ROSAT observations have shown that the Be stars HD 161103 and SAO 49725 exhibitan excess of X-ray emission over the normal shocked wind component. Therelatively modest X-ray luminosity of about 1 to 5 E32 erg/s (0.2-2.4 keV) isconsistent with that expected from a white dwarf accreting from the equatorialdisc of a Be star. Whereas models predict that they should outnumber Be +neutron star binaries by a factor of about 10, no Be + white dwarf system hasever been confirmed so far. This absence casts some doubts on our currentunderstanding of massive X-ray binary evolution. The goal of the proposedobservation is to characterize the X-ray spectral and temporal properties ofthese X-ray emitters and search for the signatures of an accreting white dwarf.
Instrument
EMOS1, EMOS2, EPN, OM, RGS1, RGS2
Temporal Coverage
2003-12-09T20:31:41Z/2004-02-26T13:49:39Z
Version
17.56_20190403_1200
Mission Description
The European Space Agencys (ESA) X-ray Multi-Mirror Mission (XMM-Newton) was launched by an Ariane 504 on December 10th 1999. XMM-Newton is ESAs second cornerstone of the Horizon 2000 Science Programme. It carries 3 high throughput X-ray telescopes with an unprecedented effective area, and an optical monitor, the first flown on a X-ray observatory. The large collecting area and ability to make long uninterrupted exposures provide highly sensitive observations. Since Earths atmosphere blocks out all X-rays, only a telescope in space can detect and study celestial X-ray sources. The XMM-Newton mission is helping scientists to solve a number of cosmic mysteries, ranging from the enigmatic black holes to the origins of the Universe itself. Observing time on XMM-Newton is being made available to the scientific community, applying for observational periods on a competitive basis.
European Space Agency, Dr CHRISTIAN MOTCH, 2008, 'THE NATURE OF THE ACCRETING OBJECT IN HD 161103 AND SAO 49725', 17.56_20190403_1200, European Space Agency, https://doi.org/10.5270/esa-eerp0yo
