DOCSLIB.ORG

The Chemistry of Extrasolar Planetary Systems

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text

Load more

The Chemistry of Extrasolar Planetary Systems Item Type text; Electronic Dissertation Authors Bond, Jade 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 26/09/2021 05:25:17 Link to Item http://hdl.handle.net/10150/194946 THE CHEMISTRY OF EXTRASOLAR PLANETARY SYSTEMS by Jade Chantelle Bond 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 2 0 0 8 2 THE UNIVERSITY OF ARIZONA GRADUATE COLLEGE As members of the Final Examination Committee, we certify that we have read the dis- sertation prepared by Jade Chantelle Bond entitled The Chemistry of Extrasolar Planetary Systems and recommend that it be accepted as fulfilling the dissertation requirement for the Degree of Doctor of Philosophy. Date: 31 October 2008 Dante S. Lauretta Date: 31 October 2008 Michael J. Drake Date: 31 October 2008 David P. O’Brien Date: 31 October 2008 Michael R. Meyer Date: 31 October 2008 Adam P. Showman Final approval and acceptance of this dissertation is contingent upon the candidate’s submission of the final copies of the dissertation to the Graduate College. I hereby certify that I have read this dissertation prepared under my direction and recommend that it be accepted as fulfilling the dissertation requirement. Date: 31 October 2008 Dissertation Director: Dante S. Lauretta 3 STATEMENT BY AUTHOR This dissertation has been submitted in partial fulfillment of requirements for an advanced degree at The University of Arizona and is deposited in the University Library to be made available to borrowers under rules of the Library. Brief quotations from this dissertation are allowable without special permission, pro- vided that accurate acknowledgment of source is made. Requests for permission for ex- tended quotation from or reproduction of this manuscript in whole or in part may be granted by the head of the major department or the Dean of the Graduate College when in his or her judgment the proposed use of the material is in the interests of scholarship. In all other instances, however, permission must be obtained from the author. SIGNED: Jade Chantelle Bond 4 ACKNOWLEDGMENTS Science, like most other activities in life, is a collaborative effort and as such there are many people who deserve thanks for their assistance with producing my dissertation. First and foremost, I’d like to thank my Ph.D. advisor, Dr. Dante Lauretta, for his invaluable support and guidance throughout my time with him. There is simply no way that this work could have been completed without his assistance, both professionally and personally, along with the support of his wife, Kate. For that, I am beyond grateful. David O’Brien deserves a massive thank you for the incredible support and assis- tance he has provided through out my entire PhD. From first helping me to move in to Hawthorne House to now providing me with countless simulations, his support has been amazing and I am so incredibly grateful for it. Chris Tinney has truly been an outstanding collaborator, supporter and friend through- out the development of my scientific career. His assistance and guidance have been amaz- ing and I am so grateful he took a chance on me. Similarly, Jay Melosh has always been willing to listen and help in any problems I may have had throughout my entire PhD study. His advice and assistance are greatly appreciated. I am very pleased to be able to call both of them friends. I’d also like to thank my entire PhD Committee for their support, ideas, feedback, assistance and tolerating a defence on Halloween! I found their guidance and ideas to be useful in developing this work. A thank you also goes to the entire Nine Circles research group (especially Glinda!) for all of their ideas and assistance and the Anglo-Australian Planet Search (AAPS) group for being so generous with their data. Thank you to Michael Meyer, Cathi Duncan and the LAPLACE group for their finan- cial support, including sending me to conferences in all the cool places! On a special note, I must thank Kathryn Gardner-Vandy, Kelly Kolb, Sarah Horst and Kristin Block for putting up with me, girls nights out, giving me a break and generally being wonderful friends, Eve Berger for going above and beyond, Mike and Jenny Bland and Matt Pasek for simply understanding and helping me to stay sane, David Choi and Colin Dundas for eating Tim Tams and gossiping, the