|Title||Pulsations from the Vela Jr. CCO: Another Phase Shifter|
|Author||Prof Jules Halpern|
|Description||We detect a possible spin period from the compact X-ray source in the Vela Jr. SNR. The period and spectrum are consistent with those of the three other CCO pulsars. The pulsed light curve has an abrupt, half-cycle phase shift at the cross-over energy of the two-blackbody fit to the spectrum, like that found for the Puppis A CCO pulsar. We propose to confirm this result and obtain the all-important second period measurement to characterize the spin-down properties of this pulsar: its energy loss rate, dipole B-field, and initial period. If a weakly magnetized NS like the other CCO pulsars, it will prove the existence of an important new class of young NSs. We will model the surface temperature and viewing geometry to address the mystery of hot spots on weakly magnetized NSs.|
|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, 2011-12-16T00:00:00Z, 065251, 17.56_20190403_1200. https://doi.org/10.5270/esa-f4wqnsc|