空间科学学报

1984 Vol. 4, No. 4

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Analysis of Stabilities of the Spiral Sector Transition Region in the Interplanetary Magnetic Fields

Wang Shui, Zhu Lie

1984, 4(4): 261-268. doi: 10.11728/cjss1984.04.261

Abstract(1833) PDF 497KB(1064)

Abstract:
By using a four-layer model, the stabilities of ME type spiral sector transition region in the interplanetary magnetic field are discussed. The results show that (1) three kinds of large-scale waves may be excited in MB type transition region, and for all of them, there exists a low-frequency cut-off; (2) the growth rates of these three kinds of instabilities all increases as k increases, but among them only the growth rate of model A has a maximum and a minimum; (3) whenk is parallel or antiparallel to the velocity V_q of solar wind in the sector regions, the excitation of waves is easier; when the angle between k and V_q become larger, the cut-off wave length moves to the shot end; when k is perpendicular to V_q, the waves can not be excited; (4) when the angle between k and V_q is 75°, the wave with a wave length of 5×10⁴ km and phase velocity 340 km/s may be excited, this is in agreement with teh observations at the earth's magnetopause obtained from Voyager 1. Hence, we deduce that the waves in the spiral sector transition region may be a perturbation source causing the K-H instability in the magnetopause.

Propagation of Jovian Electrons in the Interplanetary Space

Huang Yong-nian

1984, 4(4): 269-276. doi: 10.11728/cjss1984.04.269

Abstract(2080) PDF 445KB(1142)

Abstract:
The propagation of Jovian electrons depends on the spiral magnetic field in the interplanetary space. In this paper, the convection-diffusion equation for the Jovian electron transport is derived by using a new "spiral coordinate system", which is based on the interplanetary spiral magnetic field configuration, and a new model of Jovian electrons transport in the interplanetary space and the modulation of Jovian electrons in the orbit of the earth, which involves that of the Jupiter's synodic orbital period and the period of 27-day variations, is presented. The calculated results are coincident with the observations.

The Heating of the Solar Wind by Alfvenic Fluctuations

Tu Chuan-yi Chen Hua

1984, 4(4): 277-284. doi: 10.11728/cjss1984.04.277

Abstract(2310) PDF 535KB(685)

Abstract:
The theory of the heating of the solar wind by the Alfvenic fluctuation and two models for the attenuation of the Alfvenic fluctuation (Viscous model and Wave energy cascading model) have been tested against the observed data by Helios 1 and 2. The calculation showed that, in the space range where Helios observed, (1) from the energy equation under the assumption that the Alfvenic fluctuations changes into the heat energy of the solar wind protons, the calculated radial variation of the temperature of the solar wind protons agrees with the observed results; (2) the rate of the energy dissipation of the fluctuations predicted by the viscous model is different from the observed results. The difference is about 8 orders, so it can not discribe the process of the energy dissipation; (3) the rate of energy dissipation of the fluctuations predicted by the wave energy cascading model agrees with the observed results. The possible mechanism of the heating of the solar wind protons is the dissipation of the energy cascading to the frequency range of the proton gyro-frequency.

The Response of the Ionospheric TEC to Magnetic Storms over the Bay of Biscay

Huang Tian-xi

1984, 4(4): 285-291. doi: 10.11728/cjss1984.04.285

Abstract(2055) PDF 464KB(648)

Abstract:
This paper deals with the response of total electron content of the ionosphere over the Bay of Biscay, the Northeast Atlantic Ocean, to geomagnetic storms observed at Aberystwyth, U. K, from geostationary beacon satellites Intelsat IIF2 and SIRIO during the last ten years. The magneto-ionospheric storms selected belong to maxima of the 20th and 21st solar periods and are around the equinoxes and solstices. It is outlined that in spring months, the longish TEC depletion period appears after positive phase effect of continuous magnetic storm, and on the other hand, the short TEC depletion follows the concentrative magnetic storm. The TEC morphology associating with storms during equinoxes and solstices is influenced by some storm indices such as sudden commencement time and SSC occurrence frequency, season, storm main phase, Dst, Kp, Ap, etc.

Variations of the Electron Density and the Effective Electron Loss Rate in the Ionospheric D-region

Huang Ze-rong, Wang Xian-lin, Shen Li, Han Yi-min

1984, 4(4): 292-298. doi: 10.11728/cjss1984.04.292

Abstract(2264) PDF 437KB(1091)

Abstract:
In the paper it is pointed out that the time variations of the electron density N(h₀, t) and the effective electron loss rate φ(h₀, t) at a certain altitude in D-region may be monitored continuously on the basis of a single frequency LP data obtained at a single station. Some LF data observed at Wuchang Ionospheric Observatory (30°32' 40".64N,114°21'21"32E) are analysed thereby. It is shown that the hourly variations of N(h₀, t) and φ(h₀, t) are asymmetry about noon and the general behaviour of N (h₀, t) are in agreement with the previous published results obtained by other methods. Both the day to day variations of N(h₀, t) and φ(h₀, t) are not obvious.

