Recent observations obtained with the Soft X-ray Telescope (YOHKOH) by
Uchida et al. (1992) have suggested that a non-negligible input to the mass
and magnetic field of the solar wind is coming from the observed
continuous expansion of active regions. The mass loss in the solar wind
coming from an outward expansion of a single coronal active region is
10
- 10
g s
and the magnetic flux of
10
Mx s
.
To test the hypothesis of ARs as possible candidates as the source of the low-speed solar wind, we can compare the parameters of the solar wind observed above ARs with those above coronal holes, which on the other hand are commonly identified as the source of the high-speed solar wind. That is we compare the electron density, kinetic temperatures, flow velocities to assess the mass and energy losses in both cases.
(Observing mode as for the observing program: "Temperature gradient in coronal holes")