|Title||Calibrating the time-evolution of the high-energy emissions of GKM stars|
|Author||Dr Ignasi Ribas|
|Description||The time-evolution of X-ray to UV stellar fluxes is key to understand planetary atmospheres via effects such as photochemistry and evaporation. While the flux evolution of solar-type stars is well understood, this is not the case of K and M stars. Our approach is to determine the variation of L_x with age for KM stars by observing wide pairs with a white dwarf that serves as a chronometer. Here we plan to nail down the typical X-ray emission level at an age of virgul4 Gyr. We propose very deep X-ray observations of 3 M stars, reaching the lowest X-ray emission levels observed in volume-limited M dwarf samples of unknown age. Comparison with the distribution in a volume-limited sample will allow us to estimate the fraction of M dwarfs younger than 4 Gyr.|
|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, 2017-01-05T23:00:00Z, 076038, 17.56_20190403_1200. https://doi.org/10.5270/esa-1o0a8mv|