|Title||Seeking the origin of X-rays from chemically peculiar late B stars|
|Author||Dr Ehud Behar|
|Description||Bright X-ray emission from isolated late B stars remains unexplained, as conventional theory predicts these stars neither to have coronae nor to eject sufficiently intense stellar winds. Among those that have been detected, several of the brightest are chemically peculiar stars. We propose to observe Mu Lep, the X-ray brightest HgMn star and to use high-resolution spectroscopy to unveil the source of its X-ray emission, whether shocks in stellar winds, magnetically active regions, or an invisible companion. The X-ray abundance patterns will be compared with those in the photosphere. X-ray emission from peculiar elements, which could provide a definite association of the X-rays with the B star, will be sought using new atomic calculations.|
|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, 2004-04-16T00:00:00Z, 014337, 17.56_20190403_1200. https://doi.org/10.5270/esa-3jabzli|