Dynamical Stability of the Inner Belt Around Epsilon Eridani
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Where Are the Distant Worlds? Star Maps
W here Are the Distant Worlds? Star Maps Abo ut the Activity Whe re are the distant worlds in the night sky? Use a star map to find constellations and to identify stars with extrasolar planets. (Northern Hemisphere only, naked eye) Topics Covered • How to find Constellations • Where we have found planets around other stars Participants Adults, teens, families with children 8 years and up If a school/youth group, 10 years and older 1 to 4 participants per map Materials Needed Location and Timing • Current month's Star Map for the Use this activity at a star party on a public (included) dark, clear night. Timing depends only • At least one set Planetary on how long you want to observe. Postcards with Key (included) • A small (red) flashlight • (Optional) Print list of Visible Stars with Planets (included) Included in This Packet Page Detailed Activity Description 2 Helpful Hints 4 Background Information 5 Planetary Postcards 7 Key Planetary Postcards 9 Star Maps 20 Visible Stars With Planets 33 © 2008 Astronomical Society of the Pacific www.astrosociety.org Copies for educational purposes are permitted. Additional astronomy activities can be found here: http://nightsky.jpl.nasa.gov Detailed Activity Description Leader’s Role Participants’ Roles (Anticipated) Introduction: To Ask: Who has heard that scientists have found planets around stars other than our own Sun? How many of these stars might you think have been found? Anyone ever see a star that has planets around it? (our own Sun, some may know of other stars) We can’t see the planets around other stars, but we can see the star. -
100 Closest Stars Designation R.A
100 closest stars Designation R.A. Dec. Mag. Common Name 1 Gliese+Jahreis 551 14h30m –62°40’ 11.09 Proxima Centauri Gliese+Jahreis 559 14h40m –60°50’ 0.01, 1.34 Alpha Centauri A,B 2 Gliese+Jahreis 699 17h58m 4°42’ 9.53 Barnard’s Star 3 Gliese+Jahreis 406 10h56m 7°01’ 13.44 Wolf 359 4 Gliese+Jahreis 411 11h03m 35°58’ 7.47 Lalande 21185 5 Gliese+Jahreis 244 6h45m –16°49’ -1.43, 8.44 Sirius A,B 6 Gliese+Jahreis 65 1h39m –17°57’ 12.54, 12.99 BL Ceti, UV Ceti 7 Gliese+Jahreis 729 18h50m –23°50’ 10.43 Ross 154 8 Gliese+Jahreis 905 23h45m 44°11’ 12.29 Ross 248 9 Gliese+Jahreis 144 3h33m –9°28’ 3.73 Epsilon Eridani 10 Gliese+Jahreis 887 23h06m –35°51’ 7.34 Lacaille 9352 11 Gliese+Jahreis 447 11h48m 0°48’ 11.13 Ross 128 12 Gliese+Jahreis 866 22h39m –15°18’ 13.33, 13.27, 14.03 EZ Aquarii A,B,C 13 Gliese+Jahreis 280 7h39m 5°14’ 10.7 Procyon A,B 14 Gliese+Jahreis 820 21h07m 38°45’ 5.21, 6.03 61 Cygni A,B 15 Gliese+Jahreis 725 18h43m 59°38’ 8.90, 9.69 16 Gliese+Jahreis 15 0h18m 44°01’ 8.08, 11.06 GX Andromedae, GQ Andromedae 17 Gliese+Jahreis 845 22h03m –56°47’ 4.69 Epsilon Indi A,B,C 18 Gliese+Jahreis 1111 8h30m 26°47’ 14.78 DX Cancri 19 Gliese+Jahreis 71 1h44m –15°56’ 3.49 Tau Ceti 20 Gliese+Jahreis 1061 3h36m –44°31’ 13.09 21 Gliese+Jahreis 54.1 1h13m –17°00’ 12.02 YZ Ceti 22 Gliese+Jahreis 273 7h27m 5°14’ 9.86 Luyten’s Star 23 SO 0253+1652 2h53m 16°53’ 15.14 24 SCR 1845-6357 18h45m –63°58’ 17.40J 25 Gliese+Jahreis 191 5h12m –45°01’ 8.84 Kapteyn’s Star 26 Gliese+Jahreis 825 21h17m –38°52’ 6.67 AX Microscopii 27 Gliese+Jahreis 860 22h28m 57°42’ 9.79, -
Naming the Extrasolar Planets
Naming the extrasolar planets W. Lyra Max Planck Institute for Astronomy, K¨onigstuhl 17, 69177, Heidelberg, Germany [email protected] Abstract and OGLE-TR-182 b, which does not help educators convey the message that these planets are quite similar to Jupiter. Extrasolar planets are not named and are referred to only In stark contrast, the sentence“planet Apollo is a gas giant by their assigned scientific designation. The reason given like Jupiter” is heavily - yet invisibly - coated with Coper- by the IAU to not name the planets is that it is consid- nicanism. ered impractical as planets are expected to be common. I One reason given by the IAU for not considering naming advance some reasons as to why this logic is flawed, and sug- the extrasolar planets is that it is a task deemed impractical. gest