A New Paradigm on the Interaction of Protoplanetary Disks with the Stellar Corona

Le résumé fourni par la source

The standard picture of the interaction between protoplanetary disks and the stellar magnetic field of the host star assumes a static stellar magnetic field and a continuous disk accretion along the stellar closed magnetic loops. The physicality of this traditional picture can be easily challenged from simple plasma physics considerations. We present a three-dimensional, time-dependent MHD simulation at which the static stellar field is replaced by a more physical, non-potential, energized stellar corona that includes self-consistent coronal heating and stellar wind acceleration. This simulation also completely captures the interaction of the disk with the self-consistent stellar wind, which has not been included in most past models. Our results show that the inclusion of an energized, self-consistent stellar corona and stellar wind provide a very different picture than the traditional one, where the disk accretion is weakened, and is much more sporadic. This weaker accretion should have implications for the study of protoplanetary disk dynamics.

Ce résumé expose les affirmations des auteurs. BNTIC ne l’interprète pas comme une validation indépendante des résultats.