|Title||Probing the AGB Stellar Dynamo in the Very Young Planetary Nebula K 3-35|
|Author||Dr Martin Guerrero|
|Description||Planetary nebulae (PNe) consist of stellar material ejected by stars less massive than than 8--10 solar masses during the asymptotic giant branch (AGB) phase. There is strong evidence that fast collimated outflows or jets that occur toward the end of the AGB phase are responsible for producing the bipolar or multi-polar shapes of PNe. However, the origin of collimated outflows in PNe is not clear. Stellar magnetic field has been invoked as the launching mechanism for collimated outflows in PNe, but supporting evidence is lacking.The young PN K 3-35 is the only known PN whose bipolar outflows appear to be collimated by a magnetized torus. We request XMM-Newton observations of K 3-35 to search for the X-ray emission associated with the stellar corona powered by the magnetic field.|
|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, 2008-01-04T00:00:00Z, 030088, 17.56_20190403_1200. https://doi.org/10.5270/esa-q2ipf39|