Abstract
At present two complementary approaches to calculations of flare-generated interplanetary disturbances are beeing developed. One of them is based on Parker's model with one end of every field line rooted at the Sun and the other end somewhere in outer space (Wu et al., 1983). Another approach is based on Morrison's closed-cloud hypothesis. In this paper the dynamics of flare-generated hydromagnetic oblate clouds in the solar corona and interplanetrary space is developed. Magnetic buoyancy, gravity, and momentum loss due to interactions with the interplanetary medium are taken into account. If the magnetic fields, number density, and velocity of the external plasma are known, the equations allow a simple solutions for variations of the velocity and characteristic lengths of the clouds during their motion between the Sun and the Earth. Two theoretical velocity profiles are calculated and compared with an experimental one.
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
