Spatially-resolved FUV Spectra of the Primary Shock in the Cygnus Loop

Details Spatially-resolved FUV Spectra of the Primary Shock in the Cygnus Loop Spatially-resolved FUV Spectra of the Primary Shock in the Cygnus Loop

Dec 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997hst..prop.7289b&link_type=abstract

HST Proposal ID #7289

Physics

Hst Proposal Id #7289 Stellar Ejecta

Scientific paper

We request STIS spectroscopic {G140L} observations to determine the ionization structure behind the non-radiative, primary shock front on the northeastern edge of the Cygnus Loop supernova remnant. These measurements will allow us to determine the rate at which electron and ion temperatures come into equilibrium in the post-shock flow. We also request higher resolution STIS G140M observations of N V Lambda1238, 1242 and C IV Lambda1548, 1551 at selected positions to assess optical depth effects on the relative line intensities for comparison with models and to obtain information on the intrinsic line widths. A WFPC2 HAlpha EARLY ACQ image will be needed to establish the exact location of the shock front and set up the grid of spectral positions. These observations will permit a detailed analysis of the shock physics occurring in the primary collisionless shock front, including especially the rate of energy sharing between the ions and electrons in the postshock gas. This will allow us to discriminate between models with rapid {e.g. plasma turbulence} and slow {e.g. Coulomb collisions} equilibration, a result that has important general ramifications for understanding shock waves in a variety of astrophysical situations.

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