Chamberlain Clan for their Aussie fixes, Bob Marcialis for reading numerous drafts while sending me both sane and insane and Pete Lanagan for being . well, Pete. Thank you also to the artists of the comics featured through out this dissertation and their syndications for allowing me to reprint them in this work. Thank you, Hagen, for being so supportive and not grumbling too much at all of the early morning phone calls. Last, but certainly not least, a huge thank you goes to my Mum who always got it, even when no-one else around me did. 5 DEDICATION For Lillian and Frank Bond. “Now, Voyager, sail thou forth, to seek and find.” -Walt Whitman, Leaves of Grass 1900 Figure 1: CALVIN AND HOBBES (C) 1986 Watterson. Dist. By UNIVERSAL PRESS SYNDICATE. Reprinted with permission. All rights reserved. Originally published 3/17/1986. 6 TABLE OF CONTENTS LIST OF FIGURES . 9 LIST OF TABLES . 14 ABSTRACT . 16 CHAPTER 1 INTRODUCTION & BACKGROUND . 18 1.1 History of Extrasolar Planets . 18 1.2 Planetary System Chemical Properties . 19 1.3 Terrestrial Planets . 21 1.4 Summary of Work . 22 CHAPTER 2 R- AND S-PROCESS ELEMENTAL ABUNDANCES IN STARS WITH PLANETS . 25 2.1 Introduction . 25 2.2 Data . 27 2.2.1 Target Stars . 27 2.2.2 Spectroscopic Analysis . 28 2.3 Results . 31 2.4 Host Star Enrichment . 32 2.4.1 Enrichment over Solar . 32 2.4.2 Enrichment over Non-Host Stars . 33 2.5 Elemental Trends . 35 2.5.1 Lighter Element Trends . 38 2.5.2 Heavy Element Trends . 40 2.5.3 Correlation with Planetary Parameters . 42 2.5.4 Correlation with Stellar Parameters . 42 2.6 Discussion . 42 2.7 Summary . 45 CHAPTER 3 SOLAR SYSTEM SIMULATIONS . 47 3.1 Introduction . 47 3.2 Simulations . 50 3.2.1 Dynamical . 50 3.2.2 Chemical . 53 3.2.3 Combining Dynamics and Chemistry . 59 7 TABLE OF CONTENTS – Continued 3.2.4 Stellar Pollution . 59 3.3 Results . 62 3.3.1 Abundance Trends . 62 3.3.2 Variations with Time . 76 3.3.3 Late Veneer . 79 3.3.4 Hydrous Species . 80 3.3.5 Volatile Loss . 82 3.3.6 Solar Pollution . 87 3.4 Discussion . 89 3.5 Summary . 91 CHAPTER 4 EXTRASOLAR PLANETARY SYSTEM SIMULATIONS . 94 4.1 Introduction . 94 4.2 System Composition . 96 4.3 Simulations . 106 4.3.1 Extrasolar Planetary Systems . 106 4.3.2 Dynamical Simulations . 110 4.3.3 Chemical Simulations . 115 4.3.4 Combining Dynamics and Chemistry . 119 4.3.5 Stellar Pollution . 119 4.4 Results . 122 4.4.1 Dynamical . 122 4.4.2 Chemical . 132 4.4.3 Stellar Pollution . 155 4.5 Implications and Discussion . 163 4.5.1 Frequency of Terrestrial Planets . 163 4.5.2 Planetary Types . 163 4.5.3 Timing of Formation . 164 4.5.4 Detection of Terrestrial Planets . 165 4.5.5 Hydrous Species . 167 4.5.6 Planetary Interiors and Processes . 171 4.5.7 Planet Habitability . 175 4.5.8 Biologically Important Elements . 177 4.5.9 Mass Distribution . 178 4.5.10 Stellar Pollution . 181 4.6 Summary . 181 CHAPTER 5 SUMMARY & CONCLUSIONS . 184 APPENDIX A STELLAR PHOTOSPHERIC ABUNDANCES . 186 8 TABLE OF CONTENTS – Continued APPENDIX B SOLAR SYSTEM TERRESTRIAL PLANET ABUNDANCES . 198 APPENDIX C MIDPLANE TEMPERATURE AND PRESSURE PROFILES . 246 APPENDIX D HSC CHEMISTRY GAS ABUNDANCES . 256 APPENDIX E EXTRASOLAR TERRESTRIAL PLANET ABUDNANCES . 266 REFERENCES . 353 9 LIST OF FIGURES 1 Calvin and Hobbes, 3/17/1986 . 5 1.1 Piled Higher and Deeper, 2/26/2006 . 24 2.1 (X/H) vs. (Fe/H) for all elements studied. 36 2.2 (X/Fe) vs. (Fe/H) for all elements studied. 37 2.3 (heavy/light) vs. (Fe/H) . 41 2.4 Orbital properties of extrasolar planetary systems vs. abundance of the heavy elements. 43 2.5 Ginger Meggs, 2/13/2008 . 46 3.1 Schematic of the results of the simulations of O’Brien et al. (2006). 51 3.2 Radial pressure and temperature profiles for the nominal Soalr nebula . 60 3.3 Normalized abundances for the CJS1 and EJS1 simulations. 66 3.4 Al/Si v. Mg/Si for all Solar System simulated planets. 70 3.5 Ca/Si v. Mg/Si for all Solar System simulated planets. 71 3.6 Oxidation state plot for CJS1 and EJS1 simulated planetary abundances. 74 3.7 Distribution of mass and its composition. 77 3.8 Variation in composition with time for the final planets produced by the CJS1 and EJS1 simulations. 78 3.9 Normalized abundances for the CJS1 and EJS1 simulations after material loss in impact events has been incorporated . 86 3.10 Pearls Before Swine, 4/2/2007 . 93 4.1 Mg/Si vs. C/O for known planetary host stars. 98 4.2 Mg/Si vs.
Recommended publications
  • Nitrogen Abundances in Planet-Harbouring Stars

