High Velocity Thermal Shock Instabilities in the VELA Supernova Remnant

Details High Velocity Thermal Shock Instabilities in the VELA Supernova Remnant High Velocity Thermal Shock Instabilities in the VELA Supernova Remnant

Jul 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996hst..prop.6413s&link_type=abstract

HST Proposal ID #6413

Astronomy and Astrophysics

Astrophysics

Hst Proposal Id #6413 Interstellar Medium

Scientific paper

Supernovae dominate the ionization, heating, and mass motionsof interstellar gas in the Milky Way, yet detaileddescriptions of these processes remain elusive becauseobservational information about interstellar shocks islimited. We propose to use the GHRS to study the propertiesof high velocity gas in the Vela supernova remnant throughultraviolet absorption line spectroscopy. This approach tostudying the neutral and ionized gases in SNRs providesdetailed physical condition and profile shape informationalong infinitesimal beams at high spectral resolution. Wewill 1) Study the observational signatures of thermalinstabilities created by a loss of pressure equilibrium as thehigh velocity shock-accelerated gas cools. These catastrophicthermal instabilities affect the morphologies and diagnosticline ratios of interstellar shocks and must be understood tointerpret the physical conditions and processes occurring inshocked interstellar environments. 2) Compare the velocityoffsets, strengths, and profile shapes of the high velocityabsorption features to improve models of shock ionization andremnant-ISM interactions. 3) Determine the local physicalconditions that give rise to gas-phase abundance variations atdifferent velocities and places within the remnant. The foursight lines to be studied have a rich velocity structure thatwill allow us to explore a range of shock conditions andremnant environments.

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