|Title||The First Glitch in a CCO Pulsar|
|Author||Dr Eric Gotthelf|
|Description||CCO pulsars are stable rotators with weak dipole magnetic fields and small spin-down rates. Old radio pulsars with similar spin parameters as CCOs are never seen to glitch. However, the CCOs are much younger than their timing ages, and we have discovered the first CCO glitch, in our XMM monitoring of 1E 1207.4-5209. CCOs are theorized to have strong, buried crustal magnetic fields that will diffuse out in <1 Myr. Our discovery therefore supports a recent conjecture that glitches could be triggered by the diffusion of strong magnetic fields. We need to continue the X-ray timing of 1E 1207.4-5209 post-glitch to determine a definite value for the magnitude of its frequency change, and to test for any change in frequency derivative that could be indicative of growth of its dipole field.|
|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, 2020-01-23T23:00:00Z, 082194, 17.56_20190403_1200. https://doi.org/10.5270/esa-tn4tgio|