English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Tools annual

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Presents the access of premium content as premium feature

Premium Content

Global: Zendy Plus annual

Global: Zendy Free Plan

We have developed a numerical MHD model of the propeller candidate star AEAqr using axisymmetric magneto-hydrodynamic (MHD) simulations. We suggest thatAE Aqr is an intermediate polar-type star, where the magnetic field isrelatively weak and an accretion disc may form around the white dwarf. The staris in the propeller regime, and many of its observational properties aredetermined by the disc-magnetosphere interaction. Comparisons of thecharacteristics of the observed versus modelled AE Aqr star show that the modelcan explain many observational properties of AE Aqr. In a representative model,the magnetic field of the star is B\approx 3.3x10^5 G and the time averagedaccretion rate in the disc is 5.5\times 10^{16} g/s. Most of this matter isejected into conically-shaped winds. The numerical model explains the rapidspin-down of AE Aqr through the outflow of angular momentum from the surface ofthe star to the wind, corona and disc. The energy budget in the outflows,9x10^{33} erg/s, is sufficient for explaining the observed flaring radiation indifferent wavebands. The time scale of ejections into the wind matches theshort time scale variability in the light curves of AE Aqr.

Comparisons of MHD Propeller Model with Observations of Cataclysmic Variable AE Aqr