    Nitrogen Abundances in Planet-Harbouring Stars

    A&A 418, 703–715 (2004) Astronomy DOI: 10.1051/0004-6361:20035717 & c ESO 2004 Astrophysics Nitrogen abundances in planet-harbouring stars A. Ecuvillon1, G. Israelian1,N.C.Santos2,3, M. Mayor3,R.J.Garc´ıa L´opez1,4, and S. Randich5 1 Instituto de Astrof´ısica de Canarias, 38200 La Laguna, Tenerife, Spain 2 Centro de Astronomia e Astrofisica de Universidade de Lisboa, Observatorio Astronomico de Lisboa, Tapada de Ajuda, 1349-018 Lisboa, Portugal 3 Observatoire de Gen`eve, 51 ch. des Maillettes, 1290 Sauverny, Switzerland 4 Departamento de Astrof´ısica, Universidad de La Laguna, Av. Astrof´ısico Francisco S´anchez s/n, 38206 La Laguna, Tenerife, Spain 5 INAF/Osservatorio Astrofisico di Arcetri, Largo Fermi 5, 50125 Firenze, Italy Received 20 November 2003 / Accepted 4 February 2004 Abstract. We present a detailed spectroscopic analysis of nitrogen abundances in 91 solar-type stars, 66 with and 25 without known planetary mass companions. All comparison sample stars and 28 planet hosts were analysed by spectral synthesis of the near-UV NH band at 3360 Å observed at high resolution with the VLT/UVES, while the near-IR N 7468 Å was measured in 31 objects. These two abundance indicators are in good agreement. We found that nitrogen abundance scales with that of iron in the metallicity range −0.6 < [Fe/H] < +0.4 with the slope 1.08 ± 0.05. Our results show that the bulk of nitrogen production at high metallicities was coupled with iron. We found that the nitrogen abundance distribution in stars with exoplanets is the high [Fe/H] extension of the curve traced by the comparison sample of stars with no known planets.
  • Appendix 1 Some Astrophysical Reminders

