[Ne V] Emission on the Skin of the Crab Nebula

Details [Ne V] Emission on the Skin of the Crab Nebula [Ne V] Emission on the Skin of the Crab Nebula

May 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998aas...192.1804v&link_type=abstract

American Astronomical Society, 192nd AAS Meeting, #18.04; Bulletin of the American Astronomical Society, Vol. 30, p.844

Astronomy and Astrophysics

Astronomy

Scientific paper

The [O III] lambda 5007 Angstroms skin observed around the crab nebula is best explained as a region of cooling behind a radiative shock driven by synchrotron pressure, and sweeping up freely expanding ejecta of the supernova (Sankrit &\ Hester 1997). Shock models predict elevated [Ne V] lambda 3426 Angstroms Emission if the shock velocity is greater than 170 km/s. Ratios of [Ne V] to [O III] emission can be used to trace the velocity profile of the shock (Sankrit &\ Hester 1997). We present narrowband [Ne V] and [O III] images of the crab nebula as part of a study to measure the properties of the shock. These line filter images were taken early this year at the Steward 90 inch telescope on Kitt Peak. One set of images includes the location where Davidson observed high [Ne V] emission (Davidson 1979). While the [O III] image at this position shows the skin, filaments, and complex structure seen previously (Sankrit &\ Hester 1997), the [Ne V] emission forms a prominant smooth skin at the outer edge of the [O III] skin, with additional [Ne V] emission lining the stronger [O III] filaments. these observations support the existence of a shock and by extension support the existence of expanding ejecta from the supernova beyond the visible remnant.

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