|Title||INVESTIGATION INTO THE PLASMA OF THE DARKEST GeV SNR HB 21|
|Author||Mr Hiromasa Suzuki|
|Description||SNRs are thought to be an origin of the galactic cosmic rays. An important problem is how accelerated protons escape from the SNR shock front. From recent studies on SNRs, it is implied that there is a relation between escaping of protons and interaction with molecular clouds (MCs). We chose a GeV SNR HB 21 as the best target to study it, which must be a missing link between GeV SNRs and non-GeV SNRs with the largest size and weakest gemma-ray emission. Such facts enable us spatially resolved spectroscopy for the investigation of the relation between gamma-ray emission and interaction with MCs. Here, we propose a 45 ksec XMM observation of a north-west region of HB 21 to compare the plasma properties to those of another region obtained with Suzaku.|
|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, 2018-11-20T23:00:00Z, 080349, 17.56_20190403_1200. https://doi.org/10.5270/esa-2m51zo5|