names for the 403 extrasolar planet candidates known One source is quoted as having said “if planets are found to as of Oct 2009. The names follow a scheme of association occur very frequently in the Universe, a system of individual with the constellation that the host star pertains to, and names for planets might well rapidly be found equally im- therefore are mostly drawn from Roman-Greek mythology. practicable as it is for stars, as planet discoveries progress.” Other mythologies may also be used given that a suitable 1. This leads to a second argument. It is indeed impractical association is established. to name all stars. But some stars are named nonetheless. In fact, all other classes of astronomical bodies are named. -
Correlations Between the Stellar, Planetary, and Debris Components of Exoplanet Systems Observed by Herschel⋆
A&A 565, A15 (2014) Astronomy DOI: 10.1051/0004-6361/201323058 & c ESO 2014 Astrophysics Correlations between the stellar, planetary, and debris components of exoplanet systems observed by Herschel J. P. Marshall1,2, A. Moro-Martín3,4, C. Eiroa1, G. Kennedy5,A.Mora6, B. Sibthorpe7, J.-F. Lestrade8, J. Maldonado1,9, J. Sanz-Forcada10,M.C.Wyatt5,B.Matthews11,12,J.Horner2,13,14, B. Montesinos10,G.Bryden15, C. del Burgo16,J.S.Greaves17,R.J.Ivison18,19, G. Meeus1, G. Olofsson20, G. L. Pilbratt21, and G. J. White22,23 (Affiliations can be found after the references) Received 15 November 2013 / Accepted 6 March 2014 ABSTRACT Context. Stars form surrounded by gas- and dust-rich protoplanetary discs. Generally, these discs dissipate over a few (3–10) Myr, leaving a faint tenuous debris disc composed of second-generation dust produced by the attrition of larger bodies formed in the protoplanetary disc. Giant planets detected in radial velocity and transit surveys of main-sequence stars also form within the protoplanetary disc, whilst super-Earths now detectable may form once the gas has dissipated. Our own solar system, with its eight planets and two debris belts, is a prime example of an end state of this process. Aims. The Herschel DEBRIS, DUNES, and GT programmes observed 37 exoplanet host stars within 25 pc at 70, 100, and 160 μm with the sensitiv- ity to detect far-infrared excess emission at flux density levels only an order of magnitude greater than that of the solar system’s Edgeworth-Kuiper belt. Here we present an analysis of that sample, using it to more accurately determine the (possible) level of dust emission from these exoplanet host stars and thereafter determine the links between the various components of these exoplanetary systems through statistical analysis. -
The Search for Exomoons and the Characterization of Exoplanet Atmospheres
Corso di Laurea Specialistica in Astronomia e Astrofisica The search for exomoons and the characterization of exoplanet atmospheres Relatore interno : dott. Alessandro Melchiorri Relatore esterno : dott.ssa Giovanna Tinetti Candidato: Giammarco Campanella Anno Accademico 2008/2009 The search for exomoons and the characterization of exoplanet atmospheres Giammarco Campanella Dipartimento di Fisica Università degli studi di Roma “La Sapienza” Associate at Department of Physics & Astronomy University College London A thesis submitted for the MSc Degree in Astronomy and Astrophysics September 4th, 2009 Università degli Studi di Roma ―La Sapienza‖ Abstract THE SEARCH FOR EXOMOONS AND THE CHARACTERIZATION OF EXOPLANET ATMOSPHERES by Giammarco Campanella Since planets were first discovered outside our own Solar System in 1992 (around a pulsar) and in 1995 (around a main sequence star), extrasolar planet studies have become one of the most dynamic research fields in astronomy. Our knowledge of extrasolar planets has grown exponentially, from our understanding of their formation and evolution to the development of different methods to detect them. Now that more than 370 exoplanets have been discovered, focus has moved from finding planets to characterise these alien worlds. As well as detecting the atmospheres of these exoplanets, part of the characterisation process undoubtedly involves the search for extrasolar moons. The structure of the thesis is as follows. In Chapter 1 an historical background is provided and some general aspects about ongoing situation in the research field of extrasolar planets are shown. In Chapter 2, various detection techniques such as radial velocity, microlensing, astrometry, circumstellar disks, pulsar timing and magnetospheric emission are described. A special emphasis is given to the transit photometry technique and to the two already operational transit space missions, CoRoT and Kepler. -
