空间科学学报

1984 Vol. 4, No. 3

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An Optical and Radio Study of the Solar Limb Event of Jan. 22, 1982

Wang Jia-long, Kong Fan-xi

1984, 4(3): 177-183. doi: 10.11728/cjss1984.03.177

Abstract(1676) PDF 412KB(640)

Abstract:
The limb event with type III+V and type II bursts and H_α mass ejection of Jan. 22, 1982 is described in this paper. The characteristics of the associated radio burst in short decimeter and centimeter wave lengths is discussed using the curves of the flux density rate with time. The magnetic field strength in a main piece of the ejecta during the event (H ～12G), its mass (～10³⁸ electrons, ～10¹⁴ grams) and energy in it (～60 erg/cm³, 8×10²⁹ ergs) are estimated. An estimation of 10³⁰ ergs for the total energy of this limb event is made.

The Influence of Momentum Distribution of Source Particles on Fermi Accleration in Shock Waves

Mao Ding-yi, Wang De-yu

1984, 4(3): 184-190. doi: 10.11728/cjss1984.03.184

Abstract(1875) PDF 428KB(944)

Abstract:
The time dependent energy spectra of acclerated particles in Fermi accleration by shock waves have been calculated for various momentum distributions of source particles and parameters. It is shown that the high energy parts of acclerated particles spectra are power-law forms in the enough long time, no matter what the momentum distribution is possessed by source particles. But the time evolution of energy spectrum of acclerated particles depends on the momentum distribution of source particles. Therefore it is unsuitable for a transient shock process that the energy spectra of acclerated particles are represented by power-law form with constant index.

A Kind of Short Wave Band SID Records and Its Application in the Observation and Study of Solar X-ray Flares

Xiao Zuo, Zhang Shu-li, Zuo Ji-ching

1984, 4(3): 191-197. doi: 10.11728/cjss1984.03.191

Abstract(1913) PDF 457KB(837)

Abstract:
Solar flares with enhanced X-ray emissions usually produce excess ionizations in the ionosphere and cause what generally known as sudden ionospheric disturbances (SID). It has long been established that much of information on the X-ray emission can be based on the observation of SID's. In recent 20 years, although direct observations of the X-ray radiation by satellites have made quantitative data available, SIDmeasurements are still a useful tool, because the method iscomparatively simple, easy to give a quick and continuous patrol.In this paper a sweep frequency device was described for the continuous monitoring of SID's. Emphasis was put to the application of the records in solar X-ray 'flare studies. Analysis of the data from 1982-1983 showed that the method is sensitive to solar flare with X-ray enhancement. Its records of SID's are in very good agreement with those reported by some other stations in the world with different methods except a few small sized disturbances. This shows a reliability of the data. Furthermore, most of the solar soft X-ray (1-8 À) events with a peak flux larger than about 10^-3 erg·cm^-2·sec^-1, can be recognized from the records. The possibility of quantitative study of solar X-ray flux and its time curves with this kind of data were briefly discussed.

The Atmospheric Cyclone Disturbance Initiated By Solar Flares

Ye Zong-hai, Lu Chen, Zhang Gong-liang

1984, 4(3): 198-204. doi: 10.11728/cjss1984.03.198

Abstract(1747) PDF 445KB(914)

Abstract:
This paper provides a statistical study of the disturbance of atmospheric vorticity area index (VAI) initiated by solar flares over importance two for 1966-1978. It shows the effects induced by solar flares grouped by their potical importance, duration, season and the distance from the central meridiam. The results show that only the bright solar flares occurred in the winter season and with duration longer than 1.5 hours can significantly disturb vorticity area index. The maximum decrease on the third day after the solar flares is o'f the order of 16.4%. There is east-west asymmetry in distribution of flare's position in response to the VAIdisturbance. The bright and non-bright flares which occur on the west 0-30 from the central meridiam with duration longer than_1.5 hours, induce the largest disturbance for VAIon the third day and the seventh day after the flares respectively.

The Influences of Thunderstorm Charging on Atmospheric Potential

Zhuang Hong-chun

1984, 4(3): 205-215. doi: 10.11728/cjss1984.03.205

Abstract(1884) PDF 644KB(879)

Abstract:
In the atmosphere with an exponential electric conductivity, with given electric potential values in the ionosphere, considering the electric current source by thunderstorm charging, a steady state conservation equation of electric current is solved analytically, and an analytic expression of electric potential distribution is obtained. The expression shows that the effects of thunderstorm charging and ionospheric potential on the atmospheric potential are mainly exerted vertically. Calculation, based on observed current densities of thunderstorm charging and using the expression obtained in this article, shows that the charging by thunderstorm can enhance the potential at the altitude of electric layer to a value similar to that deduced from observations. Calculations also show that the ionospheric potential can influenee the lower atmospheric electricity in fair weather regions through its obvious effects on the potential of electric layer.

Solar Activity and Variation of Geomagnetic Disturbance

Sun Kai, Cheng Xin-hua, Ming Yue-hong, Jing Ju-ling, Wang Xu Li, Zhi-ping, Li Hong

1984, 4(3): 216-221. doi: 10.11728/cjss1984.03.216

Abstract(2104) PDF 375KB(860)

Abstract:
The events of which geomagnetic indices C9s are all larger than L (L is a constant) are noticed. The number of times of the events in a year is taken to express the level of geomagnetic disturbance of the year. Six cases are studied:L=3, 4 and 5; each of them is subdivided into two subcases: recurrent events and general events.The method of the curve fitting with piecewise polynomials is used to derive an averaged experimental relationship f(R) between the number of times in a year C_k and the sunspot relative number R_k (k is the order of the years from 1980 to 1979). Then, △_k = C_k - f_k (f_k = f(R_k)) are calculated. The result shows that: 1, for the 'solar cycles', each of which begins at he year four years before the minimum of the cor responding solar cycle, the signs of the average values of △_k alternate, ('sign alternating' fule +,-,+,-,......); 2. the 'sign alternating' rule oceurs in all the six subcases. It is mostly likely that the rule is caused by thereversal of the solar polar fields. After a further dividing of the 'cycles', every cycle has own dispersity (o) about its averaged △, △. The sequence of a shows a long term period of about 70 years.

