|Title||V471 TAU - ECLIPSING LABORATORY FOR WIND ACCRETION AND STELLAR ACTIVITY STUDIES|
|Author||Dr PASI HAKALA|
|Description||We plan to observe V471 Tau,an eclipsing 12.5h period precontact cataclysmic binary in order to study evidence for accretion via stellar wind from the active K2V secondary. HST UV spectra have established that the white dwarf surface shows inhomogenities of silicon, which could be due to magnetically funnelled accretion In this programme we plan to study the spin phase resolved X-ray spectrum of the WD together with simultaneous X-ray & UV spin lightcurves in order to model the variation and thus check the stellar wind accretion hypothesis. The eclipsing nature of the system allows us to fully separate X-ray emission from the WD and the K star. This enables us to model emission from each source separately and provides extra constraints on the location of the WD magnetic poles.|
|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, 2005-08-31T00:00:00Z, 020326, 17.56_20190403_1200. https://doi.org/10.5270/esa-07c7769|