|Title||The X-ray Emission of Late-type Companions to Planetary Nebula Nuclei|
|Author||Dr Kevin Briggs|
|Description||Rapid rotation generates strong magnetic activity in late-type stars via a dynamo. Late-type companions to the nuclei of planetary nebulae (PNe) are expected to be rapid rotators due to accretion from the slow heavy wind of the nucleus while it was an AGB star, and hence strong X-ray emitters. Yet, XMM-Newton found two of three such stars to have X-ray activity levels an order of magnitude lower than those of other fast rotators. This impacts on our understanding of unresolved X-ray sources in PNe and may give clues as to the vital ingredients for an efficient dynamo. We aim to measure the X-ray emission level of the archetype, Abell 35, and the two brightest d. symbiotics, young PNe containing late-type rapid rotators, to test the ubiquity of this low activity.|
|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, 2008-05-30T00:00:00Z, 040167, 17.56_20190403_1200. https://doi.org/10.5270/esa-jwx0vlw|