Morphology of Young Neutron Stars: Possible PSR/SNR
Associations
Although neutron stars are thought to be born mostly in supernova
explosions, there are not many known pulsar/SNR associations. This is
why the search for pulsar/SNR associations is interesting. I have
studied the morphology of some young (spin-down age < 100000 years)
pulsars and their interstellar environs. I produced a mosaic of several
ROSAT PSPC pointed observations in the field of PSR B1800-21 and
the W30 complex and detected a temperature variation across the W30 SNR
(Park et al. 1995) which supports the PSR B1800-21/W30 association as
suggested by Finley & Ogelman (1994). With the ROSAT PSPC
and HRI
observations of PSR B1823-13, a low surface brightness diffuse emission
surrounding the neutron star was detected. Possible explanations for
this 5' extended diffuse emission are the SNR where PSR B1823-13 was
born
or alternatively that PSR B1823-13 is a high velocity neutron star
interacting with very low density cavity in the ISM (Finley,
Srinivasan,
& Park 1996).
W30 & PSR B1800-21
The first ever imaging X-ray observation of the W30 complex which
contains the Galactic SNR G8.7-0.1 and the young radio pulsar PSR
1800-21. The data support the association of G8.7-0.1 and PSR 1800-21.
The peculiar morphology can be explained if the supernova which gave
birth to PSR 1800-21 occurred within, or very near, a molecular cloud.
This scenario removes the requirement of a large transverse velocity
for
the pulsar, the greatest difficulty with the association. (
Finley & Ogelman 1994, ApJ, 434L, L25 )
PSR B1823-13
The young 21,000 year old neutron star PSR B1823-13. The neutron star
is found imbedded in a compact nebula of radius 20" and surrounded by a
low surface brightness diffuse emission region of extent 4'-5'. The
diffuse extended component is consistent with the expected size for an
associated SNR given the observed size of the compact nebula.
(Finley,
Srinivasan, & Park, 1996, ApJ, 466, 938)
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