DOCSLIB.ORG

Can We Predict the Composition of an Exoplanet?

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Can We Predict the Composition of an Exoplanet? Can we predict the composition of an exoplanet? A Thesis Presented in Partial Fulfillment of the Requirements for the Degree Master of Science in the Graduate School of The Ohio State University By Joseph Gregory Schulze, B.S. Graduate Program in School of Earth Sciences The Ohio State University 2020 Master's Examination Committee: Dr. Wendy Panero, Advisor Dr. Joachim Moortgat Dr. Ji Wang c Copyright by Joseph Gregory Schulze 2020 Abstract Is the Earth unique in its habitability, or is it just one of many life-hosting planets in the universe? The key to answering this question lies in determining how rocky planets form and evolve, which can be inferred from how similar/dissimilar the com- positions of such planets are to their host stars. For instance, the terrestrial planets formed from a disk made of the same material as the Sun. The compositions of Earth, Venus, and Mars are consistent with the relative amounts of the major rock- building materials (Fe, Mg, Si) found in the Sun. Mercury, however, is much more iron-enriched relative to the Sun. This implies that it underwent a different forma- tion/evolutionary pathway, likely a single or series of catastrophic mantle-stripping collisions during the late stages of its formation. In short, Mercury and Earth have two very different histories, which is realized in how their compositions deviate from the Sun's. Therefore, understanding the relative importance of various formation and evolution processes for rocky exoplanets hinges on first determining how con- sistent the compositions of these planets are with their host stars. In this work, I develop a statistical framework for assessing the degree to which super-Earth's re- flect the refractory compositions of their host stars. I implement this framework on the 8 best-measured super-Earths for which the host star's composition is known and explore the possibility of secondary atmospheres to explain super-Earths with an apparent iron-depletion relative to their host. ii Acknowledgments I first want to thank my advisor, Dr. Wendy Panero. I am exceptionally grateful for the freedom Wendy has given me to explore the topics I find most exciting while also preventing me from going down endless rabbit holes. This thesis would not have been possible without her. I am excited to continue to grow as a scientist under her supervision as a Ph.D. student. I would also like to extend thanks to my committee members, Dr. Ji Wang and Dr. Joachim Moortgat, for their knowledge and insights provided during this research. I would also like to thank the members of the Panero Group and the Planet Group for their interest in my work. Working with these talented scientists has greatly expanded my research and exposed me to new ways of thinking about the same research questions. I wish to thank my parents, Tammy and Bob, and my siblings, Brad, Jen, Gabbert, and Millie for sitting through several practice talks and listening to my many exo- planet rambles. I would like to give a special shout-out to my Dad for first piquing my interest in exoplanets by giving me my first astronomy book, binge-watching and re-watching The Universe with me, and many, many late-night discussions. Thank you, Mr. Dad. Last, I want to thank my fellow SES graduate students for helping me navigate the waters of grad school and for providing a fun social outlet. I would especially like to thank Sam and her four-legged companion (aka The Beast) for their great presentation and writing suggestions, for finishing and restructuring my sentences, and for some much