DOCSLIB.ORG

Dissertation Submitted to the Combined Faculties of the Natural Sciences and Mathematics of the Ruperto-Carola-University Of

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Dissertation Submitted to the Combined Faculties of the Natural Sciences and Mathematics of the Ruperto-Carola-University Of Dissertation submitted to the Combined Faculties of the Natural Sciences and Mathematics of the Ruperto-Carola-University of Heidelberg. Germany for the degree of Doctor of Natural Sciences Put forward by ARIANNA MUSSO BARCUCCI born in Moncalieri, Italy Oral examination: 23 July 2020 THE RELATION BETWEEN DISCS AND YOUNG COMPANIONS - OBSERVATIONAL STUDIES REFEREES: PROF. DR. THOMAS HENNING PROF. DR. KEES DULLEMOND ABSTRACT The direct imaging technique brings advantages with respect to other, indirect methods of detect- ing planets. It is sensitive to larger separations, it can detect companions on a variety of orbital configurations, and it allows to simultaneously image both a companion and the circumstellar disc it resides in, thus being the perfect tool to study companion-disc interactions. Direct observations of Hα emission from young planetary and low-mass stellar companions can also shed light on the early gas accretion phase of planet formation. In this Thesis I use the direct imaging technique to study various aspects of planet-disc interaction and planet formation and evolution. I present the detection of a previously unknown low-mass stellar companion around HD 193571, observed as part of the NaCo Imaging Survey for Planets around Young Stars (ISPY). The companion appears to reside within the gap between the host star and its surrounding disc, making this the third low-mass stellar companion discovered within a debris disc. This system is thus the perfect laboratory where to study the relative importance between self- and companion-stirring models in discs. I also present the detection of Hα emission from the known substellar companion around the young star PZ Tel. The derived Hα luminosity, combined with age and disc information, indicates that the emission is likely due to chromospheric activity of the companion. This detection further proves the capability of using high-contrast imaging instruments and techniques to detect Hα signatures from companions around young stars. On a larger scale, I present the L’ band Imaging Survey to find Exoplanets in the North (LIStEN), which targeted ∼30 nearby stars with known and well characterised circumstellar discs. LIStEN focuses on characterising the population of wide-orbit giant planets around disc-hosting stars, as well as studying the intricacies of companion-disc interactions. I present the survey’s scientific goals, data selection and observational strategy, as well as the data reduction and analysis. No new planetary companions were detected, and the mass detection limits derived from the observations are combined with information on the disc size and morphology to constrain the presence of unseen planetary and low-mass stellar companion around these disc-hosting stars. ZUSAMMENFASSUNG Die Methodik der direkten Beobachtung hat Vorteile gegenuber¨ anderen, indirekten Methoden zum Nachweis von Exoplaneten. Sie ist empfindlicher fur¨ großere¨ Separationen, kann planetare und stellare Begleitobjekte auf einer Vielzahl von Bahnkonfigurationen nachweisen, und erlaubt es, gleichzeitig sowohl ein Begleitobjekt als auch die zirkumstellaren Scheibe abzubilden, was diese Methodik zum perfekten Werkzeug zur Untersuchung von Wechselwirkungen zwischen dem Begleiter und der Scheibe macht. Die direkte Beobachtung der Hα-Emission von jungen planetaren und massearmen stellaren Begleitern kann zudem Aufschluss uber¨ die fruhe¨ Gasakkre- tionsphase der Planetenbildung geben. In dieser Dissertation verwende ich die Methodik der direkten Beobachtung, um verschiedene Aspekte der Planeten-Scheiben-Wechselwirkung und der Entstehung und Entwicklung von Planeten zu untersuchen. Ich prasentiere¨ den Nachweis eines bisher unbekannten massearmen stellaren Begleiters um HD 193571, der im Rahmen der NaCo “Imaging Survey for Planets around Young Star” (ISPY) Beobachtungskampagne entdeckt wurde. Der Begleiter befindet sich in der Lucke¨ zwischen dem Zentralstern und der ihn umgebenden Scheibe; dieses massearme stellare Begleitobjekt ist bislang erst das dritte, das in einer Trummerscheibe¨ entdeckt wurde. Dies macht dieses System daher zum idealen Kandidaten zur Untersuchung der relativen Bedeutung von Eigen- und Fremdanregung bei der Enstehung und Entwicklung von Trummerscheiben.