|Title||Search for Inter-binary X-ray Activity of Young Eclipsing Binary Systems|
|Author||Dr Kenji Hamaguchi|
|Description||The pre-main-sequence (PMS) eclipsing binary TY CrA exhibited a strange flux increase apparently coincident with primary eclipse in an XMM observation on March 2003. Because the flux increase occurred when the star was in an active state, it may have been produced by inter-binary magnetic activity, a mechanism that is new to stellar X-ray emission. To test this hypothesis, we propose observations of the low-mass PMS binary RX J0529.4+0041 during eclipse. These observations will put useful constraints on the location of the X-ray plasma even if no increase in X-ray emission is observed during the eclipse. We also propose a short observation of the young intermediate-mass eclipsing binary EK Cep to measure the X-ray activity level from this star for comparison.|
|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, 2007-03-07T00:00:00Z, 030371, 17.56_20190403_1200. https://doi.org/10.5270/esa-ir92qhk|