Planetary Candidates Observed by Kepler. V
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
Tregloan-Reed Phd 2014.Pdf
This work is protected by copyright and other intellectual property rights and duplication or sale of all or part is not permitted, except that material may be duplicated by you for research, private study, criticism/review or educational purposes. Electronic or print copies are for your own personal, non- commercial use and shall not be passed to any other individual. No quotation may be published without proper acknowledgement. For any other use, or to quote extensively from the work, permission must be obtained from the copyright holder/s. Starspot properties and photometric parameters of transiting planets and their host stars Jeremy Tregloan-Reed Mphys (Hons) Lancaster University Doctor of Philosophy Department of Astrophysics, University of Keele. October 2014 iii Abstract To begin understanding how the architecture of hot Jupiter planetary systems can be so radically different from that of our own solar system, requires the dynamical evolution of planets to be known. By measuring the sky-projected obliquity λ of a system it is possible to determine the dominant process in the dynamical evolution. If a transiting exoplanet that crosses the disc of its host star passes over a starspot, then the amount of received intensity from the star will change. By modelling the position of the anomaly in the lightcurve it is possible to precisely determine the position of the starspot on the stellar disc. If the position of the starspot can be found at two distinct times using two closely spaced transits, then it is possible to measure λ. Before now there was no definitive model capable of accurately modelling both a planetary transit and a starspot. -
The Copernican Principle Rules out BLC1 As a Technological Radio Signal from the Alpha Centauri System
Draft version January 13, 2021 Typeset using LATEX twocolumn style in AASTeX62 The Copernican Principle Rules Out BLC1 as a Technological Radio Signal from the Alpha Centauri System Amir Siraj1 and Abraham Loeb1 1Department of Astronomy, Harvard University, 60 Garden Street, Cambridge, MA 02138, USA ABSTRACT Without evidence for occupying a special time or location, we should not assume that we inhabit privileged circumstances in the Universe. As a result, within the context of all Earth-like planets orbiting Sun-like stars, the origin of a technological civilization on Earth should be considered a single outcome of a random process. We show that in such a Copernican framework, which is inherently optimistic about the prevalence of life in the Universe, the likelihood of the nearest star system, Alpha Centauri, hosting a radio-transmitting civilization is ∼ 10−8. This rules out, a priori, Breakthrough Listen Candidate 1 (BLC1) as a technological radio signal from the Alpha Centauri system, as such a scenario would violate the Copernican principle by about eight orders of magnitude. We also show that the Copernican principle is consistent with the vast majority of Fast Radio Bursts being natural in origin. Keywords: technosignatures; astrobiology; search for extraterrestrial intelligence; biosignatures 1. INTRODUCTION lihood of searches for primitive and intelligent life, us- The Copernican principle asserts that we are not priv- ing a Drake-type approach. Westby & Conselice(2020) ileged observers of the Universe. Successes of its appli- applied the Copernican principle to the search for intel- cation include the rejection of Ptolemaic geocentrism ligent life, but in forms that featured strict boundaries and the adoption of the modern cosmological princi- in time, thereby not reflecting a truly random process. -
YETI – Search for Young Transiting Planets
