|Title||X-ray Spectroscopy of the Supersoft Source CAL87|
|Author||Dr Ken Ebisawa|
|Description||We propose to observe the supersoft source (SSS) CAL87 with XMM RGS. ASCA spectrum of CAL87 with the CCD resolution was sucessfully explained with theoretical SSS spectral models, which calculate emission from optically thick white dwarf atmosphere. However, recent XMM and Chandra grating observations of SSS indicates SSS spectra are more complex and current theoretical models cannot explain them satisfactorily. We study the energy spectrum of CAL87 using the state of the art theoretical spectral models, and examine our understanding of CAL87 and SSS. ASCA did not detect spectral changes durig orbital eclipses, which is consistent with the Accretion Disk Corona model. We critically examine this model by studying possible spectral changes during the eclipses.|
|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, 2004-05-22T00:00:00Z, 015325, 17.56_20190403_1200. https://doi.org/10.5270/esa-g44xl0v|