|Title||X-ray Observations of DW UMa: A Cure for the SW Sex Syndrome|
|Author||Dr Donald W. Hoard|
|Description||We propose a 27 ksec XMM observation (with EPIC as prime instrument) of the novalike CV and archetypal SW Sex star, DW UMa. Current models for the SW Sex syndrome involve 3 scenarios: magnetic accretion, a disk wind, and stream overflow. Our XMM light curve and spectral energy distribution (at the intrinsic energy resolution of the EPIC CCDs) will test and constrain the magnetic model. For example, DW UMa shows .flares. in its optical emission lines on timescales of tens of minutes, similar to those seen in some weakly magnetic CVs. The detection (lack) of X-ray flaring will argue strongly for (against) the magnetic scenario. Confirmation of magnetic accretion would identify the SW Sex stars as the intermediate polars with the highest mass transfer rates.|
|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, 2004-11-05T00:00:00Z, 014297, 17.56_20190403_1200. https://doi.org/10.5270/esa-bhlae5w|