20 Tambora, Sumbawa, Indonesia 1815 7 3000 0.50 Cosiguina, Nicaragua 1835 5 4000 0.11 Askja, Iceland 1875 5 1000 0.01* Krakatau, Indonesia 1883 6 1000 0.12 Okataina [Tarawera], North Island, NZ 1886 5 800 0.04 Santa Maria, Guatemala 1902 6 600 0.05 Ksudach, Kamchatka, Russia 1907 5 500 0.02 Novarupta [Katmai], Alaska, US 1912 6 500 0.15 Agung, Bali, Indonesia 1963 4 800 0.06 Mt. St. Helens, Washington, US 1980 5 500 0.00 El Chichón, Chiapas, Mexico 1982 5 800 0.06 Mt. Pinatubo, Luzon, Philippines 1991 6 1000 — Volcano – Climate Interactions Key to Volcanic Forcing is: SO2 mass loading, eruption duration plume height replenishment aerosol production, residence time 12/8/2017 5 Volcanic Forcing: sulfur dioxide sulfate aerosols SO2 75%H2SO4+ 25%H2O clear sky 1991 Pinatubo aerosols
    [Show full text]
  • Contents More Information
    Cambridge University Press 978-0-521-85003-2 - Volcanism on Io: A Comparison with Earth Ashley Gerard Davies Table of Contents More information Contents Preface page xi List of Abbreviations xiii Reproduction Permissions xv Introduction 1 Section 1 Io, 1610 to 1995: Galileo to Galileo 1 Io, 1610–1979 7 1.1 Io before Voyager 7 1.2 Prediction of volcanic activity 9 1.3 Voyager to Jupiter 9 1.4 Discovery of active volcanism 12 1.5 IRIS and volcanic thermal emission 18 1.6 Io: the view after Voyager 19 1.7 Summary 24 2 Between Voyager and Galileo: 1979–1995 27 2.1 Silicate volcanism on Io? 27 2.2 Ground-based observations 29 2.3 Observations of Io from Earth orbit 33 2.4 The Pele plume 33 2.5 Outburst eruptions 34 2.6 Stealth plumes 37 2.7 Io on the eve of Galileo 38 3 Galileo at Io 39 3.1 Instrumentation 41 3.2 Galileo observations of Io 46 Section 2 Planetary volcanism: evolution and composition 4 Io and Earth: formation, evolution, and interior structure 53 4.1 Global heat flow 53 4.2 Planetary formation 55 v © in this web service Cambridge University Press www.cambridge.org Cambridge University Press 978-0-521-85003-2 - Volcanism on Io: A Comparison with Earth Ashley Gerard Davies Table of Contents More information vi Contents 4.3 Post-formation heating 58 4.4 Interior structure 63 4.5 Volcanism over time 70 4.6 Implications 72 5 Magmas and volatiles 73 5.1 Basalt 73 5.2 Ultramafic magma 74 5.3 Lava rheology 76 5.4 Sulphur 78 5.5 Sulphur dioxide (SO2)86 Section 3 Observing and modeling volcanic activity 6 Observations: thermal remote sensing
    [Show full text]
  • Page 1 57° 50° 40° 30° 20° 10° 0° -10° -20° -30° -40° -50° -57° 57° 50
    180° 0° DODONA PLANUM 210° 330° 150° 30° 60° -60° . Bochica . Hatchawa Patera Patera . Nusku Patera . Hiruko Heno . Inti . Patera Patera Patera 70° -70° 240° 300° 60° 120° Tvashtar . Taranis Patera Iynx TARSUS Aramazd Mensa . Patera Tvashtar Paterae Haemus REGIO Montes Mensae LERNA REGIO 80° Echo -80°Mensa . Chors Nile Montes N Patera E M . Viracocha E Patera A 90° CHALYBES 270° 90° P 270° L A . Mithra N Patera U REGIO M . Vivasvant Patera . Crimea Mons 80° -80° Pyerun . Patera Dazhbog 120° 60° Patera . 300° 240° 70° -70° ILLYRIKON REGIO 60° -60° 30° 150° 330° 210° 0° 180° NORTH POLAR REGION SOUTH POLAR REGION 180° 170° 160° 150° 140° 130° 120° 110° 100° 90° 80° 70° 60° 50° 40° 30° 20° 10° 0° 350° 340° 330° 320° 310° 300° 290° 280° 270° 260° 250° 240° 230° 220° 210° 200° 190° 180° 57° 57° Nile Montes Dazhbog Patera CHALYBES REGIO 50° 50° . Kinich Ahau . Savitr Patera Patera Surt Zal Montes Lei-Kung Zal Fluctus . Fo Patera 40° 40° Patera Thor . Amaterasu . Dusura Patera Patera BULICAME . Manua Patera Shango REGIO Arinna . _ Patera Ukko . Atar Fluctus . Patera Patera Heiseb Isum 30° . 30° Fuchi Patera Patera Reshef Euxine . Patera Mons Patera Volund . Thomagata Amirani Patera . Shakuru Skythia Mons Girru . Mongibello . Tiermes Patera . Susanoo Donar Surya Estan Patera Patera . Patera Mons Patera Fluctus Patera Monan Daedalus 20° . Patera Loki . 20° Zamama Maui . Gish Bar Patera Mons Mulungu Steropes Maui . Patera . Patera Ruaumoko . Camaxtli Patera Gish Bar Sobo Patera . Patera Patera Fluctus Monan Loki Chaac . Ababinili Tien Mu Mons Llew . Balder Patera . Fjorgynn Patera .
