|Title||LMC X-3: The best test of accretion disc models|
|Author||Ms Mari Kolehmainen|
|Description||The persistent black hole binary LMC X-3 is the best system on which to test theoretical models on the shape of the accretion disc spectrum. This is due to the combination of very low absorbing column density along this line of sight, which allows the shape of the disc emission to be constrained at low energies, and its mass accretion rate, which varies by a factor 10, giving a sequence of disc dominated spectra 0.05-0.5 L-LEdd. However, there is currently only 1 good XMM-Newton observation of this source, at close to its peak luminosity. We propose an additional 4 observations which will give a sequence of disc spectra at different luminosities, enabling us to critically test the best current disc models and get the most robust constraints on black hole spin.|
|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, 2013-02-15T00:00:00Z, 067142, 17.56_20190403_1200. https://doi.org/10.5270/esa-ko1mbog|