needed comedic relief during confinement. Now back to chorin'. iii Vita June 11, 1994 . Born - Columbus, OH, USA 2017 . B.S. Physics & Astronomy, The Ohio State University 2018-2019 . .University Fellow 2019-2020 . .Graduate Teaching Associate, The Ohio State University. Publications Research Publications Page, M. R., McCullian, B. A., Purser, C. M., Schulze, J. G., Nakatani, T. M., Wolfe, C. S., Childress, J. R., McConney, M. E., Howe, B. M., Hammel, P. C. and Bhallamudi,V. P., Optically detected ferromagnetic resonance in diverse ferromag- nets via nitrogen vacancy centers in diamond. Journal of Applied Physics, 126, 12. Fields of Study Major Field: Earth Sciences iv Table of Contents Page Abstract . ii Acknowledgments . iii Vita......................................... iv List of Tables . vii List of Figures . viii 1. Introduction . .1 2. Do the compositions of rocky exoplanets reflect their star's refractory abundances? . .9 2.1 Introduction . 10 2.2 Sample Selection . 11 2.3 Planetary Structure Calculations . 14 2.4 Hypothesis testing . 16 2.5 Results . 19 2.6 Discussion and Conclusions . 25 3. ExoLens { A Compositional Calculator for Rocky Worlds . 28 3.1 Introduction . 28 v 3.2 Analytical Expression for Core Mass Fraction as a Function of Plan- etary Observables, Mass and Radius . 29 3.3 Parameter Fitting . 31 3.4 Inputs and Outputs . 33 3.5 Comparison with Zeng et al. (2016a) . 37 4. A Simple Adiabatic Model for Secondary Atmospheres . 41 4.1 Introduction . 41 4.2 The physics of atmospheric escape . 42 4.3 Atmospheric Modeling . 45 4.4 Reproducing Earth and Venus' Atmospheres . 47 4.5 Discussion . 48 Appendices 53 A. Calculation of CMF and σCMF . 53 vi List of Tables Table Page 2.1 Selected sample of well-characterized exoplanets. M-R sources: (1) Dai et al. (2019), (2) Ligi et al. (2019), (3) Espinoza et al. (2019), (4) Bonomo et al. (2019). Spectroscopy sources: (1) Santerne et al. (2018). (2) Santos et al. (2015). (3) Hypatia Catalogue (median values) (Hinkel et al., 2014). (4) Hellier et al. (2012). (5) Espinoza et al. (2019). (6) Bonomo et al. (2019). 13 2.2 Inferred properties of the selected small, well-characterized exoplanets, classified as S.E., super-Earth, S.M. super-Mercury, or S.F. super- Fluff. P.R.C. = Previously Reported Class. Sources: (1) Santerne et al. (2018), (2) Brugger et al. (2017), (3) Dorn et al. (2019), (4) Espinoza et al. (2019). (5) Bonomo et al. (2019). 21 4.1 Initial Parameters for Earth and Venus from Earth Fact Sheet and Venus Fact Sheet, respectively. 52 4.2 Summary of Results. 52 A.1 The effects of Mp, Rp, σRp and σMp on CMFρ and σCMFρ ....... 54 A.2 The effects of Fe/Mg, Si/Mg, σFe/Mg and σSi/Mg on CMF? and σCMF? . 55 vii List of Figures Figure Page 2.1 Ternary diagrams of the CMF-MMF-WMF solution space for all plan- ets in our sample with known stellar Fe/Mg and Si/Mg ratios. All so- lutions are subject to the constraint that CMF+MMF+WMF = 100% 20 2.2 CMFρ and CMF? uncertainty maps as a function of observational uncertainties. (a) Uncertainty in CMFρ as a function of mass and radius uncertainties. We plot the values for Mp = 5:0M⊕ and Rp = 1:545R⊕, whereas values in Table 2.2 are exact. (b) Uncertainty in CMF? as a function of Fe/Mg and Si/Mg uncertainties. We use Fe/Mg = 0.98 and Si/Mg = 1.0. These choices give a central value of 0.35 for both CMFρ and CMF?. Uncertainties for additional planets with measured masses and radii without stellar Fe/Mg and Si/Mg are also included. Color labels are for clarity. 