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Astron. Astrophys. 321, 835-837 (1997)

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RX J1838.4-0301: an accreting pulsar or coronal X-ray emission? *

S. Mereghetti 1, T. Belloni 2 and F.P. Nasuti 1

1 Istituto di Fisica Cosmica del CNR, Via Bassini 15, I-20133 Milano, Italy (sandro@ifctr.mi.cnr.it, nasuti@ifctr.mi.cnr.it)
2 Astronomical Institute "A.Pannekoek" and Center for High Energy Astrophysics, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands (tmb@astro.uva.nl)

Received 18 September 1996 / Accepted 25 October 1996

Abstract

The X-ray source RX J1838.4-0301 is of particular interest since it is a possible member of a small subclass of pulsars with anomalous properties. A spectroscopic study of its proposed optical counterpart and a reanalysis of the ROSAT data indicate that the observed optical and X-ray properties, with the exception of the reported [FORMULA] periodicity (Schwentker 1994), are consistent with coronal emission from an active late type star. In the lack of an independent confirmation, the presence of X-ray pulsations in RX J1838.4-0301 should be considered with caution.

Key words: pulsars – X-rays: stars – stars: RX J1838.4-0301

* Based on observations collected at the European Southern Observatory, La Silla, Chile.

Send offprint requests to: S. Mereghetti

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© European Southern Observatory (ESO) 1997

Online publication: June 30, 1998
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