We propose to obtain RGS spectra and EPIC light curves and spectra of themagnetic Be star beta Cep, to provide stringent tests of the magneticallyconfined wind shock model proposed to explain the X-ray emission observed fromthis star. Measurement of the density from the O VII triplet (as well as of theNe and Mg triplets), of the line broadening, and determination of the rotationalmodulation of the spectral characteristics will allow to discriminate X-rayemission due to this novel mechanism from either coronal emission or emissiondue to the shocked winds observed in non-magnetic high-mass stars.
Instrument
EMOS1, EMOS2, EPN, OM, RGS1, RGS2
Temporal Coverage
2005-07-27T04:06:32Z/2005-08-06T18:04:53Z
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 Fabio Favata, 2006, 'The X-ray emission mechanism in magnetic Be stars', 17.56_20190403_1200, European Space Agency, https://doi.org/10.5270/esa-x7o79tw
