MRI-driven X-ray disc coronae in cataclysmic variables
UNSPECIFIED (2006) MRI-driven X-ray disc coronae in cataclysmic variables. In: Symposium on the X-ray Universe 2005, El Escorial, SPAIN, SEP 26-30, 2005. Published in: Proceedings of the X-ray Universe 2005, Vols 1 and 2, 604 pp. 151-154.Full text not available from this repository.
A prediction of the magneto-rotational instability (MRI) model for angular momentum transport in accretion discs is that high-state discs should have X-ray coronae. This is because magnetic flux is buoyant in the disc, and floats to high scale heights and low optical depths before depositing energy through reconnection. However, the best observed accretion discs, i.e. those in cataclysmic variables, have not supported the presence of a disc corona until now. I show that observations of high-state accretion discs with XNM-Newton and Chandra are now revealing a new X-ray emission component that may arise from an MRI-driven corona.
|Item Type:||Conference Item (UNSPECIFIED)|
|Subjects:||Q Science > QB Astronomy|
|Series Name:||ESA SPECIAL PUBLICATIONS|
|Journal or Publication Title:||Proceedings of the X-ray Universe 2005, Vols 1 and 2|
|Publisher:||ESA PUBLICATIONS DIVISION C/O ESTEC|
|Number of Pages:||4|
|Page Range:||pp. 151-154|
|Title of Event:||Symposium on the X-ray Universe 2005|
|Location of Event:||El Escorial, SPAIN|
|Date(s) of Event:||SEP 26-30, 2005|
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