NDLI: Regular frequency patterns in the young δ Scuti star HD 261711 observed by the CoRoT and MOST satellites

Content Provider	EDP Sciences
Author	K. Zwintz L. Fossati D. B. Guenther T. Ryabchikova A. Baglin N. Themessl T. G. Barnes J. M. Matthews M. Auvergne D. Bohlender S. Chaintreuil R. Kuschnig A. F. J. Moffat J. F. Rowe S. M. Rucinski D. Sasselov W. W. Weiss
Abstract	Context. The internal structure of pre-main-sequence (PMS) stars is poorly constrained at present. This could change significantly through high-quality asteroseismological observations of a sample of such stars. Aims. We concentrate on an asteroseismological study of HD 261711, a rather hot δ Scuti-type pulsating member of the young open cluster NGC 2264 located at the blue border of the instability region. HD 261711 was discovered to be a PMS δ Scuti star using the time series photometry obtained by the MOST satellite in 2006. Methods. High-precision, time-series photometry of HD 261711 was obtained by the MOST and CoRoT satellites in four separate new observing runs that are put into context with the star’s fundamental atmospheric parameters obtained from spectroscopy. Frequency Analysis was performed using Period04. The spectral analysis was performed using equivalent widths and spectral synthesis.Results. With the new MOST data set from 2011/12 and the two CoRoT light curves from 2008 and 2011/12, the δ Scuti variability was confirmed and regular groups of frequencies were discovered. The two pulsation frequencies identified in the data from the first MOST observing run in 2006 are confirmed and 23 new δ Scuti-type frequencies were discovered using the CoRoT data. Weighted average frequencies for each group were determined and are related to l = 0 and l = 1 p-modes. Evidence for amplitude modulation of the frequencies in two groups is seen. The effective temperature (T_{eff_{) was derived to be 8600 ± 200 K, log g is 4.1 ± 0.2, and the projected rotational velocity (υsini) is 53 ± 1 km s^{-1^{. Using our T_{eff_{value and the radius of 1.8 ± 0.5 R_{⊙_{derived from spectral energy distribution (SED) fitting, we get a luminosity log L/L_{⊙_{of 1.20 ± 0.14 which agrees well to the seismologically determined values of 1.65 R_{⊙_{and, hence, a log L/L_{⊙_{of 1.13. The radial velocity of 14 ± 2 km s^{-1^{we derived for HD 261711, confirms the star’s membership to NGC 2264.Conclusions. Our asteroseismic models suggest that HD 261711 is a δ Scuti-type star close to the zero-age main sequence (ZAMS) with a mass of 1.8 to 1.9 M_{⊙_{. With an age of about 10 million years derived from asteroseismology, the star is either a young ZAMS star or a late PMS star just before the onset of hydrogen-core burning. The observed splittings about the l = 0 and 1 parent modes may be an artifact of the Fourier derived spectrum of frequencies with varying amplitudes.}}}}}}}}}}}}}}}}}}
Page Count	12
File Format	HTM / HTML PDF
ISSN	00046361
Alternate Webpage(s)	https://www.aanda.org/articles/aa/abs/2013/04/aa20934-12/aa20934-12.html
e-ISSN	14320746
Journal	Astronomy & Astrophysics
Volume Number	552
DOI	10.1051/0004-6361/201220934
Language	English
Publisher	EDP Sciences
Publisher Date	2013-04-01
Access Restriction	Open
Rights Holder	© ESO, 2013
Subject Keyword	stars: variables: delta Scuti stars: oscillations stars: individual: HD 261711 techniques: photometric techniques: spectroscopic stars: variables: delta Scuti / stars: oscillations / stars: individual: HD 261711 / techniques: photometric / techniques: spectroscopic
Content Type	Text
Resource Type	Article
Subject	Astronomy and Astrophysics Space and Planetary Science

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