The rapidly pulsating subdwarf B star PG 1325+101 I. Oscillation modes from multisite observations

R. Silvotti; A. Bonanno; S. Bernabei; G. Fontaine; S. Charpinet; S. Leccia; H. Kjeldsen; R. Janulis; A. Frasca; R. Østensen; S. L. Kim; B. G. Park; X. Jiang; M. D. Reed; R. S. Patterson; K. M. Gietzen; P. J. Clark; G. W. Wolf; Y. Lipkin; L. Formiggini; E. Leibowitz; T. D. Oswalt; M. Rudkin; K. Johnston; P. Brassard; P. Chayer; E. M. Green; P. Bergeron

doi:10.1051/0004-6361:20065314

The rapidly pulsating subdwarf B star PG 1325+101 I. Oscillation modes from multisite observations

R. Silvotti, A. Bonanno, S. Bernabei, G. Fontaine, S. Charpinet, S. Leccia, H. Kjeldsen, R. Janulis, A. Frasca, R. Østensen, S. L. Kim, B. G. Park, X. Jiang, M. D. Reed, R. S. Patterson, K. M. Gietzen, P. J. Clark, G. W. Wolf, Y. Lipkin, L. FormigginiE. Leibowitz, T. D. Oswalt, M. Rudkin, K. Johnston, P. Brassard, P. Chayer, E. M. Green, P. Bergeron

Steward Observatory

Research output: Contribution to journal › Article › peer-review

18 Scopus citations

Abstract

In this article we present the results of 215 h of time-series photometry on the rapidly pulsating subdwarf B star PG 1325+101 (T_eff - 35 000 K, log g = 5.8, log N(Hs)/N(H) = -1.7), obtained during 25 days of observation in Spring 2003 from nine different sites. As in previous observations, the temporal spectrum is dominated by the main peak at 7255.55 μHz, with an amplitude of about 2.7% which, however, is dropped to about 1.7% in February 2005. No secondary peaks close to the dominant pulsation mode are clearly detected. In addition, at least fourteen more pulsation frequencies are found: three of them at 7704.92, 9380.17 and 14511.10 μHz were already present in the discovery run with small differences in frequency, probably due to 1-day aliasing effects. The peak at 7704.92 μHz belongs to a triplet of almost equally spaced frequencies that could be due to rotational splitting and would imply a rotational period of about 1.6 days. Based on the results of this article, a detailed asteroseismic analysis of PG 1325+101 is presented in a separate paper (Charpinet et al. 2006b, A&A, 459, 565, Paper II).

Original language	English (US)
Pages (from-to)	557-564
Number of pages	8
Journal	Astronomy and astrophysics
Volume	459
Issue number	2
DOIs	https://doi.org/10.1051/0004-6361:20065314
State	Published - Nov 2006

Keywords

Stars: horizontal-branch
Stars: individual: PG 1325+101
Stars: interiors
Stars: oscillations

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.1051/0004-6361:20065314

Cite this

Silvotti, R., Bonanno, A., Bernabei, S., Fontaine, G., Charpinet, S., Leccia, S., Kjeldsen, H., Janulis, R., Frasca, A., Østensen, R., Kim, S. L., Park, B. G., Jiang, X., Reed, M. D., Patterson, R. S., Gietzen, K. M., Clark, P. J., Wolf, G. W., Lipkin, Y., ... Bergeron, P. (2006). The rapidly pulsating subdwarf B star PG 1325+101 I. Oscillation modes from multisite observations. Astronomy and astrophysics, 459(2), 557-564. https://doi.org/10.1051/0004-6361:20065314

Silvotti, R, Bonanno, A, Bernabei, S, Fontaine, G, Charpinet, S, Leccia, S, Kjeldsen, H, Janulis, R, Frasca, A, Østensen, R, Kim, SL, Park, BG, Jiang, X, Reed, MD, Patterson, RS, Gietzen, KM, Clark, PJ, Wolf, GW, Lipkin, Y, Formiggini, L, Leibowitz, E, Oswalt, TD, Rudkin, M, Johnston, K, Brassard, P, Chayer, P, Green, EM & Bergeron, P 2006, 'The rapidly pulsating subdwarf B star PG 1325+101 I. Oscillation modes from multisite observations', Astronomy and astrophysics, vol. 459, no. 2, pp. 557-564. https://doi.org/10.1051/0004-6361:20065314

@article{8a5988d7b95b4839a6efb99f7641febf,

title = "The rapidly pulsating subdwarf B star PG 1325+101 I. Oscillation modes from multisite observations",

abstract = "In this article we present the results of 215 h of time-series photometry on the rapidly pulsating subdwarf B star PG 1325+101 (Teff - 35 000 K, log g = 5.8, log N(Hs)/N(H) = -1.7), obtained during 25 days of observation in Spring 2003 from nine different sites. As in previous observations, the temporal spectrum is dominated by the main peak at 7255.55 μHz, with an amplitude of about 2.7% which, however, is dropped to about 1.7% in February 2005. No secondary peaks close to the dominant pulsation mode are clearly detected. In addition, at least fourteen more pulsation frequencies are found: three of them at 7704.92, 9380.17 and 14511.10 μHz were already present in the discovery run with small differences in frequency, probably due to 1-day aliasing effects. The peak at 7704.92 μHz belongs to a triplet of almost equally spaced frequencies that could be due to rotational splitting and would imply a rotational period of about 1.6 days. Based on the results of this article, a detailed asteroseismic analysis of PG 1325+101 is presented in a separate paper (Charpinet et al. 2006b, A&A, 459, 565, Paper II).",