¨ Ich prasentiere¨ des Weiteren eine Detektion von Hα Emis- sion fur¨ das bekannte substellare Begleitobjekt um den jungen Stern PZ Tel. Die hergeleitete Hα Leuchtkraft, kombiniert mit Informationen uber¨ das Alter und die Scheibe, weist darauf hin, dass die Emission wahrscheinlich auf die chromospharische¨ Aktivitat¨ des Begleiters zuruckzuf¨ uhren¨ ist. Diese Entdeckung ist ein weiterer Nachweis, dass Instrumente und Techniken zur Abbildung mit hohem Kontrast großes Potential haben, Hα-Signaturen von Begleitern um junge Sterne zu entdecken. Schließlich prasentiere¨ ich Ergebnisse der Beobachtungskampagne “L’ band Imaging Survey to find Exoplanets in the North” (LIStEN), welche ∼ 30 nahe Sterne mit bekannten und gut charakterisierten zirkumstellaren Scheiben beinhaltet. LIStEN konzentriert sich auf die Charakterisierung der Population von Riesenplaneten mit großer Umlaufbahn in zirkumstellaren Scheiben von Sternen sowie auf die Untersuchung der Wechselwirkungen zwischen Begleiter und Scheibe. Ich diskutiere die wissenschaftlichen Ziele der Studie, die Auswahl der Objekte und Beobachtungsstrategie, sowie die Analyse und Reduktion der Beobachtungsdaten. Obwohl keine neuen Planeten entdeckt wurden, kann ich die aus den Beobachtungen abgeleiteten Grenzen fur¨ die Masse von Begleitobjekten in Kombination mit Informationen uber¨ die Große¨ und Morpholo- gie der Scheiben benutzen um die Prasenz¨ von nicht detektierten planetaren oder massearmen stellaren Begleitern in den Stern-Scheiben-Systemen einzuschranken.¨ Ai miei genitori. Contents LIST OF FIGURES xiii LIST OF TABLES xv List of Abbreviations xvii 1 Introduction1 1.1 Planets and where to find them..........................2 1.1.1 Circumstellar discs............................3 1.1.2 Detection techniques...........................4 1.1.3 Current state of the field.........................6 1.2 Direct imaging..................................7 1.2.1 Advantages and drawbacks........................7 1.2.2 Direct imaging observations.......................9 1.3 What can we learn from direct imaging?.....................9 1.3.1 Companion-disc interaction.......................9 1.3.2 Hα emission from low-mass stellar companions............. 11 1.3.3 Direct imaging surveys.......................... 12 1.3.3.1 The NaCo-ISPY and the LIStEN survey........... 14 1.4 Thesis outlook and scope............................. 15 2 ISPY - NaCo Imaging Survey for Planets around Young stars Discovery of an M dwarf in the gap between HD 193571 and its debris ring 17 2.1 Introduction.................................... 17 2.2 HD 193571.................................... 18 2.3 Observations and data reduction......................... 20 2.3.1 VLT/NaCo................................ 20 2.3.2 Gemini/GPI................................ 20 2.4 Analysis and results................................ 22 2.4.1 Astrometry and photometry....................... 22 2.4.2 Physical properties............................ 25 2.4.3 Orbital motion.............................. 26 2.5 Stirring mechanisms............................... 27 ix Contents x 2.6 Conclusions.................................... 30 3 Detection of Hα emission from PZ Tel B using SPHERE/ZIMPOL 33 3.1 Introduction.................................... 33 3.2 PZ Tel B...................................... 33 3.3 Observations and data reduction......................... 35 3.4 Analysis and results................................ 36 3.4.1 Astrometry and flux contrast....................... 37 3.4.2 Photometry................................ 37 3.4.3 Orbital constraints............................ 38 3.5 Discussion and conclusions............................ 42 4 LIStEN - the L’ band Imaging Survey to find Exoplanets in the North 45 4.1 Introduction.................................... 45 4.2 Target Selection.................................. 46 4.2.1 Target master list............................. 46 4.2.2 Notes on individual targets........................ 47 4.2.2.1 HD 206860........................... 48 4.2.2.2 HD 183324, HD 191174 and HD 192425........... 48 4.2.2.3 HD 48682, HD 143894, HD 161868, HD 212695 and HD 127821 49 4.2.2.4 HD 110897........................... 49 4.2.2.5 HD 50554........................... 49 4.2.2.6 HD 8907............................ 50 4.2.2.7 HIP 83043........................... 50 4.2.2.8 HD 128311........................... 50 4.2.2.9 HD 113337........................... 51 4.3 Observations................................... 53 4.4 Data Reduction & Analysis............................ 53 4.4.1 Data processing.............................. 53 4.4.2 PynPoint analysis............................. 56 4.4.3 Contrast curves & Mass limits...................... 57 4.4.4 Infrared excess characterisation..................... 60 4.5 Planetary constraints and disc analysis...................... 61 4.5.1 Self-stirring analysis........................... 61 4.5.2 Double-belt analysis........................... 64 4.5.3 Planetary constraints from proper motion anomaly........... 66 4.6 Conclusions.................................... 72 5 Summary and future perspective 75 5.1 Summary..................................... 75 5.2 Future perspective................................. 77 5.2.1 Follow-up observations.........................
