M dwarf flare (dMe) stars provide excellent laboratories for the study ofmagnetic flaring activity, coronal heating, and chemical fractionationmechanisms. Quiescent element abundances seem to be tied to the first ionizationpotential (FIP), but the nature of that dependence varies with the stellaractivity level, whether the emission is quiescent or flaring, and other factors.Understanding flare abundances is important because much of coronal .quiescent.emission is likely the result of continuous X-class .microflares. Only eightlate-type dMe systems have been studied using XMM or Chandra gratings, and alarge gap exists between low- and high-activity versions of those stars that canonly be bridged with an observation of Ross 154.
Instrument
EMOS1, EMOS2, EPN, OM, RGS1, RGS2
Temporal Coverage
2010-03-19T13:07:30Z/2010-03-20T08:11:06Z
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 Bradford Wargelin, 2011, 'Bridging the dMe Gap with Ross 154', 17.56_20190403_1200, European Space Agency, https://doi.org/10.5270/esa-wc64fli
