Constraining the Evolution of ZZ Ceti
We report our analysis of the stability of pulsation periods in the DAV star (pulsating hydrogen atmosphere white dwarf) ZZ Ceti, also called R548. Based on observations that span 31 years, we conclude that the period 213.132605 s observed in ZZ Ceti drifts at a rate dP/dt≤(5.5±1.9)×10−15 s/s, after...
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Language: | English |
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De Gruyter
2003-03-01
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Series: | Open Astronomy |
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author |
Mukadam A. S. Kepler S. O. Winget D. E. Nather R. E. Kilic M. Mullally F. Hippel T. von Kleinman S. J. Nitta A. Guzik J. A. Bradley P. A. Matthews J. Sekiguchi K. Sullivan D. J. Shobbrook R. R. Birch P. Jiang X. J. Xu D. W. Joshi S. Ashoka B.N. Ibbetson P. Leibowitz E. Ofek E. O. Meištas E. G. Janulis R. Ališauskas D. Kalytis R. Handler G. Kilkenny D. O’Donoghue D. Kurtz D. W. Müller M. Moskalik P. Ogłoza W. Zoła S. Krzesiński J. Johannessen F. Gonzalez-Perez J. M. Solheim J-E. Silvotti R. Bernabei S. Vauclair G. Dolez N. Fu J. N. Chevreton M. Manteiga M. Súarez O. Ulla A. Cunha M. S. Metcalfe T. S. Kanaan A. Fraga L. Costa A. F. M. Giovannini O. Fontaine G. Bergeron P. O’Brien M. S. Sanwal D. Wood M. A. Ahrens T. J. Silvestri N. Klumpe E. W. Kawaler S. D. Riddle R. Reed M. D. Watson T. K. |
spellingShingle |
Mukadam A. S. Kepler S. O. Winget D. E. Nather R. E. Kilic M. Mullally F. Hippel T. von Kleinman S. J. Nitta A. Guzik J. A. Bradley P. A. Matthews J. Sekiguchi K. Sullivan D. J. Shobbrook R. R. Birch P. Jiang X. J. Xu D. W. Joshi S. Ashoka B.N. Ibbetson P. Leibowitz E. Ofek E. O. Meištas E. G. Janulis R. Ališauskas D. Kalytis R. Handler G. Kilkenny D. O’Donoghue D. Kurtz D. W. Müller M. Moskalik P. Ogłoza W. Zoła S. Krzesiński J. Johannessen F. Gonzalez-Perez J. M. Solheim J-E. Silvotti R. Bernabei S. Vauclair G. Dolez N. Fu J. N. Chevreton M. Manteiga M. Súarez O. Ulla A. Cunha M. S. Metcalfe T. S. Kanaan A. Fraga L. Costa A. F. M. Giovannini O. Fontaine G. Bergeron P. O’Brien M. S. Sanwal D. Wood M. A. Ahrens T. J. Silvestri N. Klumpe E. W. Kawaler S. D. Riddle R. Reed M. D. Watson T. K. Constraining the Evolution of ZZ Ceti Open Astronomy stars white dwarfs individual ZZ Cet R548 - stars pulsations evolution |
author_facet |
Mukadam A. S. Kepler S. O. Winget D. E. Nather R. E. Kilic M. Mullally F. Hippel T. von Kleinman S. J. Nitta A. Guzik J. A. Bradley P. A. Matthews J. Sekiguchi K. Sullivan D. J. Shobbrook R. R. Birch P. Jiang X. J. Xu D. W. Joshi S. Ashoka B.N. Ibbetson P. Leibowitz E. Ofek E. O. Meištas E. G. Janulis R. Ališauskas D. Kalytis R. Handler G. Kilkenny D. O’Donoghue D. Kurtz D. W. Müller M. Moskalik P. Ogłoza W. Zoła S. Krzesiński J. Johannessen F. Gonzalez-Perez J. M. Solheim J-E. Silvotti R. Bernabei S. Vauclair G. Dolez N. Fu J. N. Chevreton M. Manteiga M. Súarez O. Ulla A. Cunha M. S. Metcalfe T. S. Kanaan A. Fraga L. Costa A. F. M. Giovannini O. Fontaine G. Bergeron P. O’Brien M. S. Sanwal D. Wood M. A. Ahrens T. J. Silvestri N. Klumpe E. W. Kawaler S. D. Riddle R. Reed M. D. Watson T. K. |
author_sort |
Mukadam A. S. |
title |
Constraining the Evolution of ZZ Ceti |
title_short |
Constraining the Evolution of ZZ Ceti |
title_full |
Constraining the Evolution of ZZ Ceti |
title_fullStr |
Constraining the Evolution of ZZ Ceti |
title_full_unstemmed |
Constraining the Evolution of ZZ Ceti |
title_sort |
constraining the evolution of zz ceti |
publisher |
De Gruyter |
series |
Open Astronomy |
issn |
2543-6376 |
publishDate |
2003-03-01 |
description |
We report our analysis of the stability of pulsation periods in the DAV star (pulsating hydrogen atmosphere white dwarf) ZZ Ceti, also called R548. Based on observations that span 31 years, we conclude that the period 213.132605 s observed in ZZ Ceti drifts at a rate dP/dt≤(5.5±1.9)×10−15 s/s, after correcting for proper motion. Our results are consistent with previous Ṗ values for this mode and an improvement over them due to the larger time-base. The characteristic stability timescale implied for the pulsation period is |P/ Ṗ|≥1.2 Gyr, comparable to the theoretical cooling timescale for the star. Our current stability limit for the period 213.132605 s is only slightly less than the present measurement for G117-B15A for the period 215.2 s, another DAV, establishing this mode in ZZ Ceti as the second most stable optical clock known, more stable than atomic clocks and most pulsars. |
topic |
stars white dwarfs individual ZZ Cet R548 - stars pulsations evolution |
url |
http://www.degruyter.com/view/j/astro.2003.12.issue-1/astro-2017-0035/astro-2017-0035.xml?format=INT |
work_keys_str_mv |
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doaj-2f43468678c44bc7b5f349f3b424d8fd2020-11-24T22:05:37ZengDe GruyterOpen Astronomy2543-63762003-03-011217110310.1515/astro-2017-0035astro-2017-0035Constraining the Evolution of ZZ CetiMukadam A. S.0Kepler S. O.1Winget D. E.2Nather R. E.3Kilic M.4Mullally F.5Hippel T. von6Kleinman S. J.7Nitta A.8Guzik J. A.9Bradley P. A.10Matthews J.11Sekiguchi K.12Sullivan D. J.13Shobbrook R. R.14Birch P.15Jiang X. J.16Xu D. W.17Joshi S.18Ashoka B.N.19Ibbetson P.20Leibowitz E.21Ofek E. O.22Meištas E. G.23Janulis R.24Ališauskas D.25Kalytis R.26Handler G.27Kilkenny D.28O’Donoghue D.29Kurtz D. W.30Müller M.31Moskalik P.32Ogłoza W.33Zoła S.34Krzesiński J.35Johannessen F.36Gonzalez-Perez J. M.37Solheim J-E.38Silvotti R.39Bernabei S.40Vauclair G.41Dolez N.42Fu J. N.43Chevreton M.44Manteiga M.45Súarez O.46Ulla A.47Cunha M. S.48Metcalfe T. S.49Kanaan A.50Fraga L.51Costa A. F. M.52Giovannini O.53Fontaine G.54Bergeron P.55O’Brien M. S.56Sanwal D.57Wood M. A.58Ahrens T. J.59Silvestri N.60Klumpe E. W.61Kawaler S. D.62Riddle R.63Reed M. D.64Watson T. K.65University of Texas at Austin, 17.310 RLM Hall, Austin, TX -78712, U.S.A. United States of AmericaInstituto de Física, Universidade Federal do Rio Grande do Sul, 91501- 970 Porto Alegre, RS - Brazil ChileUniversity of Texas at Austin, 17.310 RLM Hall, Austin, TX -78712, U.S.A. United States of AmericaUniversity of Texas at Austin, 17.310 RLM Hall, Austin, TX -78712, U.S.A. United States of AmericaUniversity of Texas at Austin, 17.310 RLM Hall, Austin, TX -78712, U.S.A. United States of AmericaUniversity of Texas at Austin, 17.310 RLM Hall, Austin, TX -78712, U.S.A. United States of AmericaUniversity of Texas at Austin, 17.310 RLM Hall, Austin, TX -78712, U.S.A. United States of AmericaApache Point Observatory, P.O. Box 59, Sunspot, NM 88349, United States of AmericaApache Point Observatory, P.O. Box 59, Sunspot, NM 88349, United States of AmericaLos Alamos National Laboratory, X-2, MS B220, Los Alamos, NM 87545-2345, United States of AmericaLos Alamos National Laboratory, X-2, MS B220, Los Alamos, NM 87545-2345, United States of AmericaDepartment of Physics & Astronomy, University of British Columbia, V6T 1Z4, Vancouver, CanadaSubaru Telescope, National Astronomical Observatory of Japan, 650 North Aohoku Place, Hilo, Hawaii 96720, United States of AmericaSchool of Chemical and Physical Sciences, Victoria University of Wellington, P.O. Box 600, Wellington, New ZealandResearch School of Astronomy and Astrophysics, Australian National University, Weston Creek PO, ACT 2611, AustraliaPerth Observatory Walnut Rd., Bickley, Western Australia 6076, AustraliaBeijing Astronomical Observatory and Joint Laboratories of Optical Astronomy, National Astronomical Observatories of China, Beijing 100012, ChinaBeijing Astronomical Observatory and Joint Laboratories of Optical Astronomy, National Astronomical Observatories of China, Beijing 100012, ChinaUttar Pradesh State Observatory, Manora Peak-263 129, Nainital, IndiaIndian Space Research Organization, Technical Physics Division, ISRO Satellite Center, Airport Road, Bangalore 560017, IndiaSchool of Physics and Astronomy and the Wise Observatory, Tel Aviv University, Ramat Aviv, Tel Aviv 69978, IsraelSchool of Physics and Astronomy and the Wise Observatory, Tel Aviv University, Ramat Aviv, Tel Aviv 69978, IsraelSchool of Physics and Astronomy and the Wise Observatory, Tel Aviv University, Ramat Aviv, Tel Aviv 69978, IsraelInstitute of Theoretical Physics and Astronomy, Goštauto 12, Vilnius 2600, Lithuania LithuaniaInstitute of Theoretical Physics and Astronomy, Goštauto 12, Vilnius 2600, Lithuania LithuaniaVilnius University Observatory, Čiurlionio 29, Vilnius 2009, LithuaniaVilnius University Observatory, Čiurlionio 29, Vilnius 2009, LithuaniaSouth African Astronomical Observatory, PO Box 9, Observatory 7935, South AfricaSouth African Astronomical Observatory, PO Box 9, Observatory 7935, South AfricaSouth African Astronomical Observatory, PO Box 9, Observatory 7935, South AfricaCentre for Astrophysics, University of Central Lancashire, Preston, PR1 2HE, UK FranceDepartment of Astronomy, University of Cape Town, Rondebosch 7701, South AfricaN. Copernicus Astronomical Center, Polish Academy of Sciences, ul. Bartycka 18, 00-716 Warsaw, PolandN. Copernicus Astronomical Center, Polish Academy of Sciences, ul. Bartycka 18, 00-716 Warsaw, Poland PolandAstronomical Observatory, Jagiellonian University, ul. Orla 171, 30-244 Krakow, Poland PolandMount Suhora Observatory, Cracow Pedagogical University, ul. Podchorych 2, 30-084 Cracow, PolandInstitutt for Fysikk, Universitetet i Tromsø, N-9037 Tromsø, NorwayInstitutt for Fysikk, Universitetet i Tromsø, N-9037 Tromsø, NorwayInstitutt for Fysikk, Universitetet i Tromsø, N-9037 Tromsø, NorwayOsservatorio Astronomico di Capodimonte, via Moiariello 16, 80131 Napoli, ItalyOsservatorio Astronomico di Bologna, Via Ranzani 1, Bologna, ItalyObservatoire Midi-Pyrenees, 14 Avenue E. Belin, 31400 Toulouse, FranceObservatoire Midi-Pyrenees, 14 Avenue E. Belin, 31400 Toulouse, FranceObservatoire Midi-Pyrenees, 14 Avenue E. Belin, 31400 Toulouse, FranceObservatoire de Paris Meudon, 92195 Meudon, FranceUniversidade da Coruña, Departamento de Ciencias Naúticas e da Terra, SpainUniversidade da Coruña, Departamento de Ciencias Naúticas e da Terra, Spain Universidade de Vigo, Departamento de Física Aplicada, Facultade de Ciencias, Campus Marcosende–Lagoas, 36200 Vigo (Pontavedra), SpainUniversidade de Vigo, Departamento de Física Aplicada, Facultade de Ciencias, Campus Marcosende–Lagoas, 36200 Vigo (Pontavedra), SpainCentro de Astrofisica da Universidade do Porto, Rua das Estrelas, 4150 Porto, Portugal PortugalTheoretical Astrophysics Center, Institute of Physics and Astronomy, Aarhus University, 8000 Aarhus C, DenmarkDepartamento de Fisica, Universidade Federal de Santa Catarina, 88040-900, Florianopolis, SC, BrazilDepartamento de Fisica, Universidade Federal de Santa Catarina, 88040-900, Florianopolis, SC, BrazilInstituto de Física, Universidade Federal do Rio Grande do Sul, 91501-970 Porto Alegre, RS - Brazil BrazilDepartamento de Fisica e Quimica, Universidade de Caxias do Sul, 95001-970, Caxias do Sul, RS, Brazil BrazilDépartement de Physique, Université de Montréal, C.P. 6128, Succ. Centre-Ville, Montréal, Québec, H3C 3J7, CanadaDépartement de Physique, Université de Montréal, C.P. 6128, Succ. Centre-Ville, Montréal, Québec, H3C 3J7, CanadaSpace Telescope Science Institute, Baltimore, MD 21218, United States of AmericaDepartment of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802, United States of AmericaDepartment of Physics and Space Sciences & SARA Observatory, Florida Institute of Technology, 150 West University Boulevard, Melbourne, FL 32901-6975, United States of AmericaMiddle Tennessee State University, Department of Physics and Astronomy, Murfreesboro, TN 37132, United States of AmericaDepartment of Physics and Space Sciences & SARA Observatory, Florida Institute of Technology, 150 West University Boulevard, Melbourne, FL 32901-6975, United States of AmericaMiddle Tennessee State University, Department of Physics and Astronomy, Murfreesboro, TN 37132, United States of AmericaDepartment of Physics and Astronomy, Iowa State University, Ames, IA 50011, United States of AmericaDepartment of Physics and Astronomy, Iowa State University, Ames, IA 50011, United States of AmericaSouthwest Missouri State University, 901 S. National, Springfield, MO 65807, United States of AmericaInformation Technology Services, Southwestern University, Georgetown, TX 78626, United States of AmericaWe report our analysis of the stability of pulsation periods in the DAV star (pulsating hydrogen atmosphere white dwarf) ZZ Ceti, also called R548. Based on observations that span 31 years, we conclude that the period 213.132605 s observed in ZZ Ceti drifts at a rate dP/dt≤(5.5±1.9)×10−15 s/s, after correcting for proper motion. Our results are consistent with previous Ṗ values for this mode and an improvement over them due to the larger time-base. The characteristic stability timescale implied for the pulsation period is |P/ Ṗ|≥1.2 Gyr, comparable to the theoretical cooling timescale for the star. Our current stability limit for the period 213.132605 s is only slightly less than the present measurement for G117-B15A for the period 215.2 s, another DAV, establishing this mode in ZZ Ceti as the second most stable optical clock known, more stable than atomic clocks and most pulsars.http://www.degruyter.com/view/j/astro.2003.12.issue-1/astro-2017-0035/astro-2017-0035.xml?format=INTstarswhite dwarfsindividualZZ CetR548 - starspulsationsevolution |