2011/04/15 by Hilding R. Neilson, H. R. Neilson, John B. Lester +1
Physics and Astronomy · Social Sciences · #Astronomy and Astrophysical Research #Atmospheric models #Educational Leadership and Practices #Interferometry #Light curve #Limb darkening #Spherical model #Stars #Stellar atmosphere #Stellar evolution #Stellar pulsation #Stellar, planetary, and galactic studies #astro-ph.SR
paper · pdf · doi:10.1051/0004-6361/201116623
8 pages, 8 figures, figures 4 and 6 have lower resolution. A&A in press
openalex publication_date 2011/04/15 · arxiv created 2011/05/01 · arxiv updated 2015/05/28 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Context. Stellar limb darkening, I(μ = cosθ), is an important constraint for microlensing, eclipsing binary, planetary transit, and interferometric observations, but is generally treated as a parameterized curve, such as a linear-plus-square-root law. Many analyses assume limb-darkening coefficients computed from model stellar atmospheres. However, previous studies, using I(μ) from plane-parallel models, have found that fits to the flux-normalized curves pass through a fixed point, a common μ location on the stellar disk, for all values of Teff, log g and wavelength.