24 3.1 CMFρ vs. Rp curves for Mp = 0:01 (cyan) to 11M⊕ (magenta). Exo- Plex data points are denoted by squares. Fits to Equ. 3.9 are shown as solid lines. Fit residuals are shown in the top panel. While there is a clear systematic trend in the residuals, the amplitude of this trend is, at most, 0.02% which is 3 orders of magnitude smaller than the current uncertainties in CMFρ due to observational uncertainties in planetary mass and radius. 32 3.2 Fit to mean core density as a function of planetary mass. 34 3.3 Fit to mean mantle density as a function of planetary mass. 35 viii 3.4 Difference between CMFρ calculated from ExoPlex and ExoLens for 13 likely rocky exoplanets (Rp < 1:9R⊕) with σM < 20% and σR < 10%. R.M.S. = 1.4%. 36 3.5 Schematic overview of ExoLens. 38 3.6 Sample ExoLens output for K2-229b. Black solid lines correspond to nine equally-spaced confidence intervals between 10 and 90%. The dashed cyan lines are the 68% and 95% confidence intervals. (Bot- tom left) Contour lines (white) correspond to lines of constant CMFρ values. Negative values indicate M-R combinations that cannot be ex- plained by a purely MgSiO3 composition and require either an outer volatile layer or enrichment in ultra-refractory materials. (Bottom right) likelihood functions for CMFρ and CMF?............. 39 3.7 Comparison plot between Z16 and ExoLens. (Left) Z16 (dashed) and ExoLens (solid) M-R curves for varying core mass fractions. (Right) Difference in CMFρ between Z16 and ExoLens for Mp = 1:0 and 10:0M⊕. 40 4.1 Atmospheric particle mass where vthermal = vescape as a function of planet mass for 300, 1000, and 2000 K. Solid symbols for Earth, Venus, and 55 Cnc e are plotted according to their equilibrium temperature according to their orbital distance (no greenhouse). The open symbol for Venus reflects its present surface temperature. 46 4.2 My model of Earth's atmosphere (solid) compared with the 1976 U.S. standard atmosphere model (dashed). 49 4.3 My model of the Venetian atmosphere compared with Justus & Braun (2007) . 50 ix Chapter 1: Introduction The solar system contains 8 planets which can be broadly divided into two com- positional categories: the rock-dominated terrestrial planets and the light-element dominated gas/ice giants.
Load more

Recommended publications
  • Greenhouse Gases
    ClimateClimate onon terrestrialterrestrial planetsplanets H. Rauer Zentrum für Astronomie und Astrophysik, TU Berlin und Institut für Planetenforschung, DLR, Berlin-Adlershof Terrestrial Planets with Atmospheres in our Solar System Venus Earth Mars T = 735 K T = 288 K T = 216 K p = 90 bar p = 1 bar p = 0.007 bar Atmosphere: Atmosphere: Atmosphere: 96% CO2 77% N2 95% CO2 3,5 % N2 21 % O2 2,7 % N2 1 % H2O WhatWhatare aret thehe relevant relevant processesprocesses forfora a stablestablec climate?limate? AA stablestable climate climate needsneeds a a stablestable atmosphere!atmosphere! Three ways to gain a (secondary) atmosphere Ways to loose an atmosphere Could also be a gain Die Fluchtgeschwindigkeit Ep = -GmM/R 2 Ekl= 1/2mv Für Ek<Ep wird das Molekül zurückkehren Für Ek≥Ep wird das Molekül die Atmosphäre verlassen Die kleinst möglichste Geschwindigkeit, die für das Verlassen notwendig ist hat das Molekül für den Fall: Ek+Ep=0 2 1/2mve -GMm/R=0 ve=√(2GM/R) Thermischer Verlust (Jeans Escape) Einzelne Moleküle können von der obersten Schicht der Atmosphäre entweichen, wenn sie genügend Energie besitzen Die Moleküle folgen einer Maxwell-Boltzmann Verteilung: Mittlere quadratische Geschwindigkeit: v=√(2kT/m) Large escape velocities for the giants and ice planets Mars escape velocity is ~½ ve(Earth) - gas giants are massive enough to keep H-He-atmospheres - terrestrial planets atmospheres can have CO2, N2, O2, CH4, H2O, …, but little H and He Additional loss processes are important: Planets with magnetosphere are generally better protected from
    [Show full text]
  • Temperate Earth-Sized Planets Transiting a Nearby Ultracool Dwarf Star
    1 Temperate Earth-sized planets transiting a nearby ultracool dwarf star Michaël Gillon1, Emmanuël Jehin1, Susan M. Lederer2, Laetitia Delrez1, Julien de Wit3, Artem Burdanov1, Valérie Van Grootel1, Adam J. Burgasser4, Amaury H. M. J. Triaud5, Cyrielle Opitom1, Brice-Olivier Demory6, Devendra K. Sahu7, Daniella Bardalez Gagliuffi4, Pierre Magain1 & Didier Queloz6 1Institut d’Astrophysique et de Géophysique, Université de Liège, Allée du 6 Août 19C, 4000 Liège, Belgium. 2NASA Johnson Space Center, 2101 NASA Parkway, Houston, Texas, 77058, USA. 3Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, Massachusetts 02139, USA. 4Center for Astrophysics and Space Science, University of California San Diego, La Jolla, California 92093, USA. 5Institute of Astronomy, Madingley Road, Cambridge CB3 0HA, UK. 6Astrophysics Group, Cavendish Laboratory, 19 J J Thomson Avenue, Cambridge, CB3 0HE, UK. 7Indian Institute of Astrophysics, Koramangala, Bangalore 560 034, India. Star-like objects with effective temperatures of less than 2,700 kelvin are referred to as ‘ultracool dwarfs'1. This heterogeneous group includes stars of extremely low mass as well as brown dwarfs (substellar objects not massive enough to sustain hydrogen fusion), and represents about 15 per cent of the population of astronomical objects near the Sun2. Core-accretion theory predicts that, given the small masses of these ultracool dwarfs, and the small sizes of their protoplanetary disk3,4, there should be a large but hitherto undetected population of terrestrial planets orbiting them5—ranging from metal-rich Mercury-sized planets6 to more hospitable volatile-rich Earth-sized planets7. Here we report observations of three short-period Earth-sized planets transiting an 2 ultracool dwarf star only 12 parsecs away.
    [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]
  • The Earth and Its Atmosphere (Introduction) What, Why, and How???
    The Earth and Its Atmosphere (Introduction) What, Why, and How??? What is an Why do planets atmosphere? have atmospheres? What determines the yearly weather cycle? Why is the weather What is the different every year? structure of the Earth’s atmosphere? How was the Earth’s What is the atmosphere formed? Why do we study composition the atmosphere? of the Earth’s atmosphere? What processes determine How different are the daily variations in the the atmospheres of atmosphere? Are they other planets? predictable? What is an atmosphere? • A gaseous envelope surrounding a planet (satellite, comet…). • It is very, very thin compared to the size of the planet Why do planets have atmospheres? Gravity !!! PressurePressure !!!!!! Origin of the Atmosphere (How is an atmosphere formed?) • The early atmosphere of the Earth was very different from the atmosphere today! • Stage I (Primordial Atmosphere): ♦ Acquired by gravitational attraction of volatile gases from the proto planetary nebula of the Sun ♦ Consisted mostly of H2 and He ♦ Small and warm planets (Earth, Mars, Venus, Mercury) lost this atmosphere because the gravity is not strong enough to keep the light hot gases from escaping the planet. ♦ The composition of the atmosphere of the giant planets (Jupiter, Saturn, Uranus and Neptune) today is very close to their primordial atmosphere (why?). The Secondary Atmosphere • Stage II ♦ Outgassing of the terrestrial type planets during the early stages of their geological history. Volcanoes, geysers, cracks, … ♦ Most abundant gasses: H2O, CO2, SO2, H2S, CO ♦ Recall: radon mitigation ♦ On the Earth H2O condensed, formed clouds and rained out to form oceans. ♦ On the Earth most of the abundant gasses then dissolved in the ocean, leaving N2 as the dominant gas.
