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Lurking in the Shadows: Wide-Separation Gas Giants As Tracers of Planet Formation
Lurking in the Shadows: Wide-Separation Gas Giants as Tracers of Planet Formation Thesis by Marta Levesque Bryan In Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy CALIFORNIA INSTITUTE OF TECHNOLOGY Pasadena, California 2018 Defended May 1, 2018 ii © 2018 Marta Levesque Bryan ORCID: [0000-0002-6076-5967] All rights reserved iii ACKNOWLEDGEMENTS First and foremost I would like to thank Heather Knutson, who I had the great privilege of working with as my thesis advisor. Her encouragement, guidance, and perspective helped me navigate many a challenging problem, and my conversations with her were a consistent source of positivity and learning throughout my time at Caltech. I leave graduate school a better scientist and person for having her as a role model. Heather fostered a wonderfully positive and supportive environment for her students, giving us the space to explore and grow - I could not have asked for a better advisor or research experience. I would also like to thank Konstantin Batygin for enthusiastic and illuminating discussions that always left me more excited to explore the result at hand. Thank you as well to Dimitri Mawet for providing both expertise and contagious optimism for some of my latest direct imaging endeavors. Thank you to the rest of my thesis committee, namely Geoff Blake, Evan Kirby, and Chuck Steidel for their support, helpful conversations, and insightful questions. I am grateful to have had the opportunity to collaborate with Brendan Bowler. His talk at Caltech my second year of graduate school introduced me to an unexpected population of massive wide-separation planetary-mass companions, and lead to a long-running collaboration from which several of my thesis projects were born. -
Stability of Planets in Binary Star Systems
StabilityStability ofof PlanetsPlanets inin BinaryBinary StarStar SystemsSystems Ákos Bazsó in collaboration with: E. Pilat-Lohinger, D. Bancelin, B. Funk ADG Group Outline Exoplanets in multiple star systems Secular perturbation theory Application: tight binary systems Summary + Outlook About NFN sub-project SP8 “Binary Star Systems and Habitability” Stand-alone project “Exoplanets: Architecture, Evolution and Habitability” Basic dynamical types S-type motion (“satellite”) around one star P-type motion (“planetary”) around both stars Image: R. Schwarz Exoplanets in multiple star systems Observations: (Schwarz 2014, Binary Catalogue) ● 55 binary star systems with 81 planets ● 43 S-type + 12 P-type systems ● 10 multiple star systems with 10 planets Example: γ Cep (Hatzes et al. 2003) ● RV measurements since 1981 ● Indication for a “planet” (Campbell et al. 1988) ● Binary period ~57 yrs, planet period ~2.5 yrs Multiplicity of stars ~45% of solar like stars (F6 – K3) with d < 25 pc in multiple star systems (Raghavan et al. 2010) Known exoplanet host stars: single double triple+ source 77% 20% 3% Raghavan et al. (2006) 83% 15% 2% Mugrauer & Neuhäuser (2009) 88% 10% 2% Roell et al. (2012) Exoplanet catalogues The Extrasolar Planets Encyclopaedia http://exoplanet.eu Exoplanet Orbit Database http://exoplanets.org Open Exoplanet Catalogue http://www.openexoplanetcatalogue.com The Planetary Habitability Laboratory http://phl.upr.edu/home NASA Exoplanet Archive http://exoplanetarchive.ipac.caltech.edu Binary Catalogue of Exoplanets http://www.univie.ac.at/adg/schwarz/multiple.html Habitable Zone Gallery http://www.hzgallery.org Binary Catalogue Binary Catalogue of Exoplanets http://www.univie.ac.at/adg/schwarz/multiple.html Dynamical stability Stability limit for S-type planets Rabl & Dvorak (1988), Holman & Wiegert (1999), Pilat-Lohinger & Dvorak (2002) Parameters (a , e , μ) bin bin Outer limit at roughly max. -
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. -
Can There Be Additional Rocky Planets in the Habitable Zone of Tight Binary
Mon. Not. R. Astron. Soc. 000, 1–10 () Printed 24 September 2018 (MN LATEX style file v2.2) Can there be additional rocky planets in the Habitable Zone of tight binary stars with a known gas giant? B. Funk1⋆, E. Pilat-Lohinger1 and S. Eggl2 1Institute for Astronomy, University of Vienna, Vienna, Austria 2IMCCE, Observatoire de Paris, Paris, France ABSTRACT Locating planets in Habitable Zones (HZs) around other stars is a growing field in contem- porary astronomy. Since a large percentage of all G-M stars in the solar neighborhood are expected to be part of binary or multiple stellar systems, investigations of whether habitable planets are likely to be discovered in such environments are of prime interest to the scientific community. As current exoplanet statistics predicts that the chances are higher to find new worlds in systems that are already known to have planets, we examine four known extrasolar planetary systems in tight binaries in order to determine their capacity to host additional hab- itable terrestrial planets. Those systems are Gliese 86, γ Cephei, HD 41004 and HD 196885. In the case of γ Cephei, our results suggest that only the M dwarf companion could host ad- ditional potentially habitable worlds. Neither could we identify stable, potentially habitable regions around HD 196885A. HD 196885 B can be considered a slightly more promising tar- get in the search forEarth-twins.Gliese 86 A turned out to be a very good candidate, assuming that the system’s history has not been excessively violent. For HD 41004 we have identified admissible stable orbits for habitable planets, but those strongly depend on the parameters of the system. -
