|Title||Complete high-energy census of the cool stellar neighbors|
|Author||Prof Beate Stelzer|
|Description||TESS is soon to boost the number of known exoplanetary systems especially with Earth-size planets around nearby, small (M-type) stars. Irradiation by the stars. high-energy emission can severely affect the planet atmospheres which, therefore, cannot be characterized without knowing the host star X-ray-UV (XUV) properties. These emissions are also key diagnostics of stellar dynamos and a tracer of spin evolution in fully convective stars. Yet, >40% of the M dwarfs within only 10pc have no tight limit on their X-ray emission. We, thus, propose an XUV XMM-Newton survey of all 41 still X-ray undetected early- to mid-M dwarfs within 10pc, providing the ultimate constraint on M dwarf XUV emission as vital input to models of planetary atmospheres, dynamos and spin evolution.|
|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, 2021-05-05T00:00:00Z, 084084, 18.02_20200221_1200. https://doi.org/10.5270/esa-hc24t72|