|Title||Observation of the persistent Be binary pulsars RX J0440.9+4431|
|Author||Dr Nicola La Palombara|
|Description||Many X-ray binary pulsars have a soft excess below 10 keV. For the high luminosity pulsars, the fit of this component with thermal emission models usually provides low temperatures and large emission regions. On the other hand, we recently found that in persistent, low-luminosity and long-period Be pulsars the observed excess can be modeled with a rather hot blackbody component of small area, which can be interpreted as emission from the NS polar caps. We propose to observe the Galactic Be pulsar RX J0440.9+4431, which is a poorly studied member of this class of sources. Our aim is to examine, at an unprecedented sensitivity level, its spectral and timing characteristics, and to test if the description of the other persistent pulsars is applicable also in this case.|
|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, 065366, 17.56_20190403_1200. https://doi.org/10.5270/esa-znm8j8j|