The gyrofrequency does not
depend upon the physical parameters of the atmospheric model except
through its B dependence.
Unfortunately the variation of B with height is ill determined.
Roughly speaking we could assign fields of 30, 300, and 3000 G at the
base of the atmosphere for the three models we consider, but for the
quiet Sun and facula models we would expect a rapid but largely unknown
decrease of B with height.
| 10 | 30 | 100 | 300 | 1000 | 3000 | Gauss | |
| ωce | 1.76x108 | 5.28x108 | 1.76x109 | 5.28x109 | 1.76x1010 | 5.28x1010 | radian/s |
| ωcp | 9.58x103 | 2.87x105 | 9.58x105 | 2.87x106 | 9.58x106 | 2.87x107 | |
| ωcHe+ | 2.41x104 | 7.23x104 | 2.41x105 | 7.23x105 | 2.41x106 | 7.23x106 | |
| ωcHe++ | 1.92x105 | 5.75x105 | 1.92x106 | 5.75x106 | 1.92x107 | 5.75x107 |
As a rule of thumb, the electron gyrofrequency for 1000 G is 2.8 GHz. It is a nice coincidence that the F10.7 solar index is exactly at this frequency, and that 1000 G is a typical B magnitude in an active region!