DOCSLIB.ORG

Open Engagment Group A

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Open Engagment Group A Habitable Worlds 2021 Workshop Open Engagement – Group A Abstract # Title 1st Author 8 Rocky Worlds and their Siblings Lauren Weiss Exploring Biogenic Dispersion Inside Star Clusters with Javier Darío 10 System Dynamic Modeling Salcedo Dynamical and Biological Panspermia Constraints Within 11 Dimitri Veras Multiplanet Exosystems 13 Origins of Kepler-1656b's Extreme Eccentricity Isabel Angelo EUV Spectroscopy with the ESCAPE Mission: Exploring the 14 Kevin France Stellar Drivers of Exoplanet Habitability Planetary Magnetic Fields, Planetary Interiors, and 18 T. Joseph LaZio Habitability Impact of Photochemistry in Terrestrial P type Circumbinary 22 Michaela Leung Exoplanetary Atmospheres Statistical Assessment of Thermochemical Disequilibria in 23 Theresa Fisher Exoplanets: Implications for Biosignature Detection Testing key concepts of planetary habitability using 24 Martin Turbet observations of nearby rocky exoplanets New Near-UV H2O Cross-Sections & Photochemistry of Early 25 Sukrit Ranjan Earth-like Atmospheres Magnetospheres of Terrestrial Exoplanets and Exomoons - 26 James Green Implications for Habitability and Detection Modeling Flood Basalt Volcanic Climate Disruptions: 27 Scott Guzewich Implications for Terrestrial Planet Habitability MHD Effects of the Stellar Wind on Observations of Escaping 28 Laura Harbach Exoplanet Atmospheres A Framework for Relative Biosignature Yields from Future 30 Noah Tuchow Direct Imaging Missions On the prospect of detecting habitable trojan planets in the 31 Jeffrey Sudol Kepler circumbinary planetary systems 32 Inter-model Comparisons for Exoplanets Thomas FaucheZ Imaging Small Planets Around the Very Nearest Stars with 37 Rory Bowens METIS on ELT 39 The Role of Orbital Dynamics In Planetary Habitability Stephen Kane 41 On the oligarchic growth in a fully interacting system Zoltan Dencs 42 Methane: the Ideal Biosignature for the JWST Era? Maggie Thompson Using the Sun-Earth Interaction to Explore Exoplanetary 43 David Alexander Systems High pCO2 reduces sensitivity to CO2 perturbations on 44 temperate, Earth-like planets throughout most of habitable Robert Graham Zone Taking the photometric pulse of Venus, our nearest terrestrial 45 planet: Probing atmospheric super-rotation rather than surface Yeon Joo Lee features 48 Phosphine and the importance of unusual biosignatures Clara Sousa-Silva 50 Hiding Planets Near and Far Thea Faridani 51 Entering the Habitable Zone: An Earth-like Perspective Johnny Seales The Effect of Cryoconite on the Deglaciation Thresholds of 53 Nicholas Duong Snowball Planets Transmission Spectroscopy of Exo-Solar Systems in the TESS 54 Colby Ostberg Era Madeline 57 New Estimates of Nitrogen Oxide and Hydrogen Cyanide Christensen 58 Habitability Models for Exoplanet Sciences Abel MendeZ Mars ~3 Ga had river-forming climates at low average pCO2, 59 raising the likelihood of false negatives in the search for Edwin Kite habitable exoplanets Water on hot rocky exoplanets and the sub-Neptune-to-super- 60 Edwin Kite Earth transition The Large Interferometer for Exoplanets (LIFE) mission: Daniel 61 characteriZing habitable planets in the mid-infrared Angerhausen Hubble WFC3 Transmission Spectroscopy of the Habitable 62 Billy Edwards Zone Super-Earth LHS 1140 b 63 Interiors of water-rich planets: what do we know about them? Allona VaZan 64 Habitability at the End of the Universe Ray Pierrehumbert Transport of surface oxidants into internal oceans by brine 65 Marc Hesse migration through ice shells 67 Climate on High Obliquity Planet Wanying Kang 68 The Sun's Magnetic Activity is Normal for its Age Jason Curtis On the Lithology and Mineralogy of Polluted White Dwarf 69 Keith Putirka Materials Photochemistry of planetary atmospheres with 3D Global 70 Yassin JaZiri Climate Model A Snowball in Hell: The Potential Steam Atmosphere of TOI- 71 Sonny Harman 1266c Planetary Archaeology: Exploring Planets Transiting Red 74 Samuel Grunblatt Giant Stars Potential storage of molecular hydrogen in CaTiO3 perovskite 76 Suyu Fu in the deep interiors of rocky planets 81 A Bolt from the Blue - Lightning on Terrestrial Exoplanets Laura Lewis Stellar flares and planetary habitability: atmospheric escape, 82 Dimitra Atri chemistry and radiation dose enhancement Early (In)Habitability Among Exoplanets: A 1D ParameteriZed 85 Matthew Weller Approach Linking the Mantle-Tectonics-Atmospherics System Magnetic Fields, Atmospheres, and the Connection to 86 David Brain Habitability (MACH) The Effect of Radiative Time Step on the Climate of a L1 Robert Washington Habitable Planet Detecting Biosignatures of Nearby Rocky Exoplanets: L2 Simulations of High Spectral Resolution Observations with the Sophia Vaughn ELTs .
