|Title||Exploratory X-ray Observations of Quiescent Recurrent Novae in CVs|
|Author||Dr Koji Mukai|
|Description||For a binary to be a recurrent nova (RN), it must contain a massive white dwarf near the Chandrasekhar limit, making it a candidate progenitor of type Ia supernova. The symbiotic RN, T CrB, is now known to be a virgul10^34 erg-s hard X-ray source. While we have initiated a program of pointed X-ray observations of symbiotic RN systems, other RNe are in cataclysmic variable (CV) systems with a Roche-lobe filling mass donor. Because we believe that the high X-ray temperature and luminosity seen in T CrB are due to the high mass of the white dwarf, we expect that there are additional X-ray luminous objects among CV RNe. We propose to test this prediction by observing 4 such objects (V394 CrA, CI Aql, IM Nor and U Sco) in quiescence with XMM-Newton.|
|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, 2011-03-23T00:00:00Z, 060307, 17.56_20190403_1200. https://doi.org/10.5270/esa-jja58iy|