The Banana Project. Iii. Spin-Orbit Alignment in the Long-Period Eclipsing Binary Ny Cephei

Albrecht, S.; Winn, Joshua N.; Carter, Joshua A.; Snellen, I. A. G.; Mooij, Ernst de

doi:10.1088/0004-637x/726/2/68

Cited by 83 publications

(63 citation statements)

References 53 publications

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“…Jensen et al (2004) and Monin et al (2006) have reported planar alignment and misalignment for wider-separation binaries. Similar to these studies, in the case of very close binaries of semi-major axis ∼0.3 AU, there have been some examples where systems exhibit both aligned and misaligned axes (Albrecht et al 2009(Albrecht et al , 2011. More recently, Wheelwright et al (2011) have also reported coplanarity between HAe/Be binary systems and circumstellar disks.…”

Section: Introductionsupporting

confidence: 62%

Spin-orbit alignment in the very low mass binary regime

Harding

Hallinan

Konopacky

et al. 2013

A&A

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Studies of solar-type binaries have found coplanarity between the equatorial and orbital planes of systems with <40 AU separation. By comparison, the alignment of the equatorial and orbital axes in the substellar regime, and the associated implications for formation theory, are relatively poorly constrained. Here we present the discovery of the rotation period of 3.32 ± 0.15 h from 2MASS J0746+20A -the primary component of a tight (2.7 AU) ultracool dwarf binary system (L0+L1.5). The newly discovered period, together with the established period via radio observations of the other component, and the well constrained orbital parameters and rotational velocity measurements, allow us to infer alignment of the equatorial planes of both components with the orbital plane of the system to within 10 degrees. This result suggests that solar-type binary formation mechanisms may extend down into the brown dwarf mass range, and we consider a number of formation theories that may be applicable in this case. This is the first such observational result in the very low mass binary regime. In addition, the detected period of 3.32 ± 0.15 h implies that the reported radio period of 2.07 ± 0.002 h is associated with the secondary star, not the primary, as was previously claimed. This in turn refutes the claimed radius of 0.78 ± 0.1 R J for 2MASS J0746+20A, which we demonstrate to be 0.99 ± 0.03 R J .

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Section: Introductionsupporting

confidence: 62%

Spin-orbit alignment in the very low mass binary regime

Harding

Hallinan

Konopacky

et al. 2013

A&A

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“…The measurement of the spin-orbit alignment in planetary and binary systems, e.g., Triaud et al (2010) and Albrecht et al (2011), gives insight into the formation of these systems. The most frequently applied technique uses spectroscopic measurements during the transit of eclipsing systems and only determines the projected spin-orbit angle.…”

Section: Discussionmentioning

confidence: 99%

HD 5388 b is a 69 M_Jupcompanion instead of a planet

Sahlmann

Lovis

Queloz

et al. 2011

A&A

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We examined six exoplanet host stars with non-standard Hipparcos astrometric solution, which may be indicative of unrecognised orbital motion. Using Hipparcos intermediate astrometric data, we detected the astrometric orbit of HD 5388 at a significance level of 99.4% (2.7 σ). HD 5388 is a metal-deficient star and hosts a planet candidate with a minimum mass of 1.96 M J discovered in 2010. We determined its orbit inclination to be i = 178.3 +0.4 • −0.7 and the corresponding mass of its companion HD 5388 b to be M 2 = 69 ± 20 M J . The orbit is seen almost face-on and the companion mass lies at the upper end of the brown-dwarf mass range. A mass lower than 13 M J was excluded at the 3 σ-level. The astrometric motions of the five other stars had been investigated by other authors revealing two planetary companions, one stellar companion, and two statistically insignificant orbits. We conclude that HD 5388 b is not a planet but most likely a brown-dwarf companion. In addition, we find that the inclinations of the stellar rotation axis and the companion's orbital axis differ significantly.

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“…Solid black lines are observations, the dash-dotted lines are the model fit of co-aligned stars, and the solid lines are model fits that allow for spin-orbit misalignment. Adapted from Albrecht et al (2011). This is known as the Rossiter-McLaughlin effect, and has been observed in a number of stars and planets.…”

Section: Doppler Beamingmentioning

confidence: 99%

“…However, careful ground-based studies have been able to discern that the components of close binaries in a number of systems show misaligned rotational and orbital axes (Albrecht et al 2011). Observationally, this is most easily discerned via the Rossiter-McLaughlin effect, depicted in Fig.…”

Section: Spin-orbit Misalignmentmentioning

confidence: 99%

Advances in Modeling Eclipsing Binary Stars in the Era of Large All-Sky Surveys with EBAI and PHOEBE

et al. 2011

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Abstract. With the launch of NASA's Kepler mission, stellar astrophysics in general, and the eclipsing binary star field in particular, has witnessed a surge in data quality, interpretation possibilities, and the ability to confront theoretical predictions with observations. The unprecedented data accuracy and an essentially uninterrupted observing mode of over 2000 eclipsing binaries is revolutionizing the field. Amidst all this excitement, we came to realize that our best models to describe the physical and geometric properties of binaries are not good enough. Systematic errors are evident in a large range of binary light curves, and the residuals are anything but Gaussian. This is crucial because it limits us in the precision of the attained parameters. Since eclipsing binary stars are prime targets for determining the fundamental properties of stars, including their ages and distances, the penalty for this loss of accuracy affects other areas of astrophysics as well. Here, we propose to substantially revamp our current models by applying the lessons learned while reducing, modeling, and analyzing Kepler data.

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The Banana Project. Iii. Spin-Orbit Alignment in the Long-Period Eclipsing Binary Ny Cephei

Cited by 83 publications

References 53 publications

Spin-orbit alignment in the very low mass binary regime

Spin-orbit alignment in the very low mass binary regime

HD 5388 b is a 69 M_Jupcompanion instead of a planet

Advances in Modeling Eclipsing Binary Stars in the Era of Large All-Sky Surveys with EBAI and PHOEBE

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The Banana Project. Iii. Spin-Orbit Alignment in the Long-Period Eclipsing Binary Ny Cephei

Cited by 83 publications

References 53 publications

Spin-orbit alignment in the very low mass binary regime

Spin-orbit alignment in the very low mass binary regime

HD 5388 b is a 69 MJupcompanion instead of a planet

Advances in Modeling Eclipsing Binary Stars in the Era of Large All-Sky Surveys with EBAI and PHOEBE

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HD 5388 b is a 69 M_Jupcompanion instead of a planet