    [Show full text]
  • Submarine Growth of a Hawaiian Shield Volcano
    SUBMARINE GROWTH OF A HAWAIIAN SHIELD VOLCANO BASED ON VOLCANICLASTICS IN THE HAWAIIAN SCIENTIFIC DRILLING PROJECT 2 CORE A THESIS SUBMITTED TO THE GRADUATE DIVISION OF THE UNIVERSITY OF HAWAI'I IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF MASTER OF SCIENCE IN GEOLOGY & GEOPHYSICS DECEMBER 2004 By Kate Phillippa Bridges Thesis Committee: Michael O. Garcia, Chairperson Bruce Houghton Thor Thordarson ACKNOWLEDGEMENTS I would like to thank my teachers and colleagues at the University of Hawai'i at Manoa Geology and Geophysics department for their inspiration and encouragement. In particular, I would like to thank Mike Garcia for giving me the opportunity to pursue and complete a Master's degree in volcanology at the University of Hawai'i. In addition, I am very grateful for all the support he has given me throughout the past three years and his sense of humor. Mahalos also to Thor Thordarsen, who always had words of encouragement to accompany his insightful comments on the progress and outcome of this study. Thanks to Bruce Houghton for sound scientific advise and guidance. Finally, muchos mahalos to all my friends for making the journey to Masterhood fun and, of course, to my folks! iii Acknowledgements iii List of figures vii List of tables viii Abstract ix 1. INTRODUCTION 1 1.1 Geological setting 2 1.2 Models for the growth of shield volcanoes 4 1.2.1 Magma supply and stages 4 1.2.2 Deposits 5 1.2.3 Subsidence and collapse ..7 1.3 Hawaiian Scientific Drilling Project 9 1.3.1 Introduction, 9 1.3.2 Basic stratigraphy of the HSDP2 core .11 1.3.3 Introduction to the HSDP2 volcaniclastics 14 1.4 Terminology 21 1.5 Subaqueous fragmentation of basaltic magma 23 1.5.1 Magmatic explosivity 23 1.5.2 Steam explosivity 24 Littoral magma:water interaction Subaqueous magma:water interaction 1.5.3 Passive quenching and autobrecciation of lava ~ 29 1.5.4 Secondary fragmentation of basaltic magma 29 2.
