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Meridional Flow Velocities on Solar-Like Stars with Known Activity
Meridional flow velocities on solar-like stars with known activity cycles Dilyara Baklanova∗ Crimean Astrophysical Observatory, Nauchny 298409, Crimea Sergei Plachinda Crimean Astrophysical Observatory, Nauchny 298409, Crimea Abstract The direct measurements of the meridional flow velocities on stars are impossible today. To evaluate the meridional flow velocities on solar-like stars with stable activity periods, we supposed that during the stellar Hale cycle the matter on surfaces of stars passes the meridional way equivalent to 2πR⋆. We present here the dependence of the mean meridional flow velocity on Rossby number, which is an effective parameter of the stellar magnetic dynamo. Keywords: stars: solar-like; stars: activity; stars: Hale cycle; stars: meridional flow velocity 1. Introduction 2. Parameters of stars Today the physics of the large-scale flows on the Sun We selected stars with well-known activity periods. In and stars are intensively simulated by scientists to deter- the Table 1 and Table 2 we summarized the physical pa- mine the detailed mechanisms of activity cycles. Recent rameters of the stars that we have got from literature. results and bibliography are presented, for example, in the The names of the stars are listed in the first columns of papers by Upton and Hathaway (2014), Zhao et al. (2013), the Tables. Columns 2-4 in the Table 1 contain magnitude Guerrero et al. (2013), Moss et al. (2013), Kitchatinov V , spectral type and color index B − V . The rotation (2013), Kitchatinov and Olemskoy (2012). periods of the stars and the references are given in the 5th The empirical dependence of the mean meridional flow and 6th columns, the duration of activity cycles and the speed on the number of the 22-year Hale cycle (Plachinda references are given in the 7th and 8th columns. -
Laboratory Astrophysics Is the Rosetta Stone That Symposium Enables Astronomers to Understand and Interpret the Distant Cosmos
IAU Symposium IAU IAU Symposium Proceedings of the International Astronomical Union Laboratory astrophysics is the Rosetta Stone that Symposium enables astronomers to understand and interpret the distant cosmos. It provides the tools to interpret and 350 guide astronomical observations and delivers the numbers needed to quantitatively model the processes 350 taking place in space, providing a bridge between 350 Laboratory 14-19 April 2019 observers and modelers. IAU Symposium 350 was 14-19 April 2019 Cambridge, United Kingdom organized by the International Astronomical Union's Cambridge, United Kingdom Laboratory Astrophysics Commission (B5), and was the Interpretation Observations to From Astrophysics: rst topical symposium on laboratory astrophysics Laboratory sponsored by the IAU. Active researchers in observational astronomy, space missions, experimental From Observations Astrophysics: and theoretical laboratory astrophysics, and Laboratory Astrophysics: From Observations astrochemistry discuss the topics and challenges facing astronomy today. Five major topics are covered, to Interpretation to Interpretation spanning from star- and planet-formation through stellar populations to extragalactic chemistry and dark matter. Within each topic, the main themes of laboratory studies, astronomical observations, and theoretical modeling are explored, demonstrating the breadth and the plurality of disciplines engaged in the growing eld of laboratory astrophysics. Edited by Proceedings of the International Astronomical Union Salama and Linnartz Farid Salama Editor in Chief: Professor Maria Teresa Lago This series contains the proceedings of major scienti c Harold Linnartz meetings held by the International Astronomical Union. Each volume contains a series of articles on a topic of current interest in astronomy, giving a timely overview of research in the eld. With contributions by leading scientists, these books are at a level suitable for research astronomers and graduate students. -
RADIAL VELOCITIES in the ZODIACAL DUST CLOUD
