Extrasolar Planets
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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. -
Stability of Planets in Binary Star Systems
StabilityStability ofof PlanetsPlanets inin BinaryBinary StarStar SystemsSystems Ákos Bazsó in collaboration with: E. Pilat-Lohinger, D. Bancelin, B. Funk ADG Group Outline Exoplanets in multiple star systems Secular perturbation theory Application: tight binary systems Summary + Outlook About NFN sub-project SP8 “Binary Star Systems and Habitability” Stand-alone project “Exoplanets: Architecture, Evolution and Habitability” Basic dynamical types S-type motion (“satellite”) around one star P-type motion (“planetary”) around both stars Image: R. Schwarz Exoplanets in multiple star systems Observations: (Schwarz 2014, Binary Catalogue) ● 55 binary star systems with 81 planets ● 43 S-type + 12 P-type systems ● 10 multiple star systems with 10 planets Example: γ Cep (Hatzes et al. 2003) ● RV measurements since 1981 ● Indication for a “planet” (Campbell et al. 1988) ● Binary period ~57 yrs, planet period ~2.5 yrs Multiplicity of stars ~45% of solar like stars (F6 – K3) with d < 25 pc in multiple star systems (Raghavan et al. 2010) Known exoplanet host stars: single double triple+ source 77% 20% 3% Raghavan et al. (2006) 83% 15% 2% Mugrauer & Neuhäuser (2009) 88% 10% 2% Roell et al. (2012) Exoplanet catalogues The Extrasolar Planets Encyclopaedia http://exoplanet.eu Exoplanet Orbit Database http://exoplanets.org Open Exoplanet Catalogue http://www.openexoplanetcatalogue.com The Planetary Habitability Laboratory http://phl.upr.edu/home NASA Exoplanet Archive http://exoplanetarchive.ipac.caltech.edu Binary Catalogue of Exoplanets http://www.univie.ac.at/adg/schwarz/multiple.html Habitable Zone Gallery http://www.hzgallery.org Binary Catalogue Binary Catalogue of Exoplanets http://www.univie.ac.at/adg/schwarz/multiple.html Dynamical stability Stability limit for S-type planets Rabl & Dvorak (1988), Holman & Wiegert (1999), Pilat-Lohinger & Dvorak (2002) Parameters (a , e , μ) bin bin Outer limit at roughly max. -
Feb BACK BAY 2019
Feb BACK BAY 2019 The official newsletter of the Back Bay Amateur Astronomers CONTENTS COMING UP Gamma Burst 2 Feb 7 BBAA Meeting Eclipse Collage 3 7:30-9PM TCC, Virginia Beach NSN Article 6 Heart Nebula 7 Feb 8 Silent Sky Club meeting 10 10-11PM Little Theatre of VB Winter DSOs 11 Contact info 16 Feb 8 Cornwatch Photo by Chuck Jagow Canon 60Da, various exposures, iOptron mount with an Orion 80ED Calendar 17 dusk-dawn The best 9 out of 3465 images taken from about 10:00 PM on the 20th Cornland Park through 2:20 AM on the 21st. Unprocessed images (only cropped). Feb 14 Garden Stars 7-8:30PM LOOKING UP! a message from the president Norfolk Botanical Gardens This month’s most talked about astronomy event has to be the total lunar Feb 16 Saturday Sun-day eclipse. The BBAA participated by supporting the Watch Party at the 10AM-1PM Chesapeake Planetarium. Anyone in attendance will tell you it was COLD, but Elizabeth River Park manageable if you wore layers, utilized the planetarium where Dr. Robert Hitt seemed to have the thermostat set to 100 degrees, and drank copious amounts Feb 23 Skywatch of the hot coffee that Kent Blackwell brewed in the back office. 6PM-10PM The event had a huge following on Facebook but with the cold Northwest River Park temperatures, we weren’t sure how many would come out. By Kent’s estimate there were between 100–200 people in attendance. Many club members set up telescopes, as well as a few members of the public too. -
Can There Be Additional Rocky Planets in the Habitable Zone of Tight Binary
