Making sense of the spectral line profiles of Betelgeuse and other Red SuperGiants

Abstract

Spectropolarimetry of atomic lines in the spectra of Betelgeuse, and other Red SuperGiants (RSG), presents broad line profiles in linear polarization, but narrow profiles in intensity. Recent observations of the Red SuperGiant RW Cep show, on the other hand, broad intensity profiles, comparable to those in linear polarization. This observation hints that this difference in the Stokes Q/U and I profile widths noted in many RSG is just a temporary situation of the atmosphere of a given star. We propose an explanation for both cases based on the presence of strong velocity gradients larger than the thermal broadening of the spectral line. Using analytical but very simple radiative transfer we can compute intensity line profiles in such scenarios. We find that they qualitatively match the observed broadenings: large gradients are required for the narrow profiles of Betelgeuse, small gradients for the broad profiles of RW Cep. Profile bisectors are also reasonably well explained by this scenario in spite of the simple radiative transfer treatment. These results give a comprehensive explanation of both intensity and polarisation profiles. They provide also comfort to the approximationof a single-scattering event used in explaining the observed linear polarization in the inference of images of the photosphere of Betelgeuse and other Red SuperGiants as RW Cep, $μ$ Cep and CE Tau. The atmospheres of Red SuperGiants appear to be able, perhaps cyclically, to either produce large velocity gradients that prevent photospheric plasma from reaching the upper atmosphere and that must hinder large events of mass loss, either to leave vertical movements unchanged, letting plasma raising, escaping gravity and forming large dust clouds in the circumstellar environement. The origin of the velocity gradient and its modulation within the atmosphere remains an open question.