|Title||X-rays from the Most Active T Tauri Stars: Accretion Shocks or Magnetic Heating?|
|Author||Prof Frederick Walter|
|Description||What is the nature of the weak X-ray emission observed in the ..continuum. T Tauri stars, low mass PMS stars with large mass accretion rates? Do they arise in a heavily absorbed but otherwise solar-like corona, in a thin dense plasma arising from the accretion shock, or in discrete magnetospheric flaring? These three emission mechanisms produce different spectral or temporal signatures, which can be distinguished using the EPIC imagers in concert with ground-based photometry. If due to accretion, we expect the X-ray flux to correlate with the instantaneous mass accetion rate. We choose three targets that we have been following. The result of this program will be a better understanding of the coronae and magnetic fields in the youngest low mass stars.|
|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, 2006-10-04T00:00:00Z, 030390, 17.56_20190403_1200. https://doi.org/10.5270/esa-6ggrxjw|