Models for Sixty Double-Lined Binaries Containing Giants
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Arxiv:2006.10868V2 [Astro-Ph.SR] 9 Apr 2021 Spain and Institut D’Estudis Espacials De Catalunya (IEEC), C/Gran Capit`A2-4, E-08034 2 Serenelli, Weiss, Aerts Et Al
Noname manuscript No. (will be inserted by the editor) Weighing stars from birth to death: mass determination methods across the HRD Aldo Serenelli · Achim Weiss · Conny Aerts · George C. Angelou · David Baroch · Nate Bastian · Paul G. Beck · Maria Bergemann · Joachim M. Bestenlehner · Ian Czekala · Nancy Elias-Rosa · Ana Escorza · Vincent Van Eylen · Diane K. Feuillet · Davide Gandolfi · Mark Gieles · L´eoGirardi · Yveline Lebreton · Nicolas Lodieu · Marie Martig · Marcelo M. Miller Bertolami · Joey S.G. Mombarg · Juan Carlos Morales · Andr´esMoya · Benard Nsamba · KreˇsimirPavlovski · May G. Pedersen · Ignasi Ribas · Fabian R.N. Schneider · Victor Silva Aguirre · Keivan G. Stassun · Eline Tolstoy · Pier-Emmanuel Tremblay · Konstanze Zwintz Received: date / Accepted: date A. Serenelli Institute of Space Sciences (ICE, CSIC), Carrer de Can Magrans S/N, Bellaterra, E- 08193, Spain and Institut d'Estudis Espacials de Catalunya (IEEC), Carrer Gran Capita 2, Barcelona, E-08034, Spain E-mail: [email protected] A. Weiss Max Planck Institute for Astrophysics, Karl Schwarzschild Str. 1, Garching bei M¨unchen, D-85741, Germany C. Aerts Institute of Astronomy, Department of Physics & Astronomy, KU Leuven, Celestijnenlaan 200 D, 3001 Leuven, Belgium and Department of Astrophysics, IMAPP, Radboud University Nijmegen, Heyendaalseweg 135, 6525 AJ Nijmegen, the Netherlands G.C. Angelou Max Planck Institute for Astrophysics, Karl Schwarzschild Str. 1, Garching bei M¨unchen, D-85741, Germany D. Baroch J. C. Morales I. Ribas Institute of· Space Sciences· (ICE, CSIC), Carrer de Can Magrans S/N, Bellaterra, E-08193, arXiv:2006.10868v2 [astro-ph.SR] 9 Apr 2021 Spain and Institut d'Estudis Espacials de Catalunya (IEEC), C/Gran Capit`a2-4, E-08034 2 Serenelli, Weiss, Aerts et al. -
Orbits and Pulsations of the Classical Aurigae Binaries
The Astrophysical Journal, 679:1490Y1498, 2008 June 1 A # 2008. The American Astronomical Society. All rights reserved. Printed in U.S.A. ORBITS AND PULSATIONS OF THE CLASSICAL AURIGAE BINARIES Joel A. Eaton,1 Gregory W. Henry,1 and Andrew P. Odell2 Received 2007 October 12; accepted 2008 January 23 ABSTRACT We have derived new orbits for Aur, 32 Cyg, and 31 Cyg with observations from the Tennessee State University (TSU) Automatic Spectroscopic Telescope, and used them to identify nonorbital velocities of the cool supergiant components of these systems. We measure periods in those deviations, identify unexpected long-period changes in the radial velocities, and place upper limits on the rotation of these stars. These radial-velocity variations are not obviously consistent with radial pulsation theory, given what we know about the masses and sizes of the components. Our concurrent photometry detected the nonradial pulsations driven by tides (ellipsoidal variation) in both Aur and 32 Cyg, at a level and phasing roughly consistent with simple theory to first order, although they seem to require moderately large gravity darkening. However, the K component of 32 Cyg must be considerably bigger than ex- pected, or have larger gravity darkening than Aur, to fit its amplitude. However, again there is precious little evi- dence for the normal radial pulsation of cool stars in our photometry. H shows some evidence for chromospheric heating by the B component in both Aur and 32 Cyg, and the three stars show among them a meager 2Y3 outbursts in their winds of the sort seen occasionally in cool supergiants. -
The HARPS Search for Southern Extra-Solar Planets. XXXI. Magnetic
