What causes the dispersion of the O-star X-ray luminosities ?

Details What causes the dispersion of the O-star X-ray luminosities ? What causes the dispersion of the O-star X-ray luminosities ?

Oct 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010xmm..prop...83s&link_type=abstract

XMM-Newton Proposal ID #06720601

Physics

Stars, White Dwarfs, Solar System, Ic2944

Scientific paper

O-type X-ray luminosity scales with their bolometric luminosity according to canonical relation: log L_X/L_bol ~ -7. Yet, significant dispersion is observed around this relation. Binarity was often considered as a natural explanation to the observed dispersion but recent investigations tend to disprove this statement. We propose to investigate the impact of magnetic wind confinement on the X-ray properties of O stars, and whether or not it can explain the spread around the canonical relation. The nearby young open cluster, IC2944, hosts a rich late-type O-star population and is ideally suited for our purpose. It will allow us to investigate with unprecedented details a region of the parameter space where magnetic confinement is expected to have the strongest impact.

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