Multi-Planet Extrasolar Systems – Detection and Dynamics
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
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. -
Enabling Science with Gaia Observations of Naked-Eye Stars
Enabling science with Gaia observations of naked-eye stars J. Sahlmanna,b, J. Mart´ın-Fleitasb,c, A. Morab,c, A. Abreub,d, C. M. Crowleyb,e, E. Jolietb,f aEuropean Space Agency, STScI, 3700 San Martin Drive, Baltimore, MD 21218, USA; bEuropean Space Agency, ESAC, P.O. Box 78, Villanueva de la Canada,˜ 28691 Madrid, Spain; cAurora Technology, Crown Business Centre, Heereweg 345, 2161 CA Lisse, The Netherlands; dElecnor Deimos Space, Ronda de Poniente 19, Ed. Fiteni VI, 28760 Tres Cantos, Madrid, Spain; eHE Space Operations BV, Huygensstraat 44, 2201 DK Noordwijk, The Netherlands; fCalifornia Institute of Technology, Pasadena, CA, 91125, USA ABSTRACT ESA’s Gaia space astrometry mission is performing an all-sky survey of stellar objects. At the beginning of the nominal mission in July 2014, an operation scheme was adopted that enabled Gaia to routinely acquire observations of all stars brighter than the original limit of G∼6, i.e. the naked-eye stars. Here, we describe the current status and extent of those observations and their on-ground processing. We present an overview of the data products generated for G<6 stars and the potential scientific applications. Finally, we discuss how the Gaia survey could be enhanced by further exploiting the techniques we developed. Keywords: Gaia, Astrometry, Proper motion, Parallax, Bright Stars, Extrasolar planets, CCD 1. INTRODUCTION There are about 6000 stars that can be observed with the unaided human eye. Greek astronomer Hipparchus used these stars to define the magnitude system still in use today, in which the faintest stars had an apparent visual magnitude of 6. -
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. -
Gaia Search for Stellar Companions of TESS Objects of Interest
Received 1 July 2020; Revised 29 August 2020; Accepted 18 September 2020 DOI: xxx/xxxx ARTICLE TYPE Gaia Search for stellar Companions of TESS Objects of Interest M. Mugrauer* | K.-U. Michel 1Astrophysikalisches Institut und Universitäts-Sternwarte Jena The first results of a new survey are reported, which explores the 2nd data release Correspondence of the ESA-Gaia mission, in order to search for stellar companions of (Community) M. Mugrauer, Astrophysikalisches Institut und Universitäts-Sternwarte Jena, TESS Objects of Interest and to characterize their properties. In total, 193 binary and Schillergäßchen 2, D-07745 Jena, Germany. 15 hierarchical triple star systems are presented, detected among 1391 target stars, Email: [email protected] which are located at distances closer than about 500 pc around the Sun. The com- panions and the targets are equidistant and share a common proper motion, as it is expected for gravitationally bound stellar systems, proven with their accurate Gaia astrometry. The companions exhibit masses in the range between about 0.08 M⊙ and 3 M⊙ and are most frequently found in the mass range between 0.13 and 0.6 M⊙. The companions are separated from the targets by about 40 up to 9900 au, and their frequency continually decreases with increasing separation. While most of the detected companions are late K to mid M dwarfs, also 5 white dwarf companions were identified in this survey, whose true nature is revealed by their photometric properties. KEYWORDS: binaries: visual, white dwarfs, stars: individual (TOI 249 C, TOI 1259 B, TOI 1624 B, TOI 1703 B, CTOI 53309262 B) 1 INTRODUCTION explored the 2nd data release of the European Space Agency (ESA) Gaia mission (Gaia DR2 from hereon, Gaia Collabora- A key aspect in the diversity of exoplanets is the multiplicity tion, Brown, Vallenari, et al., 2018), which provides manifold of their host stars. -
Ghost Imaging of Space Objects
Ghost Imaging of Space Objects Dmitry V. Strekalov, Baris I. Erkmen, Igor Kulikov, and Nan Yu Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California 91109-8099 USA NIAC Final Report September 2014 Contents I. The proposed research 1 A. Origins and motivation of this research 1 B. Proposed approach in a nutshell 3 C. Proposed approach in the context of modern astronomy 7 D. Perceived benefits and perspectives 12 II. Phase I goals and accomplishments 18 A. Introducing the theoretical model 19 B. A Gaussian absorber 28 C. Unbalanced arms configuration 32 D. Phase I summary 34 III. Phase II goals and accomplishments 37 A. Advanced theoretical analysis 38 B. On observability of a shadow gradient 47 C. Signal-to-noise ratio 49 D. From detection to imaging 59 E. Experimental demonstration 72 F. On observation of phase objects 86 IV. Dissemination and outreach 90 V. Conclusion 92 References 95 1 I. THE PROPOSED RESEARCH The NIAC Ghost Imaging of Space Objects research program has been carried out at the Jet Propulsion Laboratory, Caltech. The program consisted of Phase I (October 2011 to September 2012) and Phase II (October 2012 to September 2014). The research team consisted of Drs. Dmitry Strekalov (PI), Baris Erkmen, Igor Kulikov and Nan Yu. The team members acknowledge stimulating discussions with Drs. Leonidas Moustakas, Andrew Shapiro-Scharlotta, Victor Vilnrotter, Michael Werner and Paul Goldsmith of JPL; Maria Chekhova and Timur Iskhakov of Max Plank Institute for Physics of Light, Erlangen; Paul Nu˜nez of Coll`ege de France & Observatoire de la Cˆote d’Azur; and technical support from Victor White and Pierre Echternach of JPL. -
Two Jovian Planets Around the Giant Star HD 202696: a Growing Population of Packed Massive Planetary Pairs Around Massive Stars?
The Astronomical Journal, 157:93 (13pp), 2019 March https://doi.org/10.3847/1538-3881/aafa11 © 2019. The American Astronomical Society. All rights reserved. Two Jovian Planets around the Giant Star HD 202696: A Growing Population of Packed Massive Planetary Pairs around Massive Stars? Trifon Trifonov1 , Stephan Stock2 , Thomas Henning1 , Sabine Reffert2 , Martin Kürster1 , Man Hoi Lee3,4 , Bertram Bitsch1 , R. Paul Butler5 , and Steven S. Vogt6 1 Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany; [email protected] 2 Landessternwarte, Zentrum für Astronomie der Universität Heidelberg, Königstuhl 12, D-69117 Heidelberg, Germany 3 Department of Earth Sciences, The University of Hong Kong, Pokfulam Road, Hong Kong 4 Department of Physics, The University of Hong Kong, Pokfulam Road, Hong Kong 5 Department of Terrestrial Magnetism, Carnegie Institution for Science, Washington, DC 20015, USA 6 UCO/Lick Observatory, Department of Astronomy and Astrophysics, University of California at Santa Cruz, Santa Cruz, CA 95064, USA Received 2018 September 24; revised 2018 December 18; accepted 2018 December 18; published 2019 February 4 Abstract We present evidence for a new two-planet system around the giant star HD 202696 (=HIP 105056, BD +26 4118). The discovery is based on public HIRES radial velocity (RV) measurements taken at Keck Observatory between +0.09 2007 July and 2014 September. We estimate a stellar mass of 1.91-0.14 M for HD 202696, which is located close to the base of the red giant branch. A two-planet self-consistent dynamical modeling MCMC scheme of the RV = +8.9 = +20.7 data followed by a long-term stability test suggests planetary orbital periods of Pb 517.8-3.9 and Pc 946.6-20.9 = +0.078 = +0.065 = +0.22 days, eccentricities of eb 0.011-0.011 and ec 0.028-0.012, and minimum dynamical masses of mb 2.00-0.10 = +0.18 fi and mc 1.86-0.23 MJup, respectively. -
Precise Radial Velocities of Giant Stars
A&A 555, A87 (2013) Astronomy DOI: 10.1051/0004-6361/201321714 & c ESO 2013 Astrophysics Precise radial velocities of giant stars V. A brown dwarf and a planet orbiting the K giant stars τ Geminorum and 91 Aquarii, David S. Mitchell1,2,SabineReffert1, Trifon Trifonov1, Andreas Quirrenbach1, and Debra A. Fischer3 1 Landessternwarte, Zentrum für Astronomie der Universität Heidelberg, Königstuhl 12, 69117 Heidelberg, Germany 2 Physics Department, California Polytechnic State University, San Luis Obispo, CA 93407, USA e-mail: [email protected] 3 Department of Astronomy, Yale University, New Haven, CT 06511, USA Received 16 April 2013 / Accepted 22 May 2013 ABSTRACT Aims. We aim to detect and characterize substellar companions to K giant stars to further our knowledge of planet formation and stellar evolution of intermediate-mass stars. Methods. For more than a decade we have used Doppler spectroscopy to acquire high-precision radial velocity measurements of K giant stars. All data for this survey were taken at Lick Observatory. Our survey includes 373 G and K giants. Radial velocity data showing periodic variations were fitted with Keplerian orbits using a χ2 minimization technique. Results. We report the presence of two substellar companions to the K giant stars τ Gem and 91 Aqr. The brown dwarf orbiting τ Gem has an orbital period of 305.5±0.1 days, a minimum mass of 20.6 MJ, and an eccentricity of 0.031±0.009. The planet orbiting 91 Aqr has an orbital period of 181.4 ± 0.1 days, a minimum mass of 3.2 MJ, and an eccentricity of 0.027 ± 0.026. -
