|Title||Fast stochastic variability in CV variable MV Lyr and source identification|
|Author||Dr Andrej Dobrotka|
|Description||Some cataclysmic variables exhibit a multicomponent power density spectrum of fast variability. High-cadence long-term Kepler data of MV Lyr showed 4 different characteristic components, while XMM X-ray observations of RU Peg in quiescence contained two different components. Modelling studies suggest a variety of accreting disc structures as the source of variability. However, we still depend on speculations because the source identification is not unambiguous without combined optical and X-ray observations of the same system. Since it is technically impossible to obtain optical Kepler data of RU Peg, we propose to observe MV Lyr in X-rays and UV with XMM. The goal is to search for the two highest break frequencies found in the Kepler data.|
|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, 2016-09-28T22:00:00Z, 076104, 17.56_20190403_1200. https://doi.org/10.5270/esa-ncdmwfo|