    Appendix 1 Some Astrophysical Reminders

    Appendix 1 Some Astrophysical Reminders Marc Ollivier 1.1 A Physics and Astrophysics Overview 1.1.1 Star or Planet? Roughly speaking, we can say that the physics of stars and planets is mainly governed by their mass and thus by two effects: 1. Gravitation that tends to compress the object, thus releasing gravitational energy 2. Nuclear processes that start as the core temperature of the object increases The mass is thus a good parameter for classifying the different astrophysical objects, the adapted mass unit being the solar mass (written Ma). As the mass decreases, three categories of objects can be distinguished: ∼ 1. if M>0.08 Ma ( 80MJ where MJ is the Jupiter mass) the mass is sufficient and, as a consequence, the gravitational contraction in the core of the object is strong enough to start hydrogen fusion reactions. The object is then called a “star” and its radius is proportional to its mass. 2. If 0.013 Ma <M<0.08 Ma (13 MJ <M<80 MJ), the core temperature is not high enough for hydrogen fusion reactions, but does allow deuterium fu- sion reactions. The object is called a “brown dwarf” and its radius is inversely proportional to the cube root of its mass. 3. If M<0.013 Ma (M<13 MJ) the temperature a the center of the object does not permit any nuclear fusion reactions. The object is called a “planet”. In this category one distinguishes giant gaseous and telluric planets. This latter is not massive enough to accrete gas. The mass limit between giant and telluric planets is about 10 terrestrial masses.
  • Li Abundances in F Stars: Planets, Rotation, and Galactic Evolution�,

    Li Abundances in F Stars: Planets, Rotation, and Galactic Evolution,

    A&A 576, A69 (2015) Astronomy DOI: 10.1051/0004-6361/201425433 & c ESO 2015 Astrophysics Li abundances in F stars: planets, rotation, and Galactic evolution, E. Delgado Mena1,2, S. Bertrán de Lis3,4, V. Zh. Adibekyan1,2,S.G.Sousa1,2,P.Figueira1,2, A. Mortier6, J. I. González Hernández3,4,M.Tsantaki1,2,3, G. Israelian3,4, and N. C. Santos1,2,5 1 Centro de Astrofisica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal e-mail: [email protected] 2 Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Rua das Estrelas, 4150-762 Porto, Portugal 3 Instituto de Astrofísica de Canarias, C/via Lactea, s/n, 38200 La Laguna, Tenerife, Spain 4 Departamento de Astrofísica, Universidad de La Laguna, 38205 La Laguna, Tenerife, Spain 5 Departamento de Física e Astronomía, Faculdade de Ciências, Universidade do Porto, Portugal 6 SUPA, School of Physics and Astronomy, University of St. Andrews, St. Andrews KY16 9SS, UK Received 28 November 2014 / Accepted 14 December 2014 ABSTRACT Aims. We aim, on the one hand, to study the possible differences of Li abundances between planet hosts and stars without detected planets at effective temperatures hotter than the Sun, and on the other hand, to explore the Li dip and the evolution of Li at high metallicities. Methods. We present lithium abundances for 353 main sequence stars with and without planets in the Teff range 5900–7200 K. We observed 265 stars of our sample with HARPS spectrograph during different planets search programs. We observed the remaining targets with a variety of high-resolution spectrographs.
  • In-Depth Study of Photometric Variability and Radiative Timescales for Atmospheric Evolution in Four L Dwarfs

    In-Depth Study of Photometric Variability and Radiative Timescales for Atmospheric Evolution in Four L Dwarfs

