|Title||Hard X-Ray Emission from Progenitors of Type Ia Supernovae|
|Author||Dr Jennifer Sokoloski|
|Description||Recurrent nova (RN) contain white dwarfs (WDs) whose masses are close to the Chandrasekhar limit. Some RN may thus be progenitors of type Ia supernovae (SNIa). But how do the WDs in these binaries accrete enough material to approach the Chandrasekhar limit? To address this question, and to develop a tool for finding SNIa progenitor candidates at an earlier stage along the path to the Chandrasekhar limit, we propose to test the degree to which hard X-ray emission is a marker for high WD mass. We thus propose to observe two RN that have no previous pointed X-ray observations in quiescence. Our targets both have red-giant mass donor stars, which makes them similar to the one RN known to produce strong, hard X-ray emission. This work is motivated in part by the advent of new hard X-ray surveys.|
|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, 2011-05-07T00:00:00Z, 060498, 17.56_20190403_1200. https://doi.org/10.5270/esa-nfqf9fe|