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X-Ray Spectroscopy of the High-Mass X-Ray Binary 4U 1700-37

Published online by Cambridge University Press:  22 February 2018

A. van der Meer ,
L. Kaper ,
T. Di Salvo ,
M. Méndez  and
M. van der Klis
A. van der Meer
Affiliation:
Sterrenkundig Instituut “Anton Pannekoek”, University of Amsterdam, Kruislaan 403, NL-1098 SJ Amsterdam, The Netherlands (ameer@science.uva.nl)
L. Kaper
Affiliation:
Sterrenkundig Instituut “Anton Pannekoek”, University of Amsterdam, Kruislaan 403, NL-1098 SJ Amsterdam, The Netherlands (ameer@science.uva.nl)
T. Di Salvo
Affiliation:
Sterrenkundig Instituut “Anton Pannekoek”, University of Amsterdam, Kruislaan 403, NL-1098 SJ Amsterdam, The Netherlands (ameer@science.uva.nl)
M. Méndez
Affiliation:
Space Research Organization of the Netherlands, National Institute for Space Research, Sorbonnelaan 2, NL-3584 CA Utrecht, The Netherlands
M. van der Klis
Affiliation:
Sterrenkundig Instituut “Anton Pannekoek”, University of Amsterdam, Kruislaan 403, NL-1098 SJ Amsterdam, The Netherlands (ameer@science.uva.nl)

Extract

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We present the first results of a monitoring campaign of the high-mass X-ray binary system 4U 1700-37/HD 153919, carried out with XMM-Newton.

We have observed the high-mass X-ray binary (HMXB) 4U 1700-37 with XMM-Newton at four orbital phases in February 2001. 4U 1700-37 is powered by the dense stellar wind of the O supergiant HD 153919. Numerous X-ray flares are observed with a typical duration, of the order of half an hour. We focus on three intervals in which the data are not affected by pile up: the eclipse, the eclipse egress and a low-flux part around orbital phase ϕ ~ 0.28.

Type
The Contributed Papers
Information
International Astronomical Union Colloquium , Volume 194: Compact binaries in the galaxy and beyond , 2004 , pp. 213
Copyright
Copyright © Instituto de astronomia/revista mexicana de astronomίa y astrofίsica 2004

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