    [Show full text]
  • Nuclear Power to Advance Space Exploration Gary L
    Poster Paper P. 7.7 First Flights: Nuclear Power to Advance Space Exploration Gary L. Bennett E. W. Johnson Metaspace Enterprises EWJ Enterprises Emmett, Idaho Centerville, Ohio International Air & Space Symposium and Exposition Dayton Convention Center 14-17 July 2003 Dayton, Ohio USA r ... penni.. l .. 10 p~bli . h ..... ..,."b ll .~, ... ~ t .d til. <Op)'rigbt 0 ........ aomod oa tho fin' po_" ...... A1M.IIdd ..., yri ,hl, ... rit< .. AIM hrmi.. lou Dop a_I, 18(11 AI . ..od ... B<l1 Ori .... S.11e SIlO , R.stu. VA. 20191""-i44 FIRST FLIGHTS: NUCLEAR POWER TO ADVANCE SPACE EXPLORATION Gary L. Bennett E. W. Johnson Metaspace Enterprises EWJ Enterprises 5000 Butte Road 1017 Glen Arbor Court Emmett, Idaho 83617-9500 Centerville, Ohio 45459-5421 Tel/Fax: 1+208.365.1210 Telephone: 1+937.435.2971 E-mail: [email protected] E-mail: [email protected] Abstract One of the 20th century's breakthroughs that enabled and/or enhanced challenging space flights was the development of nuclear power sources for space applications. Nuclear power sources have allowed spacecraft to fly into regions where sunlight is dim or virtually nonexistent. Nuclear power sources have enabled spacecraft to perform extended missions that would have been impossible with more conventional power sources (e.g., photovoltaics and batteries). It is fitting in the year of the 100th anniversary of the first powered flight to consider the advancements made in space nuclear power as a natural extension of those first flights at Kitty Hawk to extending human presence into the Solar System and beyond. Programs were initiated in the mid 1950s to develop both radioisotope and nuclear reactor power sources for space applications.
    [Show full text]
  • Geologic Mapping of Tupan Patera and Experimental Models
    Brigham Young University BYU ScholarsArchive Theses and Dissertations 2014-07-01 Paterae on Io: Geologic Mapping of Tupan Patera and Experimental Models Megan Carolee Decker Brigham Young University - Provo Follow this and additional works at: https://scholarsarchive.byu.edu/etd Part of the Geology Commons BYU ScholarsArchive Citation Decker, Megan Carolee, "Paterae on Io: Geologic Mapping of Tupan Patera and Experimental Models" (2014). Theses and Dissertations. 5306. https://scholarsarchive.byu.edu/etd/5306 This Thesis is brought to you for free and open access by BYU ScholarsArchive. It has been accepted for inclusion in Theses and Dissertations by an authorized administrator of BYU ScholarsArchive. For more information, please contact [email protected], [email protected]. Paterae on Io: Geologic Mapping of Tupan Patera and Experimental Models Megan C. Decker A thesis submitted to the faculty of Brigham Young University in partial fulfillment of the requirements for the degree of Master of Science Jani Radebaugh, Chair Eric H. Christiansen Michael J. Dorais Department of Geological Sciences Brigham Young University July 2014 Copyright © 2014 Megan C. Decker All Rights Reserved ABSTRACT Paterae on Io: Geologic Mapping of Tupan Patera and Experimental Models Megan C. Decker Department of Geological Sciences, BYU Master of Science Paterae cover approximately 2% of the surface of Io, Jupiter’s volcanically active moon. To understand the formation of these volcano-tectonic depressions we created a geologic map of a key region and compared this map with experimental models for Io paterae. Our mapping region is Tupan Patera, a patera that has experienced recent activity and is a detected hot spot.
    [Show full text]
  • Keck AO Survey of Io Global Volcanic Activity Between 2 and 5 Mu M
    Keck AO Survey of Io Global Volcanic Activity between 2 and 5µm F. Marchis Astronomy Department, University of California, Berkeley, California 94720-3411, U.S.A. and D. Le Mignant W. M. Keck Observatory, 65-1120 Mamalahoa Hwy, Kamuela, Hawaii 96743, U.S.A. and F. H. Chaffee W.M. Keck Observatory, 65-1120 Mamalahoa Hwy, Kamuela HI96743, U.S.A. and A.G. Davies Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, California 91109-8099, U.S.A. and S. H. Kwok W. M. Keck Observatory, 65-1120 Mamalahoa Hwy, Kamuela, Hawaii 96743, U.S.A. – 2 – and R. Prang´e Institut d’Astrophysique Spatiale, bat.121, Universit´eParis Sud, 91405 Orsay Cedex, France and I. de Pater Astronomy Department, University of California, Berkeley, California 94720-3411, U.S.A. and P. Amico W. M. Keck Observatory, 65-1120 Mamalahoa Hwy, Kamuela, Hawaii 96743, U.S.A. and R. Campbell W. M. Keck Observatory, 65-1120 Mamalahoa Hwy, Kamuela, Hawaii 96743, U.S.A. and T. Fusco ONERA, DOTA-E, BP 72, F-92322 Chatillon, France and – 3 – R. W. Goodrich W. M. Keck Observatory, 65-1120 Mamalahoa Hwy, Kamuela, Hawaii 96743, U.S.A. and A. Conrad W. M. Keck Observatory, 65-1120 Mamalahoa Hwy, Kamuela, Hawaii 96743, U.S.A. Received ; accepted Manuscript: 82 pages; 7 tables, 6 figures – 4 – Running title: Keck AO Survey of Io Global Volcanic Activity between 2 and 5 µm Send correspondence to F. Marchis, University of California at Berkeley, Department of Astronomy, 601 Campbell Hall, Berkeley, CA 94720, USA tel: +1 510 642 3958 e-mail: [email protected] ABSTRACT We present in this Keck AO paper the first global high angular resolution observations of Io in three broadband near-infrared filters: Kc (2.3 µm), Lp (3.8 µm) and Ms (4.7 µm).