Load more

Recommended publications
  • The Planetary Systems Imager for TMT Astro2020 APC White Paper Optical and Infrared Observations from the Ground Corresponding Author: Michael P
    The Planetary Systems Imager for TMT Astro2020 APC White Paper Optical and Infrared Observations from the Ground Corresponding Author: Michael P. Fitzgerald (University of California, Los Angeles; mpfi[email protected]) Co-authors: Diego) Vanessa Bailey (Jet Propulsion Laboratory) Takayuki Kotani (Astrobiology Center/NAOJ) Christoph Baranec (University of Hawaii) David Lafreniere` (Universite´ de Montreal)´ Natasha Batalha (University of California Santa Michael Liu (University of Hawaii) Cruz) Julien Lozi (Subaru) Bjorn¨ Benneke (Universite´ de Montreal)´ Jessica R. Lu (University of California, Berkeley) Charles Beichman (California Institute of Jared Males (University of Arizona) Technology) Mark Marley (NASA Ames Research Center) Timothy Brandt (University of California, Santa Christian Marois (NRC Canada) Barbara) Dimitri Mawet (California Institute of Jeffrey Chilcote (Notre Dame) Technology/JPL) Mark Chun (University of Hawaii) Benjamin Mazin (University of California Santa Ian Crossfield (MIT) Barbara) Thayne Currie (NASA Ames Research Center) Maxwell Millar-Blanchaer (Jet Propulsion Kristina Davis (University of California Santa Laboratory) Barbara) Soumen Mondal (SN Bose National Centre for Richard Dekany (California Institute of Technology) Basic Sciences) Jacques-Robert Delorme (California Institute of Naoshi Murakami (Hokkaido University) Technology) Ruth Murray-Clay (University of California, Santa Ruobing Dong (University of Victoria) Cruz) Rene Doyon (Universite´ de Montreal)´ Norio Narita (Astrobiology Center) Courtney Dressing
    [Show full text]
  • 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.
    [Show full text]
  • Water, Habitability, and Detectability Steve Desch
    Water, Habitability, and Detectability Steve Desch PI, “Exoplanetary Ecosystems” NExSS team School of Earth and Space Exploration, Arizona State University with Ariel Anbar, Tessa Fisher, Steven Glaser, Hilairy Hartnett, Stephen Kane, Susanne Neuer, Cayman Unterborn, Sara Walker, Misha Zolotov Astrobiology Science Strategy NAS Committee, Beckmann Center, Irvine, CA (remotely), January 17, 2018 How to look for life on (Earth-like) exoplanets: find oxygen in their atmospheres How Earth-like must an exoplanet be for this to work? Seager et al. (2013) How to look for life on (Earth-like) exoplanets: find oxygen in their atmospheres Oxygen on Earth overwhelmingly produced by photosynthesizing life, which taps Sun’s energy and yields large disequilibrium signature. Caveats: Earth had life for billions of years without O2 in its atmosphere. First photosynthesis to evolve on Earth was anoxygenic. Many ‘false positives’ recognized because O2 has abiotic sources, esp. photolysis (Luger & Barnes 2014; Harman et al. 2015; Meadows 2017). These caveats seem like exceptions to the ‘rule’ that ‘oxygen = life’. How non-Earth-like can an exoplanet be (especially with respect to water content) before oxygen is no longer a biosignature? Part 1: How much water can terrestrial planets form with? Part 2: Are Aqua Planets or Water Worlds habitable? Can we detect life on them? Part 3: How should we look for life on exoplanets? Part 1: How much water can terrestrial planets form with? Theory says: up to hundreds of oceans’ worth of water Trappist-1 system suggests hundreds of oceans, especially around M stars Many (most?) planets may be Aqua Planets or Water Worlds How much water can terrestrial planets form with? Earth- “snow line” Standard Sun distance models of distance accretion suggest abundant water.
    [Show full text]
  • Biosignatures Search in Habitable Planets
    galaxies Review Biosignatures Search in Habitable Planets Riccardo Claudi 1,* and Eleonora Alei 1,2 1 INAF-Astronomical Observatory of Padova, Vicolo Osservatorio, 5, 35122 Padova, Italy 2 Physics and Astronomy Department, Padova University, 35131 Padova, Italy * Correspondence: [email protected] Received: 2 August 2019; Accepted: 25 September 2019; Published: 29 September 2019 Abstract: The search for life has had a new enthusiastic restart in the last two decades thanks to the large number of new worlds discovered. The about 4100 exoplanets found so far, show a large diversity of planets, from hot giants to rocky planets orbiting small and cold stars. Most of them are very different from those of the Solar System and one of the striking case is that of the super-Earths, rocky planets with masses ranging between 1 and 10 M⊕ with dimensions up to twice those of Earth. In the right environment, these planets could be the cradle of alien life that could modify the chemical composition of their atmospheres. So, the search for life signatures requires as the first step the knowledge of planet atmospheres, the main objective of future exoplanetary space explorations. Indeed, the quest for the determination of the chemical composition of those planetary atmospheres rises also more general interest than that given by the mere directory of the atmospheric compounds. It opens out to the more general speculation on what such detection might tell us about the presence of life on those planets. As, for now, we have only one example of life in the universe, we are bound to study terrestrial organisms to assess possibilities of life on other planets and guide our search for possible extinct or extant life on other planetary bodies.
    [Show full text]
  • Monday, November 13, 2017 WHAT DOES IT MEAN to BE HABITABLE? 8:15 A.M. MHRGC Salons ABCD 8:15 A.M. Jang-Condell H. * Welcome C
    Monday, November 13, 2017 WHAT DOES IT MEAN TO BE HABITABLE? 8:15 a.m. MHRGC Salons ABCD 8:15 a.m. Jang-Condell H. * Welcome Chair: Stephen Kane 8:30 a.m. Forget F. * Turbet M. Selsis F. Leconte J. Definition and Characterization of the Habitable Zone [#4057] We review the concept of habitable zone (HZ), why it is useful, and how to characterize it. The HZ could be nicknamed the “Hunting Zone” because its primary objective is now to help astronomers plan observations. This has interesting consequences. 9:00 a.m. Rushby A. J. Johnson M. Mills B. J. W. Watson A. J. Claire M. W. Long Term Planetary Habitability and the Carbonate-Silicate Cycle [#4026] We develop a coupled carbonate-silicate and stellar evolution model to investigate the effect of planet size on the operation of the long-term carbon cycle, and determine that larger planets are generally warmer for a given incident flux. 9:20 a.m. Dong C. F. * Huang Z. G. Jin M. Lingam M. Ma Y. J. Toth G. van der Holst B. Airapetian V. Cohen O. Gombosi T. Are “Habitable” Exoplanets Really Habitable? A Perspective from Atmospheric Loss [#4021] We will discuss the impact of exoplanetary space weather on the climate and habitability, which offers fresh insights concerning the habitability of exoplanets, especially those orbiting M-dwarfs, such as Proxima b and the TRAPPIST-1 system. 9:40 a.m. Fisher T. M. * Walker S. I. Desch S. J. Hartnett H. E. Glaser S. Limitations of Primary Productivity on “Aqua Planets:” Implications for Detectability [#4109] While ocean-covered planets have been considered a strong candidate for the search for life, the lack of surface weathering may lead to phosphorus scarcity and low primary productivity, making aqua planet biospheres difficult to detect.
    [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]
  • 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]
  • IS HABITABILITY CONSTRAINED by PHYSICS OR BIOLOGY? the CASE for a GAIAN BOTTLENECK. Charles. H. Lineweaver1 and Aditya Chopra1
    Astrobiology Science Conference 2015 (2015) 7276.pdf IS HABITABILITY CONSTRAINED BY PHYSICS OR BIOLOGY? THE CASE FOR A GAIAN BOTTLENECK. Charles. H. Lineweaver1 and Aditya Chopra1, 1Planetary Science Institute, Research School of Astronomy and Astrophysics and Research School of Earth Sciences, Australian National University, Australia, [email protected], [email protected] The prerequisites and ingredients for life seem to Earth. We are proposing a sequence of events that can be abundantly available in the universe. However, the be summarized as: (1) uninhabitably hot, high universe does not seem to be teeming with life. The bombardment rate during planetary accretion (2) most common explanation for this is a low probability cooler, reduced bombardment (3) emergence of life in for the emergence of life (an emergence bottleneck), planetary environments that tend to evolve away from notionally due to the intricacies of the molecular habitability, continuous volatile loss. Then either (4a) recipe. Here we present an alternative explanation: a the inability of life to control atmospheric volatiles and Gaian bottleneck [1]. If life emerges on a planet, it maintain habitabililty, thus leading to extinction (left only rarely evolves quickly enough to regulate panel in figure) or (4b) the rapid evolution of Gaian temperature through albedo and atmospheric volatiles regulation and the maintenance of habitability (right and maintain habitability. Such a Gaian bottleneck panel in figure) suggests that (i) extinction is the cosmic default for most life that has ever emerged on the surface of wet Gaian Regulation rocky planets in the universe and (ii) rocky planets +2 Gyr +2 Gyr need to be inhabited, to remain habitable.
    [Show full text]
  • Open Batalha-Dissertation.Pdf
    The Pennsylvania State University The Graduate School Eberly College of Science A SYNERGISTIC APPROACH TO INTERPRETING PLANETARY ATMOSPHERES A Dissertation in Astronomy and Astrophysics by Natasha E. Batalha © 2017 Natasha E. Batalha Submitted in Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy August 2017 The dissertation of Natasha E. Batalha was reviewed and approved∗ by the following: Steinn Sigurdsson Professor of Astronomy and Astrophysics Dissertation Co-Advisor, Co-Chair of Committee James Kasting Professor of Geosciences Dissertation Co-Advisor, Co-Chair of Committee Jason Wright Professor of Astronomy and Astrophysics Eric Ford Professor of Astronomy and Astrophysics Chris Forest Professor of Meteorology Avi Mandell NASA Goddard Space Flight Center, Research Scientist Special Signatory Michael Eracleous Professor of Astronomy and Astrophysics Graduate Program Chair ∗Signatures are on file in the Graduate School. ii Abstract We will soon have the technological capability to measure the atmospheric compo- sition of temperate Earth-sized planets orbiting nearby stars. Interpreting these atmospheric signals poses a new challenge to planetary science. In contrast to jovian-like atmospheres, whose bulk compositions consist of hydrogen and helium, terrestrial planet atmospheres are likely comprised of high mean molecular weight secondary atmospheres, which have gone through a high degree of evolution. For example, present-day Mars has a frozen surface with a thin tenuous atmosphere, but 4 billion years ago it may have been warmed by a thick greenhouse atmosphere. Several processes contribute to a planet’s atmospheric evolution: stellar evolution, geological processes, atmospheric escape, biology, etc. Each of these individual processes affects the planetary system as a whole and therefore they all must be considered in the modeling of terrestrial planets.
    [Show full text]
  • Jason A. Dittmann 51 Pegasi B Postdoctoral Fellow
    Jason A. Dittmann 51 Pegasi b Postdoctoral Fellow Contact Massachusetts Institute of Technology MIT Kavli Institute: 37-438f 617-258-5928 (office) 70 Vassar St. 520-820-0928 (cell) Cambridge, MA 02139 [email protected] Education Harvard University, Cambridge, MA PhD, Astronomy and Astrophysics, May 2016 Advisor: David Charbonneau, PhD • University of Arizona, Tucson, AZ BS, Astronomy, Physics, May 2010 Advisor: Laird Close, PhD • Recent 51 Pegasi b Postdoctoral Fellow July 2017 – Present Research Earth and Planetary Science Department, MIT Positions Faculty Contact: Sara Seager Postdoctoral Researcher Feb 2017 – June 2017 Kavli Institute, MIT Supervisor: Sarah Ballard Postdoctoral Researcher July 2016 – Jan 2017 Center for Astrophysics, Harvard University Supervisor: David Charbonneau Research Assistant Sep 2010 – May 2016 Center for Astrophysics, Harvard University Advisors: David Charbonneau Publication 16 first and second authored publications Summary 22 additional co-authored publications 1 first-authored publication in Nature 1 co-authored publication in Nature Selected 51 Pegasi b Postdoctoral Fellowship 2017 – Present Awards and Pierce Fellowship 2010 – 2013 Honors Certificate of Distinction in Teaching 2012 Best Project Award, Physics Ugrd. Research Symp. 2009 Best Undergraduate Research (Steward Observatory) 2009 – 2010 Grants Principal Investigator, Hubble Space Telescope 2017, 10 orbits Awarded “Initial Reconaissance of a Transiting Rocky (maximum award) Planet in a Nearby M-Dwarf’s Habitable Zone” Principal Investigator,