YETI – search for young transiting planets Ronny Errmann, Astrophysikalisches Institut und Universitäts-Sternwarte Jena, in collaboration with: Ralph Neuhäuser, AIU Jena Gracjan Maciejewski, Centre for Astronomy of the Nicolaus Copernicus University Ronald Redmer, University of Rostock Martin Seeliger, AIU Jena YETI Observers, all over the world Mercury transit Hot Planets and Cool Stars 8. Nov. 06 (SOHO) Garching 12. November 2012 Venus transit 6. June 12 Motivation youngest transiting planets: ●Corot 2: 130 – 500 Myr (from star spots) 30 – 40 Myr (from planet radius) ●Corot 20: 100 – 800 Myr (from Li-abundance) M = 1 MJup ●Wasp 10: 200 – 350 Myr (from gyro-chronology) → younger transiting planets (Radius+true Mass) needed, to test models, and planet formation scenarios Observation strategies increase probability for transiting planet: monitoring of many young stars -> Young open clusters orbital periods: ~1 to ~10 days transit duration: ~1 to few hours → 1 to 5% of orbit in transit phase observation with single telescope: data gaps because of daytime, weather, ... increase probability for observing transit signal: long continuous observation -> YETI YETI-network (Young Exoplanet Transit Initiative) Tenagra II Llano del Gettysburg Sierra Nevada Jena Stara Lesna Byurakan Xinglong Gunma Hato Astrophysical 0.8-m telescope Observatory Collage Astronomical 1.0 and 2.6 Observatory Astronomical 1.5-m telescope Institute Observatory Institute telescopes 90/60 cm Observatory 0.9/0.6-m 0.6-m telescope 1.5-m telescope 1-m Schmidt 0.4-m telescope -
On the Rotation Rates and Axis Ratios of the Smallest Known Near-Earth
On the rotation rates and axis ratios of the smallest known near-Earth asteroids—the archetypes of the Asteroid Redirect Mission targets Patrick Hatcha, Paul A. Wiegerta,b,∗ aDepartment of Physics and Astronomy, The University of Western Ontario, London, N6A 3K7 CANADA bCentre for Planetary Science and Exploration, The University of Western Ontario, London, N6A 3K7 CANADA Abstract NASA’s Asteroid Redirect Mission (ARM) has been proposed with the aim to capture a small asteroid a few meters in size and redirect it into an orbit around the Moon. There it can be investigated at leisure by astronauts aboard an Orion or other spacecraft. The target for the mission has not yet been selected, and there are very few potential targets currently known. Though sufficiently small near-Earth asteroids (NEAs) are thought to be numerous, they are also difficult to detect and characterize with current observational facilities. Here we collect the most up-to-date information on near-Earth asteroids in this size range to outline the state of understanding of the properties of these small NEAs. Observational biases certainly mean that our sample is not an ideal representation of the true population of small NEAs. However our sample is representative of the eventual target list for the ARM mission, which will be compiled under very similar observational constraints unless dramatic changes are made to the way near-Earth asteroids are searched for and studied. We collect here information on 88 near-Earth asteroids with diameters less than 60 meters and with high quality light curves. We find that the typical rotation period is 40 minutes. -
1950 Da, 205, 269 1979 Va, 230 1991 Ry16, 183 1992 Kd, 61 1992
Cambridge University Press 978-1-107-09684-4 — Asteroids Thomas H. Burbine Index More Information 356 Index 1950 DA, 205, 269 single scattering, 142, 143, 144, 145 1979 VA, 230 visual Bond, 7 1991 RY16, 183 visual geometric, 7, 27, 28, 163, 185, 189, 190, 1992 KD, 61 191, 192, 192, 253 1992 QB1, 233, 234 Alexandra, 59 1993 FW, 234 altitude, 49 1994 JR1, 239, 275 Alvarez, Luis, 258 1999 JU3, 61 Alvarez, Walter, 258 1999 RL95, 183 amino acid, 81 1999 RQ36, 61 ammonia, 223, 301 2000 DP107, 274, 304 amoeboid olivine aggregate, 83 2000 GD65, 205 Amor, 251 2001 QR322, 232 Amor group, 251 2003 EH1, 107 Anacostia, 179 2007 PA8, 207 Anand, Viswanathan, 62 2008 TC3, 264, 265 Angelina, 175 2010 JL88, 205 angrite, 87, 101, 110, 126, 168 2010 TK7, 231 Annefrank, 274, 275, 289 2011 QF99, 232 Antarctic Search for Meteorites (ANSMET), 71 2012 DA14, 108 Antarctica, 69–71 2012 VP113, 233, 244 aphelion, 30, 251 2013 TX68, 64 APL, 275, 292 2014 AA, 264, 265 Apohele group, 251 2014 RC, 205 Apollo, 179, 180, 251 Apollo group, 230, 251 absorption band, 135–6, 137–40, 145–50, Apollo mission, 129, 262, 299 163, 184 Apophis, 20, 269, 270 acapulcoite/ lodranite, 87, 90, 103, 110, 168, 285 Aquitania, 179 Achilles, 232 Arecibo Observatory, 206 achondrite, 84, 86, 116, 187 Aristarchus, 29 primitive, 84, 86, 103–4, 287 Asporina, 177 Adamcarolla, 62 asteroid chronology function, 262 Adeona family, 198 Asteroid Zoo, 54 Aeternitas, 177 Astraea, 53 Agnia family, 170, 198 Astronautica, 61 AKARI satellite, 192 Aten, 251 alabandite, 76, 101 Aten group, 251 Alauda family, 198 Atira, 251 albedo, 7, 21, 27, 185–6 Atira group, 251 Bond, 7, 8, 9, 28, 189 atmosphere, 1, 3, 8, 43, 66, 68, 265 geometric, 7 A- type, 163, 165, 167, 169, 170, 177–8, 192 356 © in this web service Cambridge University Press www.cambridge.org Cambridge University Press 978-1-107-09684-4 — Asteroids Thomas H. -
Open Research Online Oro.Open.Ac.Uk
Open Research Online The Open University’s repository of research publications and other research outputs Extra-Solar Planetary Atmospheres and Interior Structure: Implications for Observational Signatures Thesis How to cite: Bending, Victoria Louise (2016). Extra-Solar Planetary Atmospheres and Interior Structure: Implications for Observational Signatures. PhD thesis The Open University. For guidance on citations see FAQs. c 2016 The Author https://creativecommons.org/licenses/by-nc-nd/4.0/ Version: Version of Record Link(s) to article on publisher’s website: http://dx.doi.org/doi:10.21954/ou.ro.0000ef7b Copyright and Moral Rights for the articles on this site are retained by the individual authors and/or other copyright owners. For more information on Open Research Online’s data policy on reuse of materials please consult the policies page. oro.open.ac.uk Extra-Solar Planetary Atmospheres and Interior Structure: Implications for Observational Signatures Victoria Louise Bending BA (Hons) (Open University) 2004 MPhys (Durham) 2009 This thesis is submitted for the degree of Doctor of Philosophy Department of Physical Sciences The Open University Submitted: October 2015 ProQuest Number: 13834775 All rights reserved INFORMATION TO ALL USERS The quality of this reproduction is dependent upon the quality of the copy submitted. In the unlikely event that the author did not send a com plete manuscript and there are missing pages, these will be noted. Also, if material had to be removed, a note will indicate the deletion. uest ProQuest 13834775 Published by ProQuest LLC(2019). Copyright of the Dissertation is held by the Author. All rights reserved. This work is protected against unauthorized copying under Title 17, United States C ode Microform Edition © ProQuest LLC. -
Searching For, Finding, and Imaging Young Extrasolar Planets with HST
Searching for, Finding, and Imaging Young Extrasolar Planets with HST/NICMOS 2MASSWJ 1207-334-393254b (2M1207b): A Common Proper Motion Companion of Planetary Mass to a Young Brown Dwarf G. Schneider (Steward Obs., UofA), I. Song, J. Farihi, (Gemini Obs.), B. Zuckerman, E. Becklin (UCLA), P. Lowrance (Caltech), B. Macintosh (LLNL), M. Bessell (ANU) ABSTRACT: Imaging discovery and subsequent characterization of extrasolar planet NICMOS CORONAGRAPHY DETECTION LIMITS & UNCERTAINTIES (EP) mass companions to stars has been observationally challenging due to the severe planet-to-star contrast ratios. Since the detection of the extrasolar giant planet (EGP) The ability to detect faint point sources near bright objects (e.g., planetary mass SINGLE ORBIT observations which roll the telescope about the target axis companion to 51 Peg [1], continuing discoveries of 1 – 10 Jupiter mass companions by companions to stars) is instrumentally enhanced by reducing the brightness of the (unfortunately, technically unfeasible with HST's soon to be implemented two-gyro indirect methods have revealed an unanticipated diversity in mass ranges, dynamical central star. To enable such observations, HST has provided unique resources for high guiding mode) are highly efficient and permit optimal self-subtraction of the properties, and primary-star characteristics. The past decade has seen an explosion of contrast imaging with its panchromatic complement of coronagraphically augmented underlying coronagraphic point-spread function. Such observations yield total indirect detections of EGP companions to solar-like stars through radial velocity imagers: NICMOS (near-IR), ACS (UV/Optical) and, until recently, STIS (broadband integration times of, typically, ~ 1300s. Highly repeatable point source detection limits surveys [2] and more recently, in much smaller numbers, via photometric transits [e.g., Optical). -
