Analysis of New High-Precision Transit Light Curves of WASP-10 B: Starspot Occultations, Small Planetary Radius, and High Metallicity ,
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Analysis of New High-Precision Transit Light Curves of WASP-10 B: Starspot
Astronomy & Astrophysics manuscript no. wasp10 c ESO 2018 September 10, 2018 Analysis of new high-precision transit light curves of WASP-10 b: starspot occultations, small planetary radius, and high metallicity⋆ G. Maciejewski1,2, St. Raetz2, N.Nettelmann3, M. Seeliger2, Ch. Adam2, G. Nowak1, and R. Neuh¨auser2 1 Toru´nCentre for Astronomy, Nicolaus Copernicus University, Gagarina 11, PL–87100 Toru´n, Poland e-mail: [email protected] 2 Astrophysikalisches Institut und Universit¨ats-Sternwarte, Schillerg¨asschen 2–3, D–07745 Jena, Germany 3 Institut f¨ur Physik, Universit¨at Rostock, D–18051 Rostock, Germany Received ...; accepted ... ABSTRACT Context. The WASP-10 planetary system is intriguing because different values of radius have been reported for its transiting exoplanet. The host star exhibits activity in terms of photometric variability, which is caused by the rotational modulation of the spots. Moreover, a periodic modulation has been discovered in transit timing of WASP-10 b, which could be a sign of an additional body perturbing the orbital motion of the transiting planet. Aims. We attempt to refine the physical parameters of the system, in particular the planetary radius, which is crucial for studying the internal structure of the transiting planet. We also determine new mid-transit times to confirm or refute observed anomalies in transit timing. Methods. We acquired high-precision light curves for four transits of WASP-10 b in 2010. Assuming various limb-darkening laws, we generated best-fit models and redetermined parameters of the system. The prayer-bead method and Monte Carlo simulations were used to derive error estimates. -
A Hot Subdwarf-White Dwarf Super-Chandrasekhar Candidate
A hot subdwarf–white dwarf super-Chandrasekhar candidate supernova Ia progenitor Ingrid Pelisoli1,2*, P. Neunteufel3, S. Geier1, T. Kupfer4,5, U. Heber6, A. Irrgang6, D. Schneider6, A. Bastian1, J. van Roestel7, V. Schaffenroth1, and B. N. Barlow8 1Institut fur¨ Physik und Astronomie, Universitat¨ Potsdam, Haus 28, Karl-Liebknecht-Str. 24/25, D-14476 Potsdam-Golm, Germany 2Department of Physics, University of Warwick, Coventry, CV4 7AL, UK 3Max Planck Institut fur¨ Astrophysik, Karl-Schwarzschild-Straße 1, 85748 Garching bei Munchen¨ 4Kavli Institute for Theoretical Physics, University of California, Santa Barbara, CA 93106, USA 5Texas Tech University, Department of Physics & Astronomy, Box 41051, 79409, Lubbock, TX, USA 6Dr. Karl Remeis-Observatory & ECAP, Astronomical Institute, Friedrich-Alexander University Erlangen-Nuremberg (FAU), Sternwartstr. 7, 96049 Bamberg, Germany 7Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA 91125, USA 8Department of Physics and Astronomy, High Point University, High Point, NC 27268, USA *[email protected] ABSTRACT Supernova Ia are bright explosive events that can be used to estimate cosmological distances, allowing us to study the expansion of the Universe. They are understood to result from a thermonuclear detonation in a white dwarf that formed from the exhausted core of a star more massive than the Sun. However, the possible progenitor channels leading to an explosion are a long-standing debate, limiting the precision and accuracy of supernova Ia as distance indicators. Here we present HD 265435, a binary system with an orbital period of less than a hundred minutes, consisting of a white dwarf and a hot subdwarf — a stripped core-helium burning star. -
The Extragalactic Distance Scale
