This proposal is the second element of our two-year plan to measure thespin-downrate of the pulsar in Puppis A by obtaining a phase-coherent timing solution. Ifit is a weakly magnetized neutron star like the other CCO pulsars, this is theonly practical way of measuring its spin-down. Our sensitivity to P-dot willcorrespond to a surface dipole B-field as small as 3.e10 G, comparable to ourmeasured value for the CCO pulsar PSR J1852+0040 in Kes 79. Such a result wouldprovide important support for the anti-magnetar model of CCOs. In addition,we will explore possible reasons for the unexplained surface hot spots using theenergy-dependent pulse profiles and phase-resolved spectra.
Instrument
EMOS1, EMOS2, EPN, OM, RGS1, RGS2
Temporal Coverage
2011-05-18T22:05:00Z/2012-04-10T10:18:44Z
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, 2013, 'Measuring the Spin-Down and Magnetic Field Strength of the CCO Pulsar in PuppisA', 17.56_20190403_1200, European Space Agency, https://doi.org/10.5270/esa-zzawpag