Pdfs) for Each Orbital Parameter Used in and (3) in Cumming Et Al
View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by Caltech Authors The Astrophysical Journal, 709:396–410, 2010 January 20 doi:10.1088/0004-637X/709/1/396 C 2010. The American Astronomical Society. All rights reserved. Printed in the U.S.A. RETIRED A STARS AND THEIR COMPANIONS. III. COMPARING THE MASS–PERIOD DISTRIBUTIONS OF PLANETS AROUND A-TYPE STARS AND SUN-LIKE STARS∗ Brendan P. Bowler1, John Asher Johnson1,7, Geoffrey W. Marcy2, Gregory W. Henry3, Kathryn M. G. Peek2, Debra A. Fischer4, Kelsey I. Clubb4, Michael C. Liu1, Sabine Reffert5, Christian Schwab5, and Thomas B. Lowe6 1 Institute for Astronomy, University of Hawai‘i, 2680 Woodlawn Drive, Honolulu, HI 96822, USA; [email protected] 2 Department of Astronomy, University of California, MS 3411, Berkeley, CA 94720-3411, USA 3 Center of Excellence in Information Systems, Tennessee State University, 3500 John A. Merritt Blvd., Box 9501, Nashville, TN 37209, USA 4 Department of Physics and Astronomy, San Francisco State University, San Francisco, CA 94132, USA 5 ZAH-Landessternwarte, Konigstuhl¨ 12, 69117 Heidelberg, Germany 6 UCO/Lick Observatory, Santa Cruz, CA 95064, USA Received 2009 June 10; accepted 2009 December 3; published 2009 December 31 ABSTRACT We present an analysis of ∼5 years of Lick Observatory radial velocity measurements targeting a uniform sample of 31 intermediate-mass (IM) subgiants (1.5 M∗/M 2.0) with the goal of measuring the occurrence rate of Jovian planets around (evolved) A-type stars and comparing the distributions of their orbital and physical characteristics to those of planets around Sun-like stars. -
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 -
AMD-Stability and the Classification of Planetary Systems
A&A 605, A72 (2017) DOI: 10.1051/0004-6361/201630022 Astronomy c ESO 2017 Astrophysics& AMD-stability and the classification of planetary systems? J. Laskar and A. C. Petit ASD/IMCCE, CNRS-UMR 8028, Observatoire de Paris, PSL, UPMC, 77 Avenue Denfert-Rochereau, 75014 Paris, France e-mail: [email protected] Received 7 November 2016 / Accepted 23 January 2017 ABSTRACT We present here in full detail the evolution of the angular momentum deficit (AMD) during collisions as it was described in Laskar (2000, Phys. Rev. Lett., 84, 3240). Since then, the AMD has been revealed to be a key parameter for the understanding of the outcome of planetary formation models. We define here the AMD-stability criterion that can be easily verified on a newly discovered planetary system. We show how AMD-stability can be used to establish a classification of the multiplanet systems in order to exhibit the planetary systems that are long-term stable because they are AMD-stable, and those that are AMD-unstable which then require some additional dynamical studies to conclude on their stability. The AMD-stability classification is applied to the 131 multiplanet systems from The Extrasolar Planet Encyclopaedia database for which the orbital elements are sufficiently well known. Key words. chaos – celestial mechanics – planets and satellites: dynamical evolution and stability – planets and satellites: formation – planets and satellites: general 1. Introduction motion resonances (MMR, Wisdom 1980; Deck et al. 2013; Ramos et al. 2015) could justify the Hill-type criteria, but the The increasing number of planetary systems has made it nec- results on the overlap of the MMR island are valid only for close essary to search for a possible classification of these planetary orbits and for short-term stability. -
