The coronal abundances of late-type stars have been found to show at least 3different patterns (the First Ionization Potential (FIP) effect, the Inverse-FIPeffect, and an intermediate pattern), which appear to be mostly controlled bythe level of stellar activity. The influence of stellar metallicity on stellarcoronal properties is still unclear, since most of the stars with well-studiedcoronal spectra have photospheric abundances similar to (or assumed to be) thesolar photospheric values. We propose to use XMM-Newton to observe 11 LMi (= HD82885), a known X-ray source, which has 2.0-2.5 times solar photosphericabundances, in order to study the effect of the high underlying metallicity onthe temperature structure and abundances of its coronal plasma.
Instrument
EMOS1, EMOS2, EPN, OM, RGS1, RGS2
Temporal Coverage
2009-05-06T22:40:28Z/2009-05-07T22:17:02Z
Version
17.56_20190403_1200
Mission Description
The European Space Agencys (ESA) X-ray Multi-Mirror Mission (XMM-Newton) was launched by an Ariane 504 on December 10th 1999. XMM-Newton is ESAs 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 Earths 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.
European Space Agency, Dr STEPHEN DRAKE, 2010, 'The Coronal Properties of the High-Metallicity G IV-V Star 11 LMi openParHD 82885closePar', 17.56_20190403_1200, European Space Agency, https://doi.org/10.5270/esa-pbv5ucl
