|Title||X-ray spectroscopic study of supersoft sources SSC_21|
|Author||Dr Michael Watson|
|Description||GT- Luminous supersoft X-ray sources are characterized by soft spectra and high bolometric luminosities of the order of 10^37 erg-s. We propose to observe one of the brightest of the more than 30 known sources. EPIC and-or RGS X-ray spectra will allow us to derive essential information on the origin of the X-ray emission and thus to distinguish between white dwarf (WD) and neutron star models. In the case of a WD origin, the modelling of the spectra will provide measures of the temperature, gravity and abundances which in turn allows to estimate mass accretion rates, WD masses and possibly information on its C+O or O+Ne+Mg composition. This will enable us to test the most popular version of the WD models, namely the close-binary supersoft source model.|
|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, 2002-03-29T00:00:00Z, 011115, PPS_NOT_AVAILABLE. https://doi.org/10.5270/esa-78hhnpa|