|Title||Hidden magnetic accretors in V426 Ophiuchi and LS Pegasi|
|Author||Dr Darren Baskill|
|Description||A surprising result emerged from our analysis of the entire sample of non-magnetic cataclysmic variables (CVs) observed with ASCA. We found two extremely hard systems spectrally distinct from the rest of the sample (V426 Oph & LS Peg). These may be weakly magnetic accretors, but there is no evidence of any periodic variability, the only accepted method of identification. We request XMM-Newton to verify our method of identifying weakly magnetic CVs based on their spectra, by confirming previously uncertain periodicities. In addition, the brightness of V426 Oph will allow us to carry out detailed phase resolved spectroscopy, and search for X-ray reflection and absorption in both. We propose a 30ks observation of V426 Oph, and a 35ks observation of LS Peg.|
|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, 2007-05-20T00:00:00Z, 030629, 17.56_20190403_1200. https://doi.org/10.5270/esa-iepgl63|