Publications/Talks

Conference Presentations:

  • Patel, P., Sigut, T. A. A. & Landstreet, J. 2012. ‘The Hα-UBV Signatures of Disk Growth and Dissipation in Classical Be Stars.’ CASCA (Calgary, AB).


    Abstract: Be stars are non-supergiant B type stars whose spectra show, or have shown, one or more Balmer lines of hydrogen in emission. The emission is produced in a circumstellar disk. Be stars show correlations between their Hα emission and V magnitude, and the sign of the correlation (positive or negative) is likely determined by the viewing angle of the observer. Using numerical radiative transfer, we calculate Hα and UBV colours as a Be star disk grows and dissipates with time. These basic models are shown to be consistent with the observed correlations. Modelling such correlations can be used to place constraints on the inner disk scale heights and the extent of gravitational darkening of the central stars.