For a binary to be a recurrent nova (RN), it must contain a massive white dwarf(WD) near the Chandrasekhar limit, making it a candidate progenitor of type Iasupernova. Although the WD masses and the accretion rates in RNe must all besimilarly high, the X-ray properties of RNe with red-giant donar stars can bewildly different, ranging from hard and luminous (virgul1e34 ergs/s) to softer andsignificantly fainter (below 1e32 ergs/s). Such drastic differences may indicatethat a third parameter, such as the spin period or the core temperature of theWD, may play an important role. Here we propose quiescent X-ray observations of4 RNe in cataclysmicvariable (CV) systems to test if a third parameter indeedexists.
Instrument
EMOS1, EMOS2, EPN, OM, RGS1, RGS2
Temporal Coverage
2010-09-20T23:04:57Z/2010-10-06T02:20:41Z
Version
17.56_20190403_1200
Mission Description
The European Space Agencys (ESA) X-ray Multi-Mirror Mission (XMM-Newton) was launched by an Ariane 504 on December 10th 1999. XMM-Newton is ESAs 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 Earths 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.
European Space Agency, Dr Koji Mukai, 2011, 'X-ray Observations of Quiescent Recurrent Novae in CVs', 17.56_20190403_1200, European Space Agency, https://doi.org/10.5270/esa-0j1nhua
