BRITE view of σ\sigma Scorpii, β\beta Cephei-type star studied for over a century

Preliminary results of the analysis of the combined space-based BRITE and SMEI, and ground-based Stroemgren photometry are presented. The BRITE data allowed to find seven p and three g modes in the frequency spectrum of this star; only four p modes were known in this star prior to this study. The first results of seismic modelling are also presented.Comment: 3 pages, 1 figure, to appear in the Proceedings of the 3rd BRITE Science Conference, Auberge du Lac Taureau, Canad

Constraints on rotation of B-type stars from the nitrogen abundance

We study the effects of rotation on surface abundances of CNO elements in massive stars. Nitrogen enrichment caused by rotationally induced mixing can help to constrain parameters of observed stars, especially their rotational velocities. Here we present theoretical results and apply them to the star HD 163899

BRITE view of sigma Scorpii, beta Cephei-type star studied for over a century

Preliminary results of the analysis of the combined space-based BRITE and SMEI, and ground-based Stro ̈mgren photometry are presented. The BRITE data allowed to find seven p and three g modes in the frequency spectrum of this star; only four p modes were known in this star prior to this study. The first results of seismic modelling are also presented

Modelling Spectro-photometric Characteristics of Nonradially Pulsating Stars

. We present a computing code for modelling energy flux distributions, photometric indices and spectral line profiles of (non-)radially pulsating Main-Sequence stars. The model is based on the perturbation-expansion formalism taking into account geometrical and nonadiabatic e#ects. 1. Introduction For a given mode of oscillation the harmonic time dependence, exp(i# nlm t), and spherical harmonic horizontal dependence, Y m l (#, #), are assumed for the first order perturbed quantities. The mass displacement for the spheroidal modes is described by y- and z-eigenfunctions and for toroidal modes by #-eigenfunctions, cf. Dziembowski & Goode (1992). In the case of slowly rotating stars one can use the zero-rotation approximation to describe stellar pulsations. Such a model was used already by Cugier, Dziembowski & Pamyatnykh (1994) to study nonadiabatic observables of # Cephei stars. Apart from y nlm (r) and z nlm (r) it is desirable to use the eigenfunction p nlm (r), connected with t..