    [Show full text]
  • A First Reconnaissance of the Atmospheres of Terrestrial Exoplanets Using Ground-Based Optical Transits and Space-Based UV Spectra
    A First Reconnaissance of the Atmospheres of Terrestrial Exoplanets Using Ground-Based Optical Transits and Space-Based UV Spectra The Harvard community has made this article openly available. Please share how this access benefits you. Your story matters Citation Diamond-Lowe, Hannah Zoe. 2020. A First Reconnaissance of the Atmospheres of Terrestrial Exoplanets Using Ground-Based Optical Transits and Space-Based UV Spectra. Doctoral dissertation, Harvard University, Graduate School of Arts & Sciences. Citable link https://nrs.harvard.edu/URN-3:HUL.INSTREPOS:37365825 Terms of Use This article was downloaded from Harvard University’s DASH repository, and is made available under the terms and conditions applicable to Other Posted Material, as set forth at http:// nrs.harvard.edu/urn-3:HUL.InstRepos:dash.current.terms-of- use#LAA A first reconnaissance of the atmospheres of terrestrial exoplanets using ground-based optical transits and space-based UV spectra A DISSERTATION PRESENTED BY HANNAH ZOE DIAMOND-LOWE TO THE DEPARTMENT OF ASTRONOMY IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF DOCTOR OF PHILOSOPHY IN THE SUBJECT OF ASTRONOMY HARVARD UNIVERSITY CAMBRIDGE,MASSACHUSETTS MAY 2020 c 2020 HANNAH ZOE DIAMOND-LOWE.ALL RIGHTS RESERVED. ii Dissertation Advisor: David Charbonneau Hannah Zoe Diamond-Lowe A first reconnaissance of the atmospheres of terrestrial exoplanets using ground-based optical transits and space-based UV spectra ABSTRACT Decades of ground-based, space-based, and in some cases in situ measurements of the Solar System terrestrial planets Mercury, Venus, Earth, and Mars have provided in- depth insight into their atmospheres, yet we know almost nothing about the atmospheres of terrestrial planets orbiting other stars.
    [Show full text]
  • The HARPS-N Rocky Planet Search. I. HD 219134 B: a Transiting Rocky Planet in a Multi-Planet System at 6.5 Pc from the Sun
    The HARPS-N Rocky Planet Search. I. HD 219134 b: A transiting rocky planet in a multi-planet system at 6.5 pc from the Sun Motalebi, F., Udry, S., Gillon, M., Lovis, C., Ségransan, D., Buchhave, L. A., Demory, B. O., Malavolta, L., Dressing, C. D., Sasselov, D., Rice, K., Charbonneau, D., Cameron, A. C., Latham, D., Molinari, E., Pepe, F., Affer, L., Bonomo, A. S., Cosentino, R., ... Watson, C. A. (2015). The HARPS-N Rocky Planet Search. I. HD 219134 b: A transiting rocky planet in a multi-planet system at 6.5 pc from the Sun. Astronomy and Astrophysics, 584, [A72]. https://doi.org/10.1051/0004-6361/201526822 Published in: Astronomy and Astrophysics Document Version: Publisher's PDF, also known as Version of record Queen's University Belfast - Research Portal: Link to publication record in Queen's University Belfast Research Portal Publisher rights © 2015, ESO Reproduced with permission from Astronomy & Astrophysics General rights Copyright for the publications made accessible via the Queen's University Belfast Research Portal is retained by the author(s) and / or other copyright owners and it is a condition of accessing these publications that users recognise and abide by the legal requirements associated with these rights. Take down policy The Research Portal is Queen's institutional repository that provides access to Queen's research output. Every effort has been made to ensure that content in the Research Portal does not infringe any person's rights, or applicable UK laws. If you discover content in the Research Portal that you believe breaches copyright or violates any law, please contact [email protected].
