Abundance analysis of roAp stars. III. γ Equulei.

Details Abundance analysis of roAp stars. III. γ Equulei. Abundance analysis of roAp stars. III. γ Equulei.

Jun 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997a%26a...322..234r&link_type=abstract

Astronomy and Astrophysics, v.322, p.234-241

Astronomy and Astrophysics

Astrophysics

27

Stars: Abundances, Chemically Peculiar, Magnetic Field, Oscillations, Individual: Gamma Equ

Scientific paper

A spectroscopic analysis of the rapidly oscillating chemically peculiar star γ Equ yields T_eff_=7700K, logg=4.20, a microturbulence and v.sin i which cannot be determined reliably, but which must be close to zero, because line broadening can be modelled by magnetic field effects alone. A mean magnetic field modulus of B=4.0kG is estimated by comparing synthetic Zeeman pattern with observations. This value provides another phase point for magnetic field variations of γ Equ, a CP2 star with the longest hitherto known magnetic field period of about 77 years. For a simple dipolar field geometry, the angle between the line of sight and the magnetic axis =~130° (or =~50°). We discuss in some detail the problems for abundance determinations in the presence of a strong magnetic field and we increase substantially the number of ions to 42, for which abundances are now available. In particular, we obtain a more reliable abundance of log(Eu/N_tot_)=-10.24, and find Fe and the light elements, C to Ca, to have nearly solar abundances. Co is clearly overabundant, and Nb and Mo are the most overabundant elements in γ Equ relative to the Sun.

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