Separating the X-Ray Emissions of UV Ceti A and B with Chandra

Details Separating the X-Ray Emissions of UV Ceti A and B with Chandra Separating the X-Ray Emissions of UV Ceti A and B with Chandra

2003-03-21

arxiv.org/abs/astro-ph/0303492v1

Astrophys.J. 589 (2003) 983-987

Astronomy and Astrophysics

Astrophysics

To appear in the Astrophysical Journal, Vol. 589 (2003 June 1)

Scientific paper

10.1086/374710

We present the first spatially separated X-ray observation of the active UV Ceti binary with \textit{Chandra}, providing important new information on the relative X-ray activity levels of its nearly identical dM5.5e components. The two components had similar X-ray luminosities during low-level periods and emission measure loci derived from Low Energy Transmission Grating spectra reveal similar coronal temperatures ($3 - 6$ MK). However, the B component showed a higher degree of variability, resulting in a higher average X-ray luminosity than that of UV Cet A. We discuss possible causes of this enhanced activity in UV Ceti B.

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