|Title||Expanding the Search for Accretion Luminosity in Disk-Polluted White Dwarfs|
|Author||Prof Jay Farihi|
|Description||We propose an X-ray survey of six nearby polluted white dwarfs to detect high-rate accretion states indicated by both optical data and recent theoretical models of collisional cascades within their debris disks. The models predict that the collisionally generated gas will be subject to high and low states of accretion, where the fraction of time spent in the high and detectable states constrains the size of bodies initiating the cascade. The proposed observations will directly test these models, and thus provide valuable information on the nature of the (as yet unseen) parent bodies themselves. Only with X-ray observations can we directly detect ongoing accretion, and provide an invaluable and independent determination of mass accretion rates.|
|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, 2022-07-06T00:00:00Z, 088086, 19.16_20210326_1200. https://doi.org/10.5270/esa-[xxxxxxx]|