Physics
Scientific paper
Nov 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aspc..337..305s&link_type=abstract
The Nature and Evolution of Disks Around Hot Stars, ASP Conference Series, Vol. 337, Proceedings of a meeting held 7-9 July 2004
Physics
Scientific paper
As a suspected hot analog to the Bp stars, θ1 Orionis C (O6--7V) has UV resonance lines that modulate over the rotation cycle. But do these variations follow the patterns expected from absorptions and emissions formed in a flattened co-rotating magnetosphere? In this paper we report that the observed variations are quite different from the Bp paradigm. For example, the far-blue wings of the C IV and N V doublets, formed by a fully accelerated wind, are anticorrelated with respect to the fluxes in the red half of the profiles. An observer viewing the magnetosphere edge-on sees profiles with both a depressed far-blue wing and elevated red wing. An examination of strong, excited N IV and O V lines demonstrates this same behavior. The relative changes in these line strengths are consistent with an optically thick medium not far from thermal equilibrium. We argue that the elevated red-profile fluxes arise from emission seen against the star by post-shock wind matter returning to the star. Following new MHD simulations by ud-Doula, this may correspond to hot blobs condensing in the magnetic plane and heated by ram pressure as they fall back to the star along the same magnetic lines that guided them to the equator. One corollary of our work is that there is no evidence for a static cooling disk.
Fullerton Alex W.
Smith Matthew A.
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