|Title||The energy budget of soft X-ray selected polars|
|Author||Dr Klaus Reinsch|
|Description||Since the early days of X-ray astronomy one of the central questions in our understanding of accretion onto magnetic white dwarfs in compact binaries is whether their observed ratio between soft and hard X-ray emission is in accordance with theoretical expectations or not. We propose to address this issue with XMM-Newton observations of a sample of soft X-ray selected polars from the ROSAT All-Sky Survey. The X-ray characteristics of our sample members are complementary to the parameter space covered by observations of polars in the XMM-Newton GTO programme. A detailed study of the spectral components, their flux contributions, and the physical structure of the accretion regions in these systems will, therefore, provide new insight into this long-lasting problem.|
|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, 2006-09-25T00:00:00Z, 030684, 17.56_20190403_1200. https://doi.org/10.5270/esa-y1o3cq6|