|Title||Tight surveillance of the exemplary O star zeta Ophiuchi with XMM-Newton and HST|
|Author||Dr Lidia Oskinova|
|Description||We propose a novel and decisive experiment that relies on the unrivaled joint capabilities of XMM and HST. The closest O-type star, zeta Oph, shall be observed continuously over its rotational period to reveal the physics of stellar wind heating. We will discriminate between alternative models for X-ray production in O stars: the hot plasma is generated either in stochastic wind shocks or in corotating interaction regions. The new superb X-ray image will probe the physical conditions in the circumstellar matter of an O star. No similar observations were performed before on a massive star. Observing zeta Oph for 80ks with XMM and 15 HST orbits will allow to study correlated X-ray and UV variability and achieve a breakthrough in our understanding of O stars.|
|Publication||No observations found associated with the current proposal|
|Instrument||EMOS1, EMOS2, EPN, 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, 2021-10-27T00:00:00Z, 086223, 18.02_20200221_1200. https://doi.org/10.5270/esa-[xxxxxxx]|