| |
 |
| Paper: |
Modelling Observable Properties of Rapidly Rotating Stars |
| Volume: |
506, Bright Emissaries: Be Stars as Messengers of Star-Disk Physics |
| Page: |
25 |
| Authors: |
Castañeda, D.; Deupree, R. G.; Aufdenberg, J. |
| Abstract: |
To fully understand the Be star phenomenon, one must have
a reasonable degree of knowledge about the star beneath the disk, which is often found to be rapidly rotating.
Rapid rotation complicates modelling because fundamental
properties like the stellar luminosity and effective temperature require knowledge of the
angle of inclination at which the star is observed. Furthermore our knowledge of the structure of rapidly rotating stars is
on a less sure foundation than for non-rotating stars. The uncertainties in the inclination and the surface properties
of a few rapidly rotating stars have been substantially reduced by interferometric observations over the last decade, and these stars
can be used as tests of rotating stellar models, even if those stars themselves may not be Be stars.
Vega, as an MK standard, is historically a very important star because it is used for calibration purposes.
However, several studies have suggested that Vega is a rapidly rotating star viewed at a very low inclination angle, raising questions
as to how well we really know its properties. Appropriate modelling
has been challenging and there is still room for debate over the actual properties of Vega, as opposed to its observed properties.
We have previously shown that under certain conditions both the stellar surface properties and the
deduced surface properties scale from one model to another with the same surface shape.
We used this scaling algorithm with realistic 2D models to compute high-resolution spectral energy
distributions and interferometric visibilities to determine the best rotating model fit to Vega. Detailed comparisons between
the computed and observed data will be presented. |
|
|
|
|
|