    [Show full text]
  • Surface Changes on Io During the Galileo Mission
    Icarus 169 (2004) 29–64 www.elsevier.com/locate/icarus Surface changes on Io during the Galileo mission Paul Geissler,a,∗ Alfred McEwen,b Cynthia Phillips,c Laszlo Keszthelyi,a and John Spencer d a U.S. Geological Survey, 2255 N. Gemini Dr., Flagstaff, AZ 86001, USA b Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA c SETI Institute, 2035 Landings Drive, Mountain View, CA 94043, USA d Lowell Observatory, 1400 W. Mars Hill Rd., Flagstaff, AZ 86001, USA Received 14 February 2003; revised 9 September 2003 Abstract A careful survey of Galileo SSI global monitoring images revealed more than 80 apparent surface changes that took place on Io during the 5 year period of observation, ranging from giant plume deposits to subtle changes in the color or albedo of patera surfaces. Explosive volcanic activity was discovered at four previously unrecognized centers: an unnamed patera to the south of Karei that produced a Pele-sized red ring, a patera to the west of Zal that produced a small circular bright deposit, a large orange ring detected near the north pole of Io, and a small bright ring near Io’s south pole. Only a handful of Io’s many active volcanoes produced large scale explosive eruptions, and several of these erupted repeatedly, leaving at least 83% of Io’s surface unaltered throughout the Galileo mission. Most of the hot spots detected from SSI, NIMS and ground-based thermal observations caused no noticeable surface changes greater than 10 km in extent over the five year period. Surface changes were found at every location where active plumes were identified, including Acala which was never seen in sunlight and was only detected through auroral emissions during eclipse.
    [Show full text]
  • Keck AO Survey of Io Global Volcanic Activity Between 2 and 5 Mu M
    UC Berkeley UC Berkeley Previously Published Works Title Keck AO survey of Io global volcanic activity between 2 and 5 mu m Permalink https://escholarship.org/uc/item/5346300m Journal Icarus, 176(1) ISSN 0019-1035 Authors Marchis, F Le Mignant, D Chaffee, F H et al. Publication Date 2005-07-01 Peer reviewed eScholarship.org Powered by the California Digital Library University of California Keck AO Survey of Io Global Volcanic Activity between 2 and 5µm F. Marchis Astronomy Department, University of California, Berkeley, California 94720-3411, U.S.A. and D. Le Mignant W. M. Keck Observatory, 65-1120 Mamalahoa Hwy, Kamuela, Hawaii 96743, U.S.A. and F. H. Chaffee W.M. Keck Observatory, 65-1120 Mamalahoa Hwy, Kamuela HI96743, U.S.A. and A.G. Davies Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, California 91109-8099, U.S.A. and S. H. Kwok W. M. Keck Observatory, 65-1120 Mamalahoa Hwy, Kamuela, Hawaii 96743, U.S.A. – 2 – and R. Prang´e Institut d’Astrophysique Spatiale, bat.121, Universit´eParis Sud, 91405 Orsay Cedex, France and I. de Pater Astronomy Department, University of California, Berkeley, California 94720-3411, U.S.A. and P. Amico W. M. Keck Observatory, 65-1120 Mamalahoa Hwy, Kamuela, Hawaii 96743, U.S.A. and R. Campbell W. M. Keck Observatory, 65-1120 Mamalahoa Hwy, Kamuela, Hawaii 96743, U.S.A. and T. Fusco ONERA, DOTA-E, BP 72, F-92322 Chatillon, France and – 3 – R. W. Goodrich W. M. Keck Observatory, 65-1120 Mamalahoa Hwy, Kamuela, Hawaii 96743, U.S.A.
