Dusty Shocks and Pulsar Winds: Identifying the Source Model for G70.7+1.2

Details Dusty Shocks and Pulsar Winds: Identifying the Source Model for G70.7+1.2 Dusty Shocks and Pulsar Winds: Identifying the Source Model for G70.7+1.2

Sep 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002cxo..prop.1185a&link_type=abstract

Chandra Proposal ID #04400900

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Chandra Proposal Id #04400900

Scientific paper

The optical and radio nebula G70.7+1.2 has been the object of scrutiny and speculation for more than 50 years. In the last decade, unexpected discoveries made through multiwavelength observations have helped to discredit successive models of the object's nature and the mechanisms at work within it. Two models that explain most of the observed phenomena remain, one requiring a central Be-neutron star binary, the other a single star with a dusty wind. They make specific, distinct predictions for X-ray emission from the system. We propose to use the sensitivity and spatial resolution of Chandra's ACIS-S camera to discriminate between these two models, revealing at last the true nature of G70.7+1.2, and providing a unique new laboratory for testing models of bow-shock formation.

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