Magnetic field evolution in accreting white dwarfs
Article first published online: 25 JUN 2002
Monthly Notices of the Royal Astronomical Society
Volume 333, Issue 3, pages 589–602, July 2002
How to Cite
Cumming, A. (2002), Magnetic field evolution in accreting white dwarfs. Monthly Notices of the Royal Astronomical Society, 333: 589–602. doi: 10.1046/j.1365-8711.2002.05434.x
1 Except in the very outermost layers, it is always a good approximation that the hydrostatic pressure P is much larger than the magnetic pressure B2/8π.
2 This numerical approach is similar to that of WVS, who included the advection terms in their study of cooling white dwarfs. WVS found that the significant contraction that occurs in the pre-white dwarf stages of evolution increased the rate of ohmic decay, by taking the initial n=1 decay mode and generating higher-n components. This interesting effect is not significant during the accretion process, which involves much smaller changes in white dwarf radius.
3 We thank the referee, J.-M. Hameury, for raising this issue.
4 We thank Alexander Potekhin for bringing these results to our attention. Details of these calculations and computer codes to calculate conductivities can be found at http://www.ioffe.rssi.ru/astro/conduct/index.html.
- Issue published online: 25 JUN 2002
- Article first published online: 25 JUN 2002
- Accepted 2002 February 18. Received 2002 February 12; in original form 2001 November 16