|Title||X-ray eclipse mapping of disc-accreting white dwarfs|
|Author||Dr Peter Wheatley|
|Description||We have applied the proven optical technique of eclipse mapping to X-ray observations of disc-accreting white dwarfs, allowing us to map the extent and distribution of X-ray emitting plasma around the compact object. Observations of four different systems have allowed us to build a consistent picture of the accretion geometry that depends only on accretion rate. At low rates the X-ray region is smaller than the white dwarf, but at high rates it is much larger. Here we propose an observation of ONE of our well-studied low accretion rate systems, to be triggered when it enters a high accretion rate state. This will allow us to test our basic picture in a system that differs only in accretion rate and investigate the origin of the second source of X-rays.|
|Publication||No observations found associated with the current proposal|
|Instrument||EMOS1, EMOS2, EPN, OM, RGS1, RGS2|
|Mission Description||The European Space Agency's (ESA) X-ray Multi-Mirror Mission (XMM-Newton) was launched by an Ariane 504 on December 10th 1999. XMM-Newton is ESA's 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 Earth's 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.
|Publisher And Registrant||European Space Agency|
|Credit Guidelines||European Space Agency, 2006-10-25T00:00:00Z, 030656, 17.56_20190403_1200. https://doi.org/10.5270/esa-vxa0qm0|