|Title||XMM-Newton monitoring of the binary x-ray pulsar SAX J0635+0533|
|Author||Dr giancarlo cusumano|
|Description||Modulations detected in the observed spin period of the 34virgulms x-ray pulsar SAX J0635+0533 confirm that the pulsar is in a binary system with a massive star and place a lower bound on the intrinsic period derivative of the pulsar of 4x10^-13 ss^-1. The high spin-down rate would require a very high accretion rate if produced by accretion and suggests, instead, that the pulsar is rotation powered with a characteristic age of less than 1400 yr. We propose a set of XMM-Newton observations to accurately measure the position of the source, to search for extended emission from the system, and to accurately measure the orbital parameters of the system. The latter is mandatory to fold gamma-ray data to identify SAX J0635 + 0533 as x-ray counterpart of 2EGvirgulJ0635 + 0521.|
|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, 2005-05-15T00:00:00Z, 014687, 17.56_20190403_1200. https://doi.org/10.5270/esa-cv4q2p7|