Structure of magnetic field in the solar wind
This work is concerned with empirical data on magnetic field in the solar wind in frame of a concept of dissipative solar wind, developed in earlier work. Interplanetary magnetic fields should be classified with respect to their origin. It is very important for all the theoretical problems from the necessity to specify correctly boundary and initial conditions: the magnetic field must be sewed with its source. One should select the field, connected directly with the Sun (stretched out from it), and the field of moving electric currents. It occured central in discussion about the velocity of Alfven waves, probably warming up the solar wind, relative to the Sun, the magnetic field and solar wind plasma. The selection problem corresponds to an inverse problem and obviously has no single solution. The dissipative model of the solar wind introduce the slipping and leakage of plasma relative to magnetic field. There are no `interplanetary current sheets` in it. But temporal fluctuations from the filamentation of electric currents play the key role. As a whole, the new concept requires the re-interpretation of main objects in the interplanetary magnetic field.
- Research Organization:
- California Institute of Technology (CalTech), Pasadena, CA (United States). Jet Propulsion Lab. (JPL)
- OSTI ID:
- 266946
- Report Number(s):
- N-96-24651; NASA-CR-199940; JPL-PUBL-95-13; NAS-1.26:199940; NIPS-95-06571; CONF-9506256-; TRN: 9624851
- Resource Relation:
- Conference: 8. international solar wind conference, Dana Point, CA (United States), 26-30 Jun 1995; Other Information: PBD: Jun 1995; Related Information: Is Part Of International Solar Wind 8 Conference; Hollweg, J.V.; PB: 119 p.
- Country of Publication:
- United States
- Language:
- English
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