The Spatial Distributions of the Amplitudes of Geomagnetic Daily Field and Day Variation in China During 1979-1980

Qi Yan-qin, Gao Yu-fen, Feng Zhong-xiao, Cheng Ying-fang

1984, 4(3): 222-231. doi: 10.11728/cjss1984.03.222

Abstract(2444) PDF 601KB(910)

Abstract:
Processing the data of quiet day variation with methods of filtering and harmonic analysis eliminates parts of disturbances of high frequencies. So the regular patterns of seasonal average and statistical distributions obtained can reflect the characters of spatial distribution of S_q variations much better. Data processing shows that the maximum and minimum points of spatial distribution of Zcomponent of S_q variation are inconsistent with those of Hcomponent, especially in he winter. It needs further research. Besides, the amplitudes and phases of diurnal and semidiurnal harmonics for the quiet day variations also have seasonal variations and the first phases of both of them in summer always are greater.

The Observational Features and Theoretical Explanations of the Coronal Transients

Hu Wen-rui

1984, 4(3): 232-239. doi: 10.11728/cjss1984.03.232

Abstract(2137) PDF 630KB(906)

Abstract:
The major observational features and theoretical models of the coronal transients are reviewed in the present paper. The coronal transient is the process with a large amount of mass ejection from the solar corona into the interplanetary space. There is 5×10¹⁵ grams of mass which is driven into the heliosphere with the typical velocity 500 km/sec in the period of 10³ seconds. There are close connections between the coronal transients and the events of solar flare and eruptive prominence. As a recent discovered phenomenon of the solar activity, many theoretical explanations have suggested for the coronal transient processes in the recent years. One approach is the numerical similarity, in which the coronal transient is driven by the pulsation of one of the thermodynamical quantities or the magnetic pressure at the low corona. Several analytical models consider that the loop transient is driven by the Lorentz force in the loop, or by the magnetic pressure outside the loop, or the MHD buoyancy force of the loop. By consideration of the connection between the transient and the solar flare and eruptive prominence, piston driving model suggest that the coronal transient is driven by the ejection of the dense plasma. More researches should be completed in both the observations snd the theories in future.

An New Experimental Formula of Satellite Distances and Its Explanation

Hu Zhong-wei, Chen Zhi-xiong

1984, 4(3): 240-244. doi: 10.11728/cjss1984.03.240

Abstract(2406) PDF 326KB(885)

Abstract:
In the solar system, there are three satellite systems-those of Jupiter, Saturn and Uranus. In each satellite system, there is a law of satellite distances. An new empiri-mental formuls of this law is obtained, i.e. (1) in this paper, α_n=B₁×Bⁿ, where an is the orbital semi-major axis of n-th satellite, B₁ and Bare constants for each system. Gonorally, the relative error of the value calculated from above formula with the observational value is not more than 10%. However, small satellites have larger errors.

A Preliminary Analysis on Whistler Observations at Sanya, Hainan, China

Wang You-shan, Zhu Lie, Wang Shui, Wang Jian-hua, Zhang Zuo-he

1984, 4(3): 245-252. doi: 10.11728/cjss1984.03.245

Abstract(2177) PDF 1303KB(702)

Abstract:
The main features of the whistlers, which were observed at Sanya (18.24°N, 109.5°E; Geomag. Lat. 7.04°N) early in 1983 are described. Agreat number of whistlers were recorded in the observations, including short whistlers, multisource whistlers, and mu-ltipath whistlers. Some of them (about 10%) have the low cutoff frequencies as low as nearly 0.8 kc/s. In addition to the conclusions given in papers [1,2], we further find: (1) the whistlers at Sanya almost always occured during f₀f₂ decreasing and the maximum values o'f whistler occurrence rate appeared just at the time when f₀f₂ decreased most fast, that is, when electron density changes most drastically. (2) the relation between whistler activities and magnetic storms at low latitudes have some differences with that at medium and high latitudes. Sometimes the correlations are reversed. To explain, all these, further observation and study are required.

The Anisotropy of the Diffuse Cosmic X-ray Background

Xu Chun-xian

1984, 4(3): 253-256. doi: 10.11728/cjss1984.03.253

Abstract(1994) PDF 262KB(878)

Abstract:
Using the new data of the 2-60 keVdiffuse X-ray background from HEAO-1 A2 and subtracting the model galactic X-ray component, the cosmic X-ray background data have been obtained.Considering the anisotropy caused by the Compoton-Getting effect, we derived d= (0.45±0.18)% and then V= (397 ±159) km/s. Where 6 is the anisotropy and Vis the velocity of the solar system with respect to the diffuse cosmic X-ray sea. There is no inconsistency with the well known anisotropy in the microwave background.

Study on Mossbauer Spectra of Lunan Memeorites in Yunan Province

Zhang Yu-chang, Li Zhao-lin, Hu Zhong-wei

1984, 4(3): 257-260. doi: 10.11728/cjss1984.03.257

Abstract(2319) PDF 313KB(960)

Abstract:
In this paper, the Mössbauer spectroscopic results of the Lunan meteorites failed down on the 4th, April 1980, at Lunan county, Yunnan province are analyzed and discussed. The experimental data showed that the Lunan meteorite belongs to olivine-bronzite chonelrite by Prior and Mason's classification.