Upper Limits on the X-ray Emission of “Uranium” Stars

Astrophysics, abstract
astro-ph/0301292

From: Eric M. Schlegel <ems@head-cfa.harvard.edu>

Date: Wed, 15 Jan 2003 13:47:50 GMT   (183kb)

Authors:
Eric M. Schlegel

Comments: accepted AJ, scheduled March

A paper by Qian & Wasserburg suggests the optical absorption lines of uranium
observed in the spectra of ultra-metal-poor stars (defined as [Fe/H] $<$-3)
arise from contamination from a supernova in a binary star system. Assuming the
binary survived the explosion, a collapsed compact object may be present and
implying potential accretion processes with accompanying X-ray emission. Upper
limits on X-ray emission from an accreting compact object are described here.

References and citations for this submission:

SLAC-SPIRES HEP (refers to ,
cited by, arXiv reformatted)