Variability in the Line Emission of the X-Ray Pulsar 4u 1626-67

Details Variability in the Line Emission of the X-Ray Pulsar 4u 1626-67 Variability in the Line Emission of the X-Ray Pulsar 4u 1626-67

Sep 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002cxo..prop.1073c&link_type=abstract

Chandra Proposal ID #04400027

Computer Science

Chandra Proposal Id #04400027

Scientific paper

4U1626-67 is an ultracompact system which consists of a disk-accreting magnetic neutron star and a very low mass, hydrogen-depleted companion in a 42-min binary. During AO1 we resolved the Ne/O emission line complex into Doppler pairs of broadened (~2500 km/s FWHM) lines from highly ionized Ne and O. We argue that the lines appear to originate in the outer accretion disk. Photoelectric edges of Ne and O appear stronger than expected from interstellar material. Recent XMM observations also suggested variability in the line morphology. We propose to reobserve 4U1626-67 for 100 ks in order to determine variations from the previously observed line shapes, changes in temperatures and densities, and their dependence on pulse and binary phase.

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