    [Show full text]
  • Institut Für Weltraumforschung (IWF) Österreichische Akademie Der Wissenschaften (ÖAW) Schmiedlstraße 6, 8042 Graz, Austria
    WWW.OEAW.AC.AT ANNUAL REPORT 2018 IWF INSTITUT FÜR WELTRAUMFORSCHUNG WWW.IWF.OEAW.AC.AT ANNUAL REPORT 2018 COVER IMAGE Artist's impression of the BepiColombo spacecraft in cruise configuration, with Mercury in the background (© spacecraft: ESA/ATG medialab; Mercury: NASA/JPL). TABLE OF CONTENTS INTRODUCTION 5 NEAR-EARTH SPACE 7 SOLAR SYSTEM 13 SUN & SOLAR WIND 13 MERCURY 15 VENUS 16 MARS 17 JUPITER 18 COMETS & DUST 20 EXOPLANETARY SYSTEMS 21 SATELLITE LASER RANGING 27 INFRASTRUCTURE 29 OUTREACH 31 PUBLICATIONS 35 PERSONNEL 45 IMPRESSUM INTRODUCTION INTRODUCTION The Space Research Institute (Institut für Weltraum- ESA's Cluster mission, launched in 2000, still provides forschung, IWF) in Graz focuses on the physics of space unique data to better understand space plasmas. plasmas and (exo-)planets. With about 100 staff members MMS, launched in 2015, uses four identically equipped from 20 nations it is one of the largest institutes of the spacecraft to explore the acceleration processes that Austrian Academy of Sciences (Österreichische Akademie govern the dynamics of the Earth's magnetosphere. der Wissenschaften, ÖAW, Fig. 1). The China Seismo-Electromagnetic Satellite (CSES) was IWF develops and builds space-qualified instruments and launched in February to study the Earth's ionosphere. analyzes and interprets the data returned by them. Its core engineering expertise is in building magnetometers and NASA's InSight (INterior exploration using Seismic on-board computers, as well as in satellite laser ranging, Investigations, Geodesy and Heat Transport) mission was which is performed at a station operated by IWF at the launched in May to place a geophysical lander on Mars Lustbühel Observatory.
    [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]
  • A Naprendszer-Hasonlósági Index
    Szegedi Tudományegyetem Természettudományi és Informatikai Kar Kísérleti Fizikai Tanszék Szakdolgozat A Naprendszer-hasonlósági index Készítette: Mészáros Richárd Fizika BSc szakos hallgató Témavezető: Dr. Szatmáry Károly egyetemi tanár Szeged 2020 Tartalomjegyzék 1. Bevezetés……………………………………………………………………..2 2. Az exobolygók felfedezési módszerei………………………………………..2 2.1. Közvetlen módszerek………………………………………………..2 2.2. Közvetett módszerek………………………………………..……….3 3. Az exobolygók osztályozása………………………………………...……….6 4. A Föld-hasonlósági index…………………………………………………….7 5. A Naprendszer-hasonlósági index……………………………………………8 5.1. Első verzió……………………………………………….…………..8 5.2. Második verzió……………………………………………………..11 5.3. Eredmények……………………………………………………...…13 6. Összefoglalás………………………………………………………………..24 Köszönetnyilvánítás……………………………………………………………24 Irodalomjegyzék………………………………………………………………..25 1 1. Bevezetés A felfedezett exobolygók asztrobiológiai potenciáljának vizsgálatára 2011-ben bevezetésre került a Föld-hasonlósági index (ESI, Schulze-Makuch et al. 2011,[2]). Dolgozatom témájául a felfedezett exobolygó rendszerek hasonló módon való vizsgálatát választottam. A második és harmadik fejezetben összefoglalom az exobolygók keresési módszereit és ezen bolygók típusait. A negyedik fejezetben röviden bemutatom a Föld-hasonlósági indexet. Az ötödik fejezetben a Föld-hasonlósági index mintájára bevezetem a Naprendszer-hasonlósági index fogalmát. Ismertetem kiszámításának módját, és alkalmazom a legalább 4 bolygót tartalmazó exobolygó rendszerekre. A kapott eredményekből
    [Show full text]
  • What Makes a Planet Habitable? 91
    DOSSIER: What Makes a Planet Habitable? 91 View metadata, citationWhat and similar papers Makes at core.ac.uk a Planet Habitable?brought to you by CORE provided by Repositori d'Objectes Digitals per a l'Ensenyament la Recerca i la Cultura Manuel Güdel Received 03.07.2014 - Approved 05.09.2014 Abstract / Resumen / Résumé among the countless exoplanets, which ones may be con- ducive to life, and what signs should we look for in our Before life can form and develop on a planetary surface, many condi- search for life in the universe? tions must be met that are of astrophysical nature. Radiation and par- ticles from the central star, the planetary magnetic field, the accreted or outgassed atmosphere of a young planet and several further factors These questions relate to at least two major challenges. must act together in a balanced way before life has a chance to thrive. We need to understand our biochemical origins in the dis- We will describe these crucial preconditions for habitability and discuss tant past of the Earth, and in a larger context, we need the latest state of knowledge. to identify the main conditions required to form life on a planet in the first place. While there is hope to eventually Antes de que la vida pueda surgir+ y desarrollarse en una superficie pla- netaria, son necesarias muchas condiciones de naturaleza astrofísica. answer the first question by a deeper understanding of the La radiación y las partículas provenientes de la estrella central, el cam- specific form of life here on Earth, the second challenge is po magnético del planeta, la acumulación o disipación de la atmósfera much harder to address as it boils down to defining what en un planeta joven, y varios otros factores deben actuar conjuntamente life in general is.
    [Show full text]
  • What Is CHEOPS?
    Swiss and ESA satellite CHEOPS launching soon! CHEOPS will be launching into space on the 17th of December! You may be wondering: what is CHEOPS? CHEOPS stands for CHaracterising ExOPlanet Satellite. Its goal is to study ​ ​ transits of already-known exoplanets to gain more knowledge about them. What type of information are we looking for? Scientists want to know detailed information about planets outside our Solar System, such as the mass, planet size, and density, which will in turn help to figure out the composition of these exoplanets. Studying exoplanet composition and their atmospheres is important especially for astrobiology. A planet’s chemical composition can affect its habitability for life as we know it. Scientists usually look for biosignatures such as the presence of methane or oxygen in the planet’s atmosphere, which could indicate presence of past or present life. Artist’s impression of CHEOPS. Credits: ESA / ATG medialab. The major contributors CHEOPS is a collaboration between ESA and the Swiss Space Office. The mission was proposed and is now headed by Prof. Willy Benz, from the University of Bern, which houses the mission’s consortium. The science operations consortium is at the University of Geneva, where they have many collaborators, such as the Swiss Space Center at EPFL. As it is an ESA endeavour, many other European institutions are also contributing to the mission. For example, the mission operations consortium is located in Torrejón de Ardoz, Spain. The launch The satellite has already been shipped to Kourou, French Guiana, where it will be launched by the ESA spaceport.
    [Show full text]
  • Exoplanet Tool Kit
    Exoplanet Tool Kit New Mexico Super Computing Challenge Final Report April 5, 2011 Team 35 Desert Academy Team Members Chris Brown Isaac Fischer Teacher Jocelyn Comstock Mentors Henry Brown Prakash Bhakta Table of Contents Executive Summary ................................................................................................ 2 Background ............................................................................................................ 3 Astrophysics .............................................................................................. 3 Definition and Origin of Extroplanets ....................................................... 4 Methods of Detection ............................................................................... 4 Project .................................................................................................................. 6 Methodology............................................................................................. 6 Data Results .............................................................................................. 7 Conclusion ............................................................................................................ 10 Future Study ......................................................................................................... 11 Acknowledgements.............................................................................................. 12 References ..........................................................................................................
    [Show full text]