Abstract:

Analogous to the Solar Wind, there also exists a wind for other stars. In many cases these Stellar Winds are not noticeable through visual observations, but their existence can be confirmed by a fingerprint in the spectral profile of the stars. In order to understand the characteristics of these profiles, and thus the properties of the Stellar Winds, it is of high interest to find an appropriate wind model with which these profiles can be reproduced correctly. While in most scientific papers an empirical velocity estimation is assumed for the wind, it is now the time to apply a model which bases upon fundamental theoretical assumptions and has proved itself very well in the case of the Solar Wind: The Parker Model. It will be explained how the spectral fingerprint of the Wind can be identified and how it is formed. Then there will be an extensive discussion about the modeling of these profiles and about what we can expect from the Parker Model.