Whole earth telescope observations and seismological analysis of the pre-white dwarf PG 2131 + 066

S. D. Kawaler; M. S. O'Brien; J. C. Clemens; R. E. Nather; D. E. Winget; T. K. Watson; K. Yanagida; J. S. Dixson; P. A. Bradley; M. A. Wood; D. J. Sullivan; S. J. Kleinman; E. Meištas; E. M. Leibowitz; P. Moskalik; S. Zoła; G. Pajdosz; J. Krzesiński; J. E. Solheim; A. Bruvold; D. O'Donoghue; M. Katz; G. Vauclair; N. Dolez; M. Chevreton; M. A. Barstow; A. Kanaan; S. O. Kepler; O. Giovannini; J. L. Provencal; C. J. Hansen

doi:10.1086/176145

Whole earth telescope observations and seismological analysis of the pre-white dwarf PG 2131 + 066

S. D. Kawaler^*, M. S. O'Brien, J. C. Clemens, R. E. Nather, D. E. Winget, T. K. Watson, K. Yanagida, J. S. Dixson, P. A. Bradley, M. A. Wood, D. J. Sullivan, S. J. Kleinman, E. Meištas, E. M. Leibowitz, P. Moskalik, S. Zoła, G. Pajdosz, J. Krzesiński, J. E. Solheim, A. BruvoldD. O'Donoghue, M. Katz, G. Vauclair, N. Dolez, M. Chevreton, M. A. Barstow, A. Kanaan, S. O. Kepler, O. Giovannini, J. L. Provencal, C. J. Hansen

^*Corresponding author for this work

School of Physics and Astronomy

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Abstract

As transition objects between the asymptotic giant branch (AGB) and cooling white dwarfs, the PG 1159 stars are key objects for understanding the late stages of stellar evolution. The pulsations exhibited by many members of the PG 1159 spectral class provide a mechanism for ferreting out this information. We present an analysis of the pulsation spectrum of the naked PG 1159 star PG 2131 + 066, which we completely resolve using data from the Whole Earth Telescope (WET). The pulsation spectrum shows patterns that are expected from pulsation theory; comparison of these patterns with theoretical models indicate that PG 2131 has a mass of 0.61 ± 0.02 M_⊙, a luminosity of log (L/L⊙) = 1.0 ± 0.2, and it lies at a distance of 470^+180-130 pc. It rotates with a period of 5.1 hr and shows evidence of a discontinuity in composition approximately 6 × 10^-3 M_* below the surface. Certain modes show complex structure in the power spectrum, while others show measurable frequency changes in 8 years. Fine structure in the prograde (m = -1) modes suggests the presence of nonlinear effects.

Original language	English
Pages (from-to)	350-363
Number of pages	14
Journal	Astrophysical Journal
Volume	450
Issue number	1
DOIs	https://doi.org/10.1086/176145
State	Published - 1 Sep 1995

Keywords

Stars: fundamental parameters
Stars: oscillations
White dwarfs

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10.1086/176145

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Kawaler, S. D., O'Brien, M. S., Clemens, J. C., Nather, R. E., Winget, D. E., Watson, T. K., Yanagida, K., Dixson, J. S., Bradley, P. A., Wood, M. A., Sullivan, D. J., Kleinman, S. J., Meištas, E., Leibowitz, E. M., Moskalik, P., Zoła, S., Pajdosz, G., Krzesiński, J., Solheim, J. E., ... Hansen, C. J. (1995). Whole earth telescope observations and seismological analysis of the pre-white dwarf PG 2131 + 066. Astrophysical Journal, 450(1), 350-363. https://doi.org/10.1086/176145

@article{be8ec85f4e2548af9d6b75ebff097a0c,

title = "Whole earth telescope observations and seismological analysis of the pre-white dwarf PG 2131 + 066",

abstract = "As transition objects between the asymptotic giant branch (AGB) and cooling white dwarfs, the PG 1159 stars are key objects for understanding the late stages of stellar evolution. The pulsations exhibited by many members of the PG 1159 spectral class provide a mechanism for ferreting out this information. We present an analysis of the pulsation spectrum of the naked PG 1159 star PG 2131 + 066, which we completely resolve using data from the Whole Earth Telescope (WET). The pulsation spectrum shows patterns that are expected from pulsation theory; comparison of these patterns with theoretical models indicate that PG 2131 has a mass of 0.61 ± 0.02 M⊙, a luminosity of log (L/L⊙) = 1.0 ± 0.2, and it lies at a distance of 470+180-130 pc. It rotates with a period of 5.1 hr and shows evidence of a discontinuity in composition approximately 6 × 10-3 M* below the surface. Certain modes show complex structure in the power spectrum, while others show measurable frequency changes in 8 years. Fine structure in the prograde (m = -1) modes suggests the presence of nonlinear effects.",

