|Title||Detailed investigation of the outburst cycle of a helium dwarf nova|
|Author||Dr Gavin Ramsay|
|Description||The AM CVn systems are interacting binaries with orbital periods <70 minutes. Their spectra show almost no hydrogen and are therefore excellent laboratories for the study of helium dominated accretion flows. We have a monitoring programme to detect optical outbursts from these binaries and found that KL Dra undergoes outbursts every virgul60 days. Observations made using Swift show the UV flux mirrors the optical. However, we were unable to draw firm conclusions regarding the X-ray component due to its low flux. We propose to obtain a series of observations of KL Dra over an outburst using XMM-Newton. These are necessary to drive forward theoretical models of disc instabilities these and other binaries such as X-ray transients.|
|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, 2012-10-25T00:00:00Z, 067380, 17.56_20190403_1200. https://doi.org/10.5270/esa-a4iik9n|