The Rossiter-McLaughlin Rotation Effect Observed for AI Draconis and V505 Sagittarii

Worek, T. F.

doi:10.1086/133820

Cited by 16 publications

(19 citation statements)

References 16 publications

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“…With the absolute stellar radii derived from our light‐curve solution, the predicted equatorial synchronous rotation velocities are V syn = 87.0 and 96.9 km s −1 , for the primary and secondary star, respectively. With the secondary filling its Roche lobe, the rotational velocity of the primary in good agreement with the value measured by Worek (1996), and the agreement between the value quoted for the secondary and those obtained from our spectroscopic data (100–110 km s −1 , see above), the assumption of synchronous rotation made in our analysis is well justified.…”

Section: Discussionsupporting

confidence: 90%

“…In the catalogue of Brancewicz & Dworak (1980), AI Dra is classified as a detached A0V +F9 system, with masses M 1 = 2.3 M ⊙ and M 2 = 1.1 M ⊙ For the rotational velocity of the primary star, the value v r = 97 km s −1 is given by Bernacca & Perinotto (1970) and Uesugi & Fukuda (1970). More recently, from the Rossiter–McLaughlin rotation effect on the radial velocity curve during the primary eclipse, Worek (1996) deduced for the primary a projected rotational velocity of 85.6 ± 2.8 km s −1 , slightly lower than the corresponding synchronous value.…”

Section: Introductionmentioning

confidence: 92%

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The fundamental parameters of the Algol binary AI Draconis revisited

Lázaro¹,

Martínez‐País²,

Arévalo³

2004

Monthly Notices of the Royal Astronomical Society

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We present the results of an analysis of our infrared light curves of the Algol-type binary AI Draconis in the J, H and K bands, and of published light curves in the B, V and Strömgren uvby bands, together with spectra obtained by us. The analysis of the light curves was carried out using a code based on ATLAS model atmospheres and Roche geometry.The small contribution of the secondary cool component to the total light of the system in the visible, producing light curves with very shallow secondary eclipses, makes the stellar and orbital parameters derived from light-curve analysis in the visible spectral range uncertain. The larger contribution of the secondary star to the infrared fluxes makes this range particularly well suited to the derivation of precise orbital and stellar parameters in binaries of Algol type. From the simultaneous solution of the infrared JHK light curves, we derive the following absolute orbital and stellar parameters for the two components: T eff,1 = 10 160 ± 160 K, R eq,1 = 2.12 ± 0.04 R , log( g ) 1 = 4.23; T eff,2 = 5586 ± 110 K, R eq,2 = 2.36 ± 0.04 R , log( g ) 2 = 3.76; M 1 = 2.86 ± 0.09 M , q = M 2 /M 1 = 0.44 ± 0.03; a = 7.62 ± 0.09 R , i = 76.53 • ± 0.3 • , e 0.0. Here, T eff and log( g ) indicate average surface values, R eq is the equivalent radius of the deformed star and a is the orbital size.In our light-curve solutions, the secondary star of AI Dra fills its Roche lobe (as also indicated by the spectroscopy), thus discounting claims, based on UBV light curves, that both components of the binary are located within their Roche lobes. The visible and infrared photometry show no evidence of any significant infrared excess in the system, and the distance of AI Dra is estimated as d = 169 ± 17 pc.Based on the spectra of AI Dra and template stars in the ranges 8210-9060, 6250-7130 and 4040-4920 Å, we classify the stellar components of AI Dra and find that the most probable spectral types are A0V (or perhaps A1V) for the primary and F9.5V for the secondary (although it could reach as far as G4V), respectively. From our spectroscopic observations, the spectral evolution of AI Dra with orbital phase is also presented. Furthermore, we obtain the projected rotational velocity of the secondary, whose value turns out to be compatible with the star filling its Roche lobe.

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Section: Discussionsupporting

confidence: 90%

Section: Introductionmentioning

confidence: 92%

The fundamental parameters of the Algol binary AI Draconis revisited

Lázaro¹,

Martínez‐País²,

Arévalo³

2004

Monthly Notices of the Royal Astronomical Society

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“…For example, if only the receding half of a star is visible, then the starlight is redshifted in excess of the shift one would expect from only the star's center-of-mass motion. This effect has long been observed during eclipses of binary stars (see, e.g., Worek 1996, Rauch & Werner 2003, and more recently during transits of extrasolar planets (Bundy & Marcy 2000, Queloz et al 2000, Snellen 2005, Winn et al 2005. To estimate the magnitude of the effect, suppose that a star of radius R is occulted by a straight-edged semi-infinite screen, as depicted in the left panel of Fig.…”

Section: Radial Velocitiesmentioning

confidence: 97%

The Orbit and Occultations of KH 15D

Winn

Hamilton

Herbst

et al. 2006

ApJ

132

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The unusual flux variations of the pre-main-sequence binary star KH 15D have been attributed to occultations by a circumbinary disk. We test whether or not this theory is compatible with newly available data, including recent radial velocity measurements, CCD photometry over the past decade, and photographic photometry over the past 50 years. We find the model to be successful, after two refinements: a more realistic motion of the occulting feature, and a halo around each star that probably represents scattering by the disk. The occulting feature is exceptionally sharp-edged, raising the possibility that the dust in the disk has settled into a thin layer, and providing a tool for fine-scale mapping of the immediate environment of a T Tauri star. However, the window of opportunity is closing, as the currently visible star may be hidden at all orbital phases by as early as 2008.Comment: To appear in ApJ [16 pages, 13 figures

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“…Slettebak (1985) is a good source of citations about this epoch. Worek (1996) and Hube & Couch (1982) are two examples of more recent observations of the Rossiter-McLaughlin effect. The rotation effect was also used for cataclysmic variables to determine if the accreting material comes from a disc in a plane similar to the binary's orbital plane (Young & Schneider 1980).…”

Section: Introductionmentioning

confidence: 95%

The EBLM project

Triaud¹,

Hebb²,

Anderson³

et al. 2012

A&A

101

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This paper introduces a series of papers aiming to study the dozens of low-mass eclipsing binaries (EBLM), with F, G, K primaries, that have been discovered in the course of the WASP survey. Our objects are mostly single-line binaries whose eclipses have been detected by WASP and were initially followed up as potential planetary transit candidates. These have bright primaries, which facilitates spectroscopic observations during transit and allows the study of the spin-orbit distribution of F, G, K+M eclipsing binaries through the Rossiter-McLaughlin effect. Here we report on the spin-orbit angle of WASP-30b, a transiting brown dwarf, and improve its orbital parameters. We also present the mass, radius, spin-orbit angle and orbital parameters of a new eclipsing binary, J1219-39b (1SWAPJ121921.03-395125.6, TYC 7760-484-1), which, with a mass of 95±2 M jup , is close to the limit between brown dwarfs and stars. We find that both objects have projected spin-orbit angles aligned with their primaries' rotation. Neither primaries are synchronous. J1219-39b has a modestly eccentric orbit and is in agreement with the theoretical mass-radius relationship, whereas WASP-30b lies above it.

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The Rossiter-McLaughlin Rotation Effect Observed for AI Draconis and V505 Sagittarii

Cited by 16 publications

References 16 publications

The fundamental parameters of the Algol binary AI Draconis revisited

The fundamental parameters of the Algol binary AI Draconis revisited

The Orbit and Occultations of KH 15D

The EBLM project

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