Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Full Refereed Journal Article (PDF/Postscript)
· Full Refereed Scanned Article (GIF)
· On-line Data
· References in the article
· Citations to the Article (24) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (16)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
High-resolution X-ray imaging of the supernova remnant MSH 15-52
Authors:
Brazier, K. T. S.; Becker, W.
Affiliation:
AA(Department of Physics, University of Durham, South Road, Durham DH1 3LE ), AB(Max-Planck-Institut fur extraterrestrische Physik, 85740 Garching bei Munchen, Germany)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 284, Issue 2, pp. 335-340. (MNRAS Homepage)
Publication Date:
01/1997
Origin:
MNRAS
MNRAS Keywords:
STARS: NEUTRON - PULSARS: INDIVIDUAL: PSR 1509-58 - SUPERNOVA REMNANTS - X-RAYS: STARS
Bibliographic Code:
1997MNRAS.284..335B

Abstract

We present high-resolution ROSAT observations of PSR 1509-58 and the supernova remnant MSH 15-52. The pulsar itself is resolved from the surrounding synchrotron nebula as a 75 per cent pulsed point source. The synchrotron emission forms a broad, elongated cross centred on the pulsar, and an extrapolation of the north-western arm of the cross to the supernova remnant rim coincides with the RCW 89 Hα nebula. More than half of the X-ray flux in RCW 89 is resolved into a partial ring of tight knots that closely follow the radio morphology of the region. We suggest that all of the X-ray emission in the field of PSR 1509-58 can be explained if the system is similar to the `torus' and `jets' of the Crab pulsar synchrotron nebula, but viewed at more than ~70 deg to the pulsar spin axis. For current theories, this inclination favours pulsar emission from the outer, rather than the inner, magnetosphere. The luminosity of RCW 89 is driven in our model by the pulsar wind, which suggests that the NW-SE axis of the synchrotron nebula marks a collimated outflow along the pulsar spin axis, making PSR 1509-58 the third example of an isolated pulsar with a polar outflow.

Printing Options

Print whole paper
Print Page(s) through

Return 600 dpi PDF to Acrobat/Browser. Different resolutions (200 or 600 dpi), formats (Postscript, PDF, etc), page sizes (US Letter, European A4, etc), and compression (gzip,compress,none) can be set through the Printing Preferences


More Article Retrieval Options

HELP for Article Retrieval
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)
   

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints