An Extended Benford Analysis of Exoplanet Orbital Periods
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. -
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. -
Introduction
Cambridge University Press 978-1-108-41977-2 — The Exoplanet Handbook Michael Perryman Excerpt More Information 1 Introduction 1.1 The challenge lensing provided evidence for a low-mass planet orbit- ing a star near the centre of the Galaxy nearly 30 000 HEREAREHUNDREDSOFBILLIONS of galaxies in the light-years away, with the first confirmed microlensing observable Universe, with each galaxy such as our T planet reported in 2004. In the photometric search for own containing some hundred billion stars. Surrounded transiting exoplanets, the first transit of a previously- by this seemingly limitless ocean of stars, mankind has detected exoplanet was reported in 1999, the first discov- long speculated about the existence of planetary sys- ery by transit photometry in 2003, the first of the wide- tems other than our own, and the possibility of life ex- field bright star survey discoveries in 2004, and the first isting elsewhere in the Universe. discovery from space observations in 2008. Only recently has evidence become available to be- While these manifestations of the existence of exo- gin to distinguish the extremes of thinking that has per- planets are also extremely subtle, advances in Doppler vaded for more than 2000 years, with opinions ranging measurements, photometry, microlensing, timing, from ‘There are infinite worlds both like and unlike this imaging, and astrometry, have since provided the tools world of ours’ (Epicurus, 341–270 BCE) to ‘There cannot for their detection in relatively large numbers. Now, al- be more worlds than one’ (Aristotle, 384–322 BCE). most 25 years after the first observational confirmation, Shining by reflected starlight, exoplanets compa- exoplanet detection and characterisation, and advances rable to solar system planets will be billions of times in the theoretical understanding of their formation and fainter than their host stars and, depending on their dis- evolution, are moving rapidly on many fronts. -
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 -
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 .......................................................................................................................... -
Analytic Stability Maps of Unknown Exoplanet Companions for Imaging Prioritization
Bachelor's degree thesis ANALYTIC STABILITY MAPS OF UNKNOWN EXOPLANET COMPANIONS FOR IMAGING PRIORITIZATION Carlos Gasc´on Alvarez´ Advised by Dmitry Savransky (Cornell University) Miquel Sureda (UPC) In partial fulfillment of the requirements for the Bachelor's Degree in Mathematics Bachelor's Degree in Aerospace Technology Engineering July 2019 ABSTRACT Identifying which systems are more likely to host an imageable planet can play an important role in the construction of an optimized target list for future direct imaging missions, such as the planned technology demonstration for the Wide Field Infrared Survey Telescope (WFIRST). For single-planet systems, the presence of an already detected exoplanet can severely restrict the target's stable region and should therefore be considered when searching for unknown companions. To do so, we first analyze the performance and robustness of several two-planet stability criteria by comparing them with long-term numerical simulations. We then derive the necessary formulation for the computation of (a, R) analytic stability maps, which can be used in conjunction with depth- of-search grids in order to define the stable-imageable region of a system. The dynamically stable completeness (i.e., the expected number of imageable and stable planets) can then be calculated via convolution with the selected occurrence grid, obtaining a metric that can be directly compared for imaging prioritization. Applying this procedure to all the currently known single-planet systems within a distance of 50 pc, we construct a ranked target list based on the WFIRST CGI's predicted performance and SAG13 occurrence rates. Keywords| numerical simulations - analytic stability maps - dynamical evolution and stability - direct imaging - exoplanets 1 CONTENTS 1 Introduction 3 2 Analytic Stability Criteria for Two-Planet Systems 4 2.1 Criteria Based on the Outer Pericenter to Inner Apocenter Ratio . -
