|Title||A Comprehensive Survey of Accretion in Double White Dwarfs|
|Author||Prof Thomas Maccarone|
|Description||At the present time, the X-ray measurements of AM CVn stars (systems where one white dwarf accretes from another white dwarf) are heavily biased toward short period systems. We propose to recitfy the situation by observing all AM CVn stars which do not have XMM observations in the archives but do have known periods. In fact, the X-ray measurements are more important for the long period systems than the short period systems, since in the long period systems, the boundary layers are expected to be optically thin, and a much larger fraction of the bolometric luminosity is expected to come out in X-rays, meaning that using these systems to test our understanding of evolution of double white dwarfs depends crucially on knowing their X-ray fluxes.|
|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, 2019-05-09T22:00:00Z, 080027, 17.56_20190403_1200. https://doi.org/10.5270/esa-21sb8uf|