|Title||Energy partition in SN 1006: thermal gas, relativistic particles, magnetic field|
|Author||Dr Anne Decourchelle|
|Description||We propose to carry out a deep 1 Ms XMM-Newton observation of the entire SN 1006 supernova remnant (SNR) for a major breakthrough in answering key questions on the physics of SNRs, related to particle acceleration at their shock, magnetic field amplification, heating of the electrons and ions at the shock, abundances and distribution of the chemical elements in the ejecta. This historical type Ia SNR exhibits a dual nature in X-rays with a bipolar non-thermal morphology like in radio, superposed on a fainter extended thermal emission. It is one of the best examples of shock acceleration of cosmic-ray electrons to energies approaching the "knee. of the cosmic-ray spectrum and gathers the most important issues concerning SNR physics.|
|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, 2010-04-01T00:00:00Z, 055563, 17.56_20190403_1200. https://doi.org/10.5270/esa-xewpkga|