Oscillations in the PMS <i>δ</i> Scuti star
 V346 Ori

Pinheiro, F. J. G.; Folha, D. F. M.; Marconi, M.; Ripepi, V.; Palla, F.; Monteiro, M. J. P. F. G.; Bernabei, S.

doi:10.1051/0004-6361:20021792

Cited by 15 publications

(18 citation statements)

References 14 publications

(12 reference statements)

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“…We can now compare the present results with those obtained by Pinheiro et al (2003). As a result, the two significant frequencies seen by Pinheiro et al (2003) are not in disagreement with our results.…”

Section: Frequency Analysissupporting

confidence: 82%

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Multi-site photometry of the pulsating Herbig Ae star V346 Ori

Bernabei

Ripepi

Ruoppo

et al. 2009

A&A

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Context. The study of pulsation in pre-main-sequence intermediate-mass stars represents an important tool for deriving information about fundamental stellar parameters and internal structure, as well as testing theoretical models. Interest in this class of variable stars has increased significantly during the last decade and about 30 members are presently known in the literature. Aims. After constructing the frequency spectrum of oscillations in V346 Ori, we apply asteroseismic tools to these data to estimate the intrinsic parameters (mass, luminosity, effective temperature) of V346 Ori and obtain information about its internal structure. Methods. CCD time-series photometry in the Johnson V filter was obtained for a total of 145.7 h of observations distributed over 36 nights. The resulting light curves were subjected to a detailed frequency analysis using updated numerical techniques. Photometric and spectroscopic data were also acquired to determine reliable estimates of the stellar properties. Results. We identified 13 oscillation frequencies, 6 of which with higher significance. These were compared with the predictions of non-radial adiabatic models. The resulting best-fit model corresponds to a mass of 2.1 ± 0.2 M , luminosity log L/L = 1.37 +0.11 −0.13 , and effective temperature 7300 ± 200 K. These values are marginally consistent with the association of V346 Ori to Orion OB1a. Alternatively, V346 Ori could be placed at a slightly larger distance than previously estimated.

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Section: Frequency Analysissupporting

confidence: 82%

“…As a result, the two significant frequencies seen by Pinheiro et al (2003) are not in disagreement with our results.…”

Section: Frequency Analysissupporting

confidence: 57%

Multi-site photometry of the pulsating Herbig Ae star V346 Ori

Bernabei

Ripepi

Ruoppo

et al. 2009

A&A

Self Cite

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“…Today, approximately thirteen intermediatemass PMS stars have revealed to be pulsating at timescales typical of δ Scuti variables: HR 5999 (Kurtz & Marang 1995;Kurtz & Catala 2001), HD 104237 (Donati et al 1997;Kurtz & Muller 1999, hereafter KM), as well as eleven other candidates (Kurtz & Müller 2001;Marconi et al 2001;Marconi et al 2002;Zwintz & Weiss 2003). Typical pulsation periods range from half an hour (V 346 Ori, Pinheiro et al 2003) to almost 5 h (HR 5999, Kurtz & Marang 1995). A recent review by Catala (2003) presents the status of observational studies of pulsations in these stars.…”

Section: Introductionmentioning

confidence: 99%

Spectroscopic monitoring of the Herbig Ae star HD 104237

Böhm

Catala

Balona

et al. 2004

A&A

133

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Abstract. We present the results of multisite observations spanning two years of the pre-main-sequence Herbig Ae star HD 104237. The star was observed in high resolution spectroscopy (R ≥ 35 000) for a total of 157.3 h of effective exposure time, over 42 nights, corresponding to a data base of 1888 individual echelle spectra. We confirm that the HD 104237 system includes a spectroscopic binary, whose primary component HD 104237 A is pulsating. The resulting high quality radial velocity curve allows us to detect for the first time by spectroscopic means multiperiodic oscillations in a pre-main sequence star. Five different modes are detected with very high confidence, with frequencies ranging between 28.5 and 35.6 d −1 , typical of δ Scuti pulsations; an additional 3 frequencies have been extracted from the data, but with a lower level of confidence. The pattern of frequencies indicates that at least some of the detected modes are non-radial. The precise orbit determination and the measurement of the double line spectroscopic binary observed around periastron enabled us to determine a mass ratio of 1.29 ± 0.02 between the primary and the secondary; based on the primary mass of 2.2 ± 0.1 M we conclude that the spectroscopic secondary HD 104237 b should have a mass of 1.7 ± 0.1 M and lie outside the pre-main sequence instability strip towards later spectral types. A search for pulsations in the radial velocity curve of the much weaker secondary component was not conclusive at this stage. The location of the primary in the HR diagram and its position with respect to recent pre-main sequence evolutionary tracks and isochrones implies a location of the secondary indicative of spectral type K3.

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“…Ripepi et al (2003) present multisite observations of V353 Ori in which 5 frequencies are detected. Pinheiro et al (2003) detected two periods in V346 Ori.…”

Section: Pulsations In Pre-main Sequence A-type Starsmentioning

confidence: 95%

Pulsations of A stars

Balona

2004

Proc. IAU

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Abstract.A review of recent work on pulsating A stars is presented. The types of pulsating stars are the roAp, δ Scuti, λ Bootis, Am stars, pre-Main Sequence pulsating A stars and α Cygni stars (pulsating A supergiants). Population II pulsating A stars such as SX Phe (blue stragglers) and RR Lyraes are also discussed. The emphasis is on the physics that can be derived from the study of stellar pulsations and suggestions for further progress.

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Oscillations in the PMS δ Scuti star V346 Ori

Cited by 15 publications

References 14 publications

Multi-site photometry of the pulsating Herbig Ae star V346 Ori

Multi-site photometry of the pulsating Herbig Ae star V346 Ori

Spectroscopic monitoring of the Herbig Ae star HD 104237

Pulsations of A stars

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