A Study on the Method for the Control of Height of Sight Line and the Surrounding Environment of the Stadium——With Chongqing Yuanjiagang Stadium as an Example

The geometrical model of the position of driver's eyes in simulated driving was built based on geometrical characteristics of roads,and the concept for trailing sight line was introduced.

The height of sight line and the surround-ing landscapes around Chongqing Yuanjiagang Sta-dium is controlled by following the principle of"controlby region","control by stage"and"most unfavorablecontrol",applying the method of control by region inplane sector and section plane analysis and coor-dinating various contradictions by application of thestrategy of"gross balance".

It is necessary to design a two axis gyro stabilized control platform to ensure the space stability and the automatical target tracking capability of the sight line despite of its carriage movement.

The whole system, including the HII region and the gas-dust ring, moves at a sight line velocity of -61.0 km/s in a large cloud that has a sight line velocity of - 57 km/s.

Using the Unno-Beekers equation and the Eunge-Kutta method with changed step long, FeI λ5324. 19 A line forming in magnetic fields of the solar photosphere, peumbra and umbra has been computed. When using the special birefringence filter with half width 0.15 A which is the monochromator of the Solar Magnetic Field Telescope, the coefficients of the theoretical calibration for the salar magnetic field and Solar sight line velocity field have been computed also.

The correcting plane π_k, correcting sight line and the formula of the error have been built. If these formulas can be applied to the calculation of meeting parameters, the new calculating results will be more correct.

Taking the Shenwo project as an example, this paper introduces the automatic monitoring system of transducers and its performanee, and, through the comparison with the sight line measurement, demonstrates the advantages and necessity of using the transducer for concrete dam observation.

It is discussed that a measurement method of both solar magnetic field and solar sight line velocity. The method is used in the Solar Magnetic Field Telescope (Similar video magnetograph) which is being produced. A narrow band birefringent filter is used as a monochromater which has two wave bands, one is FeI λ 5324 A with half width 0.15 A, the another is Hβ λ 4861 A with half width 0.12 A.A television-computer, a photomultiplier and two photograph are used as receivers. KD* P crystals are used as electro-optic...

It is discussed that a measurement method of both solar magnetic field and solar sight line velocity. The method is used in the Solar Magnetic Field Telescope (Similar video magnetograph) which is being produced. A narrow band birefringent filter is used as a monochromater which has two wave bands, one is FeI λ 5324 A with half width 0.15 A, the another is Hβ λ 4861 A with half width 0.12 A.A television-computer, a photomultiplier and two photograph are used as receivers. KD* P crystals are used as electro-optic light modulators. The broad sight field KD* P modulator has been researched and produced. It consist of two KD* P crystals and a wave plate with effect of 90° rotation. In 36' half sight field, the biggest error of λ/4 wave retardation is only + λ/300 instead of A/25 which exists in narrow sight field design. To observe the solar magnetic field and the solar sight line velocity, three groups of the KD* P modulators are used. High voltage power supplies of square wave with 135 e/s and sawtooth wave with 270 c/s are operated on the KD* P. The influnece of wave forms errors of the high voltage power supplies has been calculated and discussed. Eaising time and returning time are promised up T/30, T is period. But returning time of the sawtooth wave should be smaller than T/100. Voltages of half wave of above wave forms have been measured. Combination experiment of the KD* P modulator and high voltage power supply has shown that their behaviours are well.

The problem of optimal intercept guidance laws for missiles have been studied by a lot of authors at home and abroad. But the mathematical models for missiles were assumed too simple, i. e. either as an ideal particle or as a first order delay link.As a primary contribution this paper has made researches on the optimal intercept guidance laws based on a mathematical model with second order charac- teristics. By taking minimum control energy consumption as the performance index, the optimal intercept guidance...

