|Title||Long-term Monitoring of Two Isolated Neutron Stars|
|Author||Dr Peter Woods|
|Description||The spin-down rates of two Isolated Neutron Stars were recently measured using a compilation of XMM-Newton and Chandra data spanning 5 years. Both objects were found to have magnetic field strengths of 3e+13 G, intermediate between ordinary pulsars and magnetars. Interestingly, strong timing noise, spectral variability, and pulse morphology changes were observed in RX J0720.4-3125 -- characteristics commonly seen in magnetars. Here, we propose a monitoring campaign of two INSs to better constrain their timing characteristics, identify glitches, and further probe spectral variability and pulse morphology evolution. Through which, we intend to better quantify the similarities and differences with magnetars, and thus elucidate the nature of INSs as a class.|
|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, 2008-06-23T00:00:00Z, 040285, 17.56_20190403_1200. https://doi.org/10.5270/esa-jk5n15r|