Power-2 limb-darkening coefficients for the uvby, UBVRIJHK, SDSS ugriz, Gaia, Kepler, and TESS photometric systems. (arXiv:2206.11098v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Claret_A/0/1/0/all/0/1">A. Claret</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Southworth_J/0/1/0/all/0/1">J. Southworth</a>
Limb darkening is an important stellar phenomenon and must be accounted for
in the study of stellar spectra, eclipsing binaries, transiting planetary
systems, and microlensing events. The power-2 limb-darkening law provides a
good match to the specific intensities predicted by stellar atmosphere models:
it is better than other two-parameter laws and is only surpassed by the
four-parameter law. Predictions of the limb-darkening coefficients for the
power-2 law are not widely available. We therefore compute them, using stellar
atmosphere models generated by the ATLAS (plane-parallel) code. Limb-darkening
coefficients were computed for the space missions Gaia, Kepler, and TESS as
well as for the photometric systems uvby, UBVRIJHK, and SDSS ugriz.The
calculations were performed by adopting the Levenberg-Marquardt least-squares
minimisation method and were computed with a resolution of 100 equally spaced
viewing angles. We used 9586 model atmospheres covering 19 metallicities,
effective temperatures of 3500 to 50000 K, log g values from 0.0 to 5.0, and
microturbulent velocities of 0, 1, 2, 4, and 8 km. We confirm the superiority
of the power-2 law, in terms of the quality of the fits, over other
two-parameter laws. This is particularly relevant for the quadratic law, which
is widely used. We recommend the use of the power-2 law in cases where a
two-parameter law is needed.
Limb darkening is an important stellar phenomenon and must be accounted for
in the study of stellar spectra, eclipsing binaries, transiting planetary
systems, and microlensing events. The power-2 limb-darkening law provides a
good match to the specific intensities predicted by stellar atmosphere models:
it is better than other two-parameter laws and is only surpassed by the
four-parameter law. Predictions of the limb-darkening coefficients for the
power-2 law are not widely available. We therefore compute them, using stellar
atmosphere models generated by the ATLAS (plane-parallel) code. Limb-darkening
coefficients were computed for the space missions Gaia, Kepler, and TESS as
well as for the photometric systems uvby, UBVRIJHK, and SDSS ugriz.The
calculations were performed by adopting the Levenberg-Marquardt least-squares
minimisation method and were computed with a resolution of 100 equally spaced
viewing angles. We used 9586 model atmospheres covering 19 metallicities,
effective temperatures of 3500 to 50000 K, log g values from 0.0 to 5.0, and
microturbulent velocities of 0, 1, 2, 4, and 8 km. We confirm the superiority
of the power-2 law, in terms of the quality of the fits, over other
two-parameter laws. This is particularly relevant for the quadratic law, which
is widely used. We recommend the use of the power-2 law in cases where a
two-parameter law is needed.
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