|Title||Continuing the Long-Term Monitoring of the CCO Pulsar 1E1207.4-5209|
|Author||Prof Jules Halpern|
|Description||The CCO pulsar 1E1207.4-5209 is an extremely stable rotator, with a weak B-field and a small spin-down rate that has remained constant to <1% over 14.5 years. It is a unique NS whose B-field is measured as virgul9.e10 G, both spectroscopically and through timing. Yet the properties of CCO pulsars cannot be explained unless they have strong crustal magnetic fields, perhaps buried by SN fall-back material. We propose a modest program that will continue precise timing and spectroscopy of 1E1207.4-5209 to monitor for a change in B-field that may diffuse through or break the crust. These observations will also be very sensitive to torque noise due to minute levels of accretion from a hypothetical fall-back disk.|
|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, 2017-08-10T22:00:00Z, 078000, 17.56_20190403_1200. https://doi.org/10.5270/esa-cam9gfg|