The Extragalactic Distance Scale Published in "Stellar astrophysics for the local group" : VIII Canary Islands Winter School of Astrophysics. Edited by A. Aparicio, A. Herrero, and F. Sanchez. Cambridge ; New York : Cambridge University Press, 1998 Calibration of the Extragalactic Distance Scale By BARRY F. MADORE1, WENDY L. FREEDMAN2 1NASA/IPAC Extragalactic Database, Infrared Processing & Analysis Center, California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA 91125, USA 2Observatories, Carnegie Institution of Washington, 813 Santa Barbara St., Pasadena CA 91101, USA The calibration and use of Cepheids as primary distance indicators is reviewed in the context of the extragalactic distance scale. Comparison is made with the independently calibrated Population II distance scale and found to be consistent at the 10% level. The combined use of ground-based facilities and the Hubble Space Telescope now allow for the application of the Cepheid Period-Luminosity relation out to distances in excess of 20 Mpc. Calibration of secondary distance indicators and the direct determination of distances to galaxies in the field as well as in the Virgo and Fornax clusters allows for multiple paths to the determination of the absolute rate of the expansion of the Universe parameterized by the Hubble constant. At this point in the reduction and analysis of Key Project galaxies H0 = 72km/ sec/Mpc ± 2 (random) ± 12 [systematic]. Table of Contents INTRODUCTION TO THE LECTURES CEPHEIDS BRIEF SUMMARY OF THE OBSERVED PROPERTIES OF CEPHEID -
October 2006
OCTOBER 2 0 0 6 �������������� http://www.universetoday.com �������������� TAMMY PLOTNER WITH JEFF BARBOUR 283 SUNDAY, OCTOBER 1 In 1897, the world’s largest refractor (40”) debuted at the University of Chica- go’s Yerkes Observatory. Also today in 1958, NASA was established by an act of Congress. More? In 1962, the 300-foot radio telescope of the National Ra- dio Astronomy Observatory (NRAO) went live at Green Bank, West Virginia. It held place as the world’s second largest radio scope until it collapsed in 1988. Tonight let’s visit with an old lunar favorite. Easily seen in binoculars, the hexagonal walled plain of Albategnius ap- pears near the terminator about one-third the way north of the south limb. Look north of Albategnius for even larger and more ancient Hipparchus giving an almost “figure 8” view in binoculars. Between Hipparchus and Albategnius to the east are mid-sized craters Halley and Hind. Note the curious ALBATEGNIUS AND HIPPARCHUS ON THE relationship between impact crater Klein on Albategnius’ southwestern wall and TERMINATOR CREDIT: ROGER WARNER that of crater Horrocks on the northeastern wall of Hipparchus. Now let’s power up and “crater hop”... Just northwest of Hipparchus’ wall are the beginnings of the Sinus Medii area. Look for the deep imprint of Seeliger - named for a Dutch astronomer. Due north of Hipparchus is Rhaeticus, and here’s where things really get interesting. If the terminator has progressed far enough, you might spot tiny Blagg and Bruce to its west, the rough location of the Surveyor 4 and Surveyor 6 landing area. -
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, -
IAU Division C Working Group on Star Names 2019 Annual Report
IAU Division C Working Group on Star Names 2019 Annual Report Eric Mamajek (chair, USA) WG Members: Juan Antonio Belmote Avilés (Spain), Sze-leung Cheung (Thailand), Beatriz García (Argentina), Steven Gullberg (USA), Duane Hamacher (Australia), Susanne M. Hoffmann (Germany), Alejandro López (Argentina), Javier Mejuto (Honduras), Thierry Montmerle (France), Jay Pasachoff (USA), Ian Ridpath (UK), Clive Ruggles (UK), B.S. Shylaja (India), Robert van Gent (Netherlands), Hitoshi Yamaoka (Japan) WG Associates: Danielle Adams (USA), Yunli Shi (China), Doris Vickers (Austria) WGSN Website: https://www.iau.org/science/scientific_bodies/working_groups/280/ WGSN Email: [email protected] The Working Group on Star Names (WGSN) consists of an international group of astronomers with expertise in stellar astronomy, astronomical history, and cultural astronomy who research and catalog proper names for stars for use by the international astronomical community, and also to aid the recognition and preservation of intangible astronomical heritage. The Terms of Reference and membership for WG Star Names (WGSN) are provided at the IAU website: https://www.iau.org/science/scientific_bodies/working_groups/280/. WGSN was re-proposed to Division C and was approved in April 2019 as a functional WG whose scope extends beyond the normal 3-year cycle of IAU working groups. The WGSN was specifically called out on p. 22 of IAU Strategic Plan 2020-2030: “The IAU serves as the internationally recognised authority for assigning designations to celestial bodies and their surface features. To do so, the IAU has a number of Working Groups on various topics, most notably on the nomenclature of small bodies in the Solar System and planetary systems under Division F and on Star Names under Division C.” WGSN continues its long term activity of researching cultural astronomy literature for star names, and researching etymologies with the goal of adding this information to the WGSN’s online materials. -
The Fate of Planets
The Fate of Planets Eva Villaver Universidad Autónoma de Madrid, Dpto. Física Teórica, Módulo 15, Facultad de Ciencias, Campus de Cantoblanco, 28049 Madrid, Spain. e-mail: [email protected] Abstract. As a star evolves off the Main Sequence, it endures major structural changes that are capable of determining the fate of the planets orbiting it. Throughout its evolution along the Red Giant Branch, the star increases its radius by two orders of magnitude. Later, during the Asymptotic Giant Branch, it loses most of its initial mass. Finally, during the Planetary Nebulae phase, it emits intense radiation before ultimately beginning its fade as a white dwarf. We show how the several competing processes (stellar mass-loss, gravitational and frictional drag, tidal forces, planet accretion and evaporation) affect the survival of planets around evolved stars. Keywords: Planets, Evolved Stars, Giant and White Dwarf stars PACS: 97.82.j, 97.10.Me, 97.20.Li PLANET'S FATE BEYOND THE MAIN SEQUENCE The Red Giant Branch Phase Once the nuclear burning has been exhausted in the core, low- and intermediate mass stars evolve into the Red Giant Branch (RGB) phase. During the RGB, hydrogen burning continues in a shell outside the helium core, which now, devoid of energy sources, is contracting and heating up. The stellar evolution timescales (in the absence of significant mass loss) are set by the rate of consumption of the nuclear fuel. As the core contracts the envelope expands and cools. The stellar effective temperature decreases while the star’s radius and luminosity increase. There are several competing processes that affect the orbital distance between the star and the planet as the star evolves off the Main Sequence (MS): the changes in the mass of both the planet and the star (M˙p and M˙∗ respectively), the gravitational and frictional drag (Fg and Ff ), and the tidal force. -
CIRCULAR No. 170 (FEBRUARY 2010)
INTERNATIONAL ASTRONOMICAL UNION COMMISSION 26 (DOUBLE STARS) INFORMATION CIRCULAR No. 170 (FEBRUARY 2010) NEW ORBITS ADS Name P T e (2000) 2010 Author(s) ®2000± n a i ! Last ob. 2011 111 BU 391 AB 616y04 2095.68 0.103 81±75 259±0 100352 ZIRM 00094-2759 0±5925 100500 98±98 256±86 2006.940 258.9 1.346 - SEE3 406.00 1978.45 0.850 267.70 117.00 0.801 HARTKOPF 00098-3347 0.8871 1.119 41.7 77.6 2008.5490 117.70 0.814 & MASON - HDS 33 29.03 2018.12 0.378 177.0 132.0 0.189 CVETKOVIC 00143-2732 12.4010 0.251 59.8 73.9 2008.5432 141.6 0.199 - B 1024 1466. 