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22 巻, 2 号
選択された号の論文の4件中1～4を表示しています
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今津 信吾, 佐藤 弘, 竹田 吉信, 中野 義映1969 年 22 巻 2 号 p. 56-66
発行日: 1969年
公開日: 2011/08/16
ジャーナル フリーPDF形式でダウンロード (729K) -
宮島 重喜1969 年 22 巻 2 号 p. 67-90
発行日: 1969年
公開日: 2011/08/16
ジャーナル フリーThe quiet-day solar wind fully discussed by E.N, Parker on the basis of the fluid model of plasma. He found that it is a supersonic flow of the plasma in the solar gravitational field. We have here again discussed the solar wind using a two-fluid model of plasma.
Two Bernoulli equations, which a : re coupled with the electric field each others, are complicated to analyse due to the many branches of the solutions. However, for the surface of the.sun, it is possible to apply the so-called quasi-linear approximation and to have relatively simple solution. In that approximation, two parameters play important rolles; one is γ related to the square of the initial velocity of ions and the other is β connected with the solar gravitational constant. When β=3-γ then the electric potential φ gradually decreases with increasing radious. When :β<3-γ or β>3-γ then φ changes steeply or takes an extreme value at a certain radious respectively. Furthermore, we have the conditions γ≥2β and γ>1; the former is necessary in order to keep the conservation of energy and the, latter is identical to the Bohm criterion leading to the stable ion sheath. Since small. change of γ or β results in a large change of φ, so a set of the special combination of (γ, β) is required in order to find the solar wind at the orbit of the earth.
The results calculated by the quasi-linear approximation have been compared with ones computed by a machine. Finally it is, in this note, yet unclear whether “The electron Critical point” is present or not and we shall make it clear in the near future.抄録全体を表示PDF形式でダウンロード (1647K) -
下村 昇, 三谷 健次1969 年 22 巻 2 号 p. 91-98
発行日: 1969年
公開日: 2011/08/16
ジャーナル フリーThe emission from a plasma in a nuiform magnetic field Is studied near electron cyclotron harmonic frequencies. Following the dressed test perticle approach, the energy lost by one test electron is calculated and, from this, the total emission is given as the sum over all electrons weighted hi their velocity distribution by the superposition principle of the dressed test particles. In general, dispersion relation for the electrostatic wave propagating to the direction nearly perpendicular to the magnetic field has two solutions, compriing-a slow electrostatic wave and a fast electrostatic wave. It is found in the Allis diagram that the emission peaks for these waves shift from the lower harmonic side to the higher side with a considerably-different way to each other. The emission power of the slow wave is much greater than that of the fast wave, because the number of the electrons which contribute to excitation of the slow wave is large and also √λ= (thermal velocity/phase velocity) is large.抄録全体を表示PDF形式でダウンロード (670K) -
Tihiro Ohkawa1969 年 22 巻 2 号 p. 99-111
発行日: 1969年
公開日: 2011/03/04
ジャーナル フリーMED equilibria are calculated analytically for toroidal configurations with a small aspect ratio. The existence of configurations with a deep magnetic well and a large shear is demonstrated.抄録全体を表示PDF形式でダウンロード (646K)
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