|Title||The X-ray spectrum of the unusual neutron star X-ray binary SAX J2224.9+5421|
|Author||Dr Nathalie Degenaar|
|Description||We propose a 50-ks XMM-Newton observation of the unusual neutron star X-ray binary SAX J2224.9+5421. Our target was discovered by BeppoSAX-WFC when it exhibited a thermonuclear X-ray burst. Follow-up observations aiming to constrain the persistent emission were performed virgul8 h later and detected the source at a 0.5-10 keV luminosity of L_Xvirgul1E33 erg-s. This is very peculiar since neutron star X-ray binaries are generally considered to be in quiescence at luminosities of L_Xvirgul1E31-1E33 erg-s, while they display accretion outbursts with luminosities of L_Xvirgul1E34-1E38 erg-s. We propose for a detailed investigation of the X-ray spectrum of SAX J2224.9+5421 to gain insight into its nature and extraordinary behavior.|
|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, 2014-07-02T00:00:00Z, 072088, 17.56_20190403_1200. https://doi.org/10.5270/esa-0wkos1u|