|Title||The Coronal Properties of the High-Metallicity G IV-V Star 11 LMi (HD 82885)|
|Author||Dr STEPHEN DRAKE|
|Description||The coronal abundances of late-type stars have been found to show at least 3 different patterns (the First Ionization Potential (FIP) effect, the Inverse-FIP effect, and an intermediate pattern), which appear to be mostly controlled by the level of stellar activity. The influence of stellar metallicity on stellar coronal properties is still unclear, since most of the stars with well-studied coronal spectra have photospheric abundances similar to (or assumed to be) the solar photospheric values. We propose to use XMM-Newton to observe 11 LMi (= HD 82885), a known X-ray source, which has 2.0-2.5 times solar photospheric abundances, in order to study the effect of the high underlying metallicity on the temperature structure and abundances of its coronal plasma.|
|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, 2010-05-27T00:00:00Z, 060229, 17.56_20190403_1200. https://doi.org/10.5270/esa-pbv5ucl|