|Title||PSR J1734-3333: A Magnetar Progenitor?|
|Author||Prof Victoria Kaspi|
|Description||We propose X-ray observations of the radio pulsar PSR J1734-3333, a possible magnetar progenitor. This source, a 1.2 s radio pulsar, has inferred surface magnetic field 5.2e13 G, well above the quantum critical field and very close to those of bona fide magnetars. In radio timing observations we have recently measured a stable braking index for this source, n=0.9+--0.2. So low a braking index is unprecedented and suggests effective magnetic field growth, such that this source may soon become some form of magnetar. A previous deep XMM observation was significantly contaminated by background flaring. Here we request an observation to replace the exposure time lost due to flares, in order to constrain the sources spectral properties and search for pulsations.|
|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, 2014-04-12T00:00:00Z, 069296, 17.56_20190403_1200. https://doi.org/10.5270/esa-aevwlb7|