A Moving Cluster Distance to the Exoplanet 2M1207 B in the TW Hya
accepted to Astrophysical Journal, 18 July 2005 A Moving Cluster Distance to the Exoplanet 2M1207 B in the TW Hya Association Eric E. Mamajek1 Harvard-Smithsonian Center for Astrophysics, 60 Garden St., MS-42, Cambridge, MA 02138 [email protected] ABSTRACT A candidate extrasolar planet companion to the young brown dwarf 2MASSW J1207334-393254 (2M1207) was recently discovered by Chauvin et al. They find that 2M1207 B’s temperature and luminosity are consistent with being a young, ∼5 MJup planet. The 2M1207 system is purported to be a member of the TW Hya association (TWA), and situated ∼70 pc away. Using a revised space mo- tion vector for TWA, and improved proper motion for 2M1207, I use the moving cluster method to estimate the distance to the 2M1207 system and other TWA members. The derived distance for 2M1207 (53 ± 6 pc) forces the brown dwarf and planet to be half as luminous as previously thought. The inferred masses for 2M 1207 A and B decrease to ∼21 MJup and ∼3-4MJup, respectively, with the mass of B being well below the observed tip of the planetary mass function and the theoretical deuterium-burning limit. After removing probable Lower arXiv:astro-ph/0507416v1 18 Jul 2005 Centaurus-Crux (LCC) members from the TWA sample, as well as the prob- able non-member TWA 22, the remaining TWA members are found to have distances of 49 ± 3 (s.e.m.) ± 12(1σ) pc, and an internal 1D velocity dispersion of +0.3 −1 0.8−0.2 km s . There is weak evidence that the TWA is expanding, and the data are consistent with a lower limit on the expansion age of 10 Myr (95% confidence). -
Dynamical Measurements of the Interior Structure of Exoplanets
The Astrophysical Journal, 778:100 (11pp), 2013 December 1 doi:10.1088/0004-637X/778/2/100 C 2013. The American Astronomical Society. All rights reserved. Printed in the U.S.A. DYNAMICAL MEASUREMENTS OF THE INTERIOR STRUCTURE OF EXOPLANETS Juliette C. Becker1 and Konstantin Batygin2 1 Cahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 E. California Blvd., Pasadena, CA 91125, USA; [email protected] 2 Institute for Theory and Computation, Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA, USA Received 2013 January 3; accepted 2013 September 11; published 2013 November 8 ABSTRACT Giant gaseous planets often reside on orbits in sufficient proximity to their host stars for the planetary quadrupole gravitational field to become non-negligible. In presence of an additional planetary companion, a precise characterization of the system’s orbital state can yield meaningful constraints on the transiting planet’s interior structure. However, such methods can require a very specific type of system. This paper explores the dynamic range of applicability of these methods and shows that interior structure calculations are possible for a wide array of orbital architectures. The HAT-P-13 system is used as a case study, and the implications of perturbations arising from a third distant companion on the feasibility of an interior calculation are discussed. We find that the method discussed here is likely to be useful in studying other planetary systems, allowing the possibility of an expanded survey of the interiors of exoplanets. Key words: planets and satellites: dynamical evolution and stability – planets and satellites: interiors Online-only material: color figures 1. -
Arxiv:2011.11698V2 [Astro-Ph.EP] 19 May 2021
