Dynamical Measurements of the Interior Structure of Exoplanets
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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. -
Tregloan-Reed Phd 2014.Pdf
This work is protected by copyright and other intellectual property rights and duplication or sale of all or part is not permitted, except that material may be duplicated by you for research, private study, criticism/review or educational purposes. Electronic or print copies are for your own personal, non- commercial use and shall not be passed to any other individual. No quotation may be published without proper acknowledgement. For any other use, or to quote extensively from the work, permission must be obtained from the copyright holder/s. Starspot properties and photometric parameters of transiting planets and their host stars Jeremy Tregloan-Reed Mphys (Hons) Lancaster University Doctor of Philosophy Department of Astrophysics, University of Keele. October 2014 iii Abstract To begin understanding how the architecture of hot Jupiter planetary systems can be so radically different from that of our own solar system, requires the dynamical evolution of planets to be known. By measuring the sky-projected obliquity λ of a system it is possible to determine the dominant process in the dynamical evolution. If a transiting exoplanet that crosses the disc of its host star passes over a starspot, then the amount of received intensity from the star will change. By modelling the position of the anomaly in the lightcurve it is possible to precisely determine the position of the starspot on the stellar disc. If the position of the starspot can be found at two distinct times using two closely spaced transits, then it is possible to measure λ. Before now there was no definitive model capable of accurately modelling both a planetary transit and a starspot. -
Self-Intersection of the Fallback Stream in Tidal Disruption Events
Mon. Not. R. Astron. Soc. 000, 000–000 (0000) Printed 11 December 2019 (MN LATEX style file v2.2) Self-intersection of the Fallback Stream in Tidal Disruption Events Wenbin Lu1? and Clement´ Bonnerot1y 1TAPIR, Mail Code 350-17, California Institute of Technology, Pasadena, CA 91125, USA 11 December 2019 ABSTRACT We propose a semi-analytical model for the self-intersection of the fallback stream in tidal disruption events (TDEs). When the initial periapsis is less than about 15 gravitational radii, a large fraction of the shocked gas is unbound in the form of a collision-induced outflow (CIO). This is because large apsidal precession causes the stream to self-intersect near the local escape speed at radius much below the apocenter. The rest of the fallback gas is left in more tightly bound orbits and quickly joins the accretion flow. We propose that the CIO is responsible for reprocessing the hard emission from the accretion flow into the optical band. This picture naturally explains the large photospheric radius (or low blackbody temperature) and typical line widths for optical TDEs. We predict the CIO-reprocessed spectrum in the ∼0:5 infrared to be Lν / ν , shallower than a blackbody. The partial sky coverage of the CIO also provides a unification of the diverse X-ray behaviors of optical TDEs. According to this picture, optical surveys filter out a large fraction of TDEs with low-mass blackholes due to lack of a reprocessing layer, and the volumetric rate of optical TDEs is nearly flat wrt. the 7 blackhole mass in the range M . -
Virgo the Virgin
Virgo the Virgin Virgo is one of the constellations of the zodiac, the group tion Virgo itself. There is also the connection here with of 12 constellations that lies on the ecliptic plane defined “The Scales of Justice” and the sign Libra which lies next by the planets orbital orientation around the Sun. Virgo is to Virgo in the Zodiac. The study of astronomy had a one of the original 48 constellations charted by Ptolemy. practical “time keeping” aspect in the cultures of ancient It is the largest constellation of the Zodiac and the sec- history and as the stars of Virgo appeared before sunrise ond - largest constellation after Hydra. Virgo is bordered by late in the northern summer, many cultures linked this the constellations of Bootes, Coma Berenices, Leo, Crater, asterism with crops, harvest and fecundity. Corvus, Hydra, Libra and Serpens Caput. The