|Title||Why are millisecond pulsar magnetic fields low and how do their X-rays arise|
|Author||Dr Natalie Webb|
|Description||Binary millisecond pulsars (MSPs) found in the field are thought to be .recycled. from accreting pulsars. These MSPs have short periods, low spindown rates (Pdot) and consequently low surface magnetic fields (B_s) as B_s is proportional to sqrt(Pdot.P). It is unclear, however, how the MSP B_s can evolve from the high fields observed in pulsars to the low MSP values. Two models have been proposed to explain this evolution. Further, the origin of the high energy emission is unclear with too few MSP observations in the X-ray domain to differentiate between competing models. With these XMM-Newton observations of four MSPs previously unobserved in X-rays, we will discriminate between differing models describing the magnetic field evolution and the high energy emission origin.|
|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, 2008-09-27T00:00:00Z, 040662, 17.56_20190403_1200. https://doi.org/10.5270/esa-xgy81xz|