Velocity Structure of the Interstellar Shockwaves

Details Velocity Structure of the Interstellar Shockwaves Velocity Structure of the Interstellar Shockwaves

Jul 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991hst..prop.2584z&link_type=abstract

HST Proposal ID #2584

Physics

Hst Proposal Id #2584

Scientific paper

High velocity (VLSR~=100km/sec) radiatively cooling shocks may exist in the interstellar medium, but have never been directly confirmed in observation. Theories predict that for the interstellar near-uv absoprtion lines associated with the postshock gas, their relative velocities should correlate with the stages of ionization of the absorbing atoms. Hence they are sensitive to the temperature distributions in the shocked gas and are ideal probes of the shock structure. Measurements of the expected velocity differences (on the order of 6 km/sec) were not achievable in previous space-based observations, but are within the easy reach of the HRS. We propose to examine this phenomena by observing early type stars in the Orion OB Association with the high resolution mode of the HRS. The proposed program requires only a minimum amount of the HST observing time, since the two target stars chosen are bright and known to have well separated high velocity interstellar absorption features. If confirmed, this could be the most unambiguous evidence for the radiatively cooling interstellar shockwaves.

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