HUT Observations of the Non-Radiative Shock Wave of SN1006

Details HUT Observations of the Non-Radiative Shock Wave of SN1006 HUT Observations of the Non-Radiative Shock Wave of SN1006

Mar 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995aas...186.3002r&link_type=abstract

American Astronomical Society, 186th AAS Meeting, #30.02; Bulletin of the American Astronomical Society, Vol. 27, p.854

Astronomy and Astrophysics

Astrophysics

1

Scientific paper

The Hopkins Ultraviolet Telescope detected very faint emission lines of O VI, C IV, He II and perhaps N V in the spectrum of the 2000 km/s non-radiative shock wave of SN1006. The UV lines are about 2700 km/s broad. The line intensities can be used to study electron-ion temperature equilibration in shock waves, because they depend on electron temperature, while the Hα width measures ion temperature. The intensities of the UV lines imply T_e << T_i, but the rough equality of the O VI, C IV and He II lines suggests an electron temperature above 10(6) K. Therefore, some electron heating besides Coulomb collisions must occur. These results are in general agreement with the theory of Cargill and Papadopoulos, who predicted that plasma turbulence heats electrons to about 1/5 the ion temperature at the shock front. This work was supported by NASA contract NAS 5-27000 to the Johns Hopkins University and NASA Grant NAG8-1074 to the Smithsonian Astrophysical Observatory.

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