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Title:
Observations of the pulsating subdwarf B star Feige 48: Constraints on evolution and companions
Authors:
Reed, M. D.; Kawaler, S. D.; Zola, S.; Jiang, X. J.; Dreizler, S.; Schuh, S. L.; Deetjen, J. L.; Kalytis, R.; Meištas, E.; Janulis, R.; Ališauskas, D.; Krzesiński, J.; Vuckovic, M.; Moskalik, P.; Ogłoza, W.; Baran, A.; Stachowski, G.; Kurtz, D. W.; González Pérez, J. M.; Mukadam, A.; Watson, T. K.; Koen, C.; Bradley, P. A.; Cunha, M. S.; Kilic, M.; Klumpe, E. W.; Carlton, R. F.; Handler, G.; Kilkenny, D.; Riddle, R.; Dolez, N.; Vauclair, G.; Chevreton, M.; Wood, M. A.; Grauer, A.; Bromage, G.; Solheim, J. E.; Østensen, R.; Ulla, A.; Burleigh, M.; Good, S.; Hürkal, Ö.; Anderson, R.; Pakstiene, E.
Affiliation:
AA(Department of Physics, Astronomy and Material Science, Southwest Missouri State University, 901 S. National, Springfield, MO 65804 USA), AB(Department of Physics and Astronomy, Iowa State University, Ames, IA 50011 USA), AC(Astronomical Observatory, Jagiellonian University, ul. Orla 171, 30-244, Cracow, Poland), AD(National Astronomical Observatoires, Chinese Academy of Sciences, Beijing, 100012, PR China), AE(Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, D-72076, Tübingen, Germany; Universitäts-Sternwarte Göttingen, Georg-August-Universität Göttingen, Geismarlandstrasse 11, D-37083 Göttingen, Germany), AF(Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, D-72076, Tübingen, Germany), AG(Institut für Astronomie und Astrophysik, Universität Tübingen, Sand 1, D-72076, Tübingen, Germany), AH(Institute of Material Science and Applied Research of Vilnius University, Astronomical Observatory, Ciurlionio 29, Vilnius LT-2009, Lithuania), AI(Institute of Material Science and Applied Research of Vilnius University, Astronomical Observatory, Ciurlionio 29, Vilnius LT-2009, Lithuania), AJ(Institute of Theoretical Physics and Astronomy, Astronomical Observatory, Gostauto 12, Vilnius LT-2600, Lithuania), AK(Institute of Material Science and Applied Research of Vilnius University, Astronomical Observatory, Ciurlionio 29, Vilnius LT-2009, Lithuania), AL(Mt. Suhora Observatory, Crakow Pedagogical University, ul. Podchorazych 2, PL-30-084 Cracow, Poland; Apache Point Observatory, PO Box 59, Sunspot, NM 88349, USA), AM(Department of Physics and Astronomy, Iowa State University, Ames, IA 50011 USA), AN(Nicolas Copernicus Astronomical Centre, Polish Academy of Sciences, ul. Bartycka 18, 00-716 Warsaw, Poland), AO(Mt. Suhora Observatory, Crakow Pedagogical University, ul. Podchorazych 2, PL-30-084 Cracow, Poland), AP(Mt. Suhora Observatory, Crakow Pedagogical University, ul. Podchorazych 2, PL-30-084 Cracow, Poland), AQ(Astronomical Observatory, Jagiellonian University, ul. Orla 171, 30-244, Cracow, Poland; Mt. Suhora Observatory, Crakow Pedagogical University, ul. Podchorazych 2, PL-30-084 Cracow, Poland), AR(Centre for Astrophysics, University of Central Lancashire, Preston PRI 2HE), AS(Institutt for Fysikk, Universitet i Tromsø, N-9037 Tromsø, Norway), AT(Department of Astronomy, University of Texas, Austin, TX 78712, USA), AU(Southwestern University, 1001 E. University Avenue, Georgetown, TX 78626, USA), AV(Department of Astronomy, University of Texas, Austin, TX 78712, USA; South African Astronomical Observatory, PO Box 9, Observatory 7935, Cape, South Africa), AW(Los Alamos National Laboratory, X-2, MS T-085, Los Alamos, NM 87545, USA), AX(Centro de Astrofísica da Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal; Instituto Superior da Maia, Av. Carlos de Oliveira Campos, 4475-690, Avisoso S. Pedro, Castelo da Maia, Portugal), AY(Department of Astronomy, University of Texas, Austin, TX 78712, USA), AZ(Middle Tennessee State University, Department of Physics and Astronomy, Murfreesboro, TN 37132, USA), BA(Middle Tennessee State University, Department of Physics and Astronomy, Murfreesboro, TN 37132, USA), BB(South African Astronomical Observatory, PO Box 9, Observatory 7935, Cape, South Africa), BC(South African Astronomical Observatory, PO Box 9, Observatory 7935, Cape, South Africa), BD(Department of Physics and Astronomy, Iowa State University, Ames, IA 50011 USA), BE(Université Paul Sabatier, Observatoire Midi-Pyrénées, 14 Avenue E. Belin, 31400 Toulouse, France), BF(Université Paul Sabatier, Observatoire Midi-Pyrénées, 14 Avenue E. Belin, 31400 Toulouse, France), BG(Observatoire de Paris-Meudon, DAEC, 92195, Meudon, France), BH(Department of Physics and Space Sciences & SARA Observatory, Florida Institute of Technology, Melbourne, FL 32901-6975, USA), BI(Department of Physics and Astronomy, University of Arkansas at Little Rock, Little Rock, AR 72204, USA), BJ(Centre for Astrophysics, University of Central Lancashire, Preston PRI 2HE), BK(Institutt for Fysikk, Universitet i Tromsø, N-9037 Tromsø, Norway), BL(Isaac Newton Group of Telescopes, E-37800 Santa Cruz de La Palma, Canary Islands, Spain), BM(Universidade de Vigo, Depto. de Fisica Aplicada, Facultade de Ciencias, Campus Marcosende-Lagoas, 36200 Vigo, Spain), BN(Department of Physics and Astronomy, University of Leicester, Leicester LE1 7RH, England), BO(Department of Physics and Astronomy, University of Leicester, Leicester LE1 7RH, England), BP(Ege University, Science Faculty, Department of Astronomy and Space Sciences, Bornova 35100 Izmir, Turkey), BQ(Department of Physics and Astronomy, University of North Carolina, Chapel Hill, NC 27599-3255, USA), BR(Institute of Theoretical Physics and Astronomy, Astronomical Observatory, Gostauto 12, Vilnius LT-2600, Lithuania)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 348, Issue 4, pp. 1164-1174. (MNRAS Homepage)
Publication Date:
03/2004
Origin:
MNRAS
Astronomy Keywords:
stars: individual (Feige 48), stars: oscillations, stars: variables: other
DOI:
10.1111/j.1365-2966.2004.07438.x
Bibliographic Code:
2004MNRAS.348.1164R

Abstract

Since pulsating subdwarf B (sdBV or EC14026) stars were first discovered, observational efforts have tried to realize their potential for constraining the interior physics of extreme horizontal branch stars. Difficulties encountered along the way include uncertain mode identifications and a lack of stable pulsation mode properties. Here we report on Feige 48, an sdBV star for which follow-up observations have been obtained spanning more than four years. These observations show some stable pulsation modes.

We resolve the temporal spectrum into five stable pulsation periods in the range 340-380 s with amplitudes less than 1 per cent, and two additional periods that appear in one data set each. The three largest amplitude periodicities are nearly equally spaced, and we explore the consequences of identifying them as a rotationally split l= 1 triplet by consulting a representative stellar model.

The general stability of the pulsation amplitudes and phases allows us to use the pulsation phases to constrain the time-scale of evolution for this sdBV star. Additionally, we are able to place interesting limits on any stellar or planetary companion to Feige 48.


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