Exoplanet Community Report
JPL Publication 09‐3 Exoplanet Community Report Edited by: P. R. Lawson, W. A. Traub and S. C. Unwin National Aeronautics and Space Administration Jet Propulsion Laboratory California Institute of Technology Pasadena, California March 2009 The work described in this publication was performed at a number of organizations, including the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (NASA). Publication was provided by the Jet Propulsion Laboratory. Compiling and publication support was provided by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Reference herein to any specific commercial product, process, or service by trade name, trademark, manufacturer, or otherwise, does not constitute or imply its endorsement by the United States Government, or the Jet Propulsion Laboratory, California Institute of Technology. © 2009. All rights reserved. The exoplanet community’s top priority is that a line of probeclass missions for exoplanets be established, leading to a flagship mission at the earliest opportunity. iii Contents 1 EXECUTIVE SUMMARY.................................................................................................................. 1 1.1 INTRODUCTION...............................................................................................................................................1 1.2 EXOPLANET FORUM 2008: THE PROCESS OF CONSENSUS BEGINS.....................................................2 -
IAU Division C Working Group on Star Names 2019 Annual Report
IAU Division C Working Group on Star Names 2019 Annual Report Eric Mamajek (chair, USA) WG Members: Juan Antonio Belmote Avilés (Spain), Sze-leung Cheung (Thailand), Beatriz García (Argentina), Steven Gullberg (USA), Duane Hamacher (Australia), Susanne M. Hoffmann (Germany), Alejandro López (Argentina), Javier Mejuto (Honduras), Thierry Montmerle (France), Jay Pasachoff (USA), Ian Ridpath (UK), Clive Ruggles (UK), B.S. Shylaja (India), Robert van Gent (Netherlands), Hitoshi Yamaoka (Japan) WG Associates: Danielle Adams (USA), Yunli Shi (China), Doris Vickers (Austria) WGSN Website: https://www.iau.org/science/scientific_bodies/working_groups/280/ WGSN Email: [email protected] The Working Group on Star Names (WGSN) consists of an international group of astronomers with expertise in stellar astronomy, astronomical history, and cultural astronomy who research and catalog proper names for stars for use by the international astronomical community, and also to aid the recognition and preservation of intangible astronomical heritage. The Terms of Reference and membership for WG Star Names (WGSN) are provided at the IAU website: https://www.iau.org/science/scientific_bodies/working_groups/280/. WGSN was re-proposed to Division C and was approved in April 2019 as a functional WG whose scope extends beyond the normal 3-year cycle of IAU working groups. The WGSN was specifically called out on p. 22 of IAU Strategic Plan 2020-2030: “The IAU serves as the internationally recognised authority for assigning designations to celestial bodies and their surface features. To do so, the IAU has a number of Working Groups on various topics, most notably on the nomenclature of small bodies in the Solar System and planetary systems under Division F and on Star Names under Division C.” WGSN continues its long term activity of researching cultural astronomy literature for star names, and researching etymologies with the goal of adding this information to the WGSN’s online materials. -
Starshade Rendezvous Probe