Mon. Not. R. Astron. Soc. 000, 1–10 () Printed 24 September 2018 (MN LATEX style file v2.2) Can there be additional rocky planets in the Habitable Zone of tight binary stars with a known gas giant? B. Funk1⋆, E. Pilat-Lohinger1 and S. Eggl2 1Institute for Astronomy, University of Vienna, Vienna, Austria 2IMCCE, Observatoire de Paris, Paris, France ABSTRACT Locating planets in Habitable Zones (HZs) around other stars is a growing field in contem- porary astronomy. Since a large percentage of all G-M stars in the solar neighborhood are expected to be part of binary or multiple stellar systems, investigations of whether habitable planets are likely to be discovered in such environments are of prime interest to the scientific community. As current exoplanet statistics predicts that the chances are higher to find new worlds in systems that are already known to have planets, we examine four known extrasolar planetary systems in tight binaries in order to determine their capacity to host additional hab- itable terrestrial planets. Those systems are Gliese 86, γ Cephei, HD 41004 and HD 196885. In the case of γ Cephei, our results suggest that only the M dwarf companion could host ad- ditional potentially habitable worlds. Neither could we identify stable, potentially habitable regions around HD 196885A. HD 196885 B can be considered a slightly more promising tar- get in the search forEarth-twins.Gliese 86 A turned out to be a very good candidate, assuming that the system’s history has not been excessively violent. For HD 41004 we have identified admissible stable orbits for habitable planets, but those strongly depend on the parameters of the system. -
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, -
A Basic Requirement for Studying the Heavens Is Determining Where In
Abasic requirement for studying the heavens is determining where in the sky things are. To specify sky positions, astronomers have developed several coordinate systems. Each uses a coordinate grid projected on to the celestial sphere, in analogy to the geographic coordinate system used on the surface of the Earth. The coordinate systems differ only in their choice of the fundamental plane, which divides the sky into two equal hemispheres along a great circle (the fundamental plane of the geographic system is the Earth's equator) . Each coordinate system is named for its choice of fundamental plane. The equatorial coordinate system is probably the most widely used celestial coordinate system. It is also the one most closely related to the geographic coordinate system, because they use the same fun damental plane and the same poles. The projection of the Earth's equator onto the celestial sphere is called the celestial equator. Similarly, projecting the geographic poles on to the celest ial sphere defines the north and south celestial poles. However, there is an important difference between the equatorial and geographic coordinate systems: the geographic system is fixed to the Earth; it rotates as the Earth does . The equatorial system is fixed to the stars, so it appears to rotate across the sky with the stars, but of course it's really the Earth rotating under the fixed sky. The latitudinal (latitude-like) angle of the equatorial system is called declination (Dec for short) . It measures the angle of an object above or below the celestial equator. The longitud inal angle is called the right ascension (RA for short). -
The Young Open Cluster NGC 2129
Dartmouth College Dartmouth Digital Commons Dartmouth Scholarship Faculty Work 10-17-2006 The Young Open Cluster NGC 2129 Giovanni Carraro The University of Chile Brian Chaboyer Dartmouth College James Perencevich Dartmouth College Follow this and additional works at: https://digitalcommons.dartmouth.edu/facoa Part of the Astrophysics and Astronomy Commons Dartmouth Digital Commons Citation Carraro, Giovanni; Chaboyer, Brian; and Perencevich, James, "The Young Open Cluster NGC 2129" (2006). Dartmouth Scholarship. 1859. https://digitalcommons.dartmouth.edu/facoa/1859 This Article is brought to you for free and open access by the Faculty Work at Dartmouth Digital Commons. It has been accepted for inclusion in Dartmouth Scholarship by an authorized administrator of Dartmouth Digital Commons. For more information, please contact [email protected]. Mon. Not. R. Astron. Soc. 365, 867–873 (2006) doi:10.1111/j.1365-2966.2005.09762.x The young open cluster NGC 2129 , , Giovanni Carraro,1 2 3 Brian Chaboyer4 and James Perencevich4 1Departamento de Astronomia´ , Universidad de Chile, Casilla 36-D, Santiago, Chile 2Astronomy Department, Yale University, PO Box 208101, New Haven, CT 06520-8101, USA 3Dipartimento di Astronomia, Universitad` iPadova, Vicolo Osservatorio 2, I-35122 Padova, Italy 4Department of Physics and Astronomy, Dartmouth College, 6127 Wilder Laboratory, Hanover, NH 03755-3528, USA Accepted 2005 October 17. Received 2005 October 15; in original form 2005 June 7 ABSTRACT The first charge-coupled device UBV(RI)C photometric study in the area of the doubtful open cluster NGC 2129 is presented. Photometry of a field offset 15 arcmin northwards is also provided, to probe the Galactic disc population towards the cluster. -