Load more

Recommended publications
  • 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.
    [Show full text]
  • Arxiv:2105.11583V2 [Astro-Ph.EP] 2 Jul 2021 Keck-HIRES, APF-Levy, and Lick-Hamilton Spectrographs
    Draft version July 6, 2021 Typeset using LATEX twocolumn style in AASTeX63 The California Legacy Survey I. A Catalog of 178 Planets from Precision Radial Velocity Monitoring of 719 Nearby Stars over Three Decades Lee J. Rosenthal,1 Benjamin J. Fulton,1, 2 Lea A. Hirsch,3 Howard T. Isaacson,4 Andrew W. Howard,1 Cayla M. Dedrick,5, 6 Ilya A. Sherstyuk,1 Sarah C. Blunt,1, 7 Erik A. Petigura,8 Heather A. Knutson,9 Aida Behmard,9, 7 Ashley Chontos,10, 7 Justin R. Crepp,11 Ian J. M. Crossfield,12 Paul A. Dalba,13, 14 Debra A. Fischer,15 Gregory W. Henry,16 Stephen R. Kane,13 Molly Kosiarek,17, 7 Geoffrey W. Marcy,1, 7 Ryan A. Rubenzahl,1, 7 Lauren M. Weiss,10 and Jason T. Wright18, 19, 20 1Cahill Center for Astronomy & Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA 2IPAC-NASA Exoplanet Science Institute, Pasadena, CA 91125, USA 3Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA 4Department of Astronomy, University of California Berkeley, Berkeley, CA 94720, USA 5Cahill Center for Astronomy & Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA 6Department of Astronomy & Astrophysics, The Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USA 7NSF Graduate Research Fellow 8Department of Physics & Astronomy, University of California Los Angeles, Los Angeles, CA 90095, USA 9Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA 10Institute for Astronomy, University of Hawai`i,
    [Show full text]
  • Exoplanet.Eu Catalog Page 1 # Name Mass Star Name
    exoplanet.eu_catalog # name mass star_name star_distance star_mass OGLE-2016-BLG-1469L b 13.6 OGLE-2016-BLG-1469L 4500.0 0.048 11 Com b 19.4 11 Com 110.6 2.7 11 Oph b 21 11 Oph 145.0 0.0162 11 UMi b 10.5 11 UMi 119.5 1.8 14 And b 5.33 14 And 76.4 2.2 14 Her b 4.64 14 Her 18.1 0.9 16 Cyg B b 1.68 16 Cyg B 21.4 1.01 18 Del b 10.3 18 Del 73.1 2.3 1RXS 1609 b 14 1RXS1609 145.0 0.73 1SWASP J1407 b 20 1SWASP J1407 133.0 0.9 24 Sex b 1.99 24 Sex 74.8 1.54 24 Sex c 0.86 24 Sex 74.8 1.54 2M 0103-55 (AB) b 13 2M 0103-55 (AB) 47.2 0.4 2M 0122-24 b 20 2M 0122-24 36.0 0.4 2M 0219-39 b 13.9 2M 0219-39 39.4 0.11 2M 0441+23 b 7.5 2M 0441+23 140.0 0.02 2M 0746+20 b 30 2M 0746+20 12.2 0.12 2M 1207-39 24 2M 1207-39 52.4 0.025 2M 1207-39 b 4 2M 1207-39 52.4 0.025 2M 1938+46 b 1.9 2M 1938+46 0.6 2M 2140+16 b 20 2M 2140+16 25.0 0.08 2M 2206-20 b 30 2M 2206-20 26.7 0.13 2M 2236+4751 b 12.5 2M 2236+4751 63.0 0.6 2M J2126-81 b 13.3 TYC 9486-927-1 24.8 0.4 2MASS J11193254 AB 