Draft version May 20, 2021 Typeset using LATEX default style in AASTeX61 ULTRA SHORT PERIOD PLANETS IN K2 III: NEIGHBORS ARE COMMON WITH 13 NEW MULTI-PLANET SYSTEMS AND 10 NEWLY VALIDATED PLANETS IN CAMPAIGNS 0-8, 10 Elisabeth R. Adams,1 Brian Jackson,2 Samantha Johnson,3 David R. Ciardi,4 William D. Cochran,5 Michael Endl,6 Mark E. Everett,7 Elise Furlan,8 Steve B. Howell,9 Prasanna Jayanthi,2 Phillip J. MacQueen,6 Rachel A. Matson,10 Ciera Partyka-Worley,2 Joshua Schlieder,11 Nicholas J. Scott,9 Sevio M. Stanton,2 and Carl Ziegler12 1Planetary Science Institute, 1700 E. Ft. Lowell, Suite 106, Tucson, AZ 85719, USA 2Department of Physics, Boise State University, 1910 University Drive, Boise ID 83725, USA 3Department of Physics, University of North Carolina at Chapel Hill, Chapel Hill, North Carolina 27599, USA Triangle Universities Nuclear Laboratory, Duke University, Durham, North Carolina 27708, USA 4NASA Exoplanet Science Institute, 770 South Wilson Avenue, Pasadena, CA 91125, USA 5Center for Planetary Systems Habitability and McDonald Observatory, The University of Texas at Austin, Austin, TX 78712, USA 6McDonald Observatory, The University of Texas at Austin, Austin, TX 78712, USA 7NSF's Optical Infrared Astronomy Research Laboratory, 950 North Cherry Avenue Tucson, AZ 85719, USA 8NASA Exoplanet Science Institute, Caltech/IPAC, 770 South Wilson Avenue, Pasadena, CA 91125, USA 9NASA Ames Research Center, Moffett Field, CA 94035, USA 10U.S. Naval Observatory, 3450 Massachusetts Avenue NW, Washington, D.C. 20392, USA 11NASA Goddard Space Flight Center, Greenbelt, MD, USA 12Dunlap Institute for Astronomy and Astrophysics, University of Toronto, 50 St. -
A Precise Carbon and Oxygen Abundance Determination in a Hot Jupiter Atmosphere
A Precise Carbon and Oxygen Abundance Determination in a Hot Jupiter Atmosphere Michael Line ( [email protected] ) Arizona State University https://orcid.org/0000-0001-6247-8323 Matteo Brogi Warwick University Jacob Bean University of Chicago Siddharth Gandhi University of Warwick Joseph Zalesky Arizona State University Viven Parmentier University of Oxford Peter Smith Arizona State University Gregory Mace University of Texas-Austin Megan Manseld University of Chicago Eliza Kempton University of Maryland https://orcid.org/0000-0002-1337-9051 Jonathan Fortney University of California, Santa Cruz Evgenya Shkolnik Arizona State University Jennifer Patience Arizona State University Emily Rauscher University of Michigan https://orcid.org/0000-0003-3963-9672 Jean-Michel Desert University of Amsterdam Jooost Wardenier University of Oxford Physical Sciences - Article Keywords: Gas Giant Planets, Atmospheric Compositions, Giant Planet Formation, Ground-based Spectroscopy, Metallicity Posted Date: June 9th, 2021 DOI: https://doi.org/10.21203/rs.3.rs-593104/v1 License: This work is licensed under a Creative Commons Attribution 4.0 International License. Read Full License 1 A Precise Carbon and Oxygen Abundance Determination 2 in a Hot Jupiter Atmosphere 1,2 3,4,5 6 3,4 1 3 Michael R Line , Matteo Brogi , Jacob L. Bean , Siddharth Gandhi , Joseph Zalesky , 7 1 8 9 10 4 Vivien Parmentier , Peter Smith , Gregory N. Mace , Megan Mansfield , Eliza M.-R. Kempton , 11 1,2 1 12 5 Jonathan J. Fortney , Evgenya Shkolnik , Jennifer Patience , Emily Rauscher -
E a R Th» »Moon Moon: Earth: Surface Area Earth » L E N Gth of Equat
k k k 363 384 405 . E EARth-MOON DISTANCE (km) V A MIN. MIN. 0 200 400 600 800 km MAX. SEA OF HUMBOLDT MARE HUMBOLDTIANUM SEA OF COLD MARE FRIGORIS PLATO CE3 G. BRUNO L1 SEA OF SHOWERS MARE IMBRIUM L2 A15 L21 SEA OF SERENITY ARISTARCHUS MARE SERENITATIS JAckSON L13 A17 SEA OF MUSCOVY ENNINUS SEA OF CRISES MARE MOSCOVIENSE MARE CRISIUM L24 MONTES Ap KEPLER SEA OF TRANQUILITY L4 COPERNICUS MARE TRANQUILLITATIS L20 OCEAN OF STORMS S5 R8 OCEANUS PROCELLARUM S4/6 1° CE1 L15 1° S1 0° 0° S3 L-1° L-1° A12 0° A14 -1° A11 +1° 179° 180° SEA OF FECUNDITY -179° HERTZSPRUNG MARE FECUNDITATIS A16 KOROLEV R7 LANGRENUS GRIMALDI R9 SEA OF NECTAR MARE NECTARIS SEA OF CLOUDS SEA MARE NUBIUM OF MOISTURE EASTERN SEA MARE HUMORUM MARE ORIENTALE S7 APOLLO TYCHO SOUTH POLE–AITKEN BASIN V E R A G E + A 16 °C H » T DENSITY R LUNa–2 A g/m3 8001 : 10 000. 1 cm km. ≈ 108 SURFACE TemPERATURE E MOON EARTH ScHRÖDINGER LP Lambert Azimuthal Equal Area Projection. A AMERICAN MANNED SPACECRAFTS . V E OON R A: Apollo E E M A E A G R R TH E T F - O 18 U H AMERICAN SPACE PROBES P °C A Commission on Planetary Cartography. Published by Eötvös Loránd University, Budapest. Text © Henrik Hargitai 2014. http://childrensmaps.wordpress.com. M Editor: Henrik Hargitai. Illustration:Europlanet 2012 OutreachLászló FundingHerbszt. Scheme,Technical Paris Observatory,review: InternationalJim Zimbelman. CartographicISBN 978-963-284-423-7, ISBN 978-963-284-422-0 Illustration [PDF].