The Intermediate-Age Open Cluster NGC 2158
Mon. Not. R. Astron. Soc. 000, 000–000 (2002) Printed 28 October 2018 (MN LATEX style file v1.4) ⋆ The intermediate-age open cluster NGC 2158 Giovanni Carraro1, L´eo Girardi1,2 and Paola Marigo1† 1 Dipartimento di Astronomia, Universit`adi Padova, Vicolo dell’Osservatorio 2, I-35122 Padova, Italy 2 Osservatorio Astronomico di Trieste, Via G.B. Tiepolo 11, I-34131 Trieste, Italy Submitted: October 2001 ABSTRACT We report on UBV RI CCD photometry of two overlapping fields in the region of the intermediate-age open cluster NGC 2158 down to V = 21. By analyzing Colour-Colour (CC) and Colour-Magnitude Diagrams (CMD) we infer a reddening EB−V = 0.55 ± 0.10, a distance of 3600 ± 400 pc, and an age of about 2 Gyr. Synthetic CMDs performed with these parameters (but fixing EB−V = 0.60 and [Fe/H] = −0.60), and including binaries, field contamination, and photometric errors, allow a good description of the observed CMD. The elongated shape of the clump of red giants in the CMD is interpreted as resulting from a differential reddening of about ∆EB−V =0.06 across the cluster, in the direction perpendicular to the Galactic plane. NGC 2158 turns out to be an intermediate-age open cluster with an anomalously low metal content. The combination of these parameters together with the analysis of the cluster orbit, suggests that the cluster belongs to the old thin disk population. Key words: Open clusters and associations: general – open clusters and associations: individual: NGC 2158 - Hertzsprung-Russell (HR) diagram 1 INTRODUCTION the present paper. -
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Review HEAVY METAL RULES. I. EXOPLANET INCIDENCE AND METALLICITY Vardan Adibekyan1 ID 1 Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Rua das Estrelas, 4150-762 Porto, Portugal; [email protected] Academic Editor: name Received: date; Accepted: date; Published: date Abstract: Discovery of only handful of exoplanets required to establish a correlation between giant planet occurrence and metallicity of their host stars. More than 20 years have already passed from that discovery, however, many questions are still under lively debate: What is the origin of that relation? what is the exact functional form of the giant planet – metallicity relation (in the metal-poor regime)?, does such a relation exist for terrestrial planets? All these question are very important for our understanding of the formation and evolution of (exo)planets of different types around different types of stars and are subject of the present manuscript. Besides making a comprehensive literature review about the role of metallicity on the formation of exoplanets, I also revisited most of the planet – metallicity related correlations reported in the literature using a large and homogeneous data provided by the SWEET-Cat catalog. This study lead to several new results and conclusions, two of which I believe deserve to be highlighted in the abstract: i) The hosts of sub-Jupiter mass planets (∼0.6 – 0.9 M ) are systematically less metallic than the hosts of Jupiter-mass planets. This result might be relatedX to the longer disk lifetime and higher amount of planet building materials available at high metallicities, which allow a formation of more massive Jupiter-like planets. -
The Role of Resonances in Astrodynamical Systems