    Weather on Other Worlds IV: In-Depth Study of Photometric Variability and Radiative Timescales for Atmospheric Evolution in Four L Dwarfs Item Type text; Electronic Thesis Authors Flateau, Davin C. 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 30/09/2021 07:25:39 Link to Item http://hdl.handle.net/10150/594630 WEATHER ON OTHER WORLDS IV: IN-DEPTH STUDY OF PHOTOMETRIC VARIABILITY AND RADIATIVE TIMESCALES FOR ATMOSPHERIC EVOLUTION IN FOUR L DWARFS by Davin C. Flateau A Thesis Submitted to the Faculty of the DEPARTMENT OF PLANETARY SCIENCES In Partial Fulfillment of the Requirements For the Degree of MASTER OF SCIENCE In the Graduate College THE UNIVERSITY OF ARIZONA 2015 2 STATEMENT BY AUTHOR This thesis has been submitted in partial fulfillment of requirements for an advanced degree at the University of Arizona and is deposited in the University Library to be made available to borrowers under rules of the Library. Brief quotations from this thesis are allowable without special permission, provided that accurate acknowledgment of the source is made. Requests for permission for extended quotation from or reproduction of this manuscript in whole or in part may be granted by the head of the major department or the Dean of the Graduate College when in his or her judgment the proposed use of the material is in the interests of scholarship.
  • Arxiv:Astro-Ph/0603836V1 30 Mar 2006

    Arxiv:Astro-Ph/0603836V1 30 Mar 2006

    to appear in the Astrophysical Journal Two Suns in The Sky: Stellar Multiplicity in Exoplanet Systems Deepak Raghavan, Todd J. Henry Georgia State University, Atlanta, GA 30302-4106 Brian D. Mason US Naval Observatory, 3450 Massachusetts Avenue NW, Washington DC 20392-5420 John P. Subasavage, Wei-Chun Jao, Thom D. Beaulieu Georgia State University, Atlanta, GA 30302-4106 Nigel C. Hambly Institute for Astronomy, School of Physics, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, Scotland, UK [email protected] ABSTRACT We present results of a reconnaissance for stellar companions to all 131 radial- velocity-detected candidate extrasolar planetary systems known as of July 1, arXiv:astro-ph/0603836v1 30 Mar 2006 2005. Common proper motion companions were investigated using the multi- epoch STScI Digitized Sky Surveys, and confirmed by matching the trigonometric parallax distances of the primaries to companion distances estimated photometri- cally. We also attempt to confirm or refute companions listed in the Washington Double Star Catalog, the Catalogs of Nearby Stars Series by Gliese and Jahreiß, in Hipparcos results, and in Duquennoy & Mayor (1991). Our findings indicate that a lower limit of 30 (23%) of the 131 exoplanet systems have stellar companions. We report new stellar companions to HD 38529 and HD 188015, and a new candidate companion to HD 169830. We confirm many previously reported stellar companions, including six stars in five systems, that are recognized for the first time as companions to exoplanet hosts. We have found evidence that 20 entries in the Washington Double Star Catalog –2– are not gravitationally bound companions.
  • 2016 Publication Year 2021-04-23T14:32:39Z Acceptance in OA@INAF Age Consistency Between Exoplanet Hosts and Field Stars Title B

    2016 Publication Year 2021-04-23T14:32:39Z Acceptance in OA@INAF Age Consistency Between Exoplanet Hosts and Field Stars Title B

