|Title||Magnetospheric activity of a Classical T Tauri star|
|Author||Dr Kester Smith|
|Description||We propose to harness the unprecedented sensitivity of XMM to obtain the first detailed picture of the X-ray emission from a Classical T Tauri star. Classical T Tauri stars possess complex, magnetically dominated circumstellar environments, in which a stellar field truncates an active accretion disk, and forces material to corotate with the star as it falls inwards to the stellar surface. The magnetosphere-disk interaction leads to reconnection of field lines at the inner disk radius, and is probably responsible for driving bipolar jets. Thus Classical T Tauri stars possess several potential X-ray sources, powered by reconnection or shocks, with different velocities and locations in the system. This makes them prime candidates for detailed X-ray studies.|
|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, 2002-09-17T00:00:00Z, 006714, 17.56_20190403_1200. https://doi.org/10.5270/esa-kdh5mh7|