Takashi Nomura, Jun Naito, Hiromoto Shibahashi
Prior to the last decade, most observations of roAp stars have concerned the
light variations. Recently some new, striking results of spectroscopic
observations with high time resolution, high spectral dispersion, and a high
signal-to-noise ratio became available. Since the oscillations found in roAp
stars are high overtones, the vertical wavelengths of the oscillations are so
short that the amplitude and phase of the variation of each spectroscopic line
are highly dependent on the level of the line profile. Hence, analyses of the
variation of the spectroscopic lines of roAp stars potentially provide us with
new information about the vertical structure of the atmosphere of these stars.
In order to extract such information, a numerical simulation of the
line-profile variation beyond a single-surface approximation is necessary. We
carried out a numerical simulation of line-profile variation by taking account
of the finite thickness of the line forming layer. We demonstrated how
effective this treatment is, by comparing the simulation with the observed line
profiles.
View original:
http://arxiv.org/abs/1202.1379
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