    Publication Year 2016 Acceptance in OA@INAF 2021-04-23T14:32:39Z Title Age consistency between exoplanet hosts and field stars Authors Bonfanti, A.; Ortolani, S.; NASCIMBENI, VALERIO DOI 10.1051/0004-6361/201527297 Handle http://hdl.handle.net/20.500.12386/30887 Journal ASTRONOMY & ASTROPHYSICS Number 585 A&A 585, A5 (2016) Astronomy DOI: 10.1051/0004-6361/201527297 & c ESO 2015 Astrophysics Age consistency between exoplanet hosts and field stars A. Bonfanti1;2, S. Ortolani1;2, and V. Nascimbeni2 1 Dipartimento di Fisica e Astronomia, Università degli Studi di Padova, Vicolo dell’Osservatorio 3, 35122 Padova, Italy e-mail: [email protected] 2 Osservatorio Astronomico di Padova, INAF, Vicolo dell’Osservatorio 5, 35122 Padova, Italy Received 2 September 2015 / Accepted 3 November 2015 ABSTRACT Context. Transiting planets around stars are discovered mostly through photometric surveys. Unlike radial velocity surveys, photo- metric surveys do not tend to target slow rotators, inactive or metal-rich stars. Nevertheless, we suspect that observational biases could also impact transiting-planet hosts. Aims. This paper aims to evaluate how selection effects reflect on the evolutionary stage of both a limited sample of transiting-planet host stars (TPH) and a wider sample of planet-hosting stars detected through radial velocity analysis. Then, thanks to uniform deriva- tion of stellar ages, a homogeneous comparison between exoplanet hosts and field star age distributions is developed. Methods. Stellar parameters have been computed through our custom-developed isochrone placement algorithm, according to Padova evolutionary models. The notable aspects of our algorithm include the treatment of element diffusion, activity checks in terms of 0 log RHK and v sin i, and the evaluation of the stellar evolutionary speed in the Hertzsprung-Russel diagram in order to better constrain age.
  • Mètodes De Detecció I Anàlisi D'exoplanetes

    Mètodes De Detecció I Anàlisi D'exoplanetes

    MÈTODES DE DETECCIÓ I ANÀLISI D’EXOPLANETES Rubén Soussé Villa 2n de Batxillerat Tutora: Dolors Romero IES XXV Olimpíada 13/1/2011 Mètodes de detecció i anàlisi d’exoplanetes . Índex - Introducció ............................................................................................. 5 [ Marc Teòric ] 1. L’Univers ............................................................................................... 6 1.1 Les estrelles .................................................................................. 6 1.1.1 Vida de les estrelles .............................................................. 7 1.1.2 Classes espectrals .................................................................9 1.1.3 Magnitud ........................................................................... 9 1.2 Sistemes planetaris: El Sistema Solar .............................................. 10 1.2.1 Formació ......................................................................... 11 1.2.2 Planetes .......................................................................... 13 2. Planetes extrasolars ............................................................................ 19 2.1 Denominació .............................................................................. 19 2.2 Història dels exoplanetes .............................................................. 20 2.3 Mètodes per detectar-los i saber-ne les característiques ..................... 26 2.3.1 Oscil·lació Doppler ........................................................... 27 2.3.2 Trànsits
  • L0 and M0 Photometry of Ultracool Dwarfs D

    L0 and M0 Photometry of Ultracool Dwarfs D

    The Astronomical Journal, 127:3516–3536, 2004 June # 2004. The American Astronomical Society. All rights reserved. Printed in U.S.A. L0 AND M0 PHOTOMETRY OF ULTRACOOL DWARFS D. A. Golimowski,1 S. K. Leggett,2 M. S. Marley,3 X. Fan,4 T. R. Geballe,5 G. R. Knapp,6 F. J. Vrba,7 A. A. Henden,7 C. B. Luginbuhl,7 H. H. Guetter,7 J. A. Munn,7 B. Canzian,7 W. Zheng,1 Z. I. Tsvetanov,8 K. Chiu,1 K. Glazebrook,1 E. A. Hoversten,1 D. P. Schneider,9,10 and J. Brinkmann10, 11 Received 2003 November 13; accepted 2004 February 18 ABSTRACT We have compiled L0 (3.4–4.1 m) and M0 (4.6–4.8 m) photometry of 63 single and binary M, L, and T dwarfs obtained at the United Kingdom Infrared Telescope using the Mauna Kea Observatory filter set. This compilation includes new L0 measurements of eight L dwarfs and 13 T dwarfs and new M0 measurements of seven L dwarfs, five T dwarfs, and the M1 dwarf Gl 229A. These new data increase by factors of 0.6 and 1.6, 0 0 respectively, the numbers of ultracool dwarfs (Teff P 2400 K) for which L and M measurements have been 0 reported. We compute Lbol,BCK ,andTeff for 42 dwarfs whose flux-calibrated JHK spectra, L photometry, and trigonometric parallaxes are available, and we estimate these quantities for nine other dwarfs whose parallaxes and flux-calibrated spectra have been obtained. BCK is a well-behaved function of near-infrared spectral type with a dispersion of 0.1 mag for types M6–T5; it is significantly more scattered for types T5–T9.
  • Estimation of the XUV Radiation Onto Close Planets and Their Evaporation⋆

