COMMISSION G4 PULSATING STARS 1. Introduction 2. Notable
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Stellar Evolution in Real Time: Models Consistent with Direct Observation of Thermal Pulse in T Ursae Minoris Laszl´ O´ Molnar´ ,1, 2 Meridith Joyce,3 Andl Aszl´ O´ L
Draft version June 6, 2019 Typeset using LATEX twocolumn style in AASTeX62 Stellar Evolution in Real Time: Models Consistent with Direct Observation of Thermal Pulse in T Ursae Minoris Laszl´ o´ Molnar´ ,1, 2 Meridith Joyce,3 andL aszl´ o´ L. Kiss1, 4 1Konkoly Observatory, MTA CSFK, Budapest, Konkoly Thege Mikl´os´ut15-17, Hungary 2MTA CSFK Lend¨uletNear-Field Cosmology Research Group, 1121, Budapest, Konkoly Thege Mikl´os´ut15-17, Hungary 3Research School of Astronomy and Astrophysics, Australian National University, Canberra, ACT 2611, Australia 4Sydney Institute for Astronomy, School of Physics A29, University of Sydney, NSW 2006, Australia ABSTRACT Most aspects of stellar evolution proceed far too slowly to be directly observable in a single star on human timescales. The thermally pulsing asymptotic giant branch is one exception. The combination of state-of-the-art modelling techniques with data assimilated from observations collected by amateur astronomers over many decades provide, for the first time, the opportunity to identify a star occupying precisely this evolutionary stage. In this study, we show that the rapid pulsation period change and associated reduction in radius in the bright, northern variable star T Ursae Minoris are caused by the recent onset of a thermal pulse. We demonstrate that T UMi transitioned into a double-mode pulsation state, and we exploit its asteroseismic features to constrain its fundamental stellar parameters. We use evolutionary models from MESA and linear pulsation models from GYRE to track simultaneously the structural and oscillatory evolution of models with varying mass. We apply a sophisticated iterative sampling scheme to achieve time resolution ≤ 10 years at the onset of the relevant thermal pulses. -
Article a Tidally Tilted Sectoral Dipole Pulsation Mode in the Eclipsing Binary TIC 63328020
Article A tidally tilted sectoral dipole pulsation mode in the eclipsing binary TIC 63328020 Rappaport, S A, Kurtz, Donald Wayne, Handler, G, Jones, D, Nelson, L A, Saio, H, Fuller, J, Holdsworth, Daniel Luke, Vanderburg, A, Zak, J, Skarka, M, Aiken, J, Maxted, P F L, Stevens, D J, Feliz, D L and Kahraman Alicavus, F Available at http://clok.uclan.ac.uk/36745/ Rappaport, S A, Kurtz, Donald Wayne ORCID: 0000-0002-1015-3268, Handler, G, Jones, D, Nelson, L A, Saio, H, Fuller, J, Holdsworth, Daniel Luke ORCID: 0000-0003-2002-896X, Vanderburg, A et al (2021) A tidally tilted sectoral dipole pulsation mode in the eclipsing binary TIC 63328020. Monthly Notices of the Royal Astronomical Society . ISSN 0035-8711 It is advisable to refer to the publisher’s version if you intend to cite from the work. http://dx.doi.org/10.1093/mnras/stab336 For more information about UCLan’s research in this area go to http://www.uclan.ac.uk/researchgroups/ and search for <name of research Group>. For information about Research generally at UCLan please go to http://www.uclan.ac.uk/research/ All outputs in CLoK are protected by Intellectual Property Rights law, including Copyright law. Copyright, IPR and Moral Rights for the works on this site are retained by the individual authors and/or other copyright owners. Terms and conditions for use of this material are defined in the policies page. CLoK Central Lancashire online Knowledge www.clok.uclan.ac.uk MNRAS 503, 254–269 (2021) doi:10.1093/mnras/stab336 Advance Access publication 2021 February 9 A tidally tilted sectoral dipole pulsation mode in the eclipsing binary TIC 63328020 S. -
Space in Central and Eastern Europe
