Synthetic Spectra of Rotating Stars. (arXiv:2007.12779v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Lipatov_M/0/1/0/all/0/1">Mikhail Lipatov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brandt_T/0/1/0/all/0/1">Timothy D. Brandt</a>
Many early-type stars have oblate surfaces, spatial temperature variations,
and spectral line broadening that indicate large rotational velocities.
Rotation ought to have a significant effect on the full spectra of such stars.
To infer structural and life history parameters from their spectra, one must
integrate specific intensity over the two-dimensional surfaces of corresponding
stellar models. Toward this end, we offer PARS (Paint the Atmospheres of
Rotating Stars) — an integration scheme based on models that incorporate solid
body rotation, Roche mass distribution, and collinearity of gravity and energy
flux (https://github.com/mlipatov/paint_atmospheres). The scheme features a
closed-form expression for the azimuthal integral, a high-order numerical
approximation of the longitudinal integral, and a precise calculation of
surface effective temperature at rotation rates up to 99.9% of Keplerian limit.
Extensions of the scheme include synthetic color-magnitude diagrams and
planetary transit curves.
Many early-type stars have oblate surfaces, spatial temperature variations,
and spectral line broadening that indicate large rotational velocities.
Rotation ought to have a significant effect on the full spectra of such stars.
To infer structural and life history parameters from their spectra, one must
integrate specific intensity over the two-dimensional surfaces of corresponding
stellar models. Toward this end, we offer PARS (Paint the Atmospheres of
Rotating Stars) — an integration scheme based on models that incorporate solid
body rotation, Roche mass distribution, and collinearity of gravity and energy
flux (https://github.com/mlipatov/paint_atmospheres). The scheme features a
closed-form expression for the azimuthal integral, a high-order numerical
approximation of the longitudinal integral, and a precise calculation of
surface effective temperature at rotation rates up to 99.9% of Keplerian limit.
Extensions of the scheme include synthetic color-magnitude diagrams and
planetary transit curves.
http://arxiv.org/icons/sfx.gif
