|Title||X-ray Origin of the Young Intermediate Mass Eclipsing Binary, TY CrA|
|Author||Dr Kenji Hamaguchi|
|Description||Recent observations with ROSAT and ASCA have revealed that intermediate mass young stars (Herbig Ae-Be stars: HAeBes) are X-ray emitters. Our survey with ASCA suggests that the X-ray emission originates from some kind of magnetic activity, but the proper mechanism to drive it is uncertain. The possibility that the X-rays come from a nearby companion cannot be excluded. With XMM-Newton, we observe the eclipsing binary TY CrA, which comprises a HAeBe primay and a T-Tauri secondary. By detecting the eclipsing feature with the high S-N data, we will present the first direct evidence for the X-ray emission. We also search for a hot plasma component, which is not detected at the age of TY CrA, and study the spectral evolution of HAeBes.|
|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, 2004-04-25T00:00:00Z, 014639, 17.56_20190403_1200. https://doi.org/10.5270/esa-nw5qbpi|