Doppler beaming factors for white dwarfs, main sequence stars, and giant stars Limb-darkening coefficients for 3D (DA and DB) white dwarf models. (arXiv:2007.15715v1 [astro-ph.SR])

Doppler beaming factors for white dwarfs, main sequence stars, and giant stars Limb-darkening coefficients for 3D (DA and DB) white dwarf models. (arXiv:2007.15715v1 [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:+Cukanovaite_E/0/1/0/all/0/1">E. Cukanovaite</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Burdge_K/0/1/0/all/0/1">K. Burdge</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tremblay_P/0/1/0/all/0/1">P.-E. Tremblay</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Parsons_S/0/1/0/all/0/1">S. Parsons</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marsh_T/0/1/0/all/0/1">T. R. Marsh</a>

We computed Doppler beaming factors for DA, DB, and DBA white dwarf models,
as well as for main sequence and giant stars covering the transmission curves
of the Sloan, UBVRI, HiPERCAM, Kepler, TESS, and Gaia photometric systems. The
calculations of the limb-darkening coefficients for 3D models were carried out
using the least-squares method for these photometric systems.

The beaming factor calculations, which use realistic models of stellar
atmospheres, show that the black body approximation is not accurate,
particularly for the filters $u$, $u’$, $U$, $g$, $g’$, and $B$. The black body
approach is only valid for high effective temperatures and/or long effective
wavelengths. Therefore, for more accurate analyses of light curves, we
recommend the use of the beaming factors presented in this paper. Concerning
limb-darkening, the distribution of specific intensities for 3D models
indicates that, in general, these models are less bright toward the limb than
their 1D counterparts, which implies steeper profiles. To describe these
intensities better, we recommend the use of the four-term law (also for 1D
models) given the level of precision that is being achieved with Earth-based
instruments and space missions such as Kepler and TESS (and PLATO in the
future).

We computed Doppler beaming factors for DA, DB, and DBA white dwarf models,
as well as for main sequence and giant stars covering the transmission curves
of the Sloan, UBVRI, HiPERCAM, Kepler, TESS, and Gaia photometric systems. The
calculations of the limb-darkening coefficients for 3D models were carried out
using the least-squares method for these photometric systems.

The beaming factor calculations, which use realistic models of stellar
atmospheres, show that the black body approximation is not accurate,
particularly for the filters $u$, $u’$, $U$, $g$, $g’$, and $B$. The black body
approach is only valid for high effective temperatures and/or long effective
wavelengths. Therefore, for more accurate analyses of light curves, we
recommend the use of the beaming factors presented in this paper. Concerning
limb-darkening, the distribution of specific intensities for 3D models
indicates that, in general, these models are less bright toward the limb than
their 1D counterparts, which implies steeper profiles. To describe these
intensities better, we recommend the use of the four-term law (also for 1D
models) given the level of precision that is being achieved with Earth-based
instruments and space missions such as Kepler and TESS (and PLATO in the
future).

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