Amplitude and frequency variability of the pulsating DB white dwarf stars KUV 05134+2605 and PG 1654+160 observed with the Whole Earth Telescope

G. Handler, D. O'Donoghue, M. Müller, J. E. Solheim, J. M. Gonzalez-Perez, F. Johannessen, M. Paparó, B. Szeidl, G. Viraghalmy, R. Silvotti, G. Vauclair, N. Dolez, E. Pallier, M. Chevreton, D. W. Kurtz, G. E. Bromage, M. S. Cunha, R. Østensen, L. Fraga, A. KanaanA. Amorim, O. Giovannini, S. O. Kepler, A. F M Da Costa, R. F. Anderson, M. A. Wood, N. Silvestri, E. W. Klumpe, R. F. Carlton, R. H. Miller, J. P. McFarland, A. D. Grauer, S. D. Kawaler, R. L. Riddle, M. D. Reed, R. E. Nather, D. E. Winget, J. A. Hill, T. S. Metcalfe, A. S. Mukadam, M. Kilic, T. K. Watson, S. J. Kleinman, A. Nitta, J. A. Guzik, P. A. Bradley, K. Sekiguchi, D. J. Sullivan, T. Sullivan, R. R. Shobbrook, X. Jiang, P. V. Birch, B. N. Ashoka, S. Seetha, V. Girish, S. Joshi, T. N. Dorokhova, N. I. Dorokhov, M. C. Akan, E. G. Meištas, R. Janulis, R. Kalytis, D. Ališauskas, S. K. Anguma, P. C. Kalebwe, P. Moskalik, W. Ogloza, G. Stachowski, G. Pajdosz, S. Zola

Research output: Contribution to journalArticle

9 Citations (Scopus)

Abstract

We have acquired new time series photometry of the two pulsating DB white dwarf stars KUV 05134+2605 and PG1654+160 with the Whole Earth Telescope. Additional single-site photometry is also presented. We use all these data plus all available archival measurements to study the temporal behaviour of the pulsational amplitudes and frequencies of these stars for the first time. We demonstrate that both KUV 05134+2605 and PG 1654+160 pulsate in many modes, the amplitudes of which are variable in time; some frequency variability of PG 1654+160 is also indicated. Beating of multiple pulsation modes cannot explain our observations; the amplitude variability must therefore be intrinsic. We cannot find stable modes to be used for determinations of the evolutionary period changes of the stars. Some of the modes of PG 1654+160 appear at the same periods whenever detected. The mean spacing of these periods (≈40 s) suggests that they are probably caused by non-radial gravity-mode pulsations of spherical degree 1 = 1. If so, PG 1654+160 has a mass around 0.6 M⊙. The time-scales of the amplitude variability of both stars (down to two weeks) are consistent with theoretical predictions of resonant mode coupling, a conclusion which might however be affected by the temporal distribution of our data.

Original languageEnglish
Pages (from-to)1031-1038
Number of pages8
JournalMonthly Notices of the Royal Astronomical Society
Volume340
Issue number3
DOIs
Publication statusPublished - Apr 11 2003

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white dwarf stars
telescopes
stars
photometry
temporal distribution
spacing
coupled modes
time series
gravity
timescale
gravitation
prediction
predictions

Keywords

  • Stars: Oscillations
  • Stars: Variables: Other
  • Stars:individual:kuv05134+2605
  • Stars:individual:pg 1654+160

ASJC Scopus subject areas

  • Space and Planetary Science

Cite this

Amplitude and frequency variability of the pulsating DB white dwarf stars KUV 05134+2605 and PG 1654+160 observed with the Whole Earth Telescope. / Handler, G.; O'Donoghue, D.; Müller, M.; Solheim, J. E.; Gonzalez-Perez, J. M.; Johannessen, F.; Paparó, M.; Szeidl, B.; Viraghalmy, G.; Silvotti, R.; Vauclair, G.; Dolez, N.; Pallier, E.; Chevreton, M.; Kurtz, D. W.; Bromage, G. E.; Cunha, M. S.; Østensen, R.; Fraga, L.; Kanaan, A.; Amorim, A.; Giovannini, O.; Kepler, S. O.; Da Costa, A. F M; Anderson, R. F.; Wood, M. A.; Silvestri, N.; Klumpe, E. W.; Carlton, R. F.; Miller, R. H.; McFarland, J. P.; Grauer, A. D.; Kawaler, S. D.; Riddle, R. L.; Reed, M. D.; Nather, R. E.; Winget, D. E.; Hill, J. A.; Metcalfe, T. S.; Mukadam, A. S.; Kilic, M.; Watson, T. K.; Kleinman, S. J.; Nitta, A.; Guzik, J. A.; Bradley, P. A.; Sekiguchi, K.; Sullivan, D. J.; Sullivan, T.; Shobbrook, R. R.; Jiang, X.; Birch, P. V.; Ashoka, B. N.; Seetha, S.; Girish, V.; Joshi, S.; Dorokhova, T. N.; Dorokhov, N. I.; Akan, M. C.; Meištas, E. G.; Janulis, R.; Kalytis, R.; Ališauskas, D.; Anguma, S. K.; Kalebwe, P. C.; Moskalik, P.; Ogloza, W.; Stachowski, G.; Pajdosz, G.; Zola, S.

