|Title||Bridging the dMe Gap with Ross 154|
|Author||Dr Bradford Wargelin|
|Description||M dwarf flare (dMe) stars provide excellent laboratories for the study of magnetic flaring activity, coronal heating, and chemical fractionation mechanisms. Quiescent element abundances seem to be tied to the first ionization potential (FIP), but the nature of that dependence varies with the stellar activity 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 eight late-type dMe systems have been studied using XMM or Chandra gratings, and a large gap exists between low- and high-activity versions of those stars that can only be bridged with an observation of Ross 154.|
|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, 2011-04-24T00:00:00Z, 060195, 17.56_20190403_1200. https://doi.org/10.5270/esa-wc64fli|