|Title||Follow-up XMM-Newton observations of the cornerstone Wolf-Rayet binary WR140.|
|Author||Dr Michael De Becker|
|Description||WR140 is the archetypal long period WR+O colliding wind binary (CWB) system, where the wind from the WR star collides with the wind of its massive companion. Its X-ray brightness, giant IR outbursts, and distinctive non-thermal (NT) radio lightcurve are all attributed to the wind-wind collision region (WCR), the properties of which dramatically change due to the exceptionally high orbital eccentricity (e > 0.88). XMM-Newton observations through periastron passage in AO7 provided unprecedented data on this system. Follow up observations will provide data to complete our view of the X-ray emission from its colliding winds, in order determine the key parameters of this system and the physical processes occuring at the WCR.|
|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, 2012-04-16T00:00:00Z, 065130, 17.56_20190403_1200. https://doi.org/10.5270/esa-k8s27bv|