|Title||EXPLORING THE OVERLUMINOUS X-RAY EMISSION FROM PSR B0628-28|
|Author||Dr WERNER BECKER|
|Description||The ROSAT source RX J0630.8-2834 was found to be a possible X-ray counterpart of the old field pulsar PSR 0628-28. However, its corresponding X-ray luminosity, more than 380 times higher than what is expected from the pulsar, put severe doubts on the association. A recent Chandra observation, however, yielded the exact position of RX J0630.8-2834, which matches the radio pulsar position within 1.5"! Furthermore, optical observations of the Chandra error box did not detect any counterpart brighter than mag_B=25. The observational evidence thus strongly suggests that PSR B0628-28 indeed is the first overluminos rotation powered X-ray pulsar detected. We propose to observe this unique pulsar in order to establish the association and to explore its X-ray emission mechanisms in detail.|
|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, 2005-05-07T00:00:00Z, 020663, 17.56_20190403_1200. https://doi.org/10.5270/esa-8n3s8ok|