    [Show full text]
  • Mission Design for Grades 5-8 and 9-12
    MESSENGER Education Module M ISSION D ESIGN F o r G r a d e s 5-8 and 9-12 MESSENGER Education and Public Outreach (EPO) Team Education and Public Outreach Project Manager and Team Lead Julie Edmonds, Ph.D. Science Team Liaison to EPO Team Clark R. Chapman, Ph.D. The MESSENGER EPO effort is a collaboration among the following organizations: American Association for the Advancement of Science (AAAS) Bob Hirshon, Senior Project Director, Media Programs Carnegie Academy for Science Education (CASE), Carnegie Institution of Washington Julie Edmonds, Ph.D., Co-Director, CASE Center for Educational Resources (CERES) at Montana State University (MSU) – Bozeman George F. Tuthill, Ph.D., Project Director Keri Garver Hallau, Online Science Curriculum Development Specialist National Center for Earth and Space Science Education (NCESSE) Jeff J. Goldstein, Ph.D., Center Director Timothy A. Livengood, Ph.D., Senior Science Researcher Harri A. T. Vanhala, Ph.D., Science Researcher National Air and Space Museum (NASM) Thomas R. Watters, Ph.D., Senior Scientist/Geologist Science Systems and Applications, Inc. (SSAI) Heather Weir, Senior Science Education Specialist Southwest Research Institute (SwRI) Clark R. Chapman, Ph.D., Senior Scientist R E G N SE MES MESSENGER Education Module Mission Design for Grades 5-8 and 9-12 Development Team National Center for Earth and Space Science Education PO Box 3806, Capitol Heights, MD 20791-3806 Web: http://ncesse.org | Email: [email protected] Harri A. T. Vanhala, Ph.D. Elizabeth A. Miller, Ed.M. Kenneth Pulkkinen, M.S. Special Thanks Science and Education Reviews, Edits, and Field Testing Denise Edelson, MESSENGER Educator Fellow Lollie Garay, MESSENGER Educator Fellow Jane Gilbridge, MESSENGER Educator Fellow Sally Jean Jensen, MESSENGER Educator Fellow Madge Nanney, MESSENGER Educator Fellow Lora Bleacher, Science Systems and Applications, Inc.
    [Show full text]
  • Athena COUSTENIS ESSC-ESF and Paris Observatory-CNRS [email protected] ESA Science Programme
    CAPSScience Meeting Programme Committee ESA Science Programme Irvine, 12 Sept.ESAC, 2017 21 June 2017 Overview of ESA’s current and future planetary science missions Athena COUSTENIS ESSC-ESF and Paris Observatory-CNRS [email protected] SCIENCE The European Space Agency Current Scientific Programmes • Science Mandatory Programme • Human Spaceflight and Robotic Exploration Programme • Earth Observation Programme The European Space Agency Current Scientific Programmes • Science Mandatory Programme (SCI) • Human Spaceflight and Robotic Exploration Programme (HSRE): Mars & the Moon • Earth Observation Programme Basics of the SCI and HSRE Programmes .The Programmes are Science-driven and exploratory: both long-term science and exploratory planning ; mission or experiment calls are bottom-up processes, relying on broad community input, advisory structure and peer review. .The Science Programme is Mandatory: all member states contribute pro-rata to GDP providing budget stability, allowing long-term planning of its scientific goals and being the backbone of the Agency. .The Human Spaceflight and Robotic Exploration Programme is optional: 17 countries and Canada contribute. E3P encompasses ISS, astronauts, Orion, Moon and Mars destinations … ESA science programme Successes and objectives of the science mandatory programme – Based on peer-reviewed selection of missions on the basis of scientific excellence following an open call. The content of the Programme (which missions?) is decided by the SPC (national delegates). – Long-term planning to service a broad community with the annual budget over 4-5 years decided at ESA Council at Ministerial level. – Regular sequence of launches based on a balance of mission sizes (Small, Medium, Large), fostering both ambitious, high-return missions and faster, smaller missions.
    [Show full text]