Asteroseismology of RXJ 2117+3412, the hottest pulsating PG 1159 star

G. Vauclair; P. Moskalik; B. Pfeiffer; M. Chevreton; N. Dolez; B. Serre; S. J. Kleinman; M. Barstow; A. E. Sansom; J. E. Solheim; J. A. Belmonte; S. D. Kawaler; S. O. Kepler; A. Kanaan; O. Giovannini; D. E. Winget; T. K. Watson; R. E. Nather; J. C. Clemens; J. Provencal; J. S. Dixson; K. Yanagida; A. Nitta Kleinman; M. Montgomery; E. W. Klumpe; A. Bruvold; M. S. O'Brien; C. J. Hansen; A. D. Grauer; P. A. Bradley; M. A. Wood; N. Achilleos; S. Y. Jiang; J. N. Fu; T. M.K. Marar; B. N. Ashoka; E. G. Meistas; A. V. Chernyshev; T. Mazeh; E. Leibowitz; S. Hemar; J. Krzesinski; G. Pajdosz; S. Zola

doi:10.1051/0004-6361:20011483

Asteroseismology of RXJ 2117+3412, the hottest pulsating PG 1159 star

G. Vauclair^*, P. Moskalik, B. Pfeiffer, M. Chevreton, N. Dolez, B. Serre, S. J. Kleinman, M. Barstow, A. E. Sansom, J. E. Solheim, J. A. Belmonte, S. D. Kawaler, S. O. Kepler, A. Kanaan, O. Giovannini, D. E. Winget, T. K. Watson, R. E. Nather, J. C. Clemens, J. ProvencalJ. S. Dixson, K. Yanagida, A. Nitta Kleinman, M. Montgomery, E. W. Klumpe, A. Bruvold, M. S. O'Brien, C. J. Hansen, A. D. Grauer, P. A. Bradley, M. A. Wood, N. Achilleos, S. Y. Jiang, J. N. Fu, T. M.K. Marar, B. N. Ashoka, E. G. Meistas, A. V. Chernyshev, T. Mazeh, E. Leibowitz, S. Hemar, J. Krzesinski, G. Pajdosz, S. Zola

^*Corresponding author for this work

School of Physics and Astronomy

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Abstract

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 ℓ = 1 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 1.16 ± 0.05 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_-0.04^+0.02 M_⊙ and the He-rich envelope mass fraction is in the range 0.013-0.078 M*. The luminosity derived from asteroseismology is log(L/L_⊙) = 4.05_-0.32^+0.23 and the distance 760_-235⁺²³⁰ pc. At such a distance, the linear size of the planetary nebulae is 2.9 ± 0.9 pc. The role of mass loss on the excitation mechanism and its consequence on the amplitude variations is discussed.

Original language	English
Pages (from-to)	122-150
Number of pages	29
Journal	Astronomy and Astrophysics
Volume	381
Issue number	1
DOIs	https://doi.org/10.1051/0004-6361:20011483
State	Published - 2002

Keywords

Stars: fundamental parameters
Stars: individual (RXJ 2117+3412)
Stars: oscillations

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Vauclair, G., Moskalik, P., Pfeiffer, B., Chevreton, M., Dolez, N., Serre, B., Kleinman, S. J., Barstow, M., Sansom, A. E., Solheim, J. E., Belmonte, J. A., Kawaler, S. D., Kepler, S. O., Kanaan, A., Giovannini, O., Winget, D. E., Watson, T. K., Nather, R. E., Clemens, J. C., ... Zola, S. (2002). Asteroseismology of RXJ 2117+3412, the hottest pulsating PG 1159 star. Astronomy and Astrophysics, 381(1), 122-150. https://doi.org/10.1051/0004-6361:20011483

@article{1c510f75532a44cea2425714a5afe8b7,

title = "Asteroseismology of RXJ 2117+3412, the hottest pulsating PG 1159 star",

abstract = "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 ℓ = 1 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 1.16 ± 0.05 days. The trend for the rotational splitting to decrease with increasing periods is incompatible with a solid body rotation. The total mass is 0.56-0.04+0.02 M⊙ and the He-rich envelope mass fraction is in the range 0.013-0.078 M*. The luminosity derived from asteroseismology is log(L/L⊙) = 4.05-0.32+0.23 and the distance 760-235+230 pc. At such a distance, the linear size of the planetary nebulae is 2.9 ± 0.9 pc. The role of mass loss on the excitation mechanism and its consequence on the amplitude variations is discussed.",

keywords = "Stars: fundamental parameters, Stars: individual (RXJ 2117+3412), Stars: oscillations",

author = "G. Vauclair and P. Moskalik and B. Pfeiffer and M. Chevreton and N. Dolez and B. Serre and Kleinman, {S. J.} and M. Barstow and Sansom, {A. E.} and Solheim, {J. E.} and Belmonte, {J. A.} and Kawaler, {S. D.} and Kepler, {S. O.} and A. Kanaan and O. Giovannini and Winget, {D. E.} and Watson, {T. K.} and Nather, {R. E.} and Clemens, {J. C.} and J. Provencal and Dixson, {J. S.} and K. Yanagida and {Nitta Kleinman}, A. and M. Montgomery and Klumpe, {E. W.} and A. Bruvold and O'Brien, {M. S.} and Hansen, {C. J.} and Grauer, {A. D.} and Bradley, {P. A.} and Wood, {M. A.} and N. Achilleos and Jiang, {S. Y.} and Fu, {J. N.} and Marar, {T. M.K.} and Ashoka, {B. N.} and Meistas, {E. G.} and Chernyshev, {A. V.} and T. Mazeh and E. Leibowitz and S. Hemar and J. Krzesinski and G. Pajdosz and S. Zola",