The problem of optimal intercept guidance laws for missiles have been studied by a lot of authors at home and abroad. But the mathematical models for missiles were assumed too simple, i. e. either as an ideal particle or as a first order delay link.As a primary contribution this paper has made researches on the optimal intercept guidance laws based on a mathematical model with second order charac- teristics. By taking minimum control energy consumption as the performance index, the optimal intercept guidance laws have been derived from the minimum principle in the following two cases of terminal state:1. The terminal miss-distance is zero;2. The intercepting curved surface of out-of-control.The conjugate state equations and the state equations have been solved by use of Laplace Transformation. Through considerably complex computation, the optimal intercept guidance laws have been deduced in the following analytical formsThrough appropriate selection of the terminal time lf or the time of lead T, the results obtained above may be transformed into the optimal guidance laws which are composed of the proportional navigation with varied coefficients and the correctional terms associated with acceleration and angular acceleration of sight-line rotation. These results are similar to those of missiles with first order delay link in form and have no need of any additional parameter. However, the computation is more complex and the results are more accurate.Finally, the optimal intercept guidance laws are studied in the case of the proper frequency of a missile ω approaching to infinity, i. e. in the case of an ideal particle. The results are the same as those obtained by the other authors.

Spectrum of peak flux of solar type IVdm radio burst is generally characteristic of large spectral index, narrow-band, high flux. In addition decirnetric solar radio burst observed in single frequency records swings with time, period of swings is order of seconds [1, 5].According to [6], it had excluded the possibility that the narrow-band type IVdmsolar radio burst is explained by gyrosynchrotron process. It seems that only plasma emissions would be chosen.We have shown in [7] that spectral character of solar...

Spectrum of peak flux of solar type IVdm radio burst is generally characteristic of large spectral index, narrow-band, high flux. In addition decirnetric solar radio burst observed in single frequency records swings with time, period of swings is order of seconds [1, 5].According to [6], it had excluded the possibility that the narrow-band type IVdmsolar radio burst is explained by gyrosynchrotron process. It seems that only plasma emissions would be chosen.We have shown in [7] that spectral character of solar type IVdm radio burst is explained by mechanism of Langmuir's nonlinear scattering by thermal ion. In this paper, we try to explain character by wave-wave interacting nonlinear process. Our ideas are as follows. The nonthermal electrons accelerated in explosive phase are trapped in coronal mirror, it forms the source of type IVdm radio burst. These nonthermal electrons excite simultaneously low-frequency Whistler wave and high-frequency Lang-muir wave. These two waves' nonlinear coalesce process leads to produce transverse-wave of type IVdm solar radio burst. Available data are taken from [8-10].In this paper, we adopt anisotropic loss-cone gap distribution as distribution function of electrons [11-14]. Energetic part of gap distribution is taken as Gauss's wave packet with central energy of wave packet E=100keV. By means of this, we obtain emissity propagating parallel to magnetic direction and linear growth rate of Whistler indicated in (1) and (2), and that of Langmuir wave in (5)- (6). With these quantity, we may calculate wave number spectral density Wlkl (or Wkww) from solution (9) of wave's radiation transfer equation with t= Ll/vgl (orLw/vgw. The thickness of Langmuir's plasma level Ll is supposed to be Ll-Lw=500km, for example, Pig. 1 describes Wkww diagram of Wpe=2n×500 MHz plasma level. Fig. 2 indicates the diagram of Langmuir's growth rate n at plasma frequency of 2n×200MHz.Coalesce process of Langmuir wave and Whistler wave must satisfy resonance condition Eq. (10). According to [4], under coronal condition, it is not satisfied until that the angle between Langmuir wave Kl and Whistler wave Kw is less than10. Thus. we assume that Kl and KW are parallel to magnetic direction to compute Kw, Kl , Kr by means of linear dispersion relation. Such calculated Langmuir's phase velocity is larger than light velocity. But the phase velocity of Langmuir wave excited by fast electrons is less than light velocity. So Langmuir wave which, is calculated from (5) and (6) can not interact with Whistler wave. However Langmuir wave converts easily into new Langmuir wave due to nonlinear scattering by ion. In this process energy almost conserves, wave number decