Volume 381, Number 1, JanuaryI 2002
|Page(s)||122 - 150|
|Section||Interstellar and circumstellar matter|
|Published online||15 January 2002|
Asteroseismology of RXJ 2117+3412, the hottest pulsating PG 1159 star*
Université Paul Sabatier, Observatoire Midi-Pyrénées, CNRS/UMR5572, 14 Av. É. Belin, 31400 Toulouse, France
2 Copernicus Astronomical Center, Ul. Bartycka 18, 00-716 Warsaw, Poland
3 Observatoire de Paris-Meudon, DAEC, 92195 Meudon, France
4 Department of Astronomy and McDonald Observatory, Texas University at Austin, Austin, TX 78712, USA
5 Sloan Digital Sky Survey, Apache Pt. Observatory, PO Box 59, Sunspot, NM 88349, USA
6 Department of Physics and Astronomy, University of Leicester, University Road, Leicester, LE1 7RH, UK
7 Department of Physics, University of Tromso, 9037 Tromso, Norway
8 Instituto de Astrofisica de Canarias, 38200 La Laguna, Tenerife, Spain
9 Department of Physics and Astronomy, Iowa State University, Ames, IA 50011, USA
10 Instituto de Física-UFRGS, Av. B. Goncalves 9500, 91501-900 Porto-Alegre, RS, Brazil
11 Departamento de Física, Universidade Federal de Santa Catarina, CP 476, CEP 88040-900, Florianópolis, Brazil
12 Department of Physics, University of North Carolina, Chapel Hill, NC 27599-3255, USA
13 Department of Physics and Astronomy, University of Delaware, Newark, DE 19716, USA
14 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
15 Joint Institute for Laboratory Astrophysics, University of Colorado, Box 440, Boulder, CO 80309, USA
16 Department of Physics and Astronomy, University of Arkansas at Little Rock, Little Rock, AR 72204, USA
17 Los Alamos National Laboratory, X-2, MS B-220, Los Alamos, NM 87545, USA
18 Guest Observer, Institute for Astronomy, Honolulu, HI, USA
19 Department of Physics and Space Sciences and SARA Observatory, Florida Institute of Technology, Melbourne, FL 32901, USA
20 Siding Spring Observatory, and Department of Mathematics, Australian National University, Canberra, Australia
21 Beijing Astronomical Observatory, Chinese Academy of Sciences, 20A, Datun Road, Beijing 100012, PR China
22 Indian Space Research Organization, Airport Road, Vimanapura PO, Bangalore 560017, India
23 Institute of Theoretical Physics and Astronomy, Gostauto 12, Vilnius 2600, Lithuania
24 Astronomical Institute, Astronomicheskaya 33, Tashkent 700052, Uzbekistan
25 Wise Observatory, Tel Aviv University, Tel Aviv 69978, Israel
26 Mt. Suhora Observatory, Cracow Pedagogical University, Ul. Podchorazych 2, 30-084 Cracow, Poland
27 Astronomical Observatory, Jagiellonian University, ul. Orla 171, 30-244 Cracow, Poland
Corresponding author: G. Vauclair, email@example.com
Accepted: 15 October 2001
The pulsating PG 1159 planetary nebula central star RXJ 2117+3412 has been observed over three successive seasons of a multisite photometric campaign. The asteroseismological analysis of the data, based on the 37 identified modes among the 48 independent pulsation frequencies detected in the power spectrum, leads to the derivation of the rotational splitting, the period spacing and the mode trapping cycle and amplitude, from which a number of fundamental parameters can be deduced. The average rotation period is days. The trend for the rotational splitting to decrease with increasing periods is incompatible with a solid body rotation. The total mass is 0.56 and the He-rich envelope mass fraction is in the range 0.013–0.078 . The luminosity derived from asteroseismology is log( and the distance 760 pc. At such a distance, the linear size of the planetary nebulae is pc. The role of mass loss on the excitation mechanism and its consequence on the amplitude variations is discussed.
Key words: stars: fundamental parameters / stars: individual (RXJ 2117+3412) / stars: oscillations
Based on data obtained in observing time allocated by the Bernard Lyot Telescope, INSU/CNRS, France, the TCS at Teide Observatory, Tenerife, Spain, the INT and JKT Telescopes at Roque de Los Muchachos Observatory, La Palma, Spain, the Laboratorio Nacional de Astrofisica/CNPq, Brazil, the McDonal Observatory, Texas, USA, the Steward Observatory, Arizona, USA, the Mauna Kea Observatory, University of Hawaii, USA, the Mount Stromlo and Siding Spring Observatory, Australia, the Beijing Observatory, China, the Vainu Bappu Observatory, India, the Maidanak Observatory, Uzbekistan, the Wise Observatory, Israel, and the Suhora Observatory, Poland.
© ESO, 2002
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