constella- tion of Virgo is highly populated with galaxies and there Virgo is usually depicted with angel - like wings, with an are several galaxy clusters located within its boundaries, ear of wheat in her left hand, marked by the bright star each of which is home to hundreds or even thousands of Spica, which is Latin for “ear of grain”, and a tall blade of galaxies. The accepted abbreviation when enumerating grass, or a palm frond, in her right hand. Spica will be objects within the constellation is Vir, the genitive form is important for us in navigating Virgo in the modern night Virginis and meteor showers that appear to originate from sky. Spica was most likely the star that helped the Greek Virgo are called Virginids. -
Dr. Konstantin Batygin Curriculum Vitae Division of Geological & Planetary Sciences [email protected] California Institute of Technology (626) 395-2920 1200 E
Dr. Konstantin Batygin Curriculum Vitae Division of Geological & Planetary Sciences [email protected] California Institute of Technology (626) 395-2920 1200 E. California Blvd. Pasadena, CA 91125 Education Ph.D., Planetary Science (2012) California Institute of Technology doctoral advisors: David J. Stevenson & Michael E. Brown M.S., Planetary Science (2010) California Institute of Technology B.S., Astrophysics (2008) (with honors) University of California, Santa Cruz undergraduate advisor: Gregory Laughlin Academic Employment Professor of Planetary Science, Caltech May 2019 - present Van Nuys Page Scholar, Caltech May 2017 - May 2019 Assistant Professor of Planetary Science, Caltech Jun. 2014 - May 2019 Harvard ITC Postdoctoral Fellow, Harvard Center for Astrophysics Nov. 2012 - Jun. 2014 Postdoctoral Fellow, Observatoire de la Cote d’Azur, Nice, France Jul. 2012 - Nov. 2012 Visiting Scientist, Observatoire de la Cote d’Azur, Nice, France Feb. 2011 - Mar. 2011 Graduate Research Assistant/Teaching Assistant, Caltech Sep. 2008 - Jun. 2012 Research Assistant, UCO/Lick Observatory Mar. 2006 - Sep. 2008 Supplemental Instructor, University of California, Santa Cruz Mar. 2006 - Jun. 2006 Research Assistant, NASA Ames Research Center Jul. 2005 - Jan. 2006 Awards Sloan Fellowship in Physics - 2018 Packard Fellowship for Science & Engineering - 2017 Genius100 Visionary Award, Albert Einstein Legacy Foundation - 2017 Garfinkel Lectureship in Celestial Mechanics (Yale) - 2017 AAS WWT Prize in Research - 2016 Popular Science Brilliant 10 - 2016 -
Downloads/ Astero2007.Pdf) and by Aerts Et Al (2010)
This work is protected by copyright and other intellectual property rights and duplication or sale of all or part is not permitted, except that material may be duplicated by you for research, private study, criticism/review or educational purposes. Electronic or print copies are for your own personal, non- commercial use and shall not be passed to any other individual. No quotation may be published without proper acknowledgement. For any other use, or to quote extensively from the work, permission must be obtained from the copyright holder/s. i Fundamental Properties of Solar-Type Eclipsing Binary Stars, and Kinematic Biases of Exoplanet Host Stars Richard J. Hutcheon Submitted in accordance with the requirements for the degree of Doctor of Philosophy. Research Institute: School of Environmental and Physical Sciences and Applied Mathematics. University of Keele June 2015 ii iii Abstract This thesis is in three parts: 1) a kinematical study of exoplanet host stars, 2) a study of the detached eclipsing binary V1094 Tau and 3) and observations of other eclipsing binaries. Part I investigates kinematical biases between two methods of detecting exoplanets; the ground based transit and radial velocity methods. Distances of the host stars from each method lie in almost non-overlapping groups. Samples of host stars from each group are selected. They are compared by means of matching comparison samples of stars not known to have exoplanets. The detection methods are found to introduce a negligible bias into the metallicities of the host stars but the ground based transit method introduces a median age bias of about -2 Gyr. -
Basic Notations
Appendix A Basic Notations In this Appendix, the basic notations for the mathematical operators and astronom- ical and physical quantities used throughout the book are given. Note that only the most frequently used quantities are mentioned; besides, overlapping symbol definitions and deviations from the basically adopted notations are possible, when appropriate. Mathematical Quantities and Operators kxk is the length (norm) of vector x x y is the scalar product of vectors x and y rr is the gradient operator in the direction of vector r f f ; gg is the Poisson bracket of functions f and g K.m/ or K.k/ (where m D k2) is the complete elliptic integral of the first kind with modulus k E.m/ or E.k/ is the complete elliptic integral of the second kind F.˛; m/ is the incomplete elliptic integral of the first kind E.˛; m/ is the incomplete elliptic integral of the second kind ƒ0 is Heuman’s Lambda function Pi is the Legendre polynomial of degree i x0 is the initial value of a variable x Coordinates and Frames x, y, z are the Cartesian (orthogonal) coordinates r, , ˛ are the spherical coordinates (radial distance, longitude, and latitude) © Springer International Publishing Switzerland 2017 171 I. I. Shevchenko, The Lidov-Kozai Effect – Applications in Exoplanet Research and Dynamical Astronomy, Astrophysics and Space Science Library 441, DOI 10.1007/978-3-319-43522-0 172 A Basic Notations In the three-body problem: r1 is the position vector of body 1 relative to body 0 r2 is the position vector of body 2 relative to the center of mass of the inner -
Probing the Interiors of Very Hot Jupiters Using Transit Light Curves
Accepted by the Astrophysical Journal A Preprint typeset using LTEX style emulateapj v. 08/22/09 PROBING THE INTERIORS OF VERY HOT JUPITERS USING TRANSIT LIGHT CURVES Darin Ragozzine & Aaron S. Wolf∗ Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125 Accepted by the Astrophysical Journal ABSTRACT Accurately understanding the interior structure of extra-solar planets is critical for inferring their formation and evolution. The internal density distribution of a planet has a direct effect on the star- planet orbit through the gravitational quadrupole field created by the rotational and tidal bulges. These quadrupoles induce apsidal precession that is proportional to the planetary Love number (k2p, twice the apsidal motion constant), a bulk physical characteristic of the planet that depends on the internal density distribution, including the presence or absence of a massive solid core. We find that the quadrupole of the planetary tidal bulge is the dominant source of apsidal precession for very hot Jupiters (a . 0.025 AU), exceeding the effects of general relativity and the stellar quadrupole by more than an order of magnitude. For the shortest-period planets, the planetary interior induces precession of a few degrees per year. By investigating the full photometric signal of apsidal precession, we find that changes in transit shapes are much more important than transit timing variations. With its long baseline of ultra-precise photometry, the space-based Kepler mission can realistically detect apsidal precession with the accuracy necessary to infer the presence or absence of a massive core in very hot Jupiters with orbital eccentricities as low as e 0.003. -
Open Research Online Oro.Open.Ac.Uk
Open Research Online The Open University’s repository of research publications and other research outputs Extra-Solar Planetary Atmospheres and Interior Structure: Implications for Observational Signatures Thesis How to cite: Bending, Victoria Louise (2016). Extra-Solar Planetary Atmospheres and Interior Structure: Implications for Observational Signatures. PhD thesis The Open University. For guidance on citations see FAQs. c 2016 The Author https://creativecommons.org/licenses/by-nc-nd/4.0/ Version: Version of Record Link(s) to article on publisher’s website: http://dx.doi.org/doi:10.21954/ou.ro.0000ef7b Copyright and Moral Rights for the articles on this site are retained by the individual authors and/or other copyright owners. For more information on Open Research Online’s data policy on reuse of materials please consult the policies page. oro.open.ac.uk Extra-Solar Planetary Atmospheres and Interior Structure: Implications for Observational Signatures Victoria Louise Bending BA (Hons) (Open University) 2004 MPhys (Durham) 2009 This thesis is submitted for the degree of Doctor of Philosophy Department of Physical Sciences The Open University Submitted: October 2015 ProQuest Number: 13834775 All rights reserved INFORMATION TO ALL USERS The quality of this reproduction is dependent upon the quality of the copy submitted. In the unlikely event that the author did not send a com plete manuscript and there are missing pages, these will be noted. Also, if material had to be removed, a note will indicate the deletion. uest ProQuest 13834775 Published by ProQuest LLC(2019). Copyright of the Dissertation is held by the Author. All rights reserved. This work is protected against unauthorized copying under Title 17, United States C ode Microform Edition © ProQuest LLC. -