Survival of Exomoons Around Exoplanets 2
Survival of exomoons around exoplanets V. Dobos1,2,3, S. Charnoz4,A.Pal´ 2, A. Roque-Bernard4 and Gy. M. Szabo´ 3,5 1 Kapteyn Astronomical Institute, University of Groningen, 9747 AD, Landleven 12, Groningen, The Netherlands 2 Konkoly Thege Mikl´os Astronomical Institute, Research Centre for Astronomy and Earth Sciences, E¨otv¨os Lor´and Research Network (ELKH), 1121, Konkoly Thege Mikl´os ´ut 15-17, Budapest, Hungary 3 MTA-ELTE Exoplanet Research Group, 9700, Szent Imre h. u. 112, Szombathely, Hungary 4 Universit´ede Paris, Institut de Physique du Globe de Paris, CNRS, F-75005 Paris, France 5 ELTE E¨otv¨os Lor´and University, Gothard Astrophysical Observatory, Szombathely, Szent Imre h. u. 112, Hungary E-mail: [email protected] January 2020 Abstract. Despite numerous attempts, no exomoon has firmly been confirmed to date. New missions like CHEOPS aim to characterize previously detected exoplanets, and potentially to discover exomoons. In order to optimize search strategies, we need to determine those planets which are the most likely to host moons. We investigate the tidal evolution of hypothetical moon orbits in systems consisting of a star, one planet and one test moon. We study a few specific cases with ten billion years integration time where the evolution of moon orbits follows one of these three scenarios: (1) “locking”, in which the moon has a stable orbit on a long time scale (& 109 years); (2) “escape scenario” where the moon leaves the planet’s gravitational domain; and (3) “disruption scenario”, in which the moon migrates inwards until it reaches the Roche lobe and becomes disrupted by strong tidal forces. -
The Impact of Stellar Rotation on the Detectability of Habitable Planets Around M Dwarfs
THE IMPACT OF STELLAR ROTATION ON THE DETECTABILITY OF HABITABLE PLANETS AROUND M DWARFS The MIT Faculty has made this article openly available. Please share how this access benefits you. Your story matters. Citation Newton, Elisabeth R. et al. “THE IMPACT OF STELLAR ROTATION ON THE DETECTABILITY OF HABITABLE PLANETS AROUND M DWARFS.” The Astrophysical Journal 821.1 (2016): L19. © 2016 The American Astronomical Society As Published http://dx.doi.org/10.3847/2041-8205/821/1/l19 Publisher IOP Publishing Version Final published version Citable link http://hdl.handle.net/1721.1/108367 Terms of Use Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use. The Astrophysical Journal Letters, 821:L19 (6pp), 2016 April 10 doi:10.3847/2041-8205/821/1/L19 © 2016. The American Astronomical Society. All rights reserved. THE IMPACT OF STELLAR ROTATION ON THE DETECTABILITY OF HABITABLE PLANETS AROUND M DWARFS Elisabeth R. Newton1, Jonathan Irwin1, David Charbonneau1, Zachory K. Berta-Thompson2, and Jason A. Dittmann1 1 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA 2 Kavli Institute for Astrophysics and Space Research and Department of Physics, Massachusetts Institute of Technology, Cambridge, MA 02139, USA Received 2016 February 8; accepted 2016 March 9; published 2016 April 11 ABSTRACT Stellar activity and rotation frustrate the detection of exoplanets through the radial velocity technique. This effect is particularly of concern for M dwarfs, which can remain magnetically active for billions of years. -
Phd Thesis Pinamonti Final.Pdf
ii Riassunto Rivelazione e caratterizzazione dell'architettura orbitale di sistemi planetari intorno a stelle fredde Le nane M si sono dimostrate dei target affascinanti per la ricerca di esopianeti, grazie alla crescente evidenza dalle survey di transiti (ad esempio Kepler) e di velocit`aradiali (ad esempio HARPS ed HARPS-N), anche se diversi ostacoli intralciano la ricerca e l'analisi di sistemi planetari intorno ad esse. Per queste ragioni, `edi fondamentale importanza intensificare gli sforzi rivolti alla rive- lazione e caratterizzazione di pianeti extrasolari intorno a nane M, poich´ele nuove scoperte contribuiranno a portare il supporto statistico necessario allo studio di classi peculiari di pianeti, mentre la precisa caratterizzazione orbitale sia di sistemi noti che appena scoperti aiuter`aa vincolare meglio i processi di for- mazione e migrazione planetaria. Le molte domande aperte sulle nane M ospiti e sui loro sistemi planetari, e lo sviluppi di nuove metodologie per investigarle, sono la base delle motivazioni del mio lavoro di Dottorato. Nella mia tesi, per prima cosa presento la tematica dei sistemi esoplane- tari intorno a nane M, sia dal punto di vista osservativo che statistico. Poi riporto il mio lavoro di analisi delle prestazioni di tre diverse tipi di anal- isi di periodogramma, il \Generalised Lomb-Scargle periodogram" (GLS), la sua versione modificata che sfrutta la statistica bayesiana (BGLS), ed il pe- riodogramma multifrequenza chiamato FREquency DEComposer (FREDEC), motivato dall’ubiquit`adi sistemi multipli di pianeti di piccola massa. I risultati illustrati sostengono la necessit`adi rafforzare e sviluppare ulteriormente le pi`u aggressive ed efficaci strategie per la robusta identificazione di segnali planetari di piccola ampiezza nei dati di velocit`aradiale. -
Annual Report Publications 2011
Publications Publications in refereed journals based on ESO data (2011) The ESO Library maintains the ESO Telescope Bibliography (telbib) and is responsible for providing paper-based statistics. Access to the database for the years 1996 to present as well as information on basic publication statistics are available through the public interface of telbib (http://telbib.eso.org) and from the “Basic ESO Publication Statistics” document (http://www.eso.org/sci/libraries/edocs/ESO/ESOstats.pdf), respectively. In the list below, only those papers are included that are based on data from ESO facilities for which observing time is evaluated by the Observing Programmes Committee (OPC). Publications that use data from non-ESO telescopes or observations obtained during ‘private’ observing time are not listed here. Absil, O., Le Bouquin, J.-B., Berger, J.-P., Lagrange, A.-M., Chauvin, G., Alecian, E., Kochukhov, O., Neiner, C., Wade, G.A., de Batz, B., Lazareff, B., Zins, G., Haguenauer, P., Jocou, L., Kern, P., Millan- Henrichs, H., Grunhut, J.H., Bouret, J.-C., Briquet, M., Gagne, M., Gabet, R., Rochat, S., Traub, W., 2011, Searching for faint Naze, Y., Oksala, M.E., Rivinius, T., Townsend, R.H.D., Walborn, companions with VLTI/PIONIER. I. Method and first results, A&A, N.R., Weiss, W., Mimes Collaboration, M.C., 2011, First HARPSpol 535, 68 discoveries of magnetic fields in massive stars, A&A, 536, L6 Adami, C., Mazure, A., Pierre, M., Sprimont, P.G., Libbrecht, C., Allen, D.M. & Porto de Mello, G.F. 2011, Mn, Cu, and Zn abundances in Pacaud, F., -
Planet and Star Formation (2011)
Planeten- und Sternentstehung/ Planet and Star Formation (2011) Refereed Papers Absil, O., J. B. Le Bouquin, J. P. Berger, A. M. Lagrange, G. Chauvin, B. Lazareff, G. Zins, P. Haguenauer, L. Jocou, P. Kern, R. Millan-Gabet, S. Rochat and W. Traub: Searching for faint companions with VLTI/PIONIER. I. Method and first results. Astronomy and Astrophysics 535, id.A68 (2011) Akimkin, V. V., Y. N. Pavlyuchenkov, A. I. Vasyunin, D. S. Wiebe, M. S. Kirsanova and T. Henning: UV-controlled physical and chemical structure of protoplanetary disks. Astrophysics and Space Science 335, 33, 33-38 (2011) Alibert, Y., C. Mordasini and W. Benz: Extrasolar planet population synthesis. III. Formation of planets around stars of different masses. Astronomy and Astrophysics 526, id.A63, (2011) Andrei, A. H., R. L. Smart, J. L. Penna, V. A. d'Avila, B. Bucciarelli, J. I. B. Camargo, M. T. Crosta, M. Daprà, B. Goldman, H. R. A. Jones, M. G. Lattanzi, L. Nicastro, D. J. Pinfield, D. N. da Silva Neto and R. Teixeira: Parallaxes of Southern Extremely Cool Objects. I. Targets, proper motions, and first results. The Astronomical Journal 141, id. 54, (2011) Archinal, B. A., M. F. A'Hearn, A. Conrad, G. J. Consolmagno, R. Courtin, T. Fukushima, D. Hestroffer, J. L. Hilton, G. A. Krasinsky, G. Neumann, J. Oberst, P. K. Seidelmann, P. Stooke, D. J. Tholen, P. C. Thomas and I. P. Williams: Erratum to: Reports of the IAU Working Group on Cartographic Coordinates and Rotational Elements: 2006 & 2009. Celestial Mechanics and Dynamical Astronomy 110, 401-403 (2011) Assef, R. -