|Title||Does the Fe K line evolve around the color-color diagram of neutron star GX17+2|
|Author||Dr Edward Cackett|
|Description||The X-ray spectra of neutron star LMXBs vary frequently, tracing out characteristic Z or atoll tracks on color-color diagrams. However, the driving force behind this variability remains unclear. The recent discovery of broad, relativistic Fe K emission lines in these systems may finally provide the key to unlocking this secret. The asymmetric line profile observed is characteristic of emission from the inner disk around a compact object, where extreme Doppler shifts and gravitational redshifts are at play. Thus, the Fe K line acts as a useful tool to track the extent of the inner disk. With four, 30 ks XMM-Newton observations of neutron star LMXB GX 17+2, we will follow the evolution of the inner disk around the color-color diagram, testing how, and if, the inner accretion flow changes.|
|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, 2012-04-08T00:00:00Z, 065391, 17.56_20190403_1200. https://doi.org/10.5270/esa-ysr5pym|