Solar Wind and its Evolution

Abstract

By using our previous results of magnetohydrodynamical simulations for the solar wind from open flux tubes, I discuss how the solar wind in the past is different from the current solar wind. The simulations are performed in fixed one-dimensional super-radially open magnetic flux tubes by inputing various types of fluctuations from the photosphere, which automatically determines solar wind properties in a forward manner. The three important parameters which determine physical properties of the solar wind are surface fluctuation, magnetic field strengths, and the configuration of magnetic flux tubes. Adjusting these parameters to the sun at earlier times in a qualitative sense, I infer that the quasi-steady-state component of the solar wind in the past was denser and slightly slower if the effect of the magneto-centrifugal force is not significant. I also discuss effects of magneto-centrifugal force and roles of coronal mass ejections.

6 pages, 1 figure, Earth, Planets, & Space in press (based on 5th Alfven Conference) correction of discussion on a related paper

References in corpus (5)

• Magnetic fields of non-degenerate stars
• Global-Scale Turbulent Convection and Magnetic Dynamo Action in the Solar Envelope
• Large-scale magnetic topologies of early M dwarfs
• Forecasting Solar Wind Speeds
• Theoretical mass loss rates of cool main-sequence stars

Cited by in corpus (6)

• Coronal heating by MHD waves
• Detecting the oldest geodynamo and attendant shielding from the solar wind: Implications for habitability
• Saturation of Stellar Winds from Young Suns
• A Closer Earth and the Faint Young Sun Paradox: Modification of the Laws of Gravitation, or Sun/Earth Mass Losses?
• Evolution of solar-type stellar wind
• Insights into Solar Wind Flow Speeds from the Coronal Radio occultation Experiment: Findings from the Indian Mars Orbiter Mission