|Title||DETECTION OF NON-THERMAL X-RAY EMISSION FROM GAMMA2 VELORUM|
|Author||Dr Kenji Hamaguchi|
|Description||Our NuSTAR observations of two massive colliding wind binary systems presented clear evidence of high-energy, non-thermal emission, which probably originate from inverse-Compton (IC) of stellar photons by high-energy electrons accelerated at the wind-wind colliding (WWC) shocks. However, the observed emission is nearly constant unlike the WWC thermal emission, and this is not expected from the standard IC mechanism. To understand the emission mechanism, we need more colliding wind binary systems with different stellar parameters. We propose two NuSTAR observations of another colliding wind binary system, gamma2 Velorum, which shows signatures of WWC X-ray activity and has a GeV gamma-ray counterpart, to detect high-energy non-thermal 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, 2019-12-19T23:00:00Z, 083051, 17.56_20190403_1200. https://doi.org/10.5270/esa-0qmc17i|