Effects of Rotation on the Spectra of Brown Dwarfs

TL;DR

This study investigates how rotation and axis inclination influence the spectral appearance and flux of brown dwarfs, revealing significant effects on observed properties and providing formulas for flux adjustments.

Contribution

It combines atmospheric modeling with deformation simulations to quantify the impact of rotation and inclination on brown dwarf spectra and flux.

Findings

Flux can vary by up to 1.5 times with viewing angle.

Spectral shape effects increase toward equator-on views.

Bolometric luminosity estimates may need 20% adjustment for fast rotators.

Abstract

Measured rotational speeds of giant planets and brown dwarfs frequently constitute appreciable fractions of the breakup limit, resulting in centrifugal expansion of these objects at the equator. According to models of internal energy transport, this expansion ought to make the poles of a rotator significantly hotter than the equator, so that inclination of the rotational axis greatly affects both spectral shape and total flux. In this article, we explore the dependence of a substellar object's observables on its rotational speed and axis inclination. To do so, we combine PICASO (a Planetary Intensity Code for Atmospheric Spectroscopy Observations) with software PARS (Paint the Atmospheres of Rotating Stars). The former computer program models radiative transfer within plane-parallel planetary atmospheres, while the latter computes disk-integrated spectra of centrifugally deformed gaseous masses. We find that the specific flux of a typical fast-rotating brown dwarf can increase by as much as a factor of 1.5 with movement from an equator-on to a pole-on view. On the other hand, the distinctive effect of rotation on spectral shape increases toward the equator-on view. The latter effect also increases with lower effective temperature. The bolometric luminosity estimate for a typical fast rotator at extreme inclinations has to be adjusted by as much as about 20% due to the anisotropy of the object's observed flux. We provide a general formula for the calculation of the corresponding adjustment factor in terms of rotational speed and inclination.