|Title||X-ray emission as a probe of accretion in white dwarf - L dwarf binaries|
|Author||Prof Beate Stelzer|
|Description||L dwarfs in close binaries (period virgul100min) with white dwarfs are rare although expected to be the majority and representing the end stages of cataclysmic variable evolution (period-bouncers). The detection of X-rays from WD - L dwarf (WDLD) binaries is an efficient diagnostic of accretion since L dwarf coronal emission is below the sensitivity of current instrumentation. XMM-Newton is the only facility able to study these faint, moderately soft X-ray emitters. In AO14 we detected X-ray orbital modulation in a known magnetic short-period WDLD system, thus setting a tight constraint on the mass transfer rate. We here propose to continue our survey observing the only other 2 magnetic short-period WDLDs aiming at understanding the evolutionary stage of such systems.|
|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, 2021-02-03T23:00:00Z, 084038, 18.02_20200221_1200. https://doi.org/10.57780/esa-i5vpuof|