|Title||Characterizing the X-ray properties of the earliest magnetic stars|
|Author||Dr Yael Naze|
|Description||The recent detection of magnetic fields in massive stars has profoundly changed our understanding of the structure and evolution of these objects. In addition, detailed modelling shows that intense magnetic fields can have a strong impact on the X-ray emission. Currently, only a few tens of magnetic hot stars are known, and much fewer have been observed at high energies. The observed diversity of behaviours and the small sample size actually prevent us from recognizing the overall trends. By doubling the sample size with a small investment of time, we will be able to undertake such a systematic study of the X-ray properties of magnetic massive stars, which will help us better understand which parameters govern their high-energy emission.|
|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, 2011-11-05T00:00:00Z, 065032, 17.56_20190403_1200. https://doi.org/10.5270/esa-ejw2ejo|