|Title||Gas-Phase Abundance Variations from Dust Grain Sputtering in an SNR Shock|
|Author||Dr Brian Williams|
|Description||Sputtering in an SNR shock erodes dust grains, returning elements such as Fe, Si, and Mg to the gas phase. Since these elements are thought to be significantly depleted onto grains, the gas phase abundances in the post-shock region of an SNR shock should be a function of the time since the gas was shocked. This has never been directly observed, as doing so would require a large, well-resolved, edge-on shock from an SNR, detailed infrared modeling of the emission from warm dust in the post shock region, and sufficient counts in the X-ray spectra to place tight constraints on the abundances. The ..P7. region in the northeast Cygnus Loop satisfies all these criteria, and we propose a deep observation of this non-radiative shock region.|
|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, 2015-06-30T22:00:00Z, 074182, 17.56_20190403_1200. https://doi.org/10.5270/esa-o60fiep|