Probing the magnetic confinement of the winds of Oe stars

Details Probing the magnetic confinement of the winds of Oe stars Probing the magnetic confinement of the winds of Oe stars

Oct 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007xmm..prop..131n&link_type=abstract

XMM-Newton Proposal ID #05544401

Physics

Stars, White Dwarfs, Solar System, Hd155806, Xmm-Newton Proposal Id #05544401

Scientific paper

The small group of Oe stars are usually considered as the hot analogs of the Be-type objects. A possible explanation for their equatorial outflow is that their stellar wind is magnetically channeled towards the equator, where it forms a circumstellar disk. A magnetic signature is best unveiled in the high-energy domain. We therefore request observations of the three brightest Oe stars, HD45314, HD60848 and HD155806, for 20ks each in order to pinpoint the origin of their Oe characteristics.

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