keywords = "Stars: fundamental parameters, Stars: oscillations, White dwarfs",

author = "Kawaler, {S. D.} and O'Brien, {M. S.} and Clemens, {J. C.} and Nather, {R. E.} and Winget, {D. E.} and Watson, {T. K.} and K. Yanagida and Dixson, {J. S.} and Bradley, {P. A.} and Wood, {M. A.} and Sullivan, {D. J.} and Kleinman, {S. J.} and E. Mei{\v s}tas and Leibowitz, {E. M.} and P. Moskalik and S. Zo{\l}a and G. Pajdosz and J. Krzesi{\'n}ski and Solheim, {J. E.} and A. Bruvold and D. O'Donoghue and M. Katz and G. Vauclair and N. Dolez and M. Chevreton and Barstow, {M. A.} and A. Kanaan and Kepler, {S. O.} and O. Giovannini and Provencal, {J. L.} and Hansen, {C. J.}",

year = "1995",

month = sep,

day = "1",

doi = "10.1086/176145",

language = "אנגלית",

volume = "450",

pages = "350--363",

journal = "Astrophysical Journal",

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Kawaler, SD, O'Brien, MS, Clemens, JC, Nather, RE, Winget, DE, Watson, TK, Yanagida, K, Dixson, JS, Bradley, PA, Wood, MA, Sullivan, DJ, Kleinman, SJ, Meištas, E, Leibowitz, EM, Moskalik, P, Zoła, S, Pajdosz, G, Krzesiński, J, Solheim, JE, Bruvold, A, O'Donoghue, D, Katz, M, Vauclair, G, Dolez, N, Chevreton, M, Barstow, MA, Kanaan, A, Kepler, SO, Giovannini, O, Provencal, JL & Hansen, CJ 1995, 'Whole earth telescope observations and seismological analysis of the pre-white dwarf PG 2131 + 066', Astrophysical Journal, vol. 450, no. 1, pp. 350-363. https://doi.org/10.1086/176145

TY - JOUR

T1 - Whole earth telescope observations and seismological analysis of the pre-white dwarf PG 2131 + 066

AU - Kawaler, S. D.

AU - O'Brien, M. S.

AU - Clemens, J. C.

AU - Nather, R. E.

AU - Winget, D. E.

AU - Watson, T. K.

AU - Yanagida, K.

AU - Dixson, J. S.

AU - Bradley, P. A.

AU - Wood, M. A.

AU - Sullivan, D. J.

AU - Kleinman, S. J.

AU - Meištas, E.

AU - Leibowitz, E. M.

AU - Moskalik, P.

AU - Zoła, S.

AU - Pajdosz, G.

AU - Krzesiński, J.

AU - Solheim, J. E.

AU - Bruvold, A.

AU - O'Donoghue, D.

AU - Katz, M.

AU - Vauclair, G.

AU - Dolez, N.

AU - Chevreton, M.

AU - Barstow, M. A.

AU - Kanaan, A.

AU - Kepler, S. O.

AU - Giovannini, O.

AU - Provencal, J. L.

AU - Hansen, C. J.

PY - 1995/9/1

Y1 - 1995/9/1

N2 - As transition objects between the asymptotic giant branch (AGB) and cooling white dwarfs, the PG 1159 stars are key objects for understanding the late stages of stellar evolution. The pulsations exhibited by many members of the PG 1159 spectral class provide a mechanism for ferreting out this information. We present an analysis of the pulsation spectrum of the naked PG 1159 star PG 2131 + 066, which we completely resolve using data from the Whole Earth Telescope (WET). The pulsation spectrum shows patterns that are expected from pulsation theory; comparison of these patterns with theoretical models indicate that PG 2131 has a mass of 0.61 ± 0.02 M⊙, a luminosity of log (L/L⊙) = 1.0 ± 0.2, and it lies at a distance of 470+180-130 pc. It rotates with a period of 5.1 hr and shows evidence of a discontinuity in composition approximately 6 × 10-3 M* below the surface. Certain modes show complex structure in the power spectrum, while others show measurable frequency changes in 8 years. Fine structure in the prograde (m = -1) modes suggests the presence of nonlinear effects.

AB - As transition objects between the asymptotic giant branch (AGB) and cooling white dwarfs, the PG 1159 stars are key objects for understanding the late stages of stellar evolution. The pulsations exhibited by many members of the PG 1159 spectral class provide a mechanism for ferreting out this information. We present an analysis of the pulsation spectrum of the naked PG 1159 star PG 2131 + 066, which we completely resolve using data from the Whole Earth Telescope (WET). The pulsation spectrum shows patterns that are expected from pulsation theory; comparison of these patterns with theoretical models indicate that PG 2131 has a mass of 0.61 ± 0.02 M⊙, a luminosity of log (L/L⊙) = 1.0 ± 0.2, and it lies at a distance of 470+180-130 pc. It rotates with a period of 5.1 hr and shows evidence of a discontinuity in composition approximately 6 × 10-3 M* below the surface. Certain modes show complex structure in the power spectrum, while others show measurable frequency changes in 8 years. Fine structure in the prograde (m = -1) modes suggests the presence of nonlinear effects.

KW - Stars: fundamental parameters

KW - Stars: oscillations

KW - White dwarfs

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ER -

Whole earth telescope observations and seismological analysis of the pre-white dwarf PG 2131 + 066

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Keywords

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