|Title||AR Sco; the first white dwarf pulsar?|
|Author||Dr Danny Steeghs|
|Description||We recently discovered that a long-known variable star, AR Sco, is a multi- wavelength emission source that shows extraordinarily strong pulsations on a 2 minute period from far ultraviolet to radio frequencies. We believe that AR Sco is the first white dwarf radio pulsar, where the combination of a large field and rapid rotation results in the acceleration of relativistic particles that blast the inner hemisphere of its M-dwarf companion, akin to the well-known mili-second pulsars. We request XMM-Newton observations in order to test this interpretation and determine the spectral and timing properties of AR Sco.s X-ray emission. This should tell us whether there is significant accretion onto the compact object or if other processes and emission are responsible.|
|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, 2017-09-30T22:00:00Z, 078394, 17.56_20190403_1200. https://doi.org/10.5270/esa-ye2x5w5|