ESO Annual Report 2004 ESO Annual Report 2004 Presented to the Council by the Director General Dr
ESO Annual Report 2004 ESO Annual Report 2004 presented to the Council by the Director General Dr. Catherine Cesarsky View of La Silla from the 3.6-m telescope. ESO is the foremost intergovernmental European Science and Technology organi- sation in the field of ground-based as- trophysics. It is supported by eleven coun- tries: Belgium, Denmark, France, Finland, Germany, Italy, the Netherlands, Portugal, Sweden, Switzerland and the United Kingdom. Created in 1962, ESO provides state-of- the-art research facilities to European astronomers and astrophysicists. In pur- suit of this task, ESO’s activities cover a wide spectrum including the design and construction of world-class ground-based observational facilities for the member- state scientists, large telescope projects, design of innovative scientific instruments, developing new and advanced techno- logies, furthering European co-operation and carrying out European educational programmes. ESO operates at three sites in the Ataca- ma desert region of Chile. The first site The VLT is a most unusual telescope, is at La Silla, a mountain 600 km north of based on the latest technology. It is not Santiago de Chile, at 2 400 m altitude. just one, but an array of 4 telescopes, It is equipped with several optical tele- each with a main mirror of 8.2-m diame- scopes with mirror diameters of up to ter. With one such telescope, images 3.6-metres. The 3.5-m New Technology of celestial objects as faint as magnitude Telescope (NTT) was the first in the 30 have been obtained in a one-hour ex- world to have a computer-controlled main posure. -
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 -
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. -
Direct Imaging of Radial Velocity Exoplanets WFIRST-AFTA Coronagraph Study
Direct Imaging of Radial Velocity Exoplanets WFIRST-AFTA Coronagraph Study 12/18/2014 Aastha Acharya, aa533 Advisor: Dmitry Savransky, ds264 Contents Abstract .................................................................................................................................................. 2 Introduction ............................................................................................................................................ 3 Literature Review .................................................................................................................................... 4 Exoplanet Background ......................................................................................................................... 4 Detection Methods .............................................................................................................................. 4 Radial Velocity Detection Method ....................................................................................................... 7 Orbital Mechanics.............................................................................................................................. 10 Coronagraph Specification ................................................................................................................. 11 Methodology ......................................................................................................................................... 13 Results and Discussion .......................................................................................................................... -
The CORALIE Survey for Southern Extra-Solar Planets IX. a 1.3-Day
Astronomy & Astrophysics manuscript no. (will be inserted by hand later) The CORALIE survey for southern extra-solar planets⋆ IX. A 1.3-day period brown dwarf disguised as a planet N.C. Santos1, M. Mayor1, D. Naef1, F. Pepe1, D. Queloz1, S. Udry1, M. Burnet1, J.V. Clausen2, B.E. Helt2, E.H. Olsen2, and J.D. Pritchard3 1 Observatoire de Gen`eve, 51 ch. des Maillettes, CH–1290 Sauverny, Switzerland 2 Niels Bohr Institute for Astronomy, Physics, and Geophysics; Astronomical Observatory, Juliane Maries Vej 30, DK-2100 Copenhagen Ø, Denmark 3 European Southern Observatory, Santiago, Chile Received / Accepted Abstract. In this article we present the case of HD 41004 AB, a system composed of a K0V star and a 3.7- magnitude fainter M-dwarf companion. We have obtained 86 CORALIE spectra of this system with the goal of obtaining precise radial-velocity measurements. Since HD 41004 A and B are separated by only 0.5′′, in every spectrum taken for the radial-velocity measurement, we are observing the blended spectra of the two stars. An analysis of the measurements has revealed a velocity variation with an amplitude of about 50 m s−1 and a periodicity of 1.3 days. This radial-velocity signal is consistent with the expected variation induced by the presence of a companion to either HD 41004 A or HD 41004 B, or to some other effect due to e.g. activity related phenomena. In particular, such a small velocity amplitude could be the signature of the presence of a very low mass giant planetary companion to HD 41004 A, whose light dominates the spectra. -
Planet Formation in Binaries 3
