The Long History of the Rossiter-McLaughlin Effect and its Recent Applications

Albrecht, S.

doi:10.1017/s1743921311027864

Cited by 4 publications

(2 citation statements)

References 44 publications

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“…The geometry of the projected path of the exoplanet across the star (including whether it moves in a prograde or retrograde orbit) must be known to fully interpret any observed line profile variations. That can be determined through this Rossiter-McLaughlin effect; e.g., Perryman (2011) or Albrecht (2012). The effect has been measured for numerous exoplanets, while the specific issue on the influence of convective wavelength shifts and stellar line profile changes across stellar disks has been evaluated by Cegla et al (2016), Reiners et al (2016a), Shporer & Brown (2011), and Yan et al (2015a,b, 2017.…”

Section: Rossiter-mclaughlin Effectmentioning

confidence: 99%

Spatially resolved spectroscopy across stellar surfaces

Dravins

Ludwig

Dahlén

et al. 2017

A&A

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Context. High-precision stellar analyses require hydrodynamic modeling to interpret chemical abundances or oscillation modes. Exoplanet atmosphere studies require stellar background spectra to be known along the transit path while detection of Earth analogs require stellar microvariability to be understood. Hydrodynamic 3D models can be computed for widely different stars but have been tested in detail only for the Sun with its resolved surface features. Model predictions include spectral line shapes, asymmetries, and wavelength shifts, and their center-to-limb changes across stellar disks. Aims. We observe high-resolution spectral line profiles across spatially highly resolved stellar surfaces, which are free from the effects of spatial smearing and rotational broadening present in full-disk spectra, enabling comparisons to synthetic profiles from 3D models. Methods. During exoplanet transits, successive stellar surface portions become hidden and differential spectroscopy between various transit phases provides spectra of small surface segments temporarily hidden behind the planet. Planets cover no more than ∼1% of any main-sequence star, enabling high spatial resolution but demanding very precise observations. Realistically measurable quantities are identified through simulated observations of synthetic spectral lines. Results. In normal stars, line profile ratios between various transit phases may vary by ∼0.5%, requiring S /N 5000 for meaningful spectral reconstruction.While not yet realistic for individual spectral lines, this is achievable for cool stars by averaging over numerous lines with similar parameters. Conclusions. For bright host stars of large transiting planets, spatially resolved spectroscopy is currently practical. More observable targets are likely to be found in the near future by ongoing photometric searches.

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Section: Rossiter-mclaughlin Effectmentioning

confidence: 99%

Spatially resolved spectroscopy across stellar surfaces

Dravins

Ludwig

Dahlén

et al. 2017

A&A

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“…In this context, systems such as DI Her (Claret et al 2010) appeared puzzling since they seemed to defy general relativity. Studying the Rossiter-McLaughlin effect, Albrecht et al (2009) were able to demonstrate, however, that a misalignment of the orbit and spin axes in DI Her is responsible for this ostensible contradiction; more recently, an extensive review of this effect was reported as well (Albrecht 2012). Shakura (1985) derived an expression (his Eq.…”

Section: Introductionmentioning

confidence: 99%

TheαCrB binary system: A new radial velocity curve, apsidal motion, and the alignment of rotation and orbit axes

Schmitt

Schröder

Rauw

et al. 2016

A&A

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We present a new radial velocity curve for the two components of the eclipsing spectroscopic binary α CrB. This binary consists of two main-sequence stars of types A and G in a 17.3599-day orbit, according to the data from our robotic TIGRE facility that is located in Guanajuato, Mexico. We used a high-resolution solar spectrum to determine the radial velocities of the weak secondary component by cross-correlation and wavelength referencing with telluric lines for the strongly rotationally broadened primary lines (v sin(i) = 138 km s −1 ) to obtain radial velocities with an accuracy of a few hundred m/s. We combined our new RV data with older measurements, dating back to 1908 in the case of the primary, to search for evidence of apsidal motion. We find an apsidal motion period between 6600 and 10 600 yr. This value is consistent with the available data for both the primary and secondary and is also consistent with the assumption that the system has aligned orbit and rotation axes.

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Toward the Measurements of Spin-Orbit Relations for Small Planets

Hirano

2014

Springer Theses

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The Long History of the Rossiter-McLaughlin Effect and its Recent Applications

Cited by 4 publications

References 44 publications

Spatially resolved spectroscopy across stellar surfaces

Spatially resolved spectroscopy across stellar surfaces

TheαCrB binary system: A new radial velocity curve, apsidal motion, and the alignment of rotation and orbit axes

Toward the Measurements of Spin-Orbit Relations for Small Planets

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