1926.38 0.814 126.0 73.1 0.410 LING 00149-3209 0.2456 1.586 110.4 311.8 2008.5431 72.3 0.410 238 A1803AB 35.66 1950.70 0.002 124.10 306.00 0.179 HARTKOPF 00174+0853 10.0950 0.189 95.4 282.0 2008.7670 305.00 0.187 & MASON 281 BU1015 137.00 1961.65 0.557 291.20 103.80 0.483 HARTKOPF 00206+1219 2.6283 0.333 35.0 10.0 2008.8879 104.70 0.487 & MASON - HDS 56 28.05 1999.30 0.481 96.1 294.0 0.326 CVETKOVIC 00251+4803 12.8323 0.230 164.0 358.9 2007.8257 288.7 0.334 - B1909 11.35 1995.09 0.005 119.49 311.90 0.175 HARTKOPF 00284-2020 31.7093 0.202 69.8 99.0 2009.6710 334.80 0.109 & MASON 475 D2AB 2981.00 2007.00 0.923 266.00 42.80 0.067 HARTKOPF 00345-0433 0.1208 2.740 77.5 80.2 2009.7560 55.40 0.090 & MASON 520 BU395 25.02 1998.78 0.218 291.98 96.70 0.496 HARTKOPF 00373-2446 14.3905 0.675 78.6 318.1 2009.7560 101.00 0.596 & MASON - I440 196.00 2142.00 0.650 57.00 269.30 0.402 HARTKOPF 00427-6537 1.8350 0.274 157.0 344.0 2009.6710 268.70 0.405 & MASON 1 NEW ORBITS (continuation) ADS Name P T e (2000) 2010 Author(s) ®2000± n a i ! Last ob. -
Observational Cosmology - 30H Course 218.163.109.230 Et Al
Observational cosmology - 30h course 218.163.109.230 et al. (2004–2014) PDF generated using the open source mwlib toolkit. See http://code.pediapress.com/ for more information. PDF generated at: Thu, 31 Oct 2013 03:42:03 UTC Contents Articles Observational cosmology 1 Observations: expansion, nucleosynthesis, CMB 5 Redshift 5 Hubble's law 19 Metric expansion of space 29 Big Bang nucleosynthesis 41 Cosmic microwave background 47 Hot big bang model 58 Friedmann equations 58 Friedmann–Lemaître–Robertson–Walker metric 62 Distance measures (cosmology) 68 Observations: up to 10 Gpc/h 71 Observable universe 71 Structure formation 82 Galaxy formation and evolution 88 Quasar 93 Active galactic nucleus 99 Galaxy filament 106 Phenomenological model: LambdaCDM + MOND 111 Lambda-CDM model 111 Inflation (cosmology) 116 Modified Newtonian dynamics 129 Towards a physical model 137 Shape of the universe 137 Inhomogeneous cosmology 143 Back-reaction 144 References Article Sources and Contributors 145 Image Sources, Licenses and Contributors 148 Article Licenses License 150 Observational cosmology 1 Observational cosmology Observational cosmology is the study of the structure, the evolution and the origin of the universe through observation, using instruments such as telescopes and cosmic ray detectors. Early observations The science of physical cosmology as it is practiced today had its subject material defined in the years following the Shapley-Curtis debate when it was determined that the universe had a larger scale than the Milky Way galaxy. This was precipitated by observations that established the size and the dynamics of the cosmos that could be explained by Einstein's General Theory of Relativity. -
WASP-80B: a Gas Giant Transiting a Cool Dwarf⋆⋆⋆
A&A 551, A80 (2013) Astronomy DOI: 10.1051/0004-6361/201220900 & c ESO 2013 Astrophysics WASP-80b: a gas giant transiting a cool dwarf, A. H. M. J. Triaud1,D.R.Anderson2, A. Collier Cameron3,A.P.Doyle2,A.Fumel4, M. Gillon4, C. Hellier2, E. Jehin4, M. Lendl1,C.Lovis1,P.F.L.Maxted2,F.Pepe1, D. Pollacco5,D.Queloz1, D. Ségransan1,B.Smalley2, A. M. S. Smith2,6,S.Udry1,R.G.West7, and P. J. Wheatley5 1 Observatoire Astronomique de l’Université de Genève, Chemin des Maillettes 51, 1290 Sauverny, Switzerland e-mail: [email protected] 2 Astrophysics Group, Keele University, Staffordshire, ST55BG, UK 3 SUPA, School of Physics & Astronomy, University of St. Andrews, North Haugh, KY16 9SS, St. Andrews, Fife, Scotland, UK 4 Institut d’Astrophysique et de Géophysique, Université de Liège, Allée du 6 Août, 17, Bat. B5C, Liège 1, Belgium 5 Department of Physics, University of Warwick, Coventry CV4 7AL, UK 6 N. Copernicus Astronomical Centre, Polish Academy of Sciences, Bartycka 18, 00-716 Warsaw, Poland 7 Department of Physics and Astronomy, University of Leicester, Leicester, LE17RH, UK Received 13 December 2012 / Accepted 9 January 2013 ABSTRACT We report the discovery of a planet transiting the star WASP-80 (1SWASP J201240.26-020838.2; 2MASS J20124017-0208391; TYC 5165-481-1; BPM 80815; V = 11.9, K = 8.4). Our analysis shows this is a 0.55 ± 0.04 Mjup,0.95 ± 0.03 Rjup gas giant on a circular 3.07 day orbit around a star with a spectral type between K7V and M0V. -