EU 4+ SPACE IN CENTRAL AND EASTERN EUROPE OPPORTUNITIES AND CHALLENGES FOR THE EUROPEAN SPACE ENDEAVOUR Report 5, September 2007 Charlotte Mathieu, ESPI European Space Policy Institute Report 5, September 2007 1 Short Title: ESPI Report 5, September 2007 Editor, Publisher: ESPI European Space Policy Institute A-1030 Vienna, Schwarzenbergplatz 6 Austria http://www.espi.or.at Tel.: +43 1 718 11 18 - 0 Fax - 99 Copyright: ESPI, September 2007 This report was funded, in part, through a contract with the EUROPEAN SPACE AGENCY (ESA). Rights reserved - No part of this report may be reproduced or transmitted in any form or for any purpose without permission from ESPI. Citations and extracts to be published by other means are subject to mentioning “source: ESPI Report 5, September 2007. All rights reserved” and sample transmission to ESPI before publishing. Price: 11,00 EUR Printed by ESA/ESTEC Compilation, Layout and Design: M. A. Jakob/ESPI and Panthera.cc Report 5, September 2007 2 EU 4+ Executive Summary ....................................................................................... 5 Introduction…………………………………………………………………………………………7 Part I - The New EU Member States Introduction................................................................................................... 9 1. What is really at stake for Europe? ....................................................... 10 1.1. The European space community could benefit from a further cooperation with the ECS ................................................................. 10 1.2. However, their economic weight remains small in the European landscape and they still suffer from organisatorial and funding issues .... 11 1.2.1. Economic weight of the ECS in Europe ........................................... 11 1.2.2. Reality of their impact on competition ............................................ 11 1.2.3. Foreign policy issues ................................................................... 12 1.2.4. Internal challenges ..................................................................... 12 1.3. -
Arxiv:2001.10147V1
Magnetic fields in isolated and interacting white dwarfs Lilia Ferrario1 and Dayal Wickramasinghe2 Mathematical Sciences Institute, The Australian National University, Canberra, ACT 2601, Australia Adela Kawka3 International Centre for Radio Astronomy Research, Curtin University, Perth, WA 6102, Australia Abstract The magnetic white dwarfs (MWDs) are found either isolated or in inter- acting binaries. The isolated MWDs divide into two groups: a high field group (105 − 109 G) comprising some 13 ± 4% of all white dwarfs (WDs), and a low field group (B < 105 G) whose incidence is currently under investigation. The situation may be similar in magnetic binaries because the bright accretion discs in low field systems hide the photosphere of their WDs thus preventing the study of their magnetic fields’ strength and structure. Considerable research has been devoted to the vexed question on the origin of magnetic fields. One hypothesis is that WD magnetic fields are of fossil origin, that is, their progenitors are the magnetic main-sequence Ap/Bp stars and magnetic flux is conserved during their evolution. The other hypothesis is that magnetic fields arise from binary interaction, through differential rotation, during common envelope evolution. If the two stars merge the end product is a single high-field MWD. If close binaries survive and the primary develops a strong field, they may later evolve into the arXiv:2001.10147v1 [astro-ph.SR] 28 Jan 2020 magnetic cataclysmic variables (MCVs). The recently discovered population of hot, carbon-rich WDs exhibiting an incidence of magnetism of up to about 70% and a variability from a few minutes to a couple of days may support the [email protected] [email protected] [email protected] Preprint submitted to Journal of LATEX Templates January 29, 2020 merging binary hypothesis. -
Iván Almár Is Professor of Astronomy at the Konkoly Observatory of the Hungarian Academy of Sciences
Iván Almár is professor of astronomy at the Konkoly Observatory of the Hungarian Academy of Sciences. He has worked in space research (specifically, upper-atmospheric research and satellite geodesy) for more than 50 years. Prof. Almár has been a Member of the IAA since 1984, and was chairman of its Space and Society Commission from 2003 to 2005. He began presenting and publishing papers on planetary protection in 1989. Charles Cockell is professor of geomicrobiology at the Open University, UK. He obtained his PhD from the University of Oxford and held an NRC Associateship at the NASA Ames Research Centre. His interests are in microbe-mineral interactions and life in extreme environments. He is author of several books, including 'Space on Earth' (Macmillan), which explores the links between environmentalism and space exploration. His publications on ethics have focused on the place of microorganisms in environmental ethics and the protection of the space environment. He is Chair of the Earth and Space Foundation. Catharine A. Conley has served as the NASA Planetary Protection Officer since 2006. Prior to this, Conley's research at NASA Ames Research Center focused on the biochemistry and evolution of muscle tissue. Conley has been involved in several spaceflight experiments using the nematode worm, Caenorhabditis elegans, the first of which was flown on the last mission of the Space Shuttle Columbia. Flight hardware was recovered after the tragic accident, and when opened it was found that some spaceflown experimental animals were still alive, a finding of considerable relevance to Planetary Protection. Gernot Groemer has a background in astronomy and astrobiology. -
Stellar Flares with ARIEL
Stellar flares with ARIEL Krisztián Vida & Bálint Seli Konkoly Observatory, Budapest, Hungary Stellar activity as noise ● Photospheric starspots have small contribution to light variations in the IR regime ● Flares are also more prominent at shorter wavelengths Flare of an M-dwarf in multiple passbands ● A possible problem: with transit spectroscopy the removed spectral source is the whole stellar disk, but different activity contribution can cause contamination even in IR regime Rackham, Apai, Giampapa 2018 ● A possible problem: with transit spectroscopy the removed spectral source is the whole stellar disk, but different activity contribution can cause contamination even in IR regime ● This can reach a level of 10+% depending on wavelength and spot confguration Rackham, Apai, Giampapa 2018 ARIEL & stellar activity ● Magnetic activity is an important property of young, fast-rotating stars ● This can have serious consequences on their exoplanets What remains to study for later stages of star/planetary system evolution? Rotation (age) vs. X-ray luminosity ARIEL & stellar activity ● Magnetic activity is an important property of young, fast-rotating stars ● This can have serious consequences on their exoplanets ● Some models already exist discussing the effects of activity on planets, but not much is known on the additive effects and observational confrmation is also missing Model of the atmospheric changes of an Earth-like planet due to a large fare event (Segura et al. 2010) ARIEL & stellar activity ● The interaction of exoplanets and stellar magnetism is crucial for planetary evolution and for the search for life ● Can the system harbor life on long term? (frst signs of life on Eearth dates back to 4Gyr, although complex life based on eukaryotic cells took much longer time to form) ARIEL & stellar activity High resolution photometry can be crucial for fast transients – e.g. -
Astronomy Astrophysics
A&A 641, A76 (2020) https://doi.org/10.1051/0004-6361/202037625 Astronomy & © Ö. H. Detre et al. 2020 Astrophysics Herschel-PACS photometry of the five major moons of Uranus? Ö. H. Detre1, T. G. Müller2, U. Klaas1, G. Marton3,4, H. Linz1, and Z. Balog1,5 1 Max-Planck-Institut für Astronomie (MPIA), Königstuhl 17, 69117 Heidelberg, Germany e-mail: [email protected] 2 Max-Planck-Institut für extraterrestrische Physik (MPE), PO Box 1312, Giessenbachstraße, 85741 Garching, Germany 3 Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, Konkoly Thege-Miklós 15-17, 1121 Budapest, Hungary 4 ELTE Eötvös Loránd University, Institute of Physics, Pázmány Péter 1/A, 1171 Budapest, Hungary 5 Astronomisches Recheninstitut des Zentrums für Astronomie, Mönchhofstrasse 12–14, 69120 Heidelberg, Germany Received 30 January 2020 / Accepted 9 June 2020 ABSTRACT Aims. We aim to determine far-infrared fluxes at 70, 100, and 160 µm for the five major Uranus satellites, Titania, Oberon, Umbriel, Ariel, and Miranda. Our study is based on the available calibration observations at wavelengths taken with the PACS photometer aboard the Herschel Space Observatory. Methods. The bright image of Uranus was subtracted using a scaled Uranus point spread function (PSF) reference established from all maps of each wavelength in an iterative process removing the superimposed moons. The photometry of the satellites was performed using PSF photometry. Thermophysical models of the icy moons were fitted to the photometry of each measurement epoch and auxiliary data at shorter wavelengths. Results. The best-fit thermophysical models provide constraints for important properties of the moons, such as surface roughness and thermal inertia. -
