The B0.5IVe CoRoT target HD 49330

Huat, Anne-Laure; Hubert, A. M.; Baudin, F.; Floquet, M.; Neiner, C.; Frémat, Y.; Gutiérrez‐Soto, J.; Andrade, L.; Batz, B. de; Diago, P. D.; Emílio, M.; Lara, F. Espinosa; Fabregat, J.; Janot-Pacheco, E.; Leroy, B.; Martayan, C.; Semaan, T.; Suso, J.; Auvergne, M.; Catala, C.; Michel, E.; Samadi, R.

doi:10.1051/0004-6361/200911928

Cited by 104 publications

(165 citation statements)

References 13 publications

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“…Therefore, it seems that the beating effect influences the circumstellar environment. A correlation between pulsation properties and Be outbursts was observed in the star HD 49330 (Huat et al 2009). We note also that the beating frequency corresponds to a tenth of f 1, which is probably a coincidence.…”

Section: Beating Effectsmentioning

confidence: 89%

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The pulsations of the B5IVe star HD 181231 observed with CoRoT and ground-based spectroscopy

Neiner¹,

Gutiérrez‐Soto²,

Baudin

et al. 2009

A&A

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Context. HD 181231 is a B5IVe star, which has been observed with the CoRoT satellite during ∼5 consecutive months and simultaneously from the ground in spectroscopy and spectropolarimetry. Aims. By analysing these data, we aim to detect and characterize as many pulsation frequencies as possible, to search for the presence of beating effects possibly at the origin of the Be phenomenon. Our results will also provide a basis for seismic modelling. Methods. The fundamental parameters of the star are determined from spectral fitting and from the study of the circumstellar emission. The CoRoT photometric data and ground-based spectroscopy are analysed using several Fourier techniques: Clean-ng, Pasper, and Tisaft, as well as a time-frequency technique. A search for a magnetic field is performed by applying the LSD technique to the spectropolarimetric data. Results. We find that HD 181231 is a B5IVe star seen with an inclination of ∼45 degrees. No magnetic field is detected in its photosphere. We detect at least 10 independent significant frequencies of variations among the 54 detected frequencies, interpreted in terms of non-radial pulsation modes and rotation. Two longer-term variations are also detected: one at ∼14 days resulting from a beating effect between the two main frequencies of short-term variations, the other at ∼116 days due either to a beating of frequencies or to a zonal pulsation mode. Conclusions. Our analysis of the CoRoT light curve and ground-based spectroscopic data of HD 181231 has led to the determination of the fundamental and pulsational parameters of the star, including beating effects. This will allow a precise seismic modelling of this star.

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Section: Beating Effectsmentioning

confidence: 89%

“…This method is described in detail in Huat et al (2009). We either searched for frequencies with Clean-ng or Pasper in each sub-sample, or imposed the main frequencies detected over the entire run.…”

Section: Corot Photometric Datamentioning

confidence: 99%

The pulsations of the B5IVe star HD 181231 observed with CoRoT and ground-based spectroscopy

Neiner¹,

Gutiérrez‐Soto²,

Baudin

et al. 2009

A&A

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“…The error estimate on the frequency is computed as in Degroote et al (2009a), i.e., using the formula of Montgomery & O'Donoghue (1999), but also taking correlation effects into account according to the formalism by Schwarzenberg-Czerny (2003). Recent studies of CoRoT light curves of B-type stars highlighted variations in the amplitude of frequencies and in the frequencies themselves as a function of time (e.g., in the β Cep star HD 180642, Degroote et al 2009b; in the B0.5IVe star HD 49330, Huat et al 2009). In order to check the stability of the frequencies of HD 46202 listed in Table 1, we applied a short time Fourier transform.…”

Section: Frequency Analysis On Corot Photometrymentioning

confidence: 99%

An asteroseismic study of the O9V star HD 46202 from CoRoT space-based photometry

Briquet

Aerts

Baglin

et al. 2011

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The O9V star HD 46202, which is a member of the young open cluster NGC 2244, was observed by the CoRoT satellite in October/November 2008 during a short run of 34 days. From the very high-precision light curve, we clearly detect β Cep-like pulsation frequencies with amplitudes of ∼0.1 mmag and below. A comparison with stellar models was performed using a χ 2 as a measure for the goodness-of-fit between the observed and theoretically computed frequencies. The physical parameters of our best-fitting models are compatible with the ones deduced spectroscopically. A core overshooting parameter α ov = 0.10 ± 0.05 pressure scale height is required. None of the observed frequencies are theoretically excited with the input physics used in our study. More theoretical work is thus needed to overcome this shortcoming in how we understand the excitation mechanism of pulsation modes in such a massive star. A similar excitation problem has also been encountered for certain pulsation modes in β Cep stars recently modelled asteroseismically.

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“…In addition, we performed a time-frequency analysis of the original light curve by applying the pasper code to sliding windows with different sizes (for details on the method, see Huat et al 2009). The results presented in Fig.…”

Section: Frequency Analysismentioning

confidence: 99%

Pulsations in the late-type Be star HD 50 209 detected by CoRoT

Diago¹,

Gutiérrez‐Soto

Auvergne

et al. 2009

A&A

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Context. The presence of pulsations in late-type Be stars is still a matter of controversy. It constitutes an important issue to establish the relationship between non-radial pulsations and the mass-loss mechanism in Be stars. Aims. To contribute to this discussion, we analyse the photometric time series of the B8IVe star HD 50 209 observed by the CoRoT mission in the seismology field. Methods. We use standard Fourier techniques and linear and non-linear least squares fitting methods to analyse the CoRoT light curve. In addition, we applied detailed modelling of high-resolution spectra to obtain the fundamental physical parameters of the star. Results. We have found four frequencies which correspond to gravity modes with azimuthal order m = 0, −1, −2, −3 with the same pulsational frequency in the co-rotating frame. We also found a rotational period with a frequency of 0.679 cd −1 (7.754 μHz). Conclusions. HD 50 209 is a pulsating Be star as expected from its position in the HR diagram, close to the SPB instability strip.

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The B0.5IVe CoRoT target HD 49330

Cited by 104 publications

References 13 publications

The pulsations of the B5IVe star HD 181231 observed with CoRoT and ground-based spectroscopy

The pulsations of the B5IVe star HD 181231 observed with CoRoT and ground-based spectroscopy

An asteroseismic study of the O9V star HD 46202 from CoRoT space-based photometry

Pulsations in the late-type Be star HD 50 209 detected by CoRoT

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