Starshade Rendezvous Probe Starshade Rendezvous Probe Study Report Imaging and Spectra of Exoplanets Orbiting our Nearest Sunlike Star Neighbors with a Starshade in the 2020s February 2019 TEAM MEMBERS Principal Investigators Sara Seager, Massachusetts Institute of Technology N. Jeremy Kasdin, Princeton University Co-Investigators Jeff Booth, NASA Jet Propulsion Laboratory Matt Greenhouse, NASA Goddard Space Flight Center Doug Lisman, NASA Jet Propulsion Laboratory Bruce Macintosh, Stanford University Stuart Shaklan, NASA Jet Propulsion Laboratory Melissa Vess, NASA Goddard Space Flight Center Steve Warwick, Northrop Grumman Corporation David Webb, NASA Jet Propulsion Laboratory Study Team Andrew Romero-Wolf, NASA Jet Propulsion Laboratory John Ziemer, NASA Jet Propulsion Laboratory Andrew Gray, NASA Jet Propulsion Laboratory Michael Hughes, NASA Jet Propulsion Laboratory Greg Agnes, NASA Jet Propulsion Laboratory Jon Arenberg, Northrop Grumman Corporation Samuel (Case) Bradford, NASA Jet Propulsion Laboratory Michael Fong, NASA Jet Propulsion Laboratory Jennifer Gregory, NASA Jet Propulsion Laboratory Steve Matousek, NASA Jet Propulsion Laboratory Jonathan Murphy, NASA Jet Propulsion Laboratory Jason Rhodes, NASA Jet Propulsion Laboratory Dan Scharf, NASA Jet Propulsion Laboratory Phil Willems, NASA Jet Propulsion Laboratory Science Team Simone D'Amico, Stanford University John Debes, Space Telescope Science Institute Shawn Domagal-Goldman, NASA Goddard Space Flight Center Sergi Hildebrandt, NASA Jet Propulsion Laboratory Renyu Hu, NASA -
THE SEARCH for EXOMOON RADIO EMISSIONS by JOAQUIN P. NOYOLA Presented to the Faculty of the Graduate School of the University Of
THE SEARCH FOR EXOMOON RADIO EMISSIONS by JOAQUIN P. NOYOLA Presented to the Faculty of the Graduate School of The University of Texas at Arlington in Partial Fulfillment of the Requirements for the Degree of DOCTOR OF PHILOSOPHY THE UNIVERSITY OF TEXAS AT ARLINGTON December 2015 Copyright © by Joaquin P. Noyola 2015 All Rights Reserved ii Dedicated to my wife Thao Noyola, my son Layton, my daughter Allison, and our future little ones. iii Acknowledgements I would like to express my sincere gratitude to all the people who have helped throughout my career at UTA, including my advising professors Dr. Zdzislaw Musielak (Ph.D.), and Dr. Qiming Zhang (M.Sc.) for their advice and guidance. Many thanks to my committee members Dr. Andrew Brandt, Dr. Manfred Cuntz, and Dr. Alex Weiss for your interest and for your time. Also many thanks to Dr. Suman Satyal, my collaborator and friend, for all the fruitful discussions we have had throughout the years. I would like to thank my wife, Thao Noyola, for her love, her help, and her understanding through these six years of marriage and graduate school. October 19, 2015 iv Abstract THE SEARCH FOR EXOMOON RADIO EMISSIONS Joaquin P. Noyola, PhD The University of Texas at Arlington, 2015 Supervising Professor: Zdzislaw Musielak The field of exoplanet detection has seen many new developments since the discovery of the first exoplanet. Observational surveys by the NASA Kepler Mission and several other instrument have led to the confirmation of over 1900 exoplanets, and several thousands of exoplanet potential candidates. All this progress, however, has yet to provide the first confirmed exomoon. -
HST Pancet Program: a Complete Near-UV to Infrared Transmission Spectrum for the Hot Jupiter WASP-79B
Draft version April 23, 2021 Typeset using LATEX twocolumn style in AASTeX63 HST PanCET Program: A Complete Near-UV to Infrared Transmission Spectrum for the Hot Jupiter WASP-79b Alexander D. Rathcke ,1 Ryan J. MacDonald ,2 Joanna K. Barstow ,3, 4 Jayesh M. Goyal ,2 Mercedes Lopez-Morales ,5 Joao~ M. Mendonc¸a ,1 Jorge Sanz-Forcada ,6 Gregory W. Henry ,7 David K. Sing ,8 Munazza K. Alam ,5 Nikole K. Lewis ,2 Katy L. Chubb ,9 Jake Taylor ,10 Nikolay Nikolov ,11 and Lars A. Buchhave 1 1DTU Space, National Space Institute, Technical University of Denmark, Elektrovej 328, DK-2800 Kgs. Lyngby, Denmark 2Department of Astronomy and Carl Sagan Institute, Cornell University, 122 Sciences Drive, Ithaca, NY 14853, USA 3School of Physical Sciences, The Open University, Walton Hall, Milton Keynes MK7 6AA, UK 4Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK 5Center for Astrophysics j Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138, USA 