Contributed Paper KONKOLY WIDE-FIELD PLATE ARCHIVE 1
CORE Metadata, citation and similar papers at core.ac.uk Provided by Repository of the Academy's Library Proc. IV Serbian-Bulgarian Astronomical Conference, Belgrade 21{24 April 2004, eds. M. S. Dimitrijevi´c, V. Golev, L. C.ˇ Popovi´c, M. Tsvetkov, Publ. Astron. Soc. "Rudjer Boˇskovi´c" No 5, 2005, 295 - 301 Contributed paper KONKOLY WIDE-FIELD PLATE ARCHIVE 1 2 2 2 2 M. TSVETKOV , L. G. BALAZS´ , A. FRONTO´ , J. KELEMEN , A. HOLL , 1 1 1 3 K. Y. STAVREV , K. TSVETKOVA , A. BORISOVA , D. KALAGLARSKY and 3 R. BOGDANOVSKI 1Institute of Astronomy, Bulgarian Academy of Sciences, 72 Tsarigradsko Shosse blvd., 1784 Sofia, Bulgaria E{mail [email protected] 2Konkoly Observatory, Hungarian Academy of Sciences, Konkoly Thege M. ut 15-17, 1121 Budapest, Hungary E{mail [email protected] 3Space Research Institute, Bulgarian Academy of Sciences, 6 Moskovska str., 1000 Sofia, Bulgaria E{mail [email protected] Abstract. The wide-field photographic observations in Konkoly Observatory were per- formed in the period 1962 { 1997 with the 60/90/180 cm Schmidt telescope in Piszk´estet}o Mountain Station. The archive of the telescope contains more than 13 000 observations de- scribed in the Konkoly plate catalogue. After the preparation of an enlarged version of the catalogue it has been incorporated in the Wide-Field Plate Database installed in the Sofia Sky Archive Data Center with a possible on-line search at http://www.skyarchive.org/search/. Results from the analysis of the catalogue data characterizing the observational activity at Konkoly in the period 1962 { 1997 are presented. -
THE CARE of OBSOLETE INSTRUMENTS Magda Vargha
161 THE CARE OF OBSOLETE INSTRUMENTS Magda Vargha Konkoly Observatory Budapest Hungary is a little country with old traditions. Hungarian celebrate the 950th anniversary of the death of the first king Stephan I this year. As regards astronomy, during the Renaissance in the court of the Hungarian king Matthias I there was a modest flowering in astronomy and this continued until 1526, when because of the Turkish occupation, the region was cut off and remained so for centuries. I do not want to list all the tragic historical events. Rather I would like to emphasize what we know by own experiences: what it means to reconstruct destroyed buildings and to try to collect valuable old items that are thrown away by guilty negligence. Returning to the recent time, according to my experiences that also in peaceful circumstances valuable old things such as books and scientific instruments are in permanent danger. This is true especially when they are not "up to date"but not old enough for antiquarians. Furthermore, the obsolete instruments meet a worse fate. During my working period in the Konkoly Observatory many instruments considered obsolete have been eliminated while the old books have quiet places on our shelves in the library. With respect to survival, there are many differences between instru ments and books. This is the most important difference among them: while an instrument is made in one or in very few copies, the books are printed in hundreds. One source of trouble is that it is very easy for someone to modify or disassemble an instrument to the point where it is unrecognizable. -
EPSC2014-584, 2014 European Planetary Science Congress 2014 Eeuropeapn Planetarsy Science Ccongress C Author(S) 2014
EPSC Abstracts Vol. 9, EPSC2014-584, 2014 European Planetary Science Congress 2014 EEuropeaPn PlanetarSy Science CCongress c Author(s) 2014 Detection limit for the size of exomoons around Kepler planetary candidates and in simulated CHEOPS data A. E. Simon (1,2), Gy. M. Szabó (2,3) and L. L. Kiss (2) (1) Center for Space and Habitability, University of Berne, CH-3012 Bern, Switzerland (2) Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, Hungarian Academy of Sciences, H-1121 Budapest, Hungary (3) Gothard Astrophysical Observatory and Multidisciplinary Research Center of Loránd Eötvös University, H-9700 Szombathely, Hungary Abstract 2. (Un)detectable moon around Ke- The increasing number of detected exoplanets has in- pler candidates? spired a significant interest in the community as to We calculated photometric transit timing variations whether these planets can host a detectable and hab- (PTV : see TTVp in [5]) from simulated observations itable moon [4]. Here we show which are the most with increasing moon size for all Kepler candidates2 to promising Kepler planetary candidates that are capa- determine the minimum radius of a theoretical moon ble to host a detectable moon and what is the best way that can be detected in the Kepler data. to increase our chance of discovering exomoons via the forthcoming CHEOP S space telescope. 