gamma Cassiopeiae: an X-ray Be star with personality

TL;DR

This study analyzes X-ray spectra of gamma Cassiopeiae, revealing multiple thermal components, variable absorption, and unique spectral features that distinguish it from similar stars, shedding light on its peculiar X-ray emission.

Contribution

The paper provides detailed spectral analysis of gamma Cassiopeiae, highlighting its distinct X-ray properties and variability, and compares it to other Be stars to understand its unique behavior.

Findings

Dominant thermal component at ~12 keV contributes 80-90% of flux.

Absence of soft X-ray absorption in 2004 indicates changing absorbing material.

Spectral features suggest overabundance of N and Ne, and variable Fe abundance.

Abstract

gamma Cassiopeiae (gCas) is a B0.5e star with peculiar X-ray emission properties and yet the prototype of its own small class. In this paper we examine the X-ray spectra for a 2004 XMM-Newton observation and a previously published 2001 Chandra observation. In both cases the spectra can be modeled with 3 or 4 thermal components, which appear be discrete in temperature and spatially distinct. The dominant component, having kT ~ 12 keV contributes most (~80-90%) of the flux. The secondary components have temperatures in the range of 2-3 keV to 0.1 keV; these values can shift in time. Importantly, we find that the strong absorption of soft X-rays in 2001 is absent in 2004, meaning that an absorbing column in front of the source has moved off the star or has been removed. Other differences include a reduced Fe abundance from the ionized lines of the FeKalpha complex (even more subsolar than the 2001 observation), a decrease of the Fe K and possibly of the Si K fluorescence features, and from the NVII and NeX H-alpha lines, a possible overabundance of N and Ne. Also, we note common characteristics in both spectra that seem to set gCas apart from HD110342, another member of this subclass studied in detail. In this sense these stars have different "personalities." For example, for gCas rapid X-ray flaring and slower changes in the light curve are only seldomly accompanied by variations in hardness, and the hot X-ray component remains nearly constant in temperature. Moreover, the light curve shows recurrent "lulls" in flux, suggesting that a relaxation cycle is operates as part of the (unknown) X-ray generation process.