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 CCOpulsars. The pulsed light curve has an abrupt, half-cycle phase shift at thecross-over energy of the two-blackbody fit to the spectrum, like that found forthe Puppis A CCO pulsar. We propose to confirm this result and obtain theall-important second period measurement to characterize the spin-down propertiesof this pulsar: its energy loss rate, dipole B-field, and initial period. If aweakly magnetized NS like the other CCO pulsars, it will prove the existence ofan important new class of young NSs. We will model the surface temperature andviewing geometry to address the mystery of hot spots on weakly magnetized NSs.
Instrument
EMOS1, EMOS2, EPN, OM, RGS1, RGS2
Temporal Coverage
2010-11-13T18:39:57Z/2010-11-14T19:01:13Z
Version
17.56_20190403_1200
Mission Description
The European Space Agencys (ESA) X-ray Multi-Mirror Mission (XMM-Newton) was launched by an Ariane 504 on December 10th 1999. XMM-Newton is ESAs 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 Earths 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.
European Space Agency, Prof Jules Halpern, 2011, 'Pulsations from the Vela Jr. CCO: Another Phase Shifter', 17.56_20190403_1200, European Space Agency, https://doi.org/10.5270/esa-f4wqnsc