Noname manuscript No. (will be inserted by the editor) Planet formation in Binaries P. Thebault · N. Haghighipour the date of receipt and acceptance should be inserted later Abstract Spurred by the discovery of more than 60 exoplanets in multiple systems, binaries have become in recent years one of the main topics in planet formation re- search. Numerous studies have investigated to what extent the presence of a stellar companion can affect the planet formation process. Such studies have implications that can reach beyond the sole context of binaries, as they allow to test certain as- pects of the planet formation scenario by submitting them to extreme environments. We review here the current understanding on this complex problem. We show in par- ticular how each of the different stages of the planet-formation process is affected differently by binary perturbations. We focus especially on the intermediate stage of kilometre-sized planetesimal accretion, which has proven to be the most sensitive to binarity and for which the presence of some exoplanets observed in tight binaries is difficult to explain by in-situ formation following the ”standard” planet-formation scenario. Some tentative solutions to this apparent paradox are presented. The last part of our review presents a thorough description of the problem of planet habit- ability, for which the binary environment creates a complex situation because of the presence of two irradiation sources of varying distance. Keywords Planetary systems · Binary Stars 1 Introduction About half of solar-type stars reside in multiple stellar systems (Raghavan et al., 2010). As a consequence, one of the most generic environments to be considered for studying planet formation should in principle be that of a binary. -
An Extended Benford Analysis of Exoplanet Orbital Periods
Page 1 of 12 An extended Benford analysis of exoplanet orbital periods PATRICK VANOUPLINES 1,* 1University Library – Vrije Universiteit Brussel, 1050 Brussels, Belgium. *Corresponding author. E-mail: [email protected] Abstract. Shukla, Pandey and Pathak (2017) report about their findings of a Benford analysis applied to the physical properties of exoplanets. The present paper gives a short literature overview of previous research on exoplanets. We describe the methods to perform an extended Benford analysis, which considers, both the first digit, and also other digits and digit combinations. Methods for testing conformity with the Benford distribution are discussed and applied to the digits of orbital data of exoplanets. A first result of this research is that the used data pass most of the tests. It is observed that for most tests on the orbital period values, the almost 4,000 presently known and confirmed exoplanets seem to be sufficient. The analysis of the first, second and third digits (and combinations of these digits) shows a good agreement with the Benford distribution. The analysis of the last two digits indicates that the last significant zero gets lost easily during the export from the exoplanet database. The summation analysis isolates exoplanets with extremely long orbital periods. Keywords. Benford’s law – Benford analysis – exoplanets – orbital period. 1. Introduction astronomer Simon Newcomb noticed that the first pages of books containing logarithm tables where Only a small number of publications discuss the more worn than the other pages. Newcomb (1881) use of Benford’s law in astronomy. The paper by proposed a law expressing the relation between Shukla, Pandey and Pathak (2017) on the the frequency of numbers starting with a smaller evaluation of the validity of Benford’s law digit and numbers starting with a higher digit: he regarding properties of extrasolar planets was the stated that the probability (as a fraction) of a inspiration for a more in-depth study on which we number starting with digit d (from 1 to 9, the report here. -
Commission 5 Documentation and Astronomical Data (Documentation and Astronomical Data)
Transactions IAU, Volume XXVIIB Proc. XXVII IAU General Assembly, August 2009 °c 2010 International Astronomical Union Ian F. Corbett, ed. DOI: 00.0000/X000000000000000X COMMISSION 5 DOCUMENTATION AND ASTRONOMICAL DATA (DOCUMENTATION AND ASTRONOMICAL DATA) PRESIDENT Ray P. Norris VICE-PRESIDENT Masatoshi Ohishi PAST PRESIDENT Franoise Genova ORGANIZING COMMITTEE Uta Grothkopf, Bob Hanisch, Oleg Malkov, William Pence, Marion Schmitz, Xu Zhou PROCEEDINGS OF BUSINESS SESSIONS, 3–7 August 2009 1. Introduction Commission 5 and its working groups have continued to operate at a high level of activity over the last three years. In an era when the volume of astronomical data generated by next- generation instruments continues to increase dramatically, and data centres and data tools become increasingly central to front-line astronomical research, the activities of Commission 5 are becoming even more significant. However, most of the activities of Commission 5 take place through its working groups. That was reflected in the meetings at the IAU GA, where there was only one short Business Meeting of the Commission as a whole, but several vigorous meetings of the working groups. 2. Commission 5 Business Meeting, Mon 3 August 2009. Chair: Masatoshi Ohishi 2.1. New Officers of Commission 5 Nominations were requested from all members of Commission 5 for the new Organising Com- mittee (OC), and all Commission 5 members were then invited to vote for the nominees, as a result of which the following people were appointed: • Masatoshi Ohishi (Japan): President • Bob Hanisch (USA): Vice President • Ray Norris (Australia): Past President • Heinz Andernach (Mexico) • Marsha Bishop (USA) • Elizabeth Griffin (Canada) • Ajit Kembhavi (India) • Tara Murphy (Australia) • Fabio Pasian (Italy) 2.2.