In: Monthly Notices of the Royal Astronomical Society, Vol. 340, No. 3, 11.04.2003, p. 1031-1038.

Research output: Contribution to journalArticle

Handler, G, O'Donoghue, D, Müller, M, Solheim, JE, Gonzalez-Perez, JM, Johannessen, F, Paparó, M, Szeidl, B, Viraghalmy, G, Silvotti, R, Vauclair, G, Dolez, N, Pallier, E, Chevreton, M, Kurtz, DW, Bromage, GE, Cunha, MS, Østensen, R, Fraga, L, Kanaan, A, Amorim, A, Giovannini, O, Kepler, SO, Da Costa, AFM, Anderson, RF, Wood, MA, Silvestri, N, Klumpe, EW, Carlton, RF, Miller, RH, McFarland, JP, Grauer, AD, Kawaler, SD, Riddle, RL, Reed, MD, Nather, RE, Winget, DE, Hill, JA, Metcalfe, TS, Mukadam, AS, Kilic, M, Watson, TK, Kleinman, SJ, Nitta, A, Guzik, JA, Bradley, PA, Sekiguchi, K, Sullivan, DJ, Sullivan, T, Shobbrook, RR, Jiang, X, Birch, PV, Ashoka, BN, Seetha, S, Girish, V, Joshi, S, Dorokhova, TN, Dorokhov, NI, Akan, MC, Meištas, EG, Janulis, R, Kalytis, R, Ališauskas, D, Anguma, SK, Kalebwe, PC, Moskalik, P, Ogloza, W, Stachowski, G, Pajdosz, G & Zola, S 2003, 'Amplitude and frequency variability of the pulsating DB white dwarf stars KUV 05134+2605 and PG 1654+160 observed with the Whole Earth Telescope', Monthly Notices of the Royal Astronomical Society, vol. 340, no. 3, pp. 1031-1038. https://doi.org/10.1046/j.1365-8711.2003.06373.x
Handler, G. ; O'Donoghue, D. ; Müller, M. ; Solheim, J. E. ; Gonzalez-Perez, J. M. ; Johannessen, F. ; Paparó, M. ; Szeidl, B. ; Viraghalmy, G. ; Silvotti, R. ; Vauclair, G. ; Dolez, N. ; Pallier, E. ; Chevreton, M. ; Kurtz, D. W. ; Bromage, G. E. ; Cunha, M. S. ; Østensen, R. ; Fraga, L. ; Kanaan, A. ; Amorim, A. ; Giovannini, O. ; Kepler, S. O. ; Da Costa, A. F M ; Anderson, R. F. ; Wood, M. A. ; Silvestri, N. ; Klumpe, E. W. ; Carlton, R. F. ; Miller, R. H. ; McFarland, J. P. ; Grauer, A. D. ; Kawaler, S. D. ; Riddle, R. L. ; Reed, M. D. ; Nather, R. E. ; Winget, D. E. ; Hill, J. A. ; Metcalfe, T. S. ; Mukadam, A. S. ; Kilic, M. ; Watson, T. K. ; Kleinman, S. J. ; Nitta, A. ; Guzik, J. A. ; Bradley, P. A. ; Sekiguchi, K. ; Sullivan, D. J. ; Sullivan, T. ; Shobbrook, R. R. ; Jiang, X. ; Birch, P. V. ; Ashoka, B. N. ; Seetha, S. ; Girish, V. ; Joshi, S. ; Dorokhova, T. N. ; Dorokhov, N. I. ; Akan, M. C. ; Meištas, E. G. ; Janulis, R. ; Kalytis, R. ; Ališauskas, D. ; Anguma, S. K. ; Kalebwe, P. C. ; Moskalik, P. ; Ogloza, W. ; Stachowski, G. ; Pajdosz, G. ; Zola, S. / Amplitude and frequency variability of the pulsating DB white dwarf stars KUV 05134+2605 and PG 1654+160 observed with the Whole Earth Telescope. In: Monthly Notices of the Royal Astronomical Society. 2003 ; Vol. 340, No. 3. pp. 1031-1038.
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abstract = "We have acquired new time series photometry of the two pulsating DB white dwarf stars KUV 05134+2605 and PG1654+160 with the Whole Earth Telescope. Additional single-site photometry is also presented. We use all these data plus all available archival measurements to study the temporal behaviour of the pulsational amplitudes and frequencies of these stars for the first time. We demonstrate that both KUV 05134+2605 and PG 1654+160 pulsate in many modes, the amplitudes of which are variable in time; some frequency variability of PG 1654+160 is also indicated. Beating of multiple pulsation modes cannot explain our observations; the amplitude variability must therefore be intrinsic. We cannot find stable modes to be used for determinations of the evolutionary period changes of the stars. Some of the modes of PG 1654+160 appear at the same periods whenever detected. The mean spacing of these periods (≈40 s) suggests that they are probably caused by non-radial gravity-mode pulsations of spherical degree 1 = 1. If so, PG 1654+160 has a mass around 0.6 M⊙. The time-scales of the amplitude variability of both stars (down to two weeks) are consistent with theoretical predictions of resonant mode coupling, a conclusion which might however be affected by the temporal distribution of our data.",
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TY - JOUR

T1 - Amplitude and frequency variability of the pulsating DB white dwarf stars KUV 05134+2605 and PG 1654+160 observed with the Whole Earth Telescope

AU - Handler, G.

