GT-UX Ari is a very active RS CVn-type binary system that has produced some ofthe most energetic coronal flares seen on such stars. We propose to observe UX Ari for 40 ks to investigate the composition of its quiescent corona indetail, and, if a flare is seen, to follow the temperature, density, abundance,and plasma velocity histories during the evaporation and cooling processes indetail with the RGS and the EPICs. To avoid saturation, the pn and one MOScamera will be used in TIMING mode, both with the medium filter. The OM willobserve with the UVW2 filter. Coordinated radio VLA and spatially resolvedVLBA/VLBI as well as optical observations are planned to study the geometry andenergy balance of UX Ari.s atmosphere.
Instrument
EMOS1, EMOS2, EPN, OM, RGS1, RGS2
Temporal Coverage
2001-02-15T11:00:44Z/2001-02-16T04:08:11Z
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 Albert Brinkman, 2002, 'GT Observations of Active Cool Stars: UX Ari', 17.56_20190403_1200, European Space Agency, https://doi.org/10.5270/esa-2vfsbcv