A Study of the Scintillation for the Geostationary Satellite Signal

Jiang He-rong, Song Li, Xu Chu-fu

1984, 4(4): 299-306. doi: 10.11728/cjss1984.04.299

Abstract(2315) PDF 513KB(931)

Abstract:
In this paper the features of the amplitude and phase scintillations of 136 MHz signal transmited from the Japeness geostationary satellite ETS-2 and received at a mid-latitude station, Xian, were studied. They show that the high frequency features of the amplitude and phase spectra can exactly be explained by the weak scintillation theory, but at low frequency end the spectra go through a flat frequency region at first and then start to drop. These contradict the results obtained from the weak scintillation theory. These contradictions are explained in the paper. It seems that the conclusions obtained here are more reasonable.

Nitric Oxide Determination from Ionospheric Effects of Solar Flare in the Low-latitude Upper D-region

Ma Yan-hua

1984, 4(4): 307-313. doi: 10.11728/cjss1984.04.307

Abstract(2051) PDF 460KB(653)

Abstract:
Based on the oxonium ion chemistry, the NO density profiles in the low-latitude (28°38'N) upper D-region during a large solar flare are estimated. This method is valid for 80-87.5km where O⁺₂ has short lifetime and the negative ion density in comparison with positive ions can be neglected. It is found that the computed NO density profiles are in good agreement with Meira 's profile, but the minimum in 85 km is very weak.

The Effects of Topography of the Mars upon the Atmospheric Motion of the Mars and the Possible Mechanism That Produced the Dust Storm on the Mars

Li Mai-cun, Xie Ying-qi

1984, 4(4): 314-323. doi: 10.11728/cjss1984.04.314

Abstract(2196) PDF 597KB(981)

Abstract:
In this paper, the influence of the surface topography to the atmosphere of the Mars is examined on the assumption of a quasi-geostrophic model, and a rough explanation is given for the possible physical mechanism that produces the dust storm on the Mars.

Space Brain Science Research

Mei Lei

1984, 4(4): 324-330. doi: 10.11728/cjss1984.04.324

Abstract(2916) PDF 553KB(2052)

Abstract:
In this paper, the author put his emphasis to the importance of brain science research in space flight based, on the flight experinces and laboratory investigationsdur-ing the past twenty years. The theories and techniques developed in author's laboratory for astronaut brain function research are briefly summerized. The viewpoints on brain evolution in the gravitational field, the principle of frontalization of brain function and the problem of extraterrestrial intelligence are also stressed. Finally, a space brain science research program is suggested.

两颗彗星的CN和C₂彗发模型

1984, 4(4): 331-336. doi: 10.11728/cjss1984.04.331

Abstract(2040) PDF 399KB(930)

Abstract:

Models of CN and C₂ Comae for Comets Tago-Sato-Kosaka (19691X) and Bennett (197011)

Hu Zhong-wei, Chen Shu-dong, Zhao Jiang-nan

1984, 4(4): 337-337. doi: 10.11728/cjss1984.04.337

Abstract(2100) PDF 67KB(566)

Abstract:
In this paper, CN and C₂ isophotes of both comets Tago-Sato-Kosaka (1969Ⅸ) and Bennett (1970Ⅱ) obtained by J. Rahe are used to obtain their average radial intensity distributions. Using Haser's formula, scale lengths of daughter and its parent molecules have been obtained by comparision of observation with theory.

Shock Compression of Jilin Meteorite and Pyrolite Model

Lin Wen-zhu

1984, 4(4): 338-346. doi: 10.11728/cjss1984.04.338

Abstract(2235) PDF 575KB(1123)

Abstract:
Shock-wave instrumentation provides an approach for the study of phase transformation during shock compression of the Jilin meteorite. Experimental Hugoniot points for the Jilin meteorite are analyzed by a least-squares method to fit the Birech-Murnaghan or Murnaghan equation-of-state. In this paper, a method is proposed for estimating the zero-pressure parameter. Experimental result show that high-pressure phase mineral assemblages are present. The zero-pressure density is 4.395 g/cm³. It is concluded that there is a perovskite-strueture mineral with a zero-pressure density of 6.30 g/cm³. The calculation shows that the zero-pressure density of silicate in the Jilin meteorite is 4.10 g/cm³. It appears that dense silicate in the meteorite have a sufficiently high density compatible with that of lower mantle mineral assemblages at zero-pressure. The proto-lower mantle seems to be similar in composition to ordinary chon-drites, while the proto-earth's core is similar in composition to iron meteorites. So the disproportionation of iron and ferromagnesian silicates in chondrites may explain the origin of iron in the process of earth's evolution.

AN Electron Telescope for Radiation Belt Electron Measurements

Hu You-qiu, Wang Zuo-gui, Yu Guang-hua

1984, 4(4): 347-350. doi: 10.11728/cjss1984.04.347

Abstract(2193) PDF 354KB(1120)

Abstract:
A semiconductor electron telescope for measuring the electron energy distribution in the radiation-belt is described. It has three energy ranges: E_e1≥ 0.25 MeV, B_e2≥0.5 MeV and E_e3≥0.8MeV. The telescope consists of three Si(Au) surface barrier detectors. Details of the design and performance are reported. This telescope has been used in some space detections. The results show that its quality is satisfactory.