Abstract:
Regarding model atmospheres, rotation effects are mostly neglected, and, at best, the rotational broadening correction is being applied to a non-rotating synthetic spectrum. However, this approximation does not work for fast rotators (veq > 200 km s}-1), where the effect of gravity darkening starts to be prominent. The need for this correction starts to be significant for stars hotter than F7. We introduce a new model atmosphere grid covering the region of the main-sequence A- and B-type stars. The model allows more robust follow-up studies, mainly to provide an alternative method to determine the inclination angle of the rotational axis by inversion. Calculating synthetic magnitudes and colors helps constrain the Main Sequence's rotational broadening and determine other biases related to the stellar rotation that influence the parameters determined from CMD. Determining rotational parameters from gravity darkening provides an alternative way of disentangling v\sin i values and leads to a more precise understanding of the distinct populations of rotating stars.
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