Our Swift X-ray/UV monitoring campaigns have shown that the evolution of novaeis much more complex than previously believed. We have observed a high degree ofvariability in X-rays for many novae. We focus on the supersoft source phase,which is the brightest phase in X-rays. The aim is to complement our Swiftobservations with studies of short-term variations from which the spin period ofthe white dwarf can be determined and to obtain a high-resolution X-ray spectrumfrom which the chemical composition and the dynamics of the expanding shell canbe determined. Since all observed novae have behaved differently, we need toobserve many novae in order to achieve a more general understanding. We request60ks to observe the next nova that has a Swift count rate of 0.5 cps or more.
Instrument
EMOS1, EMOS2, EPN, OM, RGS1, RGS2
Temporal Coverage
2010-02-19T15:41:09Z/2010-02-20T09:24:44Z
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 Jan-Uwe Ness, 2011, 'A Bright Nova in Outburst', 17.56_20190403_1200, European Space Agency, https://doi.org/10.5270/esa-goqamcu
