Stellar Spectroscopy during Exoplanet Transits: Dissecting fine structure across stellar surfaces
Abstract
Differential spectroscopy during exoplanet transits permits to reconstruct spectra of small stellar surface portions that successively become hidden behind the planet. The center-to-limb behavior of stellar line shapes, asymmetries and wavelength shifts will enable detailed tests of 3-dimensional hydrodynamic models of stellar atmospheres, such that are required for any precise determination of abundances or seismic properties. Such models can now be computed for widely different stars but have been feasible to test in detail only for the Sun with its resolved surface structure. Although very high quality spectra are required, already current data permit reconstructions of line profiles in the brightest transit host stars such as HD209458 (G0 V).
Cite
@article{arxiv.1408.1402,
title = {Stellar Spectroscopy during Exoplanet Transits: Dissecting fine structure across stellar surfaces},
author = {Dainis Dravins and Hans-Günter Ludwig and Erik Dahlén and Hiva Pazira},
journal= {arXiv preprint arXiv:1408.1402},
year = {2014}
}
Comments
12 pages, 11 figures; Presented at 18th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun (Flagstaff, Arizona; June 2014). To appear in Proceedings of Lowell Observatory (G.van Belle, H.Harris, eds.), 2014