AU - O'Donoghue, D.

AU - Müller, M.

AU - Solheim, J. E.

AU - Gonzalez-Perez, J. M.

AU - Johannessen, F.

AU - Paparó, M.

AU - Szeidl, B.

AU - Viraghalmy, G.

AU - Silvotti, R.

AU - Vauclair, G.

AU - Dolez, N.

AU - Pallier, E.

AU - Chevreton, M.

AU - Kurtz, D. W.

AU - Bromage, G. E.

AU - Cunha, M. S.

AU - Østensen, R.

AU - Fraga, L.

AU - Kanaan, A.

AU - Amorim, A.

AU - Giovannini, O.

AU - Kepler, S. O.

AU - Da Costa, A. F M

AU - Anderson, R. F.

AU - Wood, M. A.

AU - Silvestri, N.

AU - Klumpe, E. W.

AU - Carlton, R. F.

AU - Miller, R. H.

AU - McFarland, J. P.

AU - Grauer, A. D.

AU - Kawaler, S. D.

AU - Riddle, R. L.

AU - Reed, M. D.

AU - Nather, R. E.

AU - Winget, D. E.

AU - Hill, J. A.

AU - Metcalfe, T. S.

AU - Mukadam, A. S.

AU - Kilic, M.

AU - Watson, T. K.

AU - Kleinman, S. J.

AU - Nitta, A.

AU - Guzik, J. A.

AU - Bradley, P. A.

AU - Sekiguchi, K.

AU - Sullivan, D. J.

AU - Sullivan, T.

AU - Shobbrook, R. R.

AU - Jiang, X.

AU - Birch, P. V.

AU - Ashoka, B. N.

AU - Seetha, S.

AU - Girish, V.

AU - Joshi, S.

AU - Dorokhova, T. N.

AU - Dorokhov, N. I.

AU - Akan, M. C.

AU - Meištas, E. G.

AU - Janulis, R.

AU - Kalytis, R.

AU - Ališauskas, D.

AU - Anguma, S. K.

AU - Kalebwe, P. C.

AU - Moskalik, P.

AU - Ogloza, W.

AU - Stachowski, G.

AU - Pajdosz, G.

AU - Zola, S.

PY - 2003/4/11

Y1 - 2003/4/11

N2 - We have acquired new time series photometry of the two pulsating DB white dwarf stars KUV 05134+2605 and PG1654+160 with the Whole Earth Telescope. Additional single-site photometry is also presented. We use all these data plus all available archival measurements to study the temporal behaviour of the pulsational amplitudes and frequencies of these stars for the first time. We demonstrate that both KUV 05134+2605 and PG 1654+160 pulsate in many modes, the amplitudes of which are variable in time; some frequency variability of PG 1654+160 is also indicated. Beating of multiple pulsation modes cannot explain our observations; the amplitude variability must therefore be intrinsic. We cannot find stable modes to be used for determinations of the evolutionary period changes of the stars. Some of the modes of PG 1654+160 appear at the same periods whenever detected. The mean spacing of these periods (≈40 s) suggests that they are probably caused by non-radial gravity-mode pulsations of spherical degree 1 = 1. If so, PG 1654+160 has a mass around 0.6 M⊙. The time-scales of the amplitude variability of both stars (down to two weeks) are consistent with theoretical predictions of resonant mode coupling, a conclusion which might however be affected by the temporal distribution of our data.

AB - We have acquired new time series photometry of the two pulsating DB white dwarf stars KUV 05134+2605 and PG1654+160 with the Whole Earth Telescope. Additional single-site photometry is also presented. We use all these data plus all available archival measurements to study the temporal behaviour of the pulsational amplitudes and frequencies of these stars for the first time. We demonstrate that both KUV 05134+2605 and PG 1654+160 pulsate in many modes, the amplitudes of which are variable in time; some frequency variability of PG 1654+160 is also indicated. Beating of multiple pulsation modes cannot explain our observations; the amplitude variability must therefore be intrinsic. We cannot find stable modes to be used for determinations of the evolutionary period changes of the stars. Some of the modes of PG 1654+160 appear at the same periods whenever detected. The mean spacing of these periods (≈40 s) suggests that they are probably caused by non-radial gravity-mode pulsations of spherical degree 1 = 1. If so, PG 1654+160 has a mass around 0.6 M⊙. The time-scales of the amplitude variability of both stars (down to two weeks) are consistent with theoretical predictions of resonant mode coupling, a conclusion which might however be affected by the temporal distribution of our data.

KW - Stars: Oscillations

KW - Stars: Variables: Other

KW - Stars:individual:kuv05134+2605

KW - Stars:individual:pg 1654+160

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