3.7 2MASS J11193254 AB 2MASS J1450-7841 A 40 2MASS J1450-7841 A 75.0 0.04 2MASS J1450-7841 B 40 2MASS J1450-7841 B 75.0 0.04 2MASS J2250+2325 b 30 2MASS J2250+2325 41.5 30 Ari B b 9.88 30 Ari B 39.4 1.22 38 Vir b 4.51 38 Vir 1.18 4 Uma b 7.1 4 Uma 78.5 1.234 42 Dra b 3.88 42 Dra 97.3 0.98 47 Uma b 2.53 47 Uma 14.0 1.03 47 Uma c 0.54 47 Uma 14.0 1.03 47 Uma d 1.64 47 Uma 14.0 1.03 51 Eri b 9.1 51 Eri 29.4 1.75 51 Peg b 0.47 51 Peg 14.7 1.11 55 Cnc b 0.84 55 Cnc 12.3 0.905 55 Cnc c 0.1784 55 Cnc 12.3 0.905 55 Cnc d 3.86 55 Cnc 12.3 0.905 55 Cnc e 0.02547 55 Cnc 12.3 0.905 55 Cnc f 0.1479 55
    [Show full text]
  • 121012-AAS-221 Program-14-ALL, Page 253 @ Preflight
    221ST MEETING OF THE AMERICAN ASTRONOMICAL SOCIETY 6-10 January 2013 LONG BEACH, CALIFORNIA Scientific sessions will be held at the: Long Beach Convention Center 300 E. Ocean Blvd. COUNCIL.......................... 2 Long Beach, CA 90802 AAS Paper Sorters EXHIBITORS..................... 4 Aubra Anthony ATTENDEE Alan Boss SERVICES.......................... 9 Blaise Canzian Joanna Corby SCHEDULE.....................12 Rupert Croft Shantanu Desai SATURDAY.....................28 Rick Fienberg Bernhard Fleck SUNDAY..........................30 Erika Grundstrom Nimish P. Hathi MONDAY........................37 Ann Hornschemeier Suzanne H. Jacoby TUESDAY........................98 Bethany Johns Sebastien Lepine WEDNESDAY.............. 158 Katharina Lodders Kevin Marvel THURSDAY.................. 213 Karen Masters Bryan Miller AUTHOR INDEX ........ 245 Nancy Morrison Judit Ries Michael Rutkowski Allyn Smith Joe Tenn Session Numbering Key 100’s Monday 200’s Tuesday 300’s Wednesday 400’s Thursday Sessions are numbered in the Program Book by day and time. Changes after 27 November 2012 are included only in the online program materials. 1 AAS Officers & Councilors Officers Councilors President (2012-2014) (2009-2012) David J. Helfand Quest Univ. Canada Edward F. Guinan Villanova Univ. [email protected] [email protected] PAST President (2012-2013) Patricia Knezek NOAO/WIYN Observatory Debra Elmegreen Vassar College [email protected] [email protected] Robert Mathieu Univ. of Wisconsin Vice President (2009-2015) [email protected] Paula Szkody University of Washington [email protected] (2011-2014) Bruce Balick Univ. of Washington Vice-President (2010-2013) [email protected] Nicholas B. Suntzeff Texas A&M Univ. suntzeff@aas.org Eileen D. Friel Boston Univ. [email protected] Vice President (2011-2014) Edward B. Churchwell Univ. of Wisconsin Angela Speck Univ. of Missouri [email protected] [email protected] Treasurer (2011-2014) (2012-2015) Hervey (Peter) Stockman STScI Nancy S.
