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dc.contributor.authorNerney, S.
dc.dateJan 01, 1986en_US
dc.date.accessioned2018-09-27T00:06:49Z
dc.date.available2018-09-27T00:06:49Z
dc.date.issued1986-01
dc.identifier.other19860015068
dc.identifier.urihttp://hdl.handle.net/10945/60121
dc.identifier.urihttps://ntrs.nasa.gov/search.jsp?R=19860015068
dc.descriptionSEE ParentDocumentRecord|Ntt=19860015036 "NASA. Marshall Space Flight Center Research Reports: 1985 NASA(ASEE Summer Faculty Fellowship Program"; p. 16 pen_US
dc.descriptionApproved for public release, distribution unlimiteden_US
dc.description.abstractAn analytical procedure is developed to solve the magnetohydrodynamic equations for the stellar wind problem in the strong-magnetic field, optically thick limit for hot stars. The slow-mode, Alfven, and fast-mode critical points are modified by the radiation terms in the force equation but in a manner that can be treated relatively easily. Once the velocities at the critical points and the distances to the points are known, the streamline constants are determined in a straight-forward manner. This allows the structure of the wind to be elucidated without recourse to complicated computational schemes.en_US
dc.rightsThis publication is a work of the U.S. Government as defined in Title 17, United States Code, Section 101. Copyright protection is not available for this work in the United States.en_US
dc.titleRadiatively driven winds from magnetic, fast-rotating starsen_US
dc.typeConference Paper
dc.contributor.corporateUnspecified Center
dc.subject.authorHOT STARSen_US
dc.subject.authorMAGNETOHYDRODYNAMICSen_US
dc.subject.authorSTELLAR MAGNETIC FIELDSen_US
dc.subject.authorSTELLAR ROTATIONen_US
dc.subject.authorSTELLAR WINDSen_US
dc.subject.authorACCELERATION (PHYSICS)en_US
dc.subject.authorCOMPUTATIONen_US
dc.subject.authorMATHEMATICAL MODELSen_US
dc.subject.authorMOMENTUMen_US
dc.subject.authorPROBLEM SOLVINGen_US
dc.subject.authorTHOMSON SCATTERINGen_US
dc.subject.authorVELOCITY MEASUREMENTen_US


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