|Title||Study of the spectral soft excess in high luminosity transient pulsars|
|Author||Dr Nicola La Palombara|
|Description||The spectra of many X-ray pulsars show a low-energy component in addition to the main power-law, which can be described with different models (both thermal and non-thermal). The study of this feature is essential in order to cast light on the physical processes on-going in accreting sources. Due to the low absorption in its direction, the transient pulsars in the SMC, which can reach high luminosities (Lx > 1E38 erg-s), can provide high statistic spectra at low energies; two of them (XTE J0111-7317 and RX J0059.2-7138) have already shown a clear excess during their outburst. Therefore we ask to perform a triggered observation with XMM of a selected sample of transient pulsars in the SMC, if they undergo a bright outburst, in order to characterize the properties of the soft excess.|
|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, 2015-04-07T22:00:00Z, 067473, 17.56_20190403_1200. https://doi.org/10.5270/esa-pxkbv15|