    [Show full text]
  • 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
    [Show full text]
  • VEGA Science Review P
    The CHARA Science Meeting 2021 VEGA Science Review P. Berio, L. Bigot, D. Bonneau, M. Challouf, O. Chesneau, J.M. Clausse, O. Creevey, O. Delaa, A. Domiciano, N. Jamialahmadi, R. Ligi, F. Millour, A. Meilland, F. Morand, D. Mourard, N. Nardetto, K. Perraut, E. Saldanha, A. Salsi, A. Spang, P. Stee, I. Tallon-Bosc on behalf the VEGA team VEGA Science Review 1 The CHARA Science Meeting 2021 VEGA in a few important dates 2005 - May: 1st email exchanges - November: 1st visit on the Mountain 2006 Green light after the Tucson 2-year CHARA Science Meeting 2007 - August: 8 boxes weighting about 1200 kg sent to Mt Wilson - September, 30th: 1st 2T fringes (after 3 weeks of integration) 2008 - October: 3T fringes 2009 - Summer: First remote operation 2010 - May: simultaneous CLIMB and VEGA operation - Oct, 12th: 4T fringes together with MIRC 2012 Upgraded detectors and group delay tracking VEGA Science Review 2 The CHARA Science Meeting 2021 VEGA niches Limiting magnitude Rmag = 8 @ R ~ 5000 Very high angular resolution Spectral resolution (λ/2B ~ 0.4 mas @ 330 m) (R ~ 5000, 30000) Accurate angular diameters Kinematics and environments [Mourard+2015] ] [Ligi+2016 Circumstellar disks, mass-loss, winds, chromospheric activity, spectro-imaging Fundamental parameters, Surface-Brightness Relations, parameters of multiple and hierarchic systems VEGA Science Review 3 The CHARA Science Meeting 2021 VEGA operation in a few figures 47 refereed papers • 509 nights with recorded data • 770 stars VEGA Publications 10 • 8500 observations 8 6 4 2 During these
    [Show full text]
  • Download This Article in PDF Format
    A&A 621, A87 (2019) Astronomy https://doi.org/10.1051/0004-6361/201833431 & © ESO 2019 Astrophysics Extrasolar planets and brown dwarfs around AF-type stars X. The SOPHIE sample: combining the SOPHIE and HARPS surveys to compute the close giant planet mass-period distribution around AF-type stars?,?? S. Borgniet1, A.-M. Lagrange1, N. Meunier1, F. Galland1, L. Arnold2, N. Astudillo-Defru3, J.-L. Beuzit1, I. Boisse4, X. Bonfils1, F. Bouchy4,5, K. Debondt1, M. Deleuil4, X. Delfosse1, M. Desort1, R. F. Díaz5, A. Eggenberger5, D. Ehrenreich5, T. Forveille1, G. Hébrard2,6, B. Loeillet6, C. Lovis5, G. Montagnier2,6, C. Moutou4,7, F. Pepe5, C. Perrier1, F. Pont5, D. Queloz5,8, A. Santerne4, N. C. Santos9,10, D. Ségransan5, R. da Silva11,12, J. P. Sivan2, S. Udry5, and A. Vidal-Madjar6 1 CNRS, IPAG, Université Grenoble Alpes, 38000 Grenoble, France e-mail: [email protected] 2 Observatoire de Haute-Provence, Institut Pythéas UMS 3470, CNRS, Aix-Marseille Université, 04870 St-Michel-l’Observatoire, France 3 Departamento de Astronomía, Universidad de Concepción, Casilla 160-C, Concepción, Chile 4 LAM (Laboratoire d’Astrophysique de Marseille) UMR 7326, CNRS, Aix Marseille Université, 13388 Marseille, France 5 Observatoire Astronomique de l’Université de Genève, 51 Chemin des Maillettes, 1290 Versoix, Switzerland 6 Institut d’Astrophysique de Paris, UMR 7095 CNRS, Université Pierre & Marie Curie, 98 bis Boulevard Arago, 75014 Paris, France 7 Canada-France-Hawaii Telescope Corporation, 65-1238 Mamalahoa Hwy, Kamuela, HI 96743, USA 8 Cavendish Laboratory,
    [Show full text]
  • 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.