    [Show full text]
  • Download This Article in PDF Format
    A&A 631, A7 (2019) https://doi.org/10.1051/0004-6361/201935922 Astronomy & © ESO 2019 Astrophysics Pebbles versus planetesimals: the case of Trappist-1 G. A. L. Coleman, A. Leleu?, Y. Alibert, and W. Benz Physikalisches Institut, Universität Bern, Gesellschaftsstr. 6, 3012 Bern, Switzerland e-mail: [email protected] Received 20 May 2019 / Accepted 11 August 2019 ABSTRACT We present a study into the formation of planetary systems around low mass stars similar to Trappist-1, through the accretion of either planetesimals or pebbles. The aim is to determine if the currently observed systems around low mass stars could favour one scenario over the other. To determine these differences, we ran numerous N-body simulations, coupled to a thermally evolving viscous 1D disc model, and including prescriptions for planet migration, photoevaporation, and pebble and planetesimal dynamics. We mainly examine the differences between the pebble and planetesimal accretion scenarios, but we also look at the influences of disc mass, size of planetesimals, and the percentage of solids locked up within pebbles. When comparing the resulting planetary systems to Trappist-1, we find that a wide range of initial conditions for both the pebble and planetesimal accretion scenarios can form planetary systems similar to Trappist-1, in terms of planet mass, periods, and resonant configurations. Typically these planets formed exterior to the water iceline and migrated in resonant convoys into the inner region close to the central star. When comparing the planetary systems formed through pebble accretion to those formed through planetesimal accretion, we find a large number of similarities, including average planet masses, eccentricities, inclinations, and period ratios.
    [Show full text]
  • Exoplanet.Eu Catalog Page 1 Star Distance Star Name Star Mass
    exoplanet.eu_catalog star_distance star_name star_mass Planet name mass 1.3 Proxima Centauri 0.120 Proxima Cen b 0.004 1.3 alpha Cen B 0.934 alf Cen B b 0.004 2.3 WISE 0855-0714 WISE 0855-0714 6.000 2.6 Lalande 21185 0.460 Lalande 21185 b 0.012 3.2 eps Eridani 0.830 eps Eridani b 3.090 3.4 Ross 128 0.168 Ross 128 b 0.004 3.6 GJ 15 A 0.375 GJ 15 A b 0.017 3.6 YZ Cet 0.130 YZ Cet d 0.004 3.6 YZ Cet 0.130 YZ Cet c 0.003 3.6 YZ Cet 0.130 YZ Cet b 0.002 3.6 eps Ind A 0.762 eps Ind A b 2.710 3.7 tau Cet 0.783 tau Cet e 0.012 3.7 tau Cet 0.783 tau Cet f 0.012 3.7 tau Cet 0.783 tau Cet h 0.006 3.7 tau Cet 0.783 tau Cet g 0.006 3.8 GJ 273 0.290 GJ 273 b 0.009 3.8 GJ 273 0.290 GJ 273 c 0.004 3.9 Kapteyn's 0.281 Kapteyn's c 0.022 3.9 Kapteyn's 0.281 Kapteyn's b 0.015 4.3 Wolf 1061 0.250 Wolf 1061 d 0.024 4.3 Wolf 1061 0.250 Wolf 1061 c 0.011 4.3 Wolf 1061 0.250 Wolf 1061 b 0.006 4.5 GJ 687 0.413 GJ 687 b 0.058 4.5 GJ 674 0.350 GJ 674 b 0.040 4.7 GJ 876 0.334 GJ 876 b 1.938 4.7 GJ 876 0.334 GJ 876 c 0.856 4.7 GJ 876 0.334 GJ 876 e 0.045 4.7 GJ 876 0.334 GJ 876 d 0.022 4.9 GJ 832 0.450 GJ 832 b 0.689 4.9 GJ 832 0.450 GJ 832 c 0.016 5.9 GJ 570 ABC 0.802 GJ 570 D 42.500 6.0 SIMP0136+0933 SIMP0136+0933 12.700 6.1 HD 20794 0.813 HD 20794 e 0.015 6.1 HD 20794 0.813 HD 20794 d 0.011 6.1 HD 20794 0.813 HD 20794 b 0.009 6.2 GJ 581 0.310 GJ 581 b 0.050 6.2 GJ 581 0.310 GJ 581 c 0.017 6.2 GJ 581 0.310 GJ 581 e 0.006 6.5 GJ 625 0.300 GJ 625 b 0.010 6.6 HD 219134 HD 219134 h 0.280 6.6 HD 219134 HD 219134 e 0.200 6.6 HD 219134 HD 219134 d 0.067 6.6 HD 219134 HD
    [Show full text]