The Rotating Reference Frame and the Precession of the Equinoxes
The rotating reference frame and the precession of the equinoxes Adrián G. Cornejo Electronics and Communications Engineering from Universidad Iberoamericana, Calle Santa Rosa 719, CP 76138, Col. Santa Mónica, Querétaro, Querétaro, Mexico. E-mail: [email protected] (Received 7 August 2013, accepted 27 December 2013) Abstract In this paper, angular frequency of a rotating reference frame is derived, where a given body orbiting and rotating around a fixed axis describes a periodical rosette path completing a periodical “circular motion”. Thus, by the analogy between a rotating frame of reference and the whole Solar System, angular frequency and period of a possible planetary circular motion are calculated. For the Earth's case, the circular period is calculated from motion of the orbit by the rotation effect, together with the advancing caused by the apsidal precession, which results the same amount than the period of precession of the equinoxes. This coincidence could provide an alternative explanation for this observed effect. Keywords: Rotating reference frame, Lagranian mechanics, Angular frequency, Precession of the equinoxes. Resumen En este trabajo, se deriva la frecuencia angular de un marco de referencia rotante, donde un cuerpo dado orbitando y rotando alrededor de un eje fijo describe una trayectoria en forma de una roseta periódica completando un “movimiento circular” periódico. Así, por la analogía entre un marco de referencia rotacional y el Sistema Solar como un todo, se calculan la frecuencia angular y el periodo de un posible movimiento circular planetario. Para el caso de la Tierra, el periodo circular es calculado a partir del movimiento de la órbita por el efecto de la rotación, junto con el avance causado por la precesión absidal, resultando el mismo valor que el periodo de la precesión de los equinoccios. -
Arxiv:2004.00037V2 [Astro-Ph.EP] 26 May 2020
Draft version May 27, 2020 Typeset using LATEX twocolumn style in AASTeX62 Giant Planet Influence on the Collective Gravity of a Primordial Scattered Disk Alexander Zderic1 and Ann-Marie Madigan1 1JILA and Department of Astrophysical and Planetary Sciences, CU Boulder, Boulder, CO 80309, USA ABSTRACT Axisymmetric disks of high eccentricity, low mass bodies on near-Keplerian orbits are unstable to an out-of-plane buckling. This \inclination instability" exponentially grows the orbital inclinations, raises perihelion distances and clusters in argument of perihelion. Here we examine the instability in a massive primordial scattered disk including the orbit-averaged gravitational influence of the giant planets. We show that differential apsidal precession induced by the giant planets will suppress the inclination instability unless the primordial mass is & 20 Earth masses. We also show that the instability should produce a \perihelion gap" at semi-major axes of hundreds of AU, as the orbits of the remnant population are more likely to have extremely large perihelion distances (O(100 AU)) than intermediate values. Keywords: celestial mechanics { Outer Solar System: secular dynamics 1. INTRODUCTION In Madigan et al.(2018) we explained the mechanism Structures formed by the collective gravity of numer- behind the instability: secular torques acting between ous low-mass bodies are well-studied on many astrophys- the high eccentricity orbits. We also showed how the ical scales, for example, stellar bar formation in galaxies instability timescale scaled as a function of disk param- (Sellwood & Wilkinson 1993) and apsidally-aligned disks eters. One important result is that the growth timescale of stars orbiting supermassive black holes (Kazandjian & is sensitive to the number of bodies used in N-body Touma 2013; Madigan et al.