|Title||Resolving Low energy lines from LMXRB|
|Author||Dr Lorella Angelini|
|Description||ASCA obsevations of the LMXRB X0918-54,X1543-62 and X0614+09 reveal strong emission lines in the 0.5-1 keV band.The emission is consistent with O and Fe L, but major uncertanties remain in establishing the line emission mechanism. The recombination continuum,a signature of photoionization, is missing or at lower level in all systems. A collisional plasma better reproduces the spectrum. Scattering and 3-body recombinations are other possible mechanism that can lower the recombination.We propose to observe X0918-54 and X1543-62 with the XMM gratings.These observations will differentiate line emission with an unprecedented resolving power. This capability will pin down the mechanism responsible for the line emission, and define abundances to constrain the system|
|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, 2002-07-27T00:00:00Z, 006114, 17.56_20190403_1200. https://doi.org/10.5270/esa-27apolb|