year = "2002",

doi = "10.1051/0004-6361:20011483",

language = "אנגלית",

volume = "381",

pages = "122--150",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

number = "1",

}

Vauclair, G, Moskalik, P, Pfeiffer, B, Chevreton, M, Dolez, N, Serre, B, Kleinman, SJ, Barstow, M, Sansom, AE, Solheim, JE, Belmonte, JA, Kawaler, SD, Kepler, SO, Kanaan, A, Giovannini, O, Winget, DE, Watson, TK, Nather, RE, Clemens, JC, Provencal, J, Dixson, JS, Yanagida, K, Nitta Kleinman, A, Montgomery, M, Klumpe, EW, Bruvold, A, O'Brien, MS, Hansen, CJ, Grauer, AD, Bradley, PA, Wood, MA, Achilleos, N, Jiang, SY, Fu, JN, Marar, TMK, Ashoka, BN, Meistas, EG, Chernyshev, AV, Mazeh, T , Leibowitz, E, Hemar, S, Krzesinski, J, Pajdosz, G & Zola, S 2002, 'Asteroseismology of RXJ 2117+3412, the hottest pulsating PG 1159 star', Astronomy and Astrophysics, vol. 381, no. 1, pp. 122-150. https://doi.org/10.1051/0004-6361:20011483

TY - JOUR

T1 - Asteroseismology of RXJ 2117+3412, the hottest pulsating PG 1159 star

AU - Vauclair, G.

AU - Moskalik, P.

AU - Pfeiffer, B.

AU - Chevreton, M.

AU - Dolez, N.

AU - Serre, B.

AU - Kleinman, S. J.

AU - Barstow, M.

AU - Sansom, A. E.

AU - Solheim, J. E.

AU - Belmonte, J. A.

AU - Kawaler, S. D.

AU - Kepler, S. O.

AU - Kanaan, A.

AU - Giovannini, O.

AU - Winget, D. E.

AU - Watson, T. K.

AU - Nather, R. E.

AU - Clemens, J. C.

AU - Provencal, J.

AU - Dixson, J. S.

AU - Yanagida, K.

AU - Nitta Kleinman, A.

AU - Montgomery, M.

AU - Klumpe, E. W.

AU - Bruvold, A.

AU - O'Brien, M. S.

AU - Hansen, C. J.

AU - Grauer, A. D.

AU - Bradley, P. A.

AU - Wood, M. A.

AU - Achilleos, N.

AU - Jiang, S. Y.

AU - Fu, J. N.

AU - Marar, T. M.K.

AU - Ashoka, B. N.

AU - Meistas, E. G.

AU - Chernyshev, A. V.

AU - Mazeh, T.

AU - Leibowitz, E.

AU - Hemar, S.

AU - Krzesinski, J.

AU - Pajdosz, G.

AU - Zola, S.

PY - 2002

Y1 - 2002

N2 - 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 ℓ = 1 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 1.16 ± 0.05 days. The trend for the rotational splitting to decrease with increasing periods is incompatible with a solid body rotation. The total mass is 0.56-0.04+0.02 M⊙ and the He-rich envelope mass fraction is in the range 0.013-0.078 M*. The luminosity derived from asteroseismology is log(L/L⊙) = 4.05-0.32+0.23 and the distance 760-235+230 pc. At such a distance, the linear size of the planetary nebulae is 2.9 ± 0.9 pc. The role of mass loss on the excitation mechanism and its consequence on the amplitude variations is discussed.

AB - 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 ℓ = 1 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 1.16 ± 0.05 days. The trend for the rotational splitting to decrease with increasing periods is incompatible with a solid body rotation. The total mass is 0.56-0.04+0.02 M⊙ and the He-rich envelope mass fraction is in the range 0.013-0.078 M*. The luminosity derived from asteroseismology is log(L/L⊙) = 4.05-0.32+0.23 and the distance 760-235+230 pc. At such a distance, the linear size of the planetary nebulae is 2.9 ± 0.9 pc. The role of mass loss on the excitation mechanism and its consequence on the amplitude variations is discussed.

KW - Stars: fundamental parameters

KW - Stars: individual (RXJ 2117+3412)

KW - Stars: oscillations

UR - http://www.scopus.com/inward/record.url?scp=18244422338&partnerID=8YFLogxK

U2 - 10.1051/0004-6361:20011483

DO - 10.1051/0004-6361:20011483

M3 - ???researchoutput.researchoutputtypes.contributiontojournal.article???

AN - SCOPUS:18244422338

SN - 0004-6361

VL - 381

SP - 122

EP - 150

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

IS - 1

ER -

Asteroseismology of RXJ 2117+3412, the hottest pulsating PG 1159 star

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Keywords

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