The Role of Resonances in Astrodynamical Systems Rudolf Dvorak Institut for Astronomy University Vienna e-mail: [email protected] Abstract This review intends to highlight the importance of resonances of the orbits of planets and asteroids in our Solar System. Besides the well known 5:2 mean motion resonance between Jupiter and Saturn, we discuss how secular resonances act, where the motions of the longitudes of the perihelia and/or the longitudes of the nodes are involved. Resonances are especially important for the motions of small bodies in the Solar System from the Earth crossing Near Earth Asteroids to the far moving asteroids and comets in the Kuiper belt outside Pluto's orbit. Briefly we also discuss retrograde orbits in resonances which turn out to be much more stable then prograde ones. The presence and importance of resonances in the dynamics of extrasolar planetary systems is a new exciting field for celestial mechanics. 1 Introduction In physics it is well known, that resonances play a fundamental role in any dynamical system. But, how important are resonances in astrodynamical systems? In this review we will deal first of all with our very own Solar System, where planets are trapped in so-called mean motion resonances causing chaos among asteroids and where celestial bodies generally suffer from strong perturbations due to secular resonances. With the discovery of extrasolar systems hosting planets which seem to be on highly eccentric orbits, that still are stable, another exiting chapter has been added to this topic. Such a behavior is understandable only, if these planets are locked in certain resonances. -
The Angular Size of Objects in the Sky
APPENDIX 1 The Angular Size of Objects in the Sky We measure the size of objects in the sky in terms of degrees. The angular diameter of the Sun or the Moon is close to half a degree. There are 60 minutes (of arc) to one degree (of arc), and 60 seconds (of arc) to one minute (of arc). Instead of including – of arc – we normally just use degrees, minutes and seconds. 1 degree = 60 minutes. 1 minute = 60 seconds. 1 degree = 3,600 seconds. This tells us that the Rosette nebula, which measures 80 minutes by 60 minutes, is a big object, since the diameter of the full Moon is only 30 minutes (or half a degree). It is clearly very useful to know, by looking it up beforehand, what the angular size of the objects you want to image are. If your field of view is too different from the object size, either much bigger, or much smaller, then the final image is not going to look very impressive. For example, if you are using a Sky 90 with SXVF-M25C camera with a 3.33 by 2.22 degree field of view, it would not be a good idea to expect impressive results if you image the Sombrero galaxy. The Sombrero galaxy measures 8.7 by 3.5 minutes and would appear as a bright, but very small patch of light in the centre of your frame. Similarly, if you were imaging at f#6.3 with the Nexstar 11 GPS scope and the SXVF-H9C colour camera, your field of view would be around 17.3 by 13 minutes, NGC7000 would not be the best target. -
Where Are All the Sirius-Like Binary Systems?
Mon. Not. R. Astron. Soc. 000, 1-22 (2013) Printed 20/08/2013 (MAB WORD template V1.0) Where are all the Sirius-Like Binary Systems? 1* 2 3 4 4 J. B. Holberg , T. D. Oswalt , E. M. Sion , M. A. Barstow and M. R. Burleigh ¹ Lunar and Planetary Laboratory, Sonnett Space Sciences Bld., University of Arizona, Tucson, AZ 85721, USA 2 Florida Institute of Technology, Melbourne, FL. 32091, USA 3 Department of Astronomy and Astrophysics, Villanova University, 800 Lancaster Ave. Villanova University, Villanova, PA, 19085, USA 4 Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH, UK 1st September 2011 ABSTRACT Approximately 70% of the nearby white dwarfs appear to be single stars, with the remainder being members of binary or multiple star systems. The most numerous and most easily identifiable systems are those in which the main sequence companion is an M star, since even if the systems are unresolved the white dwarf either dominates or is at least competitive with the luminosity of the companion at optical wavelengths. Harder to identify are systems where the non-degenerate component has a spectral type earlier than M0 and the white dwarf becomes the less luminous component. Taking Sirius as the prototype, these latter systems are referred to here as ‘Sirius-Like’. There are currently 98 known Sirius-Like systems. Studies of the local white dwarf population within 20 pc indicate that approximately 8 per cent of all white dwarfs are members of Sirius-Like systems, yet beyond 20 pc the frequency of known Sirius-Like systems declines to between 1 and 2 per cent, indicating that many more of these systems remain to be found.