Mean-Motion Resonances in Exoplanetary Systems
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Low Thrust Manoeuvres to Perform Large Changes of RAAN Or Inclination in LEO
Facoltà di Ingegneria Corso di Laurea Magistrale in Ingegneria Aerospaziale Master Thesis Low Thrust Manoeuvres To Perform Large Changes of RAAN or Inclination in LEO Academic Tutor: Prof. Lorenzo CASALINO Candidate: Filippo GRISOT July 2018 “It is possible for ordinary people to choose to be extraordinary” E. Musk ii Filippo Grisot – Master Thesis iii Filippo Grisot – Master Thesis Acknowledgments I would like to address my sincere acknowledgments to my professor Lorenzo Casalino, for your huge help in these moths, for your willingness, for your professionalism and for your kindness. It was very stimulating, as well as fun, working with you. I would like to thank all my course-mates, for the time spent together inside and outside the “Poli”, for the help in passing the exams, for the fun and the desperation we shared throughout these years. I would like to especially express my gratitude to Emanuele, Gianluca, Giulia, Lorenzo and Fabio who, more than everyone, had to bear with me. I would like to also thank all my extra-Poli friends, especially Alberto, for your support and the long talks throughout these years, Zach, for being so close although the great distance between us, Bea’s family, for all the Sundays and summers spent together, and my soccer team Belfiga FC, for being the crazy lovable people you are. A huge acknowledgment needs to be address to my family: to my grandfather Luciano, for being a great friend; to my grandmother Bianca, for teaching me what “fighting” means; to my grandparents Beppe and Etta, for protecting me -
Modeling Super-Earth Atmospheres in Preparation for Upcoming Extremely Large Telescopes
Modeling Super-Earth Atmospheres In Preparation for Upcoming Extremely Large Telescopes Maggie Thompson1 Jonathan Fortney1, Andy Skemer1, Tyler Robinson2, Theodora Karalidi1, Steph Sallum1 1University of California, Santa Cruz, CA; 2Northern Arizona University, Flagstaff, AZ ExoPAG 19 January 6, 2019 Seattle, Washington Image Credit: NASA Ames/JPL-Caltech/T. Pyle Roadmap Research Goals & Current Atmosphere Modeling Selecting Super-Earths for State of Super-Earth Tool (Past & Present) Follow-Up Observations Detection Preliminary Assessment of Future Observatories for Conclusions & Upcoming Instruments’ Super-Earths Future Work Capabilities for Super-Earths M. Thompson — ExoPAG 19 01/06/19 Research Goals • Extend previous modeling tool to simulate super-Earth planet atmospheres around M, K and G stars • Apply modified code to explore the parameter space of actual and synthetic super-Earths to select most suitable set of confirmed exoplanets for follow-up observations with JWST and next-generation ground-based telescopes • Inform the design of advanced instruments such as the Planetary Systems Imager (PSI), a proposed second-generation instrument for TMT/GMT M. Thompson — ExoPAG 19 01/06/19 Current State of Super-Earth Detections (1) Neptune Mass Range of Interest Earth Data from NASA Exoplanet Archive M. Thompson — ExoPAG 19 01/06/19 Current State of Super-Earth Detections (2) A Approximate Habitable Zone Host Star Spectral Type F G K M Data from NASA Exoplanet Archive M. Thompson — ExoPAG 19 01/06/19 Atmosphere Modeling Tool Evolution of Atmosphere Model • Solar System Planets & Moons ~ 1980’s (e.g., McKay et al. 1989) • Brown Dwarfs ~ 2000’s (e.g., Burrows et al. 2001) • Hot Jupiters & Other Giant Exoplanets ~ 2000’s (e.g., Fortney et al. -
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. -
![Arxiv:2011.13376V1 [Astro-Ph.EP] 26 Nov 2020 Welsh Et Al](https://docslib.b-cdn.net/cover/7378/arxiv-2011-13376v1-astro-ph-ep-26-nov-2020-welsh-et-al-47378.webp)
Arxiv:2011.13376V1 [Astro-Ph.EP] 26 Nov 2020 Welsh Et Al
On the estimation of circumbinary orbital properties Benjamin C. Bromley Department of Physics & Astronomy, University of Utah, 115 S 1400 E, Rm 201, Salt Lake City, UT 84112 [email protected] Scott J. Kenyon Smithsonian Astrophysical Observatory, 60 Garden St., Cambridge, MA 02138 [email protected] ABSTRACT We describe a fast, approximate method to characterize the orbits of satellites around a central binary in numerical simulations. A goal is to distinguish the free eccentricity | random motion of a satellite relative to a dynamically cool orbit | from oscillatory modes driven by the central binary's time-varying gravitational potential. We assess the performance of the method using the Kepler-16, Kepler-47, and Pluto-Charon systems. We then apply the method to a simulation of orbital damping in a circumbinary environment, resolving relative speeds between small bodies that are slow enough to promote mergers and growth. These results illustrate how dynamical cooling can set the stage for the formation of Tatooine-like planets around stellar binaries and the small moons around the Pluto-Charon binary planet. Subject headings: planets and satellites: formation { planets and satellites: individual: Pluto 1. Introduction Planet formation seems inevitable around nearly all stars. Even the rapidly changing gravitational field around a binary does not prevent planets from settling there (e.g., Armstrong et al. 2014). Recent observations have revealed stable planets around binaries involving main sequence stars (e.g., Kepler-16; Doyle et al. 2011), as well as evolved compact stars (the neutron star-white dwarf binary PSR B1620- 26; Sigurdsson et al. 2003). The Kepler mission (Borucki et al. -
Planetary Phase Variations of the 55 Cancri System
The Astrophysical Journal, 740:61 (7pp), 2011 October 20 doi:10.1088/0004-637X/740/2/61 C 2011. The American Astronomical Society. All rights reserved. Printed in the U.S.A. PLANETARY PHASE VARIATIONS OF THE 55 CANCRI SYSTEM Stephen R. Kane1, Dawn M. Gelino1, David R. Ciardi1, Diana Dragomir1,2, and Kaspar von Braun1 1 NASA Exoplanet Science Institute, Caltech, MS 100-22, 770 South Wilson Avenue, Pasadena, CA 91125, USA; [email protected] 2 Department of Physics & Astronomy, University of British Columbia, Vancouver, BC V6T1Z1, Canada Received 2011 May 6; accepted 2011 July 21; published 2011 September 29 ABSTRACT Characterization of the composition, surface properties, and atmospheric conditions of exoplanets is a rapidly progressing field as the data to study such aspects become more accessible. Bright targets, such as the multi-planet 55 Cancri system, allow an opportunity to achieve high signal-to-noise for the detection of photometric phase variations to constrain the planetary albedos. The recent discovery that innermost planet, 55 Cancri e, transits the host star introduces new prospects for studying this system. Here we calculate photometric phase curves at optical wavelengths for the system with varying assumptions for the surface and atmospheric properties of 55 Cancri e. We show that the large differences in geometric albedo allows one to distinguish between various surface models, that the scattering phase function cannot be constrained with foreseeable data, and that planet b will contribute significantly to the phase variation, depending upon the surface of planet e. We discuss detection limits and how these models may be used with future instrumentation to further characterize these planets and distinguish between various assumptions regarding surface conditions. -
Interior Dynamics of Super-Earth 55 Cancri E Constrained by General Circulation Models
Geophysical Research Abstracts Vol. 21, EGU2019-4167, 2019 EGU General Assembly 2019 © Author(s) 2019. CC Attribution 4.0 license. Interior dynamics of super-Earth 55 Cancri e constrained by general circulation models Tobias Meier (1), Dan J. Bower (1), Tim Lichtenberg (2), and Mark Hammond (2) (1) Center for Space and Habitability, Universität Bern , Bern, Switzerland , (2) Department of Physics, University of Oxford, Oxford, United Kingdom Close-in and tidally-locked super-Earths feature a day-side that always faces the host star and are thus subject to intense insolation. The thermal phase curve of 55 Cancri e, one of the best studied super-Earths, reveals a hotspot shift (offset of the maximum temperature from the substellar point) and a large day-night temperature contrast. Recent general circulation models (GCMs) aiming to explain these observations determine the spatial variability of the surface temperature of 55 Cnc e for different atmospheric masses and compositions. Here, we use constraints from the GCMs to infer the planet’s interior dynamics using a numerical geodynamic model of mantle flow. The geodynamic model is devised to be relatively simple due to uncertainties in the interior composition and structure of 55 Cnc e (and super-Earths in general), which preclude a detailed treatment of thermophysical parameters or rheology. We focus on several end-member models inspired by the GCM results to map the variety of interior regimes relevant to understand the present-state and evolution of 55 Cnc e. In particular, we investigate differences in heat transport and convective style between the day- and night-sides, and find that the thermal structure close to the surface and core-mantle boundary exhibits the largest deviations. -
Download the Search for New Planets
“VITAL ARTICLES ON SCIENCE/CREATION” September 1999 Impact #315 THE SEARCH FOR NEW PLANETS by Don DeYoung, Ph.D.* The nine solar system planets, from Mercury to Pluto, have been much-studied targets of the space age. In general, a planet is any massive object which orbits a star, in our case, the Sun. Some have questioned the status of Pluto, mainly because of its small size, but it remains a full-fledged planet. There is little evidence for additional solar planets beyond Pluto. Instead, attention has turned to extrasolar planets which may circle other stars. Intense competition has arisen among astronomers to detect such objects. Success insures media attention, journal publication, and continued research funding. The Interest in Planets Just one word explains the intense interest in new planets—life. Many scientists are convinced that we are not alone in space. Since life evolved on Earth, it must likewise have happened elsewhere, either on planets or their moons. The naïve assumption is that life will arise if we “just add water”: Earth-like planet + water → spontaneous life This equation is falsified by over a century of biological research showing the deep complexity of life. Scarcely is there a fact more certain than that matter does not spring into life on its own. Drake Equation Astronomer Frank Drake pioneered the Search for ExtraTerrestrial Intelligence project, or SETI, in the 1960s. He also attempted to calculate the total number of planets with life. The Drake Equation in simplified form is: Total livable Probability of Planets with planets x evolution = evolved life *Don DeYoung, Ph.D., is an Adjunct Professor of Physics at ICR. -
Gravity Recovery by Kinematic State Vector Perturbation from Satellite-To-Satellite Tracking for GRACE-Like Orbits Over Long Arcs
Gravity Recovery by Kinematic State Vector Perturbation from Satellite-to-Satellite Tracking for GRACE-like Orbits over Long Arcs by Nlingilili Habana Report No. 514 Geodetic Science The Ohio State University Columbus, Ohio 43210 January 2020 Gravity Recovery by Kinematic State Vector Perturbation from Satellite-to-Satellite Tracking for GRACE-like Orbits over Long Arcs By Nlingilili Habana Report No. 514 Geodetic Science The Ohio State University Columbus, Ohio 43210 January 2020 Copyright by Nlingilili Habana 2020 Preface This report was prepared for and submitted to the Graduate School of The Ohio State University as a dissertation in partial fulfillment of the requirements for the Degree of Doctor of Philosophy ii Abstract To improve on the understanding of Earth dynamics, a perturbation theory aimed at geopotential recovery, based on purely kinematic state vectors, is implemented. The method was originally proposed in the study by Xu (2008). It is a perturbation method based on Cartesian coordinates that is not subject to singularities that burden most conventional methods of gravity recovery from satellite-to-satellite tracking. The principal focus of the theory is to make the gravity recovery process more efficient, for example, by reducing the number of nuisance parameters associated with arc endpoint conditions in the estimation process. The theory aims to do this by maximizing the benefits of pure kinematic tracking by GNSS over long arcs. However, the practical feasibility of this theory has never been tested numerically. In this study, the formulation of the perturbation theory is first modified to make it numerically practicable. It is then shown, with realistic simulations, that Xu’s original goal of an iterative solution is not achievable under the constraints imposed by numerical integration error. -
Public HARPS Radial Velocity Database Corrected for Systematic
A&A 636, A74 (2020) Astronomy https://doi.org/10.1051/0004-6361/201936686 & c T. Trifonov et al. 2020 Astrophysics Public HARPS radial velocity database corrected for systematic errors?,?? Trifon Trifonov1,2, Lev Tal-Or3,4, Mathias Zechmeister5, Adrian Kaminski6, Shay Zucker4, and Tsevi Mazeh7 1 Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany e-mail: [email protected] 2 Department of Astronomy, Sofia University “St Kliment Ohridski”, 5 James Bourchier Blvd, 1164 Sofia, Bulgaria 3 Department of Physics, Ariel University, Ariel 40700, Israel 4 Department of Geophysics, Raymond and Beverly Sackler Faculty of Exact Sciences, Tel Aviv University, Tel Aviv 6997801, Israel 5 Institut für Astrophysik, Georg-August-Universität, Friedrich-Hund-Platz 1, 37077 Göttingen, Germany 6 Landessternwarte, Zentrum für Astronomie der Universtät Heidelberg, Königstuhl 12, 69117 Heidelberg, Germany 7 School of Physics and Astronomy, Raymond and Beverly Sackler Faculty of Exact Sciences, Tel Aviv University, Tel Aviv 6997801, Israel Received 11 September 2019 / Accepted 16 January 2020 ABSTRACT Context. The High Accuracy Radial velocity Planet Searcher (HARPS) spectrograph has been mounted since 2003 at the ESO 3.6 m telescope in La Silla and provides state-of-the-art stellar radial velocity (RV) measurements with a precision down to ∼1 m s−1. The spectra are extracted with a dedicated data-reduction software (DRS), and the RVs are computed by cross-correlating with a numerical mask. Aims. This study has three main aims: (i) Create easy access to the public HARPS RV data set. (ii) Apply the new public SpEctrum Radial Velocity AnaLyser (SERVAL) pipeline to the spectra, and produce a more precise RV data set. -
Occurrence and Core-Envelope Structure of 1–4× Earth-Size Planets Around Sun-Like Stars
Occurrence and core-envelope structure of 1–4× SPECIAL FEATURE Earth-size planets around Sun-like stars Geoffrey W. Marcya,1, Lauren M. Weissa, Erik A. Petiguraa, Howard Isaacsona, Andrew W. Howardb, and Lars A. Buchhavec aDepartment of Astronomy, University of California, Berkeley, CA 94720; bInstitute for Astronomy, University of Hawaii at Manoa, Honolulu, HI 96822; and cHarvard-Smithsonian Center for Astrophysics, Harvard University, Cambridge, MA 02138 Edited by Adam S. Burrows, Princeton University, Princeton, NJ, and accepted by the Editorial Board April 16, 2014 (received for review January 24, 2014) Small planets, 1–4× the size of Earth, are extremely common planets. The Doppler reflex velocity of an Earth-size planet − around Sun-like stars, and surprisingly so, as they are missing in orbiting at 0.3 AU is only 0.2 m s 1, difficult to detect with an − our solar system. Recent detections have yielded enough informa- observational precision of 1 m s 1. However, such Earth-size tion about this class of exoplanets to begin characterizing their planets show up as a ∼10-sigma dimming of the host star after occurrence rates, orbits, masses, densities, and internal structures. coadding the brightness measurements from each transit. The Kepler mission finds the smallest planets to be most common, The occurrence rate of Earth-size planets is a major goal of as 26% of Sun-like stars have small, 1–2 R⊕ planets with orbital exoplanet science. With three years of Kepler photometry in periods under 100 d, and 11% have 1–2 R⊕ planets that receive 1–4× hand, two groups worked to account for the detection biases in the incident stellar flux that warms our Earth. -
![Arxiv:1709.05344V1 [Astro-Ph.SR] 15 Sep 2017 (A(Li) = 2.75), Higher Than Its Companion by 0.5 Dex](https://docslib.b-cdn.net/cover/8833/arxiv-1709-05344v1-astro-ph-sr-15-sep-2017-a-li-2-75-higher-than-its-companion-by-0-5-dex-498833.webp)
Arxiv:1709.05344V1 [Astro-Ph.SR] 15 Sep 2017 (A(Li) = 2.75), Higher Than Its Companion by 0.5 Dex
Draft version September 19, 2017 Typeset using LATEX modern style in AASTeX61 KRONOS & KRIOS: EVIDENCE FOR ACCRETION OF A MASSIVE, ROCKY PLANETARY SYSTEM IN A COMOVING PAIR OF SOLAR-TYPE STARS Semyeong Oh,1, 2 Adrian M. Price-Whelan,1 John M. Brewer,3, 4 David W. Hogg,5, 6, 7, 8 David N. Spergel,1, 5 and Justin Myles3 1Department of Astrophysical Sciences, Princeton University, 4 Ivy Lane, Princeton, NJ 08544, USA 2To whom correspondence should be addressed: [email protected] 3Department of Astronomy, Yale University, 260 Whitney Ave, New Haven, CT 06511, USA 4Department of Astronomy, Columbia University, 550 West 120th Street, New York, NY 10027, USA 5Center for Computational Astrophysics, Flatiron Institute, 162 Fifth Ave, New York, NY 10010, USA 6Center for Cosmology and Particle Physics, Department of Physics, New York University, 726 Broadway, New York, NY 10003, USA 7Center for Data Science, New York University, 60 Fifth Ave, New York, NY 10011, USA 8Max-Planck-Institut f¨ur Astronomie, K¨onigstuhl17, D-69117 Heidelberg ABSTRACT We report and discuss the discovery of a comoving pair of bright solar-type stars, HD 240430 and HD 240429, with a significant difference in their chemical abundances. The two stars have an estimated 3D separation of ≈ 0:6 pc (≈ 0:01 pc projected) at a distance of r ≈ 100 pc with nearly identical three-dimensional velocities, as inferred from Gaia TGAS parallaxes and proper motions, and high-precision radial velocity measurements. Stellar parameters determined from high-resolution Keck HIRES spectra indicate that both stars are ∼ 4 Gyr old. The more metal-rich of the two, HD 240430, shows an enhancement of refractory (TC > 1200 K) elements by ≈ 0:2 dex and a marginal enhancement of (moderately) volatile elements (TC < 1200 K; C, N, O, Na, and Mn). -
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