MAGNETOSPHERES AND DISK ACCRETION IN HERBIG Ae/Be STARS

ABSTRACT We present evidence of magnetically mediated disk accretion in Herbig Ae/Be stars. Magnetospheric accretion models of Balmer and sodium profiles calculated with appropriate stellar and rotational parameters are in qualitative agreement with the observed profiles of the Herbig Ae star UX Ori and yield a mass accretion rate of $10 À8 M yr À1 . If more recent indications of an extremely large rotation rate for this object are correct, the magnetic field geometry must deviate from that of a standard dipole in order to produce line emission consistent with observed flux levels. Models of the associated accretion shock qualitatively explain the observed distribution of excess fluxes in the Balmer discontinuity for a large ensemble of Herbig Ae/Be stars and imply typically small mass accretion rates, P10 À7 M yr À1 . In order for accretion to proceed onto the star, significant amounts of gas must exist inside the dust destruction radius, which is potentially problematic for recently advocated scenarios of ''puffed'' inner dust wall geometries. However, our models of the inner gas disk show that for the typical accretion rates we have derived, the gas should generally be optically thin, thus allowing direct stellar irradiation of the inner dust edge of the disk