Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 1997
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997apj...475..224f&link_type=abstract
Astrophysical Journal v.475, p.224
Astronomy and Astrophysics
Astronomy
31
Stars: Pulsars: Individual Alphanumeric: Psr B0833-45, Ism: Supernova Remnants, Ism: Individual Name: Vela X
Scientific paper
We present a VLA image of the Vela X region, a nebula thought to be powered by the young pulsar B0833-45, at a resolution of approximately 1.'3. The morphology of this synchrotron nebula is dominated by a network of fine, overlapping linear filaments. The brightest filament lies just south of PSR B0833-45 and can be traced to the center of Vela X, 40' away. This radio filament appears to be the counterpart of an X-ray feature first detected by Markwardt & Ogelman (1995). Rather than a one-to-one position alignment between them, the radio filament is systematically offset and traces the eastern boundary of the X-ray feature. We consider several models for the origin of the radio filament and its relation to the X-ray feature. At present, the data cannot distinguish between whether the radio emission is due to electrons accelerated in situ or whether the radio emission results from the compression of the relativistic pulsar wind. We suggest several possible observations to enable us to distinguish which hypothesis is correct.
Bietenholz Michael F.
Frail Dale A.
Markwardt Craig B.
Oegelman Hakki
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