|Title||X-ray emission of ultracool dwarfs across the radio-loud - radio-quiet boundary|
|Author||Prof Beate Stelzer|
|Description||Ongoing studies of magnetic activity at the end of the stellar main-sequence have revealed an emerging dichotomy in the X-ray and radio properties. The hetero- geneous properties of ultracool dwarfs (spectral type M7 and later) display either strong coronal-like X-rays with low radio luminosities or predominantly planet-like strong radio emissions with weak X-ray luminosities. This bifurcation is likely driven by the properties of the magnetic field and the stellar rotation. We will explicitly test this hypothesis by filling the parameter space with a TESS-selected sample: The new TESS rotation period will be complemented here with both radio and X-ray data spanning the rotation period threshold across which the dichotomy appears.|
|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, 2021-12-18T00:00:00Z, 086020, 18.02_20200221_1200. https://doi.org/10.5270/esa-[xxxxxxx]|