|Title||The stellar wind of hot subdwarf stars|
|Author||Dr Nicola La Palombara|
|Description||All we know about hot subdwarf (sd) stars is based on studies in the optical and UV domain, while none of them has been detected at X-rays. The only exception is the sdO binary HD49798, in which the WD companion shows a significant X-ray emission, due to the matter accreted from the sd primary. A recent XMM observation of this source has revealed a significant X-ray emission also during the eclipse phase, when the WD is obscured by the primary subdwarf, thus suggesting that the observed X-ray flux is due to the subdwarf itself. In order to investigate if also other sdO stars are characterized by an intrinsic X-ray emission, we propose to observe BD+37 442: it is a nearby and bright sdO star with a strong stellar wind, therefore it is the best candidate to perform this type of search.|
|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, 2012-09-13T00:00:00Z, 067139, 17.56_20190403_1200. https://doi.org/10.5270/esa-vv7pyiu|