Recent ROSAT and ASCA observations have revealed that intermediate mass young stars are X-ray emitters. We found that the X-ray emission probably originates from the magnetic activity, which continues the early phase of the main-sequencestage for B-type stars. With the Chandra and ASCA observations, we found two young stars, rho Oph S1 and HR 6000, showed characteristic X-ray features; low abundance thermal or non-thermal emission and rapid variation, but the detailed feature is uncertain due to the lack of photon statistics. With XMM-Newton, we determine whether the X-ray emission is thermal or not, and see the variation of X-ray intensity in a short timescale. From these features, we reveal the X-ray emission mechanism.
Instrument
EMOS1, EMOS2, EPN, OM, RGS1, RGS2
Temporal Coverage
2003-09-06T06:11:08Z/2003-09-06T12:32:09Z
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 Kenji Hamaguchi, 2004, 'Intermediate Mass Young Stars Showing Peculiar X-ray Features', 17.56_20190403_1200, European Space Agency, https://doi.org/10.5270/esa-10rli2e
