|Title||X-Ray Line Beaming in Cataclysmic Variables due to Resonance Scattering|
|Author||Mr Yukikatsu TERADA|
|Description||Galactic compact objects with extremely strong ionized Fe emission lines, with the equivalent width (EW) reaching sim 4000 eV, have been discovered with ASCA, including AXvirgulJ1842.8-0423 and RXvirgulJ1802.1+1804. These objects are thought to be binary systems containing magnetized white dwarf (WD). A possible interpretation of the strong Fe-K line is the line-photon beaming in the WD accretion column, due to resonance scattering of line photons augmented by the vertical velocity gradient there. To firmly establish the proposed mechanism, an XMM observation of a similar system, AXvirgulJ2315-592, is proposed. Uninterrupted coverage will accurately quantify how the line equivalent widths of many ion species change as the white dwarf rotates.|
|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, 2006-11-22T00:00:00Z, 007994, 17.56_20190403_1200. https://doi.org/10.5270/esa-geopyvj|