Solar Cycle 24 Group B
From RHESSI Wiki
Working Group B: Fast Wind / Plumes
in attendance:
- Jonathan Cirtain
- Craig DeForest
- Yang Liu
- James McLaughlin
- Karin Muglach
- Nour-Eddine Raouafi
- Llan Roth
- Leif Svalgaard
- Luca Teriaca
- Marco Velli
- Yi-Ming Wang
Discussion of Casalbuoni et al (1999) - an extension of the results of Parker (1964). Paper concludes that adding an ad hoc heating profile is no better than specifying the temperature profile.
Discussion of Borovsky (2008) - argument that the inner heliosphere is filled with a network of entangled magnetic flux tubes and that these tubes are fossil structures that originate at the solar surface. Marco doesn't agree with this interpretation of this observation result.
Discussion of Verdini & Velli (2007) - propagation and dissipation of Alfvénic turbulence in a model solar atmosphere.
Filamentary Structure
Plumes have internal structure / filamentary structure.
Acceleration Mechanisms
You can't make a fast solar wind purely based on the temperature profile; you need to add something extra to push it along.
There are 30 - 50 plumes (per polar cap) at any given time.
Cyclotron Waves
Proton solar wind distribution function leads to ANISOTROPIC + BEAM (Marsh et al 1982, Helios data). This leads to motivation for cyclotron wave interpretation. But Marco believes a proper model of lower frequency waves with explain this. Also, Cranmer et al (1999) reports on broad line profiles in O VI. Again, this leads to an interpretation that we don't like. Rebuttal put forward by Raoaufi & Solanki (2004a,b;2006a,6;2007), concluding that there is no need for large anisotropies.
