|Title||X-rays at the Latest Stage of a Massive Star.s Life: A thorough study of WR6|
|Author||Dr Lidia Oskinova|
|Description||We propose to obtain the first high-resolution spectrum of a single Wolf-Rayet (WR) type star. WR stars are immediate progenitors of core-collapse SNe and GRBs. The low-resolution spectra accumulated by XMM-Newton and Chandra revealed that the X-ray emission of WR stars depends on yet unknown factors - wind anisotropy, magnetic field and rotation are possible suspects. The RGS spectrum of the X-ray brightest single WR star, WR 6, analyzed by means of comprehensive models, will unveil how X-rays are produced in WR stars. The wind shock origin of X-rays will be firmly proved or disproved. The unique capabilities of XMM-Newton will ^ate our knowledge about massive stars in their latest evolutionary stages to a qualitatively new level.|
|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, 2011-11-30T00:00:00Z, 065225, 17.56_20190403_1200. https://doi.org/10.5270/esa-mqu7s3r|