Eclipsing binaries in the MOST satellite fields

Pribulla, T.; Ruciński, S. M.; Latham, David W.; Quinn, Samuel N.; Siwak, M.; Matthews, J. M.; Kuschnig, R.; Rowe, Jason F.; Guenther, D. B.; Moffat, A. F. J.; Sasselov, Dimitar; Walker, G. A. H.; Weiß, W. W.

doi:10.1002/asna.201011351

Cited by 22 publications

(21 citation statements)

References 32 publications

(41 reference statements)

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“…In this paper we examine the pulsation properties of four pulsators studied with the MOST satellite. Here we note that MOST satellite measurements were already suc-cessfully used in the study of the spectroscopic binary HD 73709 by Pribulla et al (2009Pribulla et al ( , 2010.…”

Section: Introductionmentioning

confidence: 99%

Delta Scuti stars in the Praesepe cluster observed by the MOST satellite

et al. 2012

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The Praesepe cluster contains a number of δ Sct and γ Dor pulsators. Asteroseismology of cluster stars is simplified by the common distance, age and stellar abundances. Since asteroseismology requires a large number of known frequencies, the small pulsation amplitudes of these stars require space satellite campaigns. The present study utilizes photometric MOST satellite measurements in order to determine the pulsation frequencies of two evolved (EP Cnc, BT Cnc) and two main-sequence (BS Cnc, HD 73872) δ Sct stars in the Praesepe cluster. The frequency analysis of the 2008 and 2009 data detected up to 34 frequencies per star with most amplitudes in the submillimag range. In BS Cnc, two modes showed strong amplitude variability between 2008 and 2009. The frequencies ranged from 0.76 to 41.7 cd −1 . After considering the different evolutionary states and mean stellar densities of these four stars, the differences and large ranges in frequency remain.

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Section: Introductionmentioning

confidence: 99%

Delta Scuti stars in the Praesepe cluster observed by the MOST satellite

et al. 2012

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“…If ω 90 • nor 270 • , for sufficiently low inclination angles the minimum occurring further away from the periastron can disappear and the observer can detect only one system of minima. This is the case for e.g., BD+37 410 (Pribulla et al 2010) or NY Cep (see Holmgren et al 1990). …”

Section: Orientation Of the Orbitmentioning

confidence: 92%

The nearby eclipsing stellar systemδVelorum

Pribulla¹,

Mérand²,

Kervella³

et al. 2011

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Context. The nearby multiple system δ Velorum contains a widely detached eclipsing binary and a third component. Aims. We take advantage of this system offering the opportunity to determine the set of fundamental parameters (masses, luminosities, and radii) of three coeval stars with sufficient precision to test models of stellar evolution. Methods. Extensive high-resolution spectroscopy is analyzed by the broadening function technique to provide the first spectroscopic orbit of the eclipsing pair. Simultaneous analysis of the spectroscopic data and the SMEI satellite light curve is performed to provide astrophysical parameters for the components. We use a modified Roche model assuming an eccentric orbit and asynchronous rotation. Results. The observations show that components of the eclipsing pair rotate at about two-thirds of the break-up velocity, which excludes any chemical peculiarity and results in a non-uniform surface brightness. Although the inner orbit is eccentric, no apsidal motion is seen during the SMEI photometric observations. For the inner orbit, the orbital parameters are eccentricity e = 0.290, longitude of the periastron passage ω = 109 • , and inclination 89.0 • . Conclusions. The component masses of M Aa = 2.53 ± 0.11 M , M Ab = 2.37 ± 0.10 M , and M B ∼ 1.5 M combined with the inferred radii of the Aa and Ab components indicate that the eclipsing pair has already left the main sequence and that the estimated age of the system is about 400 Myr.

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“…This work has subsequently been continued by MOST (Pribulla et al, 2010), CoRoT (e.g. Maceroni et al, 2009) and now Kepler.…”

Section: Eclipsing Binary Stars From Spacementioning

confidence: 95%

Space-Based Photometry of Eclipsing Binaries

Southworth¹

2011

Proc. IAU

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Abstract. I briefly review the history and prospects for the study of eclipsing binary star systems from space-based observatories. The benefits of shifting to space satellites lie in the high precision and cadence achievable, as well as the ability to access wavelength regions which are unattainable from the ground. Whilst small amounts of data on eclipsing binaries were obtained by the Voyager, IUE, OAO-II, Hipparcos and MOST, the more recent CoRoT and Kepler missions were the first to provide extensive data on large numbers of systems. The future holds the prospect of the PLATO satellite, which will go bigger, better and brighter.

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Eclipsing binaries in the MOST satellite fields

Cited by 22 publications

References 32 publications

Delta Scuti stars in the Praesepe cluster observed by the MOST satellite

Delta Scuti stars in the Praesepe cluster observed by the MOST satellite

The nearby eclipsing stellar systemδVelorum

Space-Based Photometry of Eclipsing Binaries

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