|Title||RGS Observations of the Two X-Ray-Brightest Planetary Nebulae: Origin of Hot Gas|
|Author||Dr Martin Guerrero|
|Description||Planetary nebulae (PNe) consist of material ejected by stars with masses less than 8-10 solar masses. The current fast stellar wind sweeps up the previous slow AGB wind to form the PN shell, and the shell interior is expected to be filled with hot gas that emits X-rays. Chandra and XMM-Newton have detected diffuse X-rays from PNe at levels much lower than theoretical expectations. The different abundances of the fast stellar wind and the slow AGB wind traces the origin of the hot gas in PNe. We request XMM-Newton RGS observations of the two X-ray-brightest PNe, BD+30 3639 and NGC 6543, to determine the chemical abundances and origin of the hot gas and further use these to constrain the amount of heat conduction between the hot gas and the cool nebular shell.|
|Publication||No observations found associated with the current proposal|
|Instrument||EPN, OM, RGS1, RGS2, EMOS1, EMOS2|
|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, 2008-08-29T00:00:00Z, 030057, 17.56_20190403_1200. https://doi.org/10.5270/esa-qod49tm|