Multisite observations of the PMS <i>δ</i>Scuti star V351 Ori

Ripepi, V.; Marconi, M.; Bernabei, S.; Palla, F.; Pinheiro, F. J. G.; Folha, D. F. M.; Oswalt, Terry D.; Terranegra, L.; Ferro, A. Arellano; Jiang, Xiaojun; Alcalá, J. M.; Marinoni, S.; Monteiro, M. J. P. F. G.; Rudkin, M.; Johnston, K.

doi:10.1051/0004-6361:20031011

Cited by 23 publications

(30 citation statements)

References 18 publications

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“…It has been proposed that a temporarily strong accretion of matter onto the star or extinction by circumstellar dust clouds takes place to explain the remarkable V351 Ori change of behaviour from "that of a [HAeBe] star with strong photometric variations [...] to that of an almost non-variable star" (van den Ancker et al 1996). The main period of pulsations of V351 Ori is only of the order of 0.06 d with a peak-to-peak amplitude of about 0.1 mag (van den Ancker et al 1998;Marconi et al 2001;Ripepi et al 2003). The pre-main sequence nature of the star is supported by the presence of Hα in emission, a pronounced inverse P Cygni profile, S I λ1296Å and O I λ1304Å lines in emission, and infrared excess (Valenti et al 2000 and references above).…”

Section: V351 Ori (No 70)mentioning

confidence: 99%

Finding the most variable stars in the Orion Belt with the All Sky Automated Survey

2010

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We look for high-amplitude variable young stars in the open clusters and associations of the Orion Belt. We use public data from the ASAS-3 Photometric V -band Catalogue of the All Sky Automated Survey, infrared photometry from the 2MASS and IRAS catalogues, proper motions, and the Aladin sky atlas to obtain a list of the most variable stars in a survey area of side 5 deg centred on the bright star Alnilam (ǫ Ori) in the centre of the Orion Belt. We identify 32 highly-variable stars, of which 16 had not been reported to vary before. They are mostly variable young stars and candidates (16) and background giants (8), but there are also field cataclysmic variables, contact binaries, and eclipsing binary candidates. Of the young stars, which typically are active Herbig Ae/Be and T Tauri stars with Hα emission and infrared flux excess, we discover four new variables and confirm the variability status of another two. Some of them belong to the well known σ Orionis cluster. Besides, six of the eight giants are new variables, and three are new periodic variables.

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Section: V351 Ori (No 70)mentioning

confidence: 99%

Finding the most variable stars in the Orion Belt with the All Sky Automated Survey

2010

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“…After the seminal work by Marconi & Palla (1998), who established the locus of the theoretical instability strip in the HR diagram, it has become clear that these stars pulsate as δ Sct variables (see e.g. Ripepi et al 2002Ripepi et al , 2003Marconi & Palla 2004;Ripepi et al 2006a,b;Zwintz 2008 and references therein). More recently, highprecision photometry from space missions such as MOST and CoRoT showed that intermediate-mass PMS stars can also pulsate as hybrid δ Sct/γ Dor stars (Ripepi et al 2011) or pure γ Dor stars (Zwintz et al 2013).…”

Section: Introductionmentioning

confidence: 99%

Keplerobservations of A–F pre-main-sequence stars in Upper Scorpius: discovery of six new δ Scuti and one γ Doradus stars

Ripepi¹,

Balona²,

Catanzaro³

et al. 2015

Mon. Not. R. Astron. Soc.

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We present light curves and periodograms for 27 stars in the young Upper Scorpius association (age=11 ± 1 Myr) obtained with the Kepler spacecraft. This association is only the second stellar grouping to host several pulsating pre-main sequence (PMS) stars which have been observed from space.From an analysis of the periodograms, we identify six δ Scuti variables and one γ Doradus star. These are most likely PMS stars or else very close to the zero-age main sequence. Four of the δ Scuti variables were observed in short-cadence mode, which allows us to resolve the entire frequency spectrum. For these four stars, we are able to infer some qualitative information concerning their ages. For the remaining two δ Scuti stars, only long-cadence data are available, which means that some of the frequencies are likely to be aliases. One of the stars appears to be a rotational variable in a hierarchical triple system. This is a particularly important object, as it allows the possibility of an accurate mass determination when radial velocity observations become available. We also report on new high-resolution echelle spectra obtained for some of the stars of our sample.

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“…Since the work by MP98, many new PMS δ Scuti candidates have been observed and the current census of known or suspected candidates includes about 30 stars (see e.g., Ripepi et al 2006a;Zwintz 2008). However, only a few of these have been studied in detail (e.g., Ripepi et al 2003;Böhm et al 2004;Ripepi et al 2006b). Thus, the overall properties of this class of variable stars remain poorly determined.…”

Section: Introductionmentioning

confidence: 99%

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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Multisite observations of the PMS δScuti star V351 Ori

Cited by 23 publications

References 18 publications

Finding the most variable stars in the Orion Belt with the All Sky Automated Survey

Finding the most variable stars in the Orion Belt with the All Sky Automated Survey

Keplerobservations of A–F pre-main-sequence stars in Upper Scorpius: discovery of six new δ Scuti and one γ Doradus stars

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

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