Upload resources

Upload your works to SEDICI to increase its visibility and improve its impact

 

Show simple item record

dc.date.accessioned 2010-09-27T16:28:10Z
dc.date.available 2010-09-27T03:00:00Z
dc.date.issued 2001
dc.identifier.uri http://sedici.unlp.edu.ar/handle/10915/2085
dc.description.abstract Line driven wind theory has been improved including non-spherical expansion in order to study its influence upon disk formation in early-type stars. Assuming that magnetic field controls the flow geometry, the plasma must flow downstream through open magnetic field lines. It is found that in the polar direction rapid flow tube divergence almost does not modify the location of the critical (singular) point and the calculated terminal velocity is incremented about 400 km/sec. On the other band in the equatorial direction, for a fast rotation case, the location of the critical point is unchanged and the terminal velocity shows slightly variations of about 50 km/sec. This conclusion is the polar direction is contrary to previous results, where the finite disk correction has not been taken into account. These results suggest, that open magnetic field lines do not influence disk formation in Be-stars. en
dc.format.extent 415-418 es
dc.language en es
dc.subject Geofísica, astronomía y astrofísica es
dc.title Influence of magnetic in Be-stars disk formation due to rotation in line driven in stellar winds en
dc.type Articulo es
sedici.identifier.uri http://articles.adsabs.harvard.edu//full/2001ASPC..248..415C/0000415.000.html es
sedici.creator.person Curé, Michel es
sedici.creator.person Cidale, Lydia Sonia es
sedici.subject.materias Ciencias Astronómicas es
sedici.description.fulltext true es
mods.originInfo.place Facultad de Ciencias Astronómicas y Geofísicas es
sedici.subtype Articulo es
sedici.rights.license Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International (CC BY-NC-ND 4.0)
sedici.rights.uri http://creativecommons.org/licenses/by-nc-nd/4.0/
sedici.relation.event Magnetic Fields Across the Hertzsprung-Russell Diagram, ASP Conference (2001) es
sedici.description.peerReview peer-review es
sedici2003.identifier ARG-UNLP-ART-0000006572 es
sedici.relation.journalTitle ASP Conference Series es
sedici.relation.journalVolumeAndIssue vol. 248 es


Download Files

This item appears in the following Collection(s)

Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International (CC BY-NC-ND 4.0) Except where otherwise noted, this item's license is described as Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International (CC BY-NC-ND 4.0)