    [Show full text]
  • Exoplanet.Eu Catalog Page 1 Star Distance Star Name Star Mass
    exoplanet.eu_catalog star_distance star_name star_mass Planet name mass 1.3 Proxima Centauri 0.120 Proxima Cen b 0.004 1.3 alpha Cen B 0.934 alf Cen B b 0.004 2.3 WISE 0855-0714 WISE 0855-0714 6.000 2.6 Lalande 21185 0.460 Lalande 21185 b 0.012 3.2 eps Eridani 0.830 eps Eridani b 3.090 3.4 Ross 128 0.168 Ross 128 b 0.004 3.6 GJ 15 A 0.375 GJ 15 A b 0.017 3.6 YZ Cet 0.130 YZ Cet d 0.004 3.6 YZ Cet 0.130 YZ Cet c 0.003 3.6 YZ Cet 0.130 YZ Cet b 0.002 3.6 eps Ind A 0.762 eps Ind A b 2.710 3.7 tau Cet 0.783 tau Cet e 0.012 3.7 tau Cet 0.783 tau Cet f 0.012 3.7 tau Cet 0.783 tau Cet h 0.006 3.7 tau Cet 0.783 tau Cet g 0.006 3.8 GJ 273 0.290 GJ 273 b 0.009 3.8 GJ 273 0.290 GJ 273 c 0.004 3.9 Kapteyn's 0.281 Kapteyn's c 0.022 3.9 Kapteyn's 0.281 Kapteyn's b 0.015 4.3 Wolf 1061 0.250 Wolf 1061 d 0.024 4.3 Wolf 1061 0.250 Wolf 1061 c 0.011 4.3 Wolf 1061 0.250 Wolf 1061 b 0.006 4.5 GJ 687 0.413 GJ 687 b 0.058 4.5 GJ 674 0.350 GJ 674 b 0.040 4.7 GJ 876 0.334 GJ 876 b 1.938 4.7 GJ 876 0.334 GJ 876 c 0.856 4.7 GJ 876 0.334 GJ 876 e 0.045 4.7 GJ 876 0.334 GJ 876 d 0.022 4.9 GJ 832 0.450 GJ 832 b 0.689 4.9 GJ 832 0.450 GJ 832 c 0.016 5.9 GJ 570 ABC 0.802 GJ 570 D 42.500 6.0 SIMP0136+0933 SIMP0136+0933 12.700 6.1 HD 20794 0.813 HD 20794 e 0.015 6.1 HD 20794 0.813 HD 20794 d 0.011 6.1 HD 20794 0.813 HD 20794 b 0.009 6.2 GJ 581 0.310 GJ 581 b 0.050 6.2 GJ 581 0.310 GJ 581 c 0.017 6.2 GJ 581 0.310 GJ 581 e 0.006 6.5 GJ 625 0.300 GJ 625 b 0.010 6.6 HD 219134 HD 219134 h 0.280 6.6 HD 219134 HD 219134 e 0.200 6.6 HD 219134 HD 219134 d 0.067 6.6 HD 219134 HD
    [Show full text]
  • Structure and Evolution of Debris Disks Around F-Type Stars
    The Astrophysical Journal Supplement Series,193:4(25pp),2011March doi:10.1088/0067-0049/193/1/4 C 2011. The American Astronomical Society. All rights reserved. Printed in the U.S.A. ! STRUCTURE AND EVOLUTION OF DEBRIS DISKS AROUND F-TYPE STARS. I. OBSERVATIONS, DATABASE, AND BASIC EVOLUTIONARY ASPECTS A. Moor´ 1,I.Pascucci2, A.´ Kosp´ al´ 3,P.Abrah´ am´ 1,T.Csengeri4,L.L.Kiss1,5,D.Apai2,C.Grady6,7,Th.Henning8, Cs. Kiss1, D. Bayliss9,A.Juhasz´ 8,J.Kovacs´ 10,andT.Szalai11 1 Konkoly Observatory of the Hungarian Academy of Sciences, P.O. Box 67, H-1525 Budapest, Hungary; [email protected] 2 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA 3 Leiden Observatory, Leiden University, Niels Bohrweg 2, NL-2333 CA Leiden, The Netherlands 4 Laboratoire AIM, CEA/DSM, IRFU/Service d’Astrophysique, 91191 Gif-sur-Yvette Cedex, France 5 Sydney Institute for Astronomy, School of Physics A28, University of Sydney, NSW 2006, Australia 6 NASA Goddard Space Flight Center, Code 667, Greenbelt, MD 20771, USA 7 Eureka Scientific, 2452 Delmer Street, Suite 100, Oakland, CA 94602, USA 8 Max-Planck-Institut fur¨ Astronomie, Konigstuhl¨ 17, 69117 Heidelberg, Germany 9 Research School of Astronomy and Astrophysics, The Australian National University, Mount Stromlo Observatory, Cotter Road, Weston Creek, ACT 2611, Australia 10 Gothard Astrophysical Observatory, ELTE University, 9707 Szombathely, Hungary 11 Department of Optics and Quantum Electronics, University of Szeged, 6720 Szeged, Dom´ ter´ 9, Hungary Received 2010 May 30; accepted 2010 December 10; published 2011 January 20 ABSTRACT Although photometric and spectroscopic surveys with the Spitzer Space Telescope remarkably increased the number of well-studied debris disks around A-type and Sun-like stars, detailed analyses of debris disks around F-type stars remained less frequent.
