Symbiotic stars are interacting binaries, containing white dwarfs accreting athigh rates from a wind of the red giant companion. These systems are possibleprogenitors for type Ia supernovae. The most crucial parameter in symbioticsystems is the accretion rate, since i) it determines (together with the mass)the lifetime of the white dwarf until a possible supernova explosion and ii)possibly explains the striking dichotomy concerning the fraction of objects withand without jets in symbiotics and CVs. In this project, we will search for hardX-ray emission from symbiotic stars which is the most valuable probe for theaccretion process. We will determine the fraction of sources which produce hardX-rays, the mass distribution of white dwarfs, the distribution of accretion rates and their lifetimes.
Instrument
EMOS1, EMOS2, EPN, OM, RGS1, RGS2
Temporal Coverage
2009-05-02T10:37:52Z/2010-03-06T08:06:56Z
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 Matthias Stute, 2011, 'A survey in hard X-rays for probing accretion and ejection in Symbiotic Stars', 17.56_20190403_1200, European Space Agency, https://doi.org/10.5270/esa-6q1zhgr
