Young stars can produce X-rays by different mechanisms: Coronal activity,accretion shocks and shocks in outflows. We propose to observe two targetswithin one field-of-view (FOV): SU Aur is accreting mass from a disk and showsviolent coronal activity. We will study the time evolution of stellar flares ontime scales from seconds to minutes using the high count rate in the EPIC andthe OM to discover interactions with the accretion streams: The signature of theflare onset will differ in X-rays and UV between flares on coronal loops andflares on those field lines, which carry the accretion stream from the disk. ABAur is more massive, it shows a tentative modulation in the X-ray luminosityapparently without spectral changes and contrary to model expectations.
Instrument
EMOS1, EMOS2, EPN, OM, RGS1, RGS2
Temporal Coverage
2012-02-15T20:48:40Z/2012-02-17T01:27:38Z
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 Hans Moritz Guenther, 2012, 'Interactions of flares comma accretion and wind in young stars', 17.56_20190403_1200, European Space Agency, https://doi.org/10.5270/esa-f3j0nz2