    Estimation of the XUV Radiation Onto Close Planets and Their Evaporation⋆

    A&A 532, A6 (2011) Astronomy DOI: 10.1051/0004-6361/201116594 & c ESO 2011 Astrophysics Estimation of the XUV radiation onto close planets and their evaporation J. Sanz-Forcada1, G. Micela2,I.Ribas3,A.M.T.Pollock4, C. Eiroa5, A. Velasco1,6,E.Solano1,6, and D. García-Álvarez7,8 1 Departamento de Astrofísica, Centro de Astrobiología (CSIC-INTA), ESAC Campus, PO Box 78, 28691 Villanueva de la Cañada, Madrid, Spain e-mail: [email protected] 2 INAF – Osservatorio Astronomico di Palermo G. S. Vaiana, Piazza del Parlamento, 1, 90134, Palermo, Italy 3 Institut de Ciènces de l’Espai (CSIC-IEEC), Campus UAB, Fac. de Ciències, Torre C5-parell-2a planta, 08193 Bellaterra, Spain 4 XMM-Newton SOC, European Space Agency, ESAC, Apartado 78, 28691 Villanueva de la Cañada, Madrid, Spain 5 Dpto. de Física Teórica, C-XI, Facultad de Ciencias, Universidad Autónoma de Madrid, Cantoblanco, 28049 Madrid, Spain 6 Spanish Virtual Observatory, Centro de Astrobiología (CSIC-INTA), ESAC Campus, Madrid, Spain 7 Instituto de Astrofísica de Canarias, 38205 La Laguna, Spain 8 Grantecan CALP, 38712 Breña Baja, La Palma, Spain Received 27 January 2011 / Accepted 1 May 2011 ABSTRACT Context. The current distribution of planet mass vs. incident stellar X-ray flux supports the idea that photoevaporation of the atmo- sphere may take place in close-in planets. Integrated effects have to be accounted for. A proper calculation of the mass loss rate through photoevaporation requires the estimation of the total irradiation from the whole XUV (X-rays and extreme ultraviolet, EUV) range. Aims. The purpose of this paper is to extend the analysis of the photoevaporation in planetary atmospheres from the accessible X-rays to the mostly unobserved EUV range by using the coronal models of stars to calculate the EUV contribution to the stellar spectra.
  • Density Estimation for Projected Exoplanet Quantities

    Density Estimation for Projected Exoplanet Quantities

    Density Estimation for Projected Exoplanet Quantities Robert A. Brown Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 [email protected] ABSTRACT Exoplanet searches using radial velocity (RV) and microlensing (ML) produce samples of “projected” mass and orbital radius, respectively. We present a new method for estimating the probability density distribution (density) of the un- projected quantity from such samples. For a sample of n data values, the method involves solving n simultaneous linear equations to determine the weights of delta functions for the raw, unsmoothed density of the unprojected quantity that cause the associated cumulative distribution function (CDF) of the projected quantity to exactly reproduce the empirical CDF of the sample at the locations of the n data values. We smooth the raw density using nonparametric kernel density estimation with a normal kernel of bandwidth σ. We calibrate the dependence of σ on n by Monte Carlo experiments performed on samples drawn from a the- oretical density, in which the integrated square error is minimized. We scale this calibration to the ranges of real RV samples using the Normal Reference Rule. The resolution and amplitude accuracy of the estimated density improve with n. For typical RV and ML samples, we expect the fractional noise at the PDF peak to be approximately 80 n− log 2. For illustrations, we apply the new method to 67 RV values given a similar treatment by Jorissen et al. in 2001, and to the 308 RV values listed at exoplanets.org on 20 October 2010. In addition to an- alyzing observational results, our methods can be used to develop measurement arXiv:1011.3991v3 [astro-ph.IM] 21 Mar 2011 requirements—particularly on the minimum sample size n—for future programs, such as the microlensing survey of Earth-like exoplanets recommended by the Astro 2010 committee.
  • • August the 26Th 2004 Detection of the Radial-Velocity Signal Induced by OGLE-TR-111 B Using UVES/FLAMES on the VLT (See Pont Et Al