Chemistry on Gliese 229B with Observed Abundance (Cf
Atmospheric Chemistry on Substellar Objects Channon Visscher Lunar and Planetary Institute, USRA UHCL Spring Seminar Series 2010 Image Credit: NASA/JPL-Caltech/R. Hurt Outline • introduction to substellar objects; recent discoveries – what can exoplanets tell us about the formation and evolution of planetary systems? • clouds and chemistry in substellar atmospheres – role of thermochemistry and disequilibrium processes • Jupiter’s bulk water inventory • chemical regimes on brown dwarfs and exoplanets • understanding the underlying physics and chemistry in substellar atmospheres is essential for guiding, interpreting, and explaining astronomical observations of these objects Methods of inquiry • telescopic observations (Hubble, Spitzer, Kepler, etc) • spacecraft exploration (Voyager, Galileo, Cassini, etc) • assume same physical principles apply throughout universe • allows the use of models to interpret observations A simple model; Ike vs. the Great Red Spot Field of study • stars: • sustained H fusion • spectral classes OBAFGKM • > 75 MJup (0.07 MSun) • substellar objects: • brown dwarfs (~750) • temporary D fusion • spectral classes L and T • 13 to 75 MJup • planets (~450) • no fusion • < 13 MJup Field of study • Sun (5800 K), M (3200-2300 K), L (2500-1400 K), T (1400-700 K), Jupiter (124 K) • upper atmospheres of substellar objects are cool enough for interesting chemistry! substellar objects Dr. Robert Hurt, Infrared Processing and Analysis Center Worlds without end… • prehistory: (Earth), Venus, Mars, Jupiter, Saturn • 1400 BC: Mercury -
Binocular Challenges
This page intentionally left blank Cosmic Challenge Listing more than 500 sky targets, both near and far, in 187 challenges, this observing guide will test novice astronomers and advanced veterans alike. Its unique mix of Solar System and deep-sky targets will have observers hunting for the Apollo lunar landing sites, searching for satellites orbiting the outermost planets, and exploring hundreds of star clusters, nebulae, distant galaxies, and quasars. Each target object is accompanied by a rating indicating how difficult the object is to find, an in-depth visual description, an illustration showing how the object realistically looks, and a detailed finder chart to help you find each challenge quickly and effectively. The guide introduces objects often overlooked in other observing guides and features targets visible in a variety of conditions, from the inner city to the dark countryside. Challenges are provided for viewing by the naked eye, through binoculars, to the largest backyard telescopes. Philip S. Harrington is the author of eight previous books for the amateur astronomer, including Touring the Universe through Binoculars, Star Ware, and Star Watch. He is also a contributing editor for Astronomy magazine, where he has authored the magazine’s monthly “Binocular Universe” column and “Phil Harrington’s Challenge Objects,” a quarterly online column on Astronomy.com. He is an Adjunct Professor at Dowling College and Suffolk County Community College, New York, where he teaches courses in stellar and planetary astronomy. Cosmic Challenge The Ultimate Observing List for Amateurs PHILIP S. HARRINGTON CAMBRIDGE UNIVERSITY PRESS Cambridge, New York, Melbourne, Madrid, Cape Town, Singapore, Sao˜ Paulo, Delhi, Dubai, Tokyo, Mexico City Cambridge University Press The Edinburgh Building, Cambridge CB2 8RU, UK Published in the United States of America by Cambridge University Press, New York www.cambridge.org Information on this title: www.cambridge.org/9780521899369 C P.