|Title||Magnetic Flux and Coronal X-ray Emission in the Late Stages of Stellar Evolution|
|Author||Dr Rodolfo Montez|
|Description||Surface magnetic fields strengths of 2-10 G have been measured from the evolved stars chi Cyg and U Mon. These measurements support the notion that large-scale magnetic fields thread the circumstellar environment of asymptotic giant branch (AGB) and post-AGB stars. Magnetic fields are possible triggers of the superwind phase of AGB stars and asymmetric shaping of mass loss into the post-AGB phase. The low surface magnetic field strengths imply X-ray fluxes that are within reach of deep XMM exposures. We propose XMM X-ray observations of these two evolved stars to detect their predicted low level X-ray emission and establish a coronal origin for any X-ray emission. Ultimately, these observations provide insight into the evolution of stellar magnetic processes.|
|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, 2017-11-11T23:00:00Z, 078207, 17.56_20190403_1200. https://doi.org/10.5270/esa-4vrmpoe|