A SURVEY OF RADIAL VELOCITIES in the ZODIACAL DUST CLOUD Brian Harold May Astrophysics Group Department of Physics Imperial College London Thesis submitted for the Degree of Doctor of Philosophy to Imperial College of Science, Technology and Medicine London · 2007 · 2 Abstract This thesis documents the building of a pressure-scanned Fabry-Perot Spectrometer, equipped with a photomultiplier and pulse-counting electronics, and its deployment at the Observatorio del Teide at Izaña in Tenerife, at an altitude of 7,700 feet (2567 m), for the purpose of recording high-resolution spectra of the Zodiacal Light. The aim was to achieve the first systematic mapping of the MgI absorption line in the Night Sky, as a function of position in heliocentric coordinates, covering especially the plane of the ecliptic, for a wide variety of elongations from the Sun. More than 250 scans of both morning and evening Zodiacal Light were obtained, in two observing periods – September-October 1971, and April 1972. The scans, as expected, showed profiles modified by components variously Doppler-shifted with respect to the unshifted shape seen in daylight. Unexpectedly, MgI emission was also discovered. These observations covered for the first time a span of elongations from 25º East, through 180º (the Gegenschein), to 27º West, and recorded average shifts of up to six tenths of an angstrom, corresponding to a maximum radial velocity relative to the Earth of about 40 km/s. The set of spectra obtained is in this thesis compared with predictions made from a number of different models of a dust cloud, assuming various distributions of dust density as a function of position and particle size, and differing assumptions about their speed and direction. -
Panoptes, a Project Building Tool for Citizen Science
Panoptes, a Project Building Tool for Citizen Science Alex Bowyer Chris Lintott Greg Hines Campbell Allen Ed Paget [email protected] [email protected] [email protected] [email protected] [email protected] Zooniverse / Zooniverse / Zooniverse / Zooniverse / Zooniverse / University of Oxford University of Oxford University of Oxford University of Oxford Adler Planetarium Abstract and supporting projects from ecology to planetary science2. An early test project, Snapshot Supernova(Campbell and et. We will demonstrate the newly deployed Panoptes sys- al. 2015), showed that the system was able to cope with large tem for building citizen science projects which involve spikes in traffic, receiving more than a million classifications the public in the crowdsourced analysis of images. Panoptes supports projects built by the Zooniverse, the in under twenty minutes. world’s most successful collection of such projects, and Unlike previous crowdsourcing platforms, Panoptes pro- allows end users - typically scientists and researchers duces more than a list of raw classifications for project sci- with large data sets - to construct advanced classifica- entists. Standard algorithms (e.g (Hines and et. al. 2015)) ag- tion workflows using simple, browser based tools. A gregate individual users’ input into combined results. These particular strength of Panoptes is its ability to support algorithms can be used to implement complex retirement complex retirement and aggregation tools and proce- rules and task assignment, increasing the efficiency of clas- dures, as well as a mechanism for sending notifications sification. As an example of this kind of more advanced task to users as they classify. It thus provides a valuable 3 testbed for those wishing to build their own projects for assignment, we have integrated the SWAPR code devel- the purposes of investigating the behaviour of human- oped by the SpaceWarps ((et. -
Wiyn Consortium, Inc. 950 N
WIYN CONSORTIUM, INC. 950 N. Cherry Avenue • P. O. Box 26732 Tucson, AZ 85726-6732 (520) 318-8396 University of Wisconsin • Indiana University • Yale University • National Optical Astronomy Observatory January 30, 2012 To: NSF Portfolio Review Committee Dear Colleagues: The three member universities of the WIYN consortium strongly recommend continuing NSF investment in WIYN through the US OIR national observatory, NOAO. The WIYN partnership among state and private universities and NSF/NOAO has produced a state-of-the-art facility with highly productive yet cost-effective operations. Our most recent external review accurately summarizes the state of the Observatory. The review found that: • WIYN delivers the best images over a wide field-of-view of any continental US facility. • Operations have achieved an outstanding level of reliability and efficiency. • WIYN has had a major impact on the research opportunities available to member universities, involving a broad base of faculty and providing important career development paths for younger faculty and postdocs. • The number of Ph.D. dissertations making important use of the facility is especially impressive. For the astronomy departments of the university partners, WIYN is the largest source of experimental data for doctoral theses. • WIYN has served national interests by 1) providing a proving ground for technological innovations; 2) enabling access to wide-field multi-object spectroscopy for the US astronomical community; and 3) providing substantial aperture very cost-effectively. We believe that few, if any, of the successes of the WIYN Observatory would have been possible without the major contributions of NOAO to our partnership. This letter attempts to document the current and future importance of NOAO as a partner in the WIYN collaboration. -
Characterization of the Gaseous Companion Κ Andromedae B⋆
UvA-DARE (Digital Academic Repository) Characterization of the gaseous companion κ Andromedae b. New Keck and LBTI high-contrast observations Bonnefoy, M.; et al., [Unknown]; Thalmann, C. DOI 10.1051/0004-6361/201322119 Publication date 2014 Document Version Final published version Published in Astronomy & Astrophysics Link to publication Citation for published version (APA): Bonnefoy, M., et al., U., & Thalmann, C. (2014). Characterization of the gaseous companion κ Andromedae b. New Keck and LBTI high-contrast observations. Astronomy & Astrophysics, 562, A111. https://doi.org/10.1051/0004-6361/201322119 General rights It is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), other than for strictly personal, individual use, unless the work is under an open content license (like Creative Commons). Disclaimer/Complaints regulations If you believe that digital publication of certain material infringes any of your rights or (privacy) interests, please let the Library know, stating your reasons. In case of a legitimate complaint, the Library will make the material inaccessible and/or remove it from the website. Please Ask the Library: https://uba.uva.nl/en/contact, or a letter to: Library of the University of Amsterdam, Secretariat, Singel 425, 1012 WP Amsterdam, The Netherlands. You will be contacted as soon as possible. UvA-DARE is a service provided by the library of the University of Amsterdam (https://dare.uva.nl) Download date:23 Sep 2021 A&A 562, A111 (2014) Astronomy DOI: 10.1051/0004-6361/201322119 & c ESO 2014 Astrophysics Characterization of the gaseous companion κ Andromedae b? New Keck and LBTI high-contrast observations?? M. -
KEPLER-21B: a 1.6 Rearth PLANET TRANSITING the BRIGHT OSCILLATING F SUBGIANT STAR HD 179070 Steve B
The Astrophysical Journal, 746:123 (18pp), 2012 February 20 doi:10.1088/0004-637X/746/2/123 C 2012. The American Astronomical Society. All rights reserved. Printed in the U.S.A. ∗ KEPLER-21b: A 1.6 REarth PLANET TRANSITING THE BRIGHT OSCILLATING F SUBGIANT STAR HD 179070 Steve B. Howell1,2,36, Jason F. Rowe2,3,36, Stephen T. Bryson2, Samuel N. Quinn4, Geoffrey W. Marcy5, Howard Isaacson5, David R. Ciardi6, William J. Chaplin7, Travis S. Metcalfe8, Mario J. P. F. G. Monteiro9, Thierry Appourchaux10, Sarbani Basu11, Orlagh L. Creevey12,13, Ronald L. Gilliland14, Pierre-Olivier Quirion15, Denis Stello16, Hans Kjeldsen17,Jorgen¨ Christensen-Dalsgaard17, Yvonne Elsworth7, Rafael A. Garc´ıa18, Gunter¨ Houdek19, Christoffer Karoff7, Joanna Molenda-Zakowicz˙ 20, Michael J. Thompson8, Graham A. Verner7,21, Guillermo Torres4, Francois Fressin4, Justin R. Crepp23, Elisabeth Adams4, Andrea Dupree4, Dimitar D. Sasselov4, Courtney D. Dressing4, William J. Borucki2, David G. Koch2, Jack J. Lissauer2, David W. Latham4, Lars A. Buchhave22,35, Thomas N. Gautier III24, Mark Everett1, Elliott Horch25, Natalie M. Batalha26, Edward W. Dunham27, Paula Szkody28,36, David R. Silva1,36, Ken Mighell1,36, Jay Holberg29,36,Jeromeˆ Ballot30, Timothy R. Bedding16, Hans Bruntt12, Tiago L. Campante9,17, Rasmus Handberg17, Saskia Hekker7, Daniel Huber16, Savita Mathur8, Benoit Mosser31, Clara Regulo´ 12,13, Timothy R. White16, Jessie L. Christiansen3, Christopher K. Middour32, Michael R. Haas2, Jennifer R. Hall32,JonM.Jenkins3, Sean McCaulif32, Michael N. Fanelli33, Craig -
THE CASE of the HERBIG F STAR SAO 206462 (HD 135344B)A,B,C,D,E,F
The Astrophysical Journal, 699:1822–1842, 2009 July 10 doi:10.1088/0004-637X/699/2/1822 C 2009. The American Astronomical Society. All rights reserved. Printed in the U.S.A. REVEALING THE STRUCTURE OF A PRE-TRANSITIONAL DISK: THE CASE OF THE HERBIG F STAR SAO 206462 (HD 135344B)a,b,c,d,e,f C. A. Grady1,2,3, G. Schneider4,M.L.Sitko5,6,19, G. M. Williger7,8,9, K. Hamaguchi10,11,3, S. D. Brittain12, K. Ablordeppey6,D.Apai4, L. Beerman6, W. J. Carpenter6, K. A. Collins7,20, M. Fukagawa13,H.B.Hammel5,19, Th. Henning14,D.Hines5,R.Kimes6,D.K.Lynch15,19,F.Menard´ 16, R. Pearson15,19,R.W.Russell15,19, M. Silverstone1, P. S. Smith4, M. Troutman12,21,D.Wilner17, B. Woodgate18,3, and M. Clampin18 1 Eureka Scientific, 2452 Delmer, Suite 100, Oakland, CA 96002, USA 2 ExoPlanets and Stellar Astrophysics Laboratory, Code 667, Goddard Space Flight Center, Greenbelt, MD 20771, USA 3 Goddard Center for Astrobiology, NASA Goddard Space Flight Center, Greenbelt, MD, USA 4 Steward Observatory, The University of Arizona, Tucson, AZ 85721, USA 5 Space Science Institute, 4750 Walnut Street, Suite 205, Boulder, CO 80301, USA 6 Department of Physics, University of Cincinnati, Cincinnati, OH 45221-0011, USA 7 Department of Physics, University of Louisville, Louisville, KY 40292, USA 8 Department of Physics and Astronomy, John Hopkins University, Baltimore, MD 21218-2686, USA 9 Department of Physics, The Catholic University of America, Washington, DC 20064, USA 10 CRESST, X-Ray Astrophysics Laboratory, NASA/GSFC, Greenbelt, MD 20771, USA 11 Department of Physics, University -
A Tail Structure Associated with Protoplanetary Disk Around SU
Draft version February 28, 2019 A Preprint typeset using LTEX style emulateapj v. 12/16/11 A TAIL STRUCTURE ASSOCIATED WITH PROTOPLANETARY DISK AROUND SU AURIGAE EIJI AKIYAMA1, EDUARD I. VOROBYOV2,3, HAUYU BAOBABU LIU4,5, RUOBING DONG5,6, JEROME de LEON7, SHENG-YUAN LIU5, MOTOHIDE TAMURA7,8,9 1Institute for the Advancement of Higher Education, Hokkaido University, Kita17, Nishi8, Kita-ku, Sapporo, 060-0817, Japan; [email protected] 2Department of Astrophysics, University of Vienna, Vienna 1018, Austria 3Research Institute of Physics, Southern Federal University, Rostov-on-Don, 344090, Russia 4European Southern Observatory, Karl Schwarzschild Str 2, 85748 Garching bei M¨unchen, Germany 5Institute of Astronomy and Astrophysics, Academia Sinica, P.O. Box 23-141, Taipei, 10617, Taiwan 6Department of Astronomy/Steward Observatory, The University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA 7Department of Astronomy, The University of Tokyo, 7-3-1, Hongo, Bunkyo-ku, Tokyo, 113-0033, Japan 8Astrobiology Center of NINS, 2-21-1, Osawa, Mitaka, Tokyo, 181-8588, Japan 9National Astronomical Observatory of Japan, 2-21-1, Osawa, Mitaka, Tokyo, 181-8588, Japan Draft version February 28, 2019 ABSTRACT We present Atacama Large Millimeter/submillimeter Array (ALMA) observations of the CO (J=2– 1) line emission from the protoplanetary disk around T-Tauri star SU Aurigae (hereafter SU Aur). Previous observations in optical and near infrared wavelengths find a unique structure in SU Aur. One of the highlights of the observational results is that an extended tail-like structure is associated with the disk, indicating mass transfer from or into the disk. -
The 3-Dimensional Architecture of the Upsilon Andromedae Planetary System
Draft version August 14, 2018 Preprint typeset using LATEX style emulateapj v. 04/17/13 THE 3-DIMENSIONAL ARCHITECTURE OF THE υ ANDROMEDAE PLANETARY SYSTEM Russell Deitrick Department of Astronomy, University of Washington, Seattle, WA 98195-1580, USA Rory Barnes Department of Astronomy, University of Washington, Seattle, WA 98195-1580, USA Barbara McArthur Department of Astronomy, University of Texas at Austin, TX 78712, USA Thomas R. Quinn Department of Astronomy, University of Washington, Seattle, WA 98195-1580, USA Rodrigo Luger Department of Astronomy, University of Washington, Seattle, WA 98195-1580, USA Adrienne Antonsen Department of Astronomy, University of Washington, Seattle, WA 98195-1580, USA and G. Fritz Benedict Department of Astronomy, University of Texas at Austin, TX 78712, USA (Dated:) Draft version August 14, 2018 ABSTRACT The Upsilon Andromedae system is the first exoplanetary system to have the relative inclination of two planets' orbital planes directly measured, and therefore offers our first window into the 3- dimensional configurations of planetary systems. We present, for the first time, full 3-dimensional, dynamically stable configurations for the 3 planets of the system consistent with all observational constraints. While the outer 2 planets, c and d, are inclined by ∼ 30◦, the inner planet's orbital plane has not been detected. We use N-body simulations to search for stable 3-planet configurations that are consistent with the combined radial velocity and astrometric solution. We find that only 10 trials out of 1000 are robustly stable on 100 Myr timescales, or ∼ 8 billion orbits of planet b. Planet b's orbit must lie near the invariable plane of planets c and d, but can be either prograde or retrograde. -
Nd AAS Meeting Abstracts
nd AAS Meeting Abstracts 101 – Kavli Foundation Lectureship: The Outreach Kepler Mission: Exoplanets and Astrophysics Search for Habitable Worlds 200 – SPD Harvey Prize Lecture: Modeling 301 – Bridging Laboratory and Astrophysics: 102 – Bridging Laboratory and Astrophysics: Solar Eruptions: Where Do We Stand? Planetary Atoms 201 – Astronomy Education & Public 302 – Extrasolar Planets & Tools 103 – Cosmology and Associated Topics Outreach 303 – Outer Limits of the Milky Way III: 104 – University of Arizona Astronomy Club 202 – Bridging Laboratory and Astrophysics: Mapping Galactic Structure in Stars and Dust 105 – WIYN Observatory - Building on the Dust and Ices 304 – Stars, Cool Dwarfs, and Brown Dwarfs Past, Looking to the Future: Groundbreaking 203 – Outer Limits of the Milky Way I: 305 – Recent Advances in Our Understanding Science and Education Overview and Theories of Galactic Structure of Star Formation 106 – SPD Hale Prize Lecture: Twisting and 204 – WIYN Observatory - Building on the 308 – Bridging Laboratory and Astrophysics: Writhing with George Ellery Hale Past, Looking to the Future: Partnerships Nuclear 108 – Astronomy Education: Where Are We 205 – The Atacama Large 309 – Galaxies and AGN II Now and Where Are We Going? Millimeter/submillimeter Array: A New 310 – Young Stellar Objects, Star Formation 109 – Bridging Laboratory and Astrophysics: Window on the Universe and Star Clusters Molecules 208 – Galaxies and AGN I 311 – Curiosity on Mars: The Latest Results 110 – Interstellar Medium, Dust, Etc. 209 – Supernovae and Neutron -
Thesis, Anton Pannekoek Institute, Universiteit Van Amsterdam
UvA-DARE (Digital Academic Repository) The peculiar climates of ultra-hot Jupiters Arcangeli, J. Publication date 2020 Document Version Final published version License Other Link to publication Citation for published version (APA): Arcangeli, J. (2020). The peculiar climates of ultra-hot Jupiters. General rights It is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), other than for strictly personal, individual use, unless the work is under an open content license (like Creative Commons). Disclaimer/Complaints regulations If you believe that digital publication of certain material infringes any of your rights or (privacy) interests, please let the Library know, stating your reasons. In case of a legitimate complaint, the Library will make the material inaccessible and/or remove it from the website. Please Ask the Library: https://uba.uva.nl/en/contact, or a letter to: Library of the University of Amsterdam, Secretariat, Singel 425, 1012 WP Amsterdam, The Netherlands. You will be contacted as soon as possible. UvA-DARE is a service provided by the library of the University of Amsterdam (https://dare.uva.nl) Download date:09 Oct 2021 Jacob Arcangeli of Ultra-hot Jupiters The peculiar climates The peculiar climates of Ultra-hot Jupiters Jacob Arcangeli The peculiar climates of Ultra-hot Jupiters Jacob Arcangeli © 2020, Jacob Arcangeli Contact: [email protected] The peculiar climates of Ultra-hot Jupiters Thesis, Anton Pannekoek Institute, Universiteit van Amsterdam Cover by Imogen Arcangeli ([email protected]) Printed by Amsterdam University Press ANTON PANNEKOEK INSTITUTE The research included in this thesis was carried out at the Anton Pannekoek Institute for Astronomy (API) of the University of Amsterdam.