Hollow H II regions. II - Mechanism for wind energy dissipation and diffuse X-ray emission

Details Hollow H II regions. II - Mechanism for wind energy dissipation and diffuse X-ray emission Hollow H II regions. II - Mechanism for wind energy dissipation and diffuse X-ray emission

May 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...177..243d&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 177, no. 1-2, May 1987, p. 243-257.

Astronomy and Astrophysics

Astrophysics

30

Energy Dissipation, H Ii Regions, Nebulae, Stellar Winds, X Ray Sources, Conductive Heat Transfer, Electron Density (Concentration), Hot Electrons, Interstellar Matter, Shock Wave Propagation, Thermal Conductivity

Scientific paper

The mechanism by which stellar-wind energy is dissipated near the shock in a hollow H II region (HHR) around a massive star is investigated theoretically, in the context of the HHR model developed by Dorland et al. (1986). The principles of nonlinear thermal conduction (especially the delocalizaton of conductive heat flux postulated for laboratory fusion plasmas) are reviewed; expressions for estimating heat fluxes are derived; a two-temperature approximation is employed to describe coupling between thermal conduction and wind-energy dissipation; and the determination of the flux-limit factor from X-ray observations is explained. The model is then applied to observational data for the Rosette nebula and Eta Car, and the results are presented graphically. The diffuse X-ray temperatures of HHRs are found to be in the range 2-16 keV and to depend uniquely on stellar-wind velocity, the value for an O star with wind velocity 2500 km/s being about 5 keV.

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