1. Introduction Despite the efforts during the past 8 years that aimed on a discovery of an exomoon in the Kepler data [9, 5, 6, 7, 2], there has no firm evidence for an exomoon found as of today [8, 3]. From the analysis of the data provided by the Kepler spacecraft shows an apparent contradiction between the number of examined KOI systems by date and the lack of any firm detection. -
Tidally Trapped Pulsations in a Close Binary Star System Discovered by TESS G
Tidally Trapped Pulsations in a close binary star system discovered by TESS G. Handler,1 D. W. Kurtz,2 S. A. Rappaport,3 H. Saio,4 J. Fuller,5 D. Jones,6; 7 Z. Guo,8 S. Chowdhury,1 P. Sowicka,1 F. Kahraman Ali¸cavu¸s,1; 9 M. Streamer,10 S. J. Murphy,11 R. Gagliano,12 T. L. Jacobs13 and A. Vanderburg 14; 15 Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, ul. Bartycka 18, 00-716, Warsaw, Poland 2 Jeremiah Horrocks Institute, University of Central Lancashire, Preston PR1 2HE, UK 3 Department of Physics, and Kavli Institute for Astrophysics and Space Research, M.I.T., Cambridge, MA 02139, USA 4 Astronomical Institute, Graduate School of Science, Tohoku University, Sendai 980-8578, Japan 5 Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA 91125, USA 6 Instituto de Astrof´ısicade Canarias, E-38205 La Laguna, Tenerife, Spain 7 Departamento de Astrof´ısica,Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain 8 Department of Astronomy and Astrophysics, Pennsylvania State University, 421 Davey Lab, University Park, PA 16802, USA 9 C¸anakkale Onsekiz Mart University, Faculty of Sciences and Arts, Physics Department, 17100, C¸anakkale, Turkey 10 Research School of Astronomy and Astrophysics, Australian National University, Can- berra, ACT, Australia 11 Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, NSW 2006, Australia 12 Planet Hunters 13 Amateur Astronomer, 12812 SE 69th Place Bellevue, WA 98006, USA 14 Department of Astronomy, The University of Texas at Austin, 2515 Speedway, Stop C1400, Austin, TX 78712, USA 15 NASA Sagan Fellow arXiv:2003.04071v1 [astro-ph.SR] 9 Mar 2020 1 It has long been suspected that tidal forces in close binary stars could modify the orientation of the pulsation axis of the constituent stars. -
Pennsylvania Science Olympiad State Finals 2017 Astronomy C Division
PENNSYLVANIA SCIENCE OLYMPIAD STATE FINALS 2017 ASTRONOMY C DIVISION EXAM APRIL 29, 2017 TEAM NUMBER _____________ SCHOOL NAME_____________________________________ PARTICIPANTS__________________________________________________________________ _______________________________________________________________________________ INSTRUCTIONS: 1. Turn in all exam materials at the end of this event. Missing exam materials will result in immediate disqualification of the team in question. There is an exam packet, an image packet, and 3 blank answer sheets. 2. You may separate the exam pages. 3. Only the answers provided on the answer page will be considered. Do not write outside the designated spaces for each answer. You may write in the exam booklet. 4. Write your team number, school name, and participants’ names on the title page of the test booklet. By writing your participants’ names, you agree to the General Rules, Code of Ethics, and Spirit of the Problem as defined on the Science Olympiad website: https://www.soinc.org/code-ethics-general-rules. 5. Write your team number, school name, and participants’ names in the appropriate spaces on the answer sheets. 6. Each question is worth one point. Tiebreaker questions are indicated with a (T#) in which the number indicates the order of consultation in the event of a tie. Tiebreaker questions count toward the overall raw score, and are only used as tiebreakers when there is a tie. In such cases, (T1) will be examined first, then (T2), and so on until the tie is broken. There are 16 tiebreakers. 7. Pay close attention to the units given in the problem and the units asked for in the answer. 8. When the time is up, the time is up.