|Title||Coronal abundances in RS CVn with well determined photospheric abundances|
|Author||Dr Fabio Favata|
|Description||We propose to obtain good S-N RGS observations of two RS CVn-type binaries (V851 Cen and AG Dor) for which we have recently obtained detailed chemical analysis of their photospheric composition. This will allow to study the presence of a FIP (or inverse FIP, as recently indicated by XMM RGS analyses of other active binaries) by detailed comparison with their photospheric abundance -- rather than by comparison with a solar mix. This appears to be particularly r^ant as our photospheric analysis shows that the photosphere chemical composition for these stars appears to be significantly different from the solar one. The data obtained here will thus allow a detailed discussion of whether an inverse FIP effect is present in the corona of active binaries.|
|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, 2004-03-25T00:00:00Z, 014035, 17.56_20190403_1200. https://doi.org/10.5270/esa-2h8ktyy|