نتایج جستجو برای: corona wind
تعداد نتایج: 96504 فیلتر نتایج به سال:
Applying corona wind as a novel technique can lead to a great level of heat and mass transfer augmentation by using very small amount of energy. Enhancement of forced flow evaporation rate by applying electric field (corona wind) has been experimentally evaluated in this study. Corona wind produced by a fine wire electrode which is charged with positive high DC voltage impinges to water surface...
The magnetic field of the Sun and the plasma properties of its atmosphere, such as temperature distribution, density stratification, photospheric convection and waves in the corona, determine the origin, energetics and evolution of the solar wind. The solar wind comes in three main kinds, as steady fast streams, variable slow flows and transient slow and fast coronal mass ejections. The three t...
Applying corona wind as a novel technique can lead to a great level of heat and mass transfer augmentation by using a very small amount of energy. The enhancement of forced flow evaporation rate by applying electric field (corona wind) has been experimentally evaluated in this study. Corona wind produced by a fine wire electrode charged with positive high DC voltage impinges on water surface an...
This tutorial focuses on basic physical concepts relevant to the heating of the corona and acceleration of the solar wind. We begin with a discussion of observations of the solar wind and solar corona and then develop a simple theoretical framework that allows us to explore some implications of the observations. Next we turn to observations of the lower solar atmosphere and their implications f...
[1] There are compelling observations of a clear anticorrelation between solar wind flow speed and coronal electron temperature, as determined from solar wind ionic charge states. A simple theory is presented which can account for these observations, including the functional form of the correlation: Solar wind flow speed squared varies essentially linearly as the inverse of the coronal electron...
[1] The solar wind has been measured directly from 0.3 AU outward, and the Sun’s atmosphere has been imaged from the photosphere out through the corona. These observations have significantly advanced our understanding of the influence of the Sun’s varying magnetic field on the structure and dynamics of the corona and the solar wind. However, how the corona is heated and accelerated to produce t...
We present in this Letter the first coordinated radio occultation measurements and ultraviolet observations of the inner corona below 5.5 Rs, obtained during the Galileo solar conjunction in January 1997, to establish the origin of the slow solar wind. Limits on the flow speed are derived from the Doppler dimming of the resonantly scattered component of the oxygen 1032 Å and 1037 Å lines as mea...
While the fast solar wind is nerally thought to originate from coronal holes, the ~, Oa% source of the slow solar wind is only known to be associated with the highly structured and — highly variable streamer belt. There is growing evidence from multiple-station intensity scintillation measurements of solar wind velocity — usually referred to as IPS for interplanetary scintillation— that the slo...
Plasma in the Sun's hot corona expands into the heliosphere as a supersonic and highly magnetized solar wind. This paper provides an overview of our current understanding of how the corona is heated and how the solar wind is accelerated. Recent models of magnetohydrodynamic turbulence have progressed to the point of successfully predicting many observed properties of this complex, multi-scale s...
We investigate possibilities of solar coronal heating by acoustic waves generated not at the photosphere but in the corona, aiming at heating in the midto low-latitude corona where the low-speed wind is expected to come from. Acoustic waves of period τ ∼ 100s are triggered by chromospheric reconnection, one model of small scale magnetic reconnection events recently proposed by Sturrock. These w...
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