Arxiv:1901.01935V2 [Astro-Ph.EP] 30 Jan 2019
Draft version January 31, 2019 Preprint typeset using LATEX style AASTeX6 v. 1.0 TWO JOVIAN PLANETS AROUND THE GIANT STAR HD 202696. A GROWING POPULATION OF PACKED MASSIVE PLANETARY PAIRS AROUND MASSIVE STARS? Trifon Trifonov1, Stephan Stock2, Thomas Henning1, Sabine Reffert2, Martin Kurster¨ 1, Man Hoi Lee3,4, Bertram Bitsch1, R. Paul Butler5, Steven S. Vogt6 1 Max-Planck-Institut f¨urAstronomie, K¨onigstuhl17, D-69117 Heidelberg, Germany 2 Landessternwarte, Zentrum f¨urAstronomie der Universit¨atHeidelberg, K¨onigstuhl12, D-69117 Heidelberg, Germany 3 Department of Earth Sciences, The University of Hong Kong, Pokfulam Road, Hong Kong 4 Department of Physics, The University of Hong Kong, Pokfulam Road, Hong Kong 5 Department of Terrestrial Magnetism, Carnegie Institution for Science, Washington, DC 20015, USA and 6 UCO/Lick Observatory, Department of Astronomy and Astrophysics, University of California at Santa Cruz, Santa Cruz, CA 95064, USA ABSTRACT We present evidence for a new two-planet system around the giant star HD 202696 (= HIP 105056, BD +26 4118). The discovery is based on public HIRES radial velocity (RV) measurements taken at +0:09 Keck Observatory between 2007 July and 2014 September. We estimate a stellar mass of 1.91−0:14M for HD 202696, which is located close to the base of the red giant branch. A two-planet self-consistent dynamical modeling MCMC scheme of the RV data followed by a long-term stability test suggests +8:9 +20:7 +0:078 planetary orbital periods of Pb = 517.8−3:9 and Pc = 946.6−20:9 days, eccentricities of eb = 0.011−0:011 +0:065 +0:22 +0:18 and ec = 0.028−0:012 , and minimum dynamical masses of mb = 2.00−0:10 MJup and mc = 1.86−0:23 MJup, respectively. -
JOHN MICHAEL BREWER Yale Astronomy 52 Hillhouse Avenue Room 219 New Haven CT 06511
JOHN MICHAEL BREWER Yale Astronomy 52 Hillhouse Avenue Room 219 New Haven CT 06511 C (510) 847-9676 [email protected] REFEREED PUBLICATIONS [42] The Mass of the White Dwarf Companion in the Self-Lensing Binary KOI-3278: Einstein vs. Newton Yahalomi, Daniel A., Shvartzvald, Yossi, Agol, Eric et al. [incl. Brewer] (2019). ApJ (Submitted), arxiv.org/abs/1904.11063 [41] Modeling the Echelle Spectra Continuum with Alpha Shapes and Local Regression Fitting Xu, Xin, Cisewski-Kehe, Jessi, Davis, Allen B., Fischer, Debra A., Brewer, John M. (2019). AJ (Accepted), arxiv.org/abs/1904.10065 [40] Benchmarking Substellar Evolutionary Models Using New Age Estimates for HD 4747 B and HD 19467 B Wood, Charlotte M., Boyajian, Tabetha, von Braun, Kaspar, Brewer, John M., et al. (2019), ApJ (Accepted), arxiv.org/abs/1901.03687 [39] HD 202772A b: A Transiting Hot Jupiter around a Bright, Mildly Evolved Star in a Visual Binary Discovered by TESS Songhu Wang, Matias Jones, Avi Shporer, et al. [incl. Brewer] (2019), AJ, 157, 2, iopscience.iop.org/article/10.3847/1538-3881/aaf1b7/meta [38] Compact Multi-planet Systems More Common Around Metal Poor Hosts Brewer, John M., Wang, Songhu, Fischer, Debra A., Foreman-Mackey, Dan (2018). ApJL, 867(1), doi.org/10.3847/2041-8213/aae710. [37] Spectral Properties of Cool Stars: Extended Abundance Analysis of Kepler Objects of Interest Brewer, John M., Fischer, Debra A. (2018). ApJS, 237(2) doi.org/10.3847/1538-4365/ aad501 [36] Stellar Spin–Orbit Alignment for Kepler-9, a Multi-transiting Planetary System with Two Outer Planets Near 2:1 Resonance Wang, Songhu, Addison, Brett, Fischer, Debra A., Brewer, John M.