    [Show full text]
  • September 2017 BRAS Newsletter
    September 2017 Issue September 2017 Next Meeting: Monday, September 11th at 7PM at HRPO nd (2 Mondays, Highland Road Park Observatory) September Program: GAE (Great American. Eclipse) Membership Reports. Club members are invited to “approach the mike. ” and share their experiences travelling hither and thither to observe the August total eclipse. What's In This Issue? HRPO’s Great American Eclipse Event Summary (Page 2) President’s Message Secretary's Summary Outreach Report - FAE Light Pollution Committee Report Recent Forum Entries 20/20 Vision Campaign Messages from the HRPO Spooky Spectrum Observe The Moon Night Observing Notes – Draco The Dragon, & Mythology Like this newsletter? See past issues back to 2009 at http://brastro.org/newsletters.html Newsletter of the Baton Rouge Astronomical Society September 2017 The Great American Eclipse is now a fond memory for our Baton Rouge community. No ornery clouds or“washout”; virtually the entire three-hour duration had an unobstructed view of the Sun. Over an hour before the start of the event, we sold 196 solar viewers in thirty-five minutes. Several families and children used cereal box viewers; many, many people were here for the first time. We utilized the Coronado Solar Max II solar telescope and several nighttime telescopes, each outfitted with either a standard eyepiece or a “sun funnel”—a modified oil funnel that projects light sent through the scope tube to fabric stretched across the front of the funnel. We provided live feeds on the main floor from NASA and then, ABC News. The official count at 1089 patrons makes this the best- attended event in HRPO’s twenty years save for the historic Mars Opposition of 2003.
    [Show full text]
  • TRUE MASSES of RADIAL-VELOCITY EXOPLANETS Robert A
    APP Template V1.01 Article id: apj513330 Typesetter: MPS Date received by MPS: 19/05/2015 PE: CE : LE: UNCORRECTED PROOF The Astrophysical Journal, 00:000000 (28pp), 2015 Month Day © 2015. The American Astronomical Society. All rights reserved. TRUE MASSES OF RADIAL-VELOCITY EXOPLANETS Robert A. Brown Space Telescope Science Institute, USA; [email protected] Received 2015 January 12; accepted 2015 April 14; published 2015 MM DD ABSTRACT We study the task of estimating the true masses of known radial-velocity (RV) exoplanets by means of direct astrometry on coronagraphic images to measure the apparent separation between exoplanet and host star. Initially, we assume perfect knowledge of the RV orbital parameters and that all errors are due to photon statistics. We construct design reference missions for four missions currently under study at NASA: EXO-S and WFIRST-S, with external star shades for starlight suppression, EXO-C and WFIRST-C, with internal coronagraphs. These DRMs reveal extreme scheduling constraints due to the combination of solar and anti-solar pointing restrictions, photometric and obscurational completeness, image blurring due to orbital motion, and the “nodal effect,” which is the independence of apparent separation and inclination when the planet crosses the plane of the sky through the host star. Next, we address the issue of nonzero uncertainties in RV orbital parameters by investigating their impact on the observations of 21 single-planet systems. Except for two—GJ 676 A b and 16 Cyg B b, which are observable only by the star-shade missions—we find that current uncertainties in orbital parameters generally prevent accurate, unbiased estimation of true planetary mass.
    [Show full text]