Quiescent X-ray transients provide a superb laboratory for investigatingthe properties of the residual accretion flow onto their neutron star (NS)and black hole (BH) compact objects. It has been claimed that thepresence of an event horizon causes a significant difference in theirquiescent behaviour. However, current results are equivocal as there are avariety of factors which can complicate the NS behaviour as well asdetermining whether their mass transfer rates really are similar. It istherefore essential to observe NS systems with greater sensitivity. Ourproposal is to observe 4 NS transients in quiescence, in order to quantifythe luminosity difference and properties of these two classes of SXTs.
Instrument
EMOS1, EMOS2, EPN, OM, RGS1, RGS2
Temporal Coverage
2003-10-25T08:24:34Z/2003-10-25T17:19:48Z
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 Ulrich Kolb, 2004, 'Why are Neutron Star Transients Brigher in Quiescence than Black Holes', 17.56_20190403_1200, European Space Agency, https://doi.org/10.5270/esa-towxq54
