The Winds of Main Sequence B Stars in NGC 6231, Evidence for Shocks in Weak Winds.

Details The Winds of Main Sequence B Stars in NGC 6231, Evidence for Shocks in Weak Winds. The Winds of Main Sequence B Stars in NGC 6231, Evidence for Shocks in Weak Winds.

Jul 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996hst..prop.6690m&link_type=abstract

HST Proposal ID #6690

Astronomy and Astrophysics

Astrophysics

Hst Proposal Id #6690 Hot Stars

Scientific paper

Because the main sequence B stars in NGC 6231 have abnormallystrong C iv wind lines, they are the only main sequence Bstars with distinct edge velocities. Although the underlyingcause for the strong lines remains unknown, these stars doprovide an opportunity to test two important ideas concerningB star winds: 1) that the driving ions in the winds of starswith low mass loss rates decouple from the general flow, and;2) that shocks deep in the winds of main sequence B stars areresponsible for their observed X-rays. In both of thesemodels, the wind accelerates toward a terminal velocity,v_infty, far greater than the observed value, shocking ordecoupling well before it can attain the high v_infty. As aresult, the observable wind accelerates very rapidly, leadingto wind flushing times less than 30 minutes. If theseconjectures are correct, then the winds of main sequence Bstars should be highly variable on time scales of minutes.Model fitting of available IUE data are consistant with thegeneral notion of a rapidly accelerating wind, shocking wellbefore its actual v_infty. However, these are 5 hourexposures, so the fits are to ill-defined mean wind flows.The new GHRS observations will provide adequate spectral andtemporal resolution to observe the expected variability and,thereby, verify the existance of two important astrophysicalprocesses.

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