    • August the 26Th 2004 Detection of the Radial-Velocity Signal Induced by OGLE-TR-111 B Using UVES/FLAMES on the VLT (See Pont Et Al

    2004 • August the 26th 2004 Detection of the radial-velocity signal induced by OGLE-TR-111 b using UVES/FLAMES on the VLT (see Pont et al. 2004, A&A in press, astro-ph/0408499). • August the 25th 2004 TrES-1b: A new transiting exoplanet detected by the Trans-Atlantic Exoplanet Survey (TreS) team . (see Boulder Press release or Alonso et al.) • August the 25th 2004 HD 160691 c : A 14 Earth-mass planet detected with HARPS (see ESO Press Release or Santos et al.) • July the 8th 2004 HD 37605 b: The first extra-solar planet detected with HRS on the Hobby- Eberly Telescope (Cochran et al.) • May the 3rd 2004 HD 219452 Bb withdrawn by Desidera et al. • April the 28th 2004 Orbital solution for OGLE-TR-113 confirmed by Konacki et al • April the 15th 2004 OGLE 2003-BLG-235/MOA 2003-BLG-53: a planetary microlensing event (Bond et al.) • April the 14th 2004 FLAMES-UVES spectroscopic orbits for two OGLE III transiting candidates: OGLE-TR-113 and OGLE-TR-132 (Bouchy et al.) • February 2004 Detection of Carbon and Oxygen in the evaporating atmosphere of HD 209458 b by A. Vidal-Madjar et al. (from HST observations). • January the 5th 2004 Two planets orbiting giant stars announced by Mitchell et al. during the AAS meeting: HD 59686 b and 91 Aqr b (HD 219499 b). Two other more massive companions, Tau Gem b (HD 54719 b) and nu Oph b (HD 163917 b), have also been announced by the same authors. 2003 • December 2003 First planet detected with HARPS: HD 330075 b (see Mayor et al., in the ESO Messenger No 114) • July the 3rd 2003 A long-period planet on a circular orbit around HD 70642 announced by the AAT team (Carter et al.
  • Lab 09 - Exoplanets

    Lab 09 - Exoplanets

    LAB 09 - EXOPLANETS NAME ____________________________ CLASS (CIRCLE ONE) DAY NIGHT DATE ____________________________ INTRODUCTION In this lab, you are going to use real data obtained from observations of exoplanets to determine their orbital characteristics. An exoplanet is a planet that orbits another star (i.e. they are planets that do not orbit our sun). There are many methods used to detect exoplanets, but the most successful has been the transit method. In this method, the planet’s orbit is aligned such that, as it moves between us and its parent star, it blocks a small amount of the light from that star. The amount of starlight that is blocked is extremely small and requires many careful observations to discern. There are many current and past observation projects dedicated to the search for exoplanets. PROCEDURES Go to the premier online repository of exoplanetary data at http://www.exoplanet.eu/catalog/ and use the ​ search feature to complete the table below. Input the name of each star into the Planet Search feature on the page and it will filter the list to show you the planets that are known to be part of that star system. For each star system, you will record the following information: ● Star Name - Record the star’s name in the first column. ● Planet Letter - The first planet will be designated “b” the next one “c” and so on. For example, first planet in the 16 Cygni system is called 16 Cygni b. ● Mass - The number you see in the table is a multiple of the mass of Jupiter (MJupiter).