keywords = "Stars: horizontal-branch, Stars: individual: PG 1325+101, Stars: interiors, Stars: oscillations",

author = "R. Silvotti and A. Bonanno and S. Bernabei and G. Fontaine and S. Charpinet and S. Leccia and H. Kjeldsen and R. Janulis and A. Frasca and R. {\O}stensen and Kim, {S. L.} and Park, {B. G.} and X. Jiang and Reed, {M. D.} and Patterson, {R. S.} and Gietzen, {K. M.} and Clark, {P. J.} and Wolf, {G. W.} and Y. Lipkin and L. Formiggini and E. Leibowitz and Oswalt, {T. D.} and M. Rudkin and K. Johnston and P. Brassard and P. Chayer and Green, {E. M.} and P. Bergeron",

year = "2006",

month = nov,

doi = "10.1051/0004-6361:20065314",

language = "English (US)",

volume = "459",

pages = "557--564",

journal = "Astronomy and astrophysics",

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TY - JOUR

T1 - The rapidly pulsating subdwarf B star PG 1325+101 I. Oscillation modes from multisite observations

AU - Silvotti, R.

AU - Bonanno, A.

AU - Bernabei, S.

AU - Fontaine, G.

AU - Charpinet, S.

AU - Leccia, S.

AU - Kjeldsen, H.

AU - Janulis, R.

AU - Frasca, A.

AU - Østensen, R.

AU - Kim, S. L.

AU - Park, B. G.

AU - Jiang, X.

AU - Reed, M. D.

AU - Patterson, R. S.

AU - Gietzen, K. M.

AU - Clark, P. J.

AU - Wolf, G. W.

AU - Lipkin, Y.

AU - Formiggini, L.

AU - Leibowitz, E.

AU - Oswalt, T. D.

AU - Rudkin, M.

AU - Johnston, K.

AU - Brassard, P.

AU - Chayer, P.

AU - Green, E. M.

AU - Bergeron, P.

PY - 2006/11

Y1 - 2006/11

N2 - In this article we present the results of 215 h of time-series photometry on the rapidly pulsating subdwarf B star PG 1325+101 (Teff - 35 000 K, log g = 5.8, log N(Hs)/N(H) = -1.7), obtained during 25 days of observation in Spring 2003 from nine different sites. As in previous observations, the temporal spectrum is dominated by the main peak at 7255.55 μHz, with an amplitude of about 2.7% which, however, is dropped to about 1.7% in February 2005. No secondary peaks close to the dominant pulsation mode are clearly detected. In addition, at least fourteen more pulsation frequencies are found: three of them at 7704.92, 9380.17 and 14511.10 μHz were already present in the discovery run with small differences in frequency, probably due to 1-day aliasing effects. The peak at 7704.92 μHz belongs to a triplet of almost equally spaced frequencies that could be due to rotational splitting and would imply a rotational period of about 1.6 days. Based on the results of this article, a detailed asteroseismic analysis of PG 1325+101 is presented in a separate paper (Charpinet et al. 2006b, A&A, 459, 565, Paper II).

AB - In this article we present the results of 215 h of time-series photometry on the rapidly pulsating subdwarf B star PG 1325+101 (Teff - 35 000 K, log g = 5.8, log N(Hs)/N(H) = -1.7), obtained during 25 days of observation in Spring 2003 from nine different sites. As in previous observations, the temporal spectrum is dominated by the main peak at 7255.55 μHz, with an amplitude of about 2.7% which, however, is dropped to about 1.7% in February 2005. No secondary peaks close to the dominant pulsation mode are clearly detected. In addition, at least fourteen more pulsation frequencies are found: three of them at 7704.92, 9380.17 and 14511.10 μHz were already present in the discovery run with small differences in frequency, probably due to 1-day aliasing effects. The peak at 7704.92 μHz belongs to a triplet of almost equally spaced frequencies that could be due to rotational splitting and would imply a rotational period of about 1.6 days. Based on the results of this article, a detailed asteroseismic analysis of PG 1325+101 is presented in a separate paper (Charpinet et al. 2006b, A&A, 459, 565, Paper II).

KW - Stars: horizontal-branch

KW - Stars: individual: PG 1325+101

KW - Stars: interiors

KW - Stars: oscillations

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UR - http://www.scopus.com/inward/citedby.url?scp=33750995288&partnerID=8YFLogxK

U2 - 10.1051/0004-6361:20065314

DO - 10.1051/0004-6361:20065314

M3 - Article

AN - SCOPUS:33750995288

SN - 0004-6361

VL - 459

SP - 557

EP - 564

JO - Astronomy and astrophysics

JF - Astronomy and astrophysics

IS - 2

ER -

The rapidly pulsating subdwarf B star PG 1325+101 I. Oscillation modes from multisite observations

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The rapidly pulsating subdwarf B star PG 1325+101 I. Oscillation modes from multisite observations

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Keywords

ASJC Scopus subject areas

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Oscillation modes of PG 1325+101

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