Astronomy & Astrophysics manuscript no. magnetic˙cycles c ESO 2011 July 28, 2011 The HARPS search for southern extra-solar planets⋆ XXXI. Magnetic activity cycles in solar-type stars: statistics and impact on precise radial velocities C. Lovis1, X. Dumusque1,2, N. C. Santos2,3,1, F. Bouchy4,5, M. Mayor1, F. Pepe1, D. Queloz1, D. S´egransan1, and S. Udry1 1 Observatoire de Gen`eve, Universit´ede Gen`eve, 51 ch. des Maillettes, CH-1290 Versoix, Switzerland e-mail: [email protected] 2 Centro de Astrof´ısica, Universidade do Porto, Rua das Estrelas, P4150-762 Porto, Portugal 3 Departamento de F´ısica e Astronomia, Faculdade de Ciˆencias, Universidade do Porto, Portugal 4 Institut d’Astrophysique de Paris, UMR7095 CNRS, Universit´ePierre & Marie Curie, 98bis Bd Arago, F-75014 Paris, France 5 Observatoire de Haute-Provence, CNRS/OAMP, F-04870 St. Michel l’Observatoire, France Received 26 July 2011 / Accepted ... ABSTRACT Context. Searching for extrasolar planets through radial velocity measurements relies on the stability of stellar photospheres. Several phenomena are known to affect line profiles in solar-type stars, among which stellar oscillations, granulation and magnetic activity through spots, plages and activity cycles. Aims. We aim at characterizing the statistical properties of magnetic activity cycles, and studying their impact on spectroscopic measurements such as radial velocities, line bisectors and line shapes. Methods. We use data from the HARPS high-precision planet-search sample comprising 304 FGK stars followed over about 7 ′ years. We obtain high-precision Ca II H&K chromospheric activity measurements and convert them to RHK indices using an updated ′ calibration taking into account stellar metallicity. -
The Minor Planet Bulletin, Alan W
THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 42, NUMBER 2, A.D. 2015 APRIL-JUNE 89. ASTEROID LIGHTCURVE ANALYSIS AT THE OAKLEY SOUTHERN SKY OBSERVATORY: 2014 SEPTEMBER Lucas Bohn, Brianna Hibbler, Gregory Stein, Richard Ditteon Rose-Hulman Institute of Technology, CM 171 5500 Wabash Avenue, Terre Haute, IN 47803, USA [email protected] (Received: 24 November) Photometric data were collected over the course of seven nights in 2014 September for eight asteroids: 1334 Lundmarka, 1904 Massevitch, 2571 Geisei, 2699 Kalinin, 3197 Weissman, 7837 Mutsumi, 14927 Satoshi, and (29769) 1999 CE28. Eight asteroids were remotely observed from the Oakley Southern Sky Observatory in New South Wales, Australia. The observations were made on 2014 September 12-14, 16-19 using a 0.50-m f/8.3 Ritchey-Chretien optical tube assembly on a Paramount ME mount and SBIG STX-16803 CCD camera, binned 3x3, with a luminance filter. Exposure times ranged from 90 to 180 sec depending on the magnitude of the target. The resulting image scale was 1.34 arcseconds per pixel. Raw images were processed in MaxIm DL 6 using twilight flats, bias, and dark frames. MPO Canopus was used to measure the processed images and produce lightcurves. In order to maximize the potential for data collection, target asteroids were selected based upon their position in the sky approximately one hour after sunset. Only asteroids with no previously published results were targeted. Lightcurves were produced for 1334 Lundmarka, 1904 Massevitch, 2571 Geisei, 3197 Weissman, and (29769) 1999 CE28. -
Index to JRASC Volumes 61-90 (PDF)
THE ROYAL ASTRONOMICAL SOCIETY OF CANADA GENERAL INDEX to the JOURNAL 1967–1996 Volumes 61 to 90 inclusive (including the NATIONAL NEWSLETTER, NATIONAL NEWSLETTER/BULLETIN, and BULLETIN) Compiled by Beverly Miskolczi and David Turner* * Editor of the Journal 1994–2000 Layout and Production by David Lane Published by and Copyright 2002 by The Royal Astronomical Society of Canada 136 Dupont Street Toronto, Ontario, M5R 1V2 Canada www.rasc.ca — [email protected] Table of Contents Preface ....................................................................................2 Volume Number Reference ...................................................3 Subject Index Reference ........................................................4 Subject Index ..........................................................................7 Author Index ..................................................................... 121 Abstracts of Papers Presented at Annual Meetings of the National Committee for Canada of the I.A.U. (1967–1970) and Canadian Astronomical Society (1971–1996) .......................................................................168 Abstracts of Papers Presented at the Annual General Assembly of the Royal Astronomical Society of Canada (1969–1996) ...........................................................207 JRASC Index (1967-1996) Page 1 PREFACE The last cumulative Index to the Journal, published in 1971, was compiled by Ruth J. Northcott and assembled for publication by Helen Sawyer Hogg. It included all articles published in the Journal during the interval 1932–1966, Volumes 26–60. In the intervening years the Journal has undergone a variety of changes. In 1970 the National Newsletter was published along with the Journal, being bound with the regular pages of the Journal. In 1978 the National Newsletter was physically separated but still included with the Journal, and in 1989 it became simply the Newsletter/Bulletin and in 1991 the Bulletin. That continued until the eventual merger of the two publications into the new Journal in 1997. -
The Structures and Extents of the Chromospheres of Late-Type Stars
The Structures and Extents of the Chromospheres of Late-type Stars A dissertation submitted to the University of Dublin for the degree of Doctor of Philosophy Neal O´ Riain Trinity College Dublin, September 2015 School of Physics University of Dublin Trinity College Declaration I declare that this thesis has not been submitted as an exercise for a degree at this or any other university and it is entirely my own work. I agree to deposit this thesis in the University's open access institu- tional repository or allow the library to do so on my behalf, subject to Irish Copyright Legislation and Trinity College Library conditions of use and acknowledgement. Name: Neal O´ Riain Signature: ........................................ Date: .......................... Summary The chromosphere is the region of a star, above what is traditionally defined as the stellar surface, from which photons freely escape. As the definition implies, this region is characterised by complexity, non- equilibrium, and specifying its structure is a vastly non-linear, non- local problem. In this work we are concerned with the chromospheres of late-type stars, objects of spectral type K to M, the thermodynamic structure, extent, and heating mechanisms of whose chromospheres are not well understood. We use a number of observational and computa- tional methods in order to gain a detailed quantitative understanding of these chromospheres. We construct a model to compute the mm, thermal bremsstrahlung flux from the chromospheres of late-type objects, based on a number of simplifying assumptions concerning their thermodynamic structure. We compare this model with archival and recent observations, and find that the model is capable of reproducing the observed flux from objects of spectral type K to mid-M in the frequency range 100 GHz { 350 GHz. -
Arxiv:1108.4369V1
THE ASTROPHYSICAL JOURNAL, 2011, IN PRESS Preprint typeset using LATEX style emulateapj v. 03/07/07 TESTING A PREDICTIVE THEORETICAL MODEL FOR THE MASS LOSS RATES OF COOL STARS STEVEN R. CRANMER AND STEVEN H. SAAR Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 Draft version February 7, 2018 ABSTRACT The basic mechanisms responsible for producing winds from cool, late-type stars are still largely unknown. We take inspiration from recent progress in understanding solar wind acceleration to develop a physically motivated model of the time-steady mass loss rates of cool main-sequence stars and evolved giants. This model follows the energy flux of magnetohydrodynamic turbulence from a subsurface convection zone to its eventual dissipation and escape through open magnetic flux tubes. We show how Alfvén waves and turbulence can produce winds in either a hot corona or a cool extended chromosphere, and we specify the conditions that determine whether or not coronal heating occurs. These models do not utilize arbitrary normalization factors, but instead predict the mass loss rate directly from a star’s fundamental properties. We take account of stellar magnetic activity by extending standard age-activity-rotation indicators to include the evolution of the filling factor of strong photospheric magnetic fields. We compared the predicted mass loss rates with observed values for 47 stars and found significantly better agreement than was obtained from the popular scaling laws of Reimers, Schröder, and Cuntz. The algorithm used to compute cool-star mass loss rates is provided as a self-contained and efficient computer code. We anticipate that the results from this kind of model can be incorporated straightforwardly into stellar evolution calculations and population synthesis techniques. -
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Theory of Stellar Atmospheres
© Copyright, Princeton University Press. No part of this book may be distributed, posted, or reproduced in any form by digital or mechanical means without prior written permission of the publisher. EXTENDED BIBLIOGRAPHY References [1] D. Abbott. The terminal velocities of stellar winds from early{type stars. Astrophys. J., 225, 893, 1978. [2] D. Abbott. The theory of radiatively driven stellar winds. I. A physical interpretation. Astrophys. J., 242, 1183, 1980. [3] D. Abbott. The theory of radiatively driven stellar winds. II. The line acceleration. Astrophys. J., 259, 282, 1982. [4] D. Abbott. The theory of radiation driven stellar winds and the Wolf{ Rayet phenomenon. In de Loore and Willis [938], page 185. Astrophys. J., 259, 282, 1982. [5] D. Abbott. Current problems of line formation in early{type stars. In Beckman and Crivellari [358], page 279. [6] D. Abbott and P. Conti. Wolf{Rayet stars. Ann. Rev. Astr. Astrophys., 25, 113, 1987. [7] D. Abbott and D. Hummer. Photospheres of hot stars. I. Wind blan- keted model atmospheres. Astrophys. J., 294, 286, 1985. [8] D. Abbott and L. Lucy. Multiline transfer and the dynamics of stellar winds. Astrophys. J., 288, 679, 1985. [9] D. Abbott, C. Telesco, and S. Wolff. 2 to 20 micron observations of mass loss from early{type stars. Astrophys. J., 279, 225, 1984. [10] C. Abia, B. Rebolo, J. Beckman, and L. Crivellari. Abundances of light metals and N I in a sample of disc stars. Astr. Astrophys., 206, 100, 1988. [11] M. Abramowitz and I. Stegun. Handbook of Mathematical Functions. (Washington, DC: U.S. Government Printing Office), 1972. -
International Astronomical Union Commission 42 BIBLIOGRAPHY
International Astronomical Union Commission 42 BIBLIOGRAPHY OF CLOSE BINARIES No. 74 Editor-in-Chief: C.D. Scarfe Editors: H. Drechsel D.R. Faulkner V.G. Karetnikov E. Lapasset C. Maceroni Y. Nakamura P.G. Niarchos R.G. Samec W. Van Hamme M. Wolf Material published by March 15, 2002 BCB issues are available via URL: http://www.sternwarte.uni-erlangen.de/ftp/bcb or via anonymous ftp from: ftp://www.sternwarte.uni-erlangen.de/pub/bcb This issue is also available via URL: http://www.astro.washington.edu/szkody/c42/ The bibliographical entries for Individual Stars and Collections of Data are categorized according to the following coding scheme: 1. Observational data a. Photometry b. Spectroscopy c. Spectrophotometry d. Polarimetry e. Astrometry, interferometry f. Times of minima g. γ-ray data i. Infrared data o. Optical data p. Photographic data r. Radio data u. Ultraviolet data v. Visual estimates x. X-ray data 2. Derived physical data a. Orbital elements b. Absolute dimensions, masses c. New or improved ephemeris, period variations d. Apsidal motion e. Physical properties of stellar atmospheres f. Chemical abundances g. Accretion disks and accretion phenomena 3. Catalogues, discoveries, charts a. Catalogues b. Discoveries of new binaries and novae c. Identification of optical counterparts of X-ray, IR, or radio sources d. Finding charts 4. Observational techniques 5. Theoretical investigations 6. Statistical investigations 7. Miscellaneous a. Abstract b. Addenda or errata Abbreviations AD accretion disk HMXB high-mass x-ray binary QPO quasi-periodic oscillation BH black hole IP intermediate polar RV radial velocity CB close binary LC light curve SB spectroscopic binary CV cataclysmic variable LMXB low-mass x-ray binary WD white dwarf EB eclipsing binary NS neutron star WR Wolf-Rayet star Several entries of this issue use the abbreviation: OAP | Odessa Astronomical Publications (issue of the Odessa Astronomical Observatory of the Odessa State University, Ukraine), Astroprint Publishing Company, Ukraine Individual Stars Z And Kilpio, E.Y. -