6Centro de Astrobiolog´ıa(CSIC-INTA), ESAC Campus, Villanueva de la Ca~nada,Madrid, Spain 7Center of Excellence in Information Systems, Tennessee State University, Nashville, TN 30209 USA 8Department of Earth and Planetary Sciences, Johns Hopkins University, Baltimore, MD 21218, USA 9SRON Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA, Utrecht, Netherlands 10Department of Physics (Atmospheric, Oceanic and Planetary Physics), University of Oxford, Parks Rd, Oxford, OX1 3PU, UK 11Space Telescope Science Institute, 3700 San Martin Dr, Baltimore, MD 21218, USA Submitted to AJ ABSTRACT We present a new optical transmission spectrum of the hot Jupiter WASP-79b. -
Signatures of Giant Planets on the Solar System Kuiper Belt Dust Disk and Implications for Extrasolar Planet in Epsilon Eridani
Lunar and Planetary Science XXX 1698.pdf SIGNATURES OF GIANT PLANETS ON THE SOLAR SYSTEM KUIPER BELT DUST DISK AND IMPLICATIONS FOR EXTRASOLAR PLANET IN EPSILON ERIDANI. J.-C. Liou1 and H. A. Zook2, 1GB Tech/Lockheed Martin, C104 Lockheed Martin, 2400 NASA Rd. One, Houston, TX 77058, 2SN2, NASA Johnson Space Center, Houston, TX 77052. Summary: One method to detect extrasolar Dust disks in Beta Pictoris, Epsilon Eridani, planetary systems is to deduce the perturbations of and other systems are analogues to our Solar Sys- planets on the observed circumstellar dust disks. tem’s Kuiper Belt dust disk. Therefore, it is of Our Solar System, with its known configuration of great interest to understanding how the Kuiper planets, provide an excellent example to study how Belt IDP distribution is affected by the giant plan- the distribution of dust particles is affected by the ets in our Solar System. We have numerically existence of different planets. Numerical simula- simulated the orbital evolution of Kuiper Belt tions of the orbital evolution of dust particles from IDPs, including gravitational perturbations from 7 Kuiper Belt objects show that the four giant plan- planets (Mercury and Pluto are not included due to ets, especially Neptune and Jupiter, impose distinct their small masses), solar radiation pressure, and and dramatic signatures on the overall distribution PR and solar wind drag. Dust particles range from of Kuiper belt dust particles. The signatures are 3 to 23 micrometers in diameter. For a given size, very similar to those observed in Epsilon Eridani. 100 IDPs are included in the simulations. -
Planetquest Outreach Toolkit Manual and Resources Cd
Outreach ToolKit Manual DISTRIBUTED FOR MEMBERS OF THE NASA NIGHT SKY NETWORK THE NIGHT SKY NETWORK IS SPONSORED AND SUPPORTED BY JPL'S PLANETQUEST PUBLIC ENGAGEMENT PROGRAM. PLANETQUEST IS A PART OF JPL’S NAVIGATOR PROGRAM, WHICH ENCOMPASSES SEVERAL OF NASA'S EXTRA-SOLAR PLANET- FINDING MISSIONS, INCLUDING THE KECK INTERFEROMETER, THE SPACE INTERFEROMETRY MISSION (SIM), THE TERRESTRIAL PLANET FINDER (TPF), THE LARGE BINOCULAR TELESCOPE INTERFEROMETER (LBTI), AND THE MICHELSON SCIENCE CENTER. NASA NIGHT SKY NETWORK: http://nightsky.jpl.nasa.gov/ PLANETQUEST: http://planetquest.jpl.nasa.gov/ Contacts The non-profit Astronomical Society of the Pacific (ASP), one of the nation’s leading organizations devoted to astronomy and space science education, is managing the Night Sky Network in cooperation with JPL. Learn more about the ASP at http://www.astrosociety.org. For support contact: Astronomical Society of the Pacific (ASP) 390 Ashton Avenue San Francisco, CA 94112 415-337-1100 ext. 116 [email protected] Copyright © 2004 NASA/JPL and Astronomical Society of the Pacific. Copies of this manual and documents may be made for educational and public outreach purposes only and are to be supplied at no charge to participants. Any other use is not permitted. CREDITS: All photos and images in the ToolKit Manual unless otherwise noted are provided courtesy of Marni Berendsen and Rich Berendsen. Your Club’s Membership in the NASA Night Sky Network Welcome to the NASA Night Sky Network! Your membership in the Night Sky Network will provide many opportunities for your club to expand its public education and outreach. Your club has at least two members who are the Night Sky Network Club Coordinators.