|Title||GT Observations of Active Cool Stars: UV Cet|
|Author||Dr Albert Brinkman|
|Description||GT-UV Cet is a binary of two low-mass dMe stars at a distance of 2.6 pc. Their combined light curve is continuously variable due to the presence of numerous flares. This star is ideal to study the role of relatively modest flares for coronal heating. By combining observations with radio VLA and possibly VLBA observations, we will investigate details of the flare energy release, flare statistics, and flare heating. The RGS will be used to search for mass motions, density and abundance variations during flares, and to obtain, together with the EPICs, detailed time-dependent emission measure distribution models. One MOS is in TIMING mode, and the pn camera will be used in SML window-medium filter mode to optimize for soft photons. The OM will operate with the UVW1 filter.|
|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, 2002-09-05T00:00:00Z, 011143, 17.56_20190403_1200. https://doi.org/10.5270/esa-l41b1rr|