The Structure of the Accretion Flow on pre-main-sequence stars

Details The Structure of the Accretion Flow on pre-main-sequence stars The Structure of the Accretion Flow on pre-main-sequence stars

Jul 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999hst..prop.8206c&link_type=abstract

HST Proposal ID #8206

Physics

Hst Proposal Id #8206 Young Stars And Circumstellar Material

Scientific paper

We propose to test an essential prediction of the magnetospheric accretion model for T Tauri stars. STIS echelle spectra will be used to search for the relatively narrow high-temperature emission lines that must result from the magnetospheric accretion shock, but are not expected in the previous, alternative boundary layer model. By combining the results from high temperature {10^5 K} lines, accessible only with HST, with optical lines and optical-UV continuum emission, we will develop physically self-consistent models of accretion shock structure. The geometrically distribution of the emitting gas as derived from our results will test theories of mass-loading of magnetic field lines at the magnetosphere-disk interface. Analysis of the UV emission lines will also provide improved calibrations between ultraviolet continuum emission and accretion luminosities, and thus improve estimates of mass accretion rates for T Tauri stars.

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