Variations of the high-level Balmer line spectrum of the helium-strong star Sigma Orionis E

TL;DR

This study uses high-resolution Balmer line spectra to analyze the density, temperature, and geometry of magnetospheric disk segments in the helium-strong star Sigma Orionis E, revealing complex disk structures and occultation behaviors.

Contribution

It provides detailed modeling of the disk geometry and thermodynamics of Sigma Orionis E using high-level Balmer lines, uncovering complex, non-coplanar disk structures.

Findings

Two disk segments cause occultations with distinct properties.

Disk densities are near 10^{12} cm^{-3} and temperatures around 10500K and 12000K.

Disks exhibit complex, non-coplanar geometries.

Abstract

Using the high-level Balmer lines and continuum, we trace the density structure of two magnetospheric disk segments of the prototypical Bp star sigma Ori E (B2p) as these segments occult portions of the star during the rotational cycle. High-resolution spectra of the Balmer lines >H9 and Balmer edge were obtained on seven nights in January-February 2007 at an average sampling of 0.01 cycles. We measured equivalent width variations due to the star occultations by two disk segments 0.4 cycles apart and constructed differential spectra of the migrations of the corresponding absorptions across the Balmer line profiles. We first estimated the rotational and magnetic obliquity angles. We then simulated the observed Balmer jump variation using the model atmosphere codes synspec/circus and evaluated the disk geometry and gas thermodynamics. We find that the two occultations are caused by two disk segments. The first of these transits quickly, indicating that the segment resides in a range of distances, perhaps 2.5-6R_star, from the star. The second consists of a more slowly moving segment situated closer to the surface and causing two semi-resolved absorbing maxima. During its transit this segment brushes across the star's "lower" limb. Judging from the line visibility up to H23-H24 during the occultations, both disk segments have mean densities near 10^{12} cm^{-3} and are opaque in the lines and continuum. They have semiheights less than 1/2 of a stellar radius, and their temperatures are near 10500K and 12000K, respectively. In all, the disks of Bp stars have a much more complicated geometry than has been anticipated, as evidenced by their (sometimes) non-coplanarity, de-centerness, and from star to star, differences in disk height.