| |
 |
| Paper: |
Modeling the Radio Outbursts in AE Aquarii |
| Volume: |
315, Magnetic Cataclysmic Variables (IAU Colloquium 190) |
| Page: |
307 |
| Authors: |
Venter, L.A.; Meintjes, P.J. |
| Abstract: |
In this paper we model the non-thermal radio to infra-red flares from AE Aqr. In our model the non-thermal flares originate in highly magnetized (Bblob ≥ 2000 G) blobs that may be among the propeller ejected outflow. It was shown that the condition β ≤ 1 constrains the frozen-in magnetic field in these blobs to Bblob ≥ 2000 G, which is of the same order of magnitude as the inferred polar field of the secondary. As these magnetized blobs encounter the violent mhd-propeller, processes such as reconnection, magnetic pumping, and shocks will result in continuous acceleration of electrons from (γ = 2 → 30; δ = 2.8 → 2.6) with resultant synchrotron emission. The total radio to infra-red flare spectrum was modelled in terms of such expanding magnetized synchrotron emitting blobs in various stages of their evolution from ρ = (r/r°) = 1 → 400. In terms of our model, the total integrated flux during outbursts, over the wide frequency range from 1 GHz is the result of several (∼ 20) synchrotron emitting blobs observed in different stages of their evolution, resulting in a spectrum showing a peak flux of Sν ∼ 148 mJy at ν ∼ 1805 GHz (∼ 166 microns), where the spectrum changes from a typical self-absorbed Sν ∝ να spectrum to Sν ∝ ν-(δ-1)/2 spectrum, i.e. where the blobs are combined optically thin. |
|
|
|
|
|
