|Title||Probing centrifugal magnetospheres of B-type stars|
|Author||Dr Veronique Petit|
|Description||Recently, a new generation of polarimetric instruments has uncovered a population of massive OB-stars hosting strong, organized magnetic fields. Magnetic channeling of these OB stars. strong winds leads to the formation of large-scale shock-heated magnetospheres. Using the new analysis of trends in 64 magnetic OB stars (Petit et al. 2013), we have identified an important region of magnetosphere parameter space for which X-ray trends can provide important constraints on the shock physics and general properties of these magnetospheres. We propose to probe the centrifugal magnetospheres of B-type stars using EPIC observations of 7 stars that will provide stringent tests of the Magnetically Confined Wind Shock (MCWS) paradigm of massive star X-ray 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, 2015-09-19T22:00:00Z, 074234, 17.56_20190403_1200. https://doi.org/10.5270/esa-kk4ef08|