Physics
Scientific paper
Oct 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999aps..4cf..ee01v&link_type=abstract
American Physical Society, Four Corners Section Fall Meeting, October 1-2, 1999 The University of Arizona Tucson, AZ, abstract #
Physics
Scientific paper
The observations of a skin of [O III] λ5007Å emission around the edge of the visible Crab supernova remnant has been explained as a cooling region behind a radiative shock, driven by synchrotron pressure and sweeping up freely expanding ejecta from the original supernova explosion (Sankrit & Hester 1997). Higher ionization species such as [Ne V] λ3426Å provide an opportunity for tracing shocks with velocities in excess of about 170 km/sec. With recent observations of [NeV] in the southern portion of the remnant (Van Tassell et al. 1998), little doubt is left about the existence of a shock, and the production of high ionization line emission in the cooling region behind it. We are presenting images of the entire remnant in emission from [NeV] and compare these with observations in [OIII]. Images of the Crab in narrowband filters were taken this winter at the Steward Observatory 2.3 meter telescope on Kitt Peak. Preliminary analysis of these data is presented, and their implications as to shock properties are discussed. Partial funding for this project was provided by a NASA Space Grant, and by NASA support of the WFPC2 IDT.
Hester Jeff
Sankrit Ravi
Szentgyorgi Andrew
van Tassell Heidi
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