International Astronomical Union Commission 42 BIBLIOGRAPHY
International Astronomical Union Commission 42 BIBLIOGRAPHY OF CLOSE BINARIES No. 73 Editor-in-Chief: C.D. Scarfe Editors: H. Drechsel D.R. Faulkner V.G. Karetnikov E. Lapasset C. Maceroni Y. Nakamura P.G. Niarchos R.G. Samec M. Wolf Material published by September 15, 2001 BCB issues are available via URL: http://www.sternwarte.uni-erlangen.de/ftp/bcb or via anonymous ftp from: ftp://www.sternwarte.uni-erlangen.de/pub/bcb This issue is also available via URL: http://www.astro.washington.edu/szkody/c42/ The bibliographical entries for Individual Stars and Collections of Data are categorized according to the following coding scheme: 1. Observational data a. Photometry b. Spectroscopy c. Spectrophotometry d. Polarimetry e. Astrometry, interferometry f. Times of minima g. γ-ray data i. Infrared data o. Optical data p. Photographic data r. Radio data u. Ultraviolet data v. Visual estimates x. X-ray data 2. Derived physical data a. Orbital elements b. Absolute dimensions, masses c. New or improved ephemeris, period variations d. Apsidal motion e. Physical properties of stellar atmospheres f. Chemical abundances g. Accretion disks and accretion phenomena 3. Catalogues, discoveries, charts a. Catalogues b. Discoveries of new binaries and novae c. Identification of optical counterparts of X-ray, IR, or radio sources d. Finding charts 4. Observational techniques 5. Theoretical investigations 6. Statistical investigations 7. Miscellaneous a. Abstract b. Addenda or errata Abbreviations AD accretion disk HMXB high-mass X-ray binary QPO quasi-periodic oscillation BH black hole IP intermediate polar RV radial velocity CB close binary LC light curve SB spectroscopic binary CV cataclysmic variable LMXB low-mass X-ray binary WD white dwarf EB eclipsing binary NS neutron star WR Wolf-Rayet star Individual Stars RT And Ekmekci, F., Ak, H. -
Congressional Record United States Th of America PROCEEDINGS and DEBATES of the 114 CONGRESS, FIRST SESSION
E PL UR UM IB N U U S Congressional Record United States th of America PROCEEDINGS AND DEBATES OF THE 114 CONGRESS, FIRST SESSION Vol. 161 WASHINGTON, THURSDAY, MAY 21, 2015 No. 79 House of Representatives The House met at 10 a.m. and was last day’s proceedings and announces MEMORIAL DAY called to order by the Speaker pro tem- to the House his approval thereof. (Mr. WILSON of South Carolina pore (Mr. GRAVES of Louisiana). Pursuant to clause 1, rule I, the Jour- asked and was given permission to ad- f nal stands approved. dress the House for 1 minute and to re- vise and extend his remarks.) DESIGNATION OF THE SPEAKER f PRO TEMPORE Mr. WILSON of South Carolina. Mr. PLEDGE OF ALLEGIANCE Speaker, on Memorial Day, Americans The SPEAKER pro tempore laid be- will remember and honor those who fore the House the following commu- The SPEAKER pro tempore. Will the have served this Nation to protect and nication from the Speaker: gentleman from Illinois (Mr. DOLD) defend the freedoms we cherish. As we WASHINGTON, DC, come forward and lead the House in the reflect on the heroism and devotion of May 21, 2015. Pledge of Allegiance. the brave servicemembers who have I hereby appoint the Honorable GARRET Mr. DOLD led the Pledge of Alle- given their lives in defense of our Na- GRAVES to act as Speaker pro tempore on giance as follows: this day. tion, we must never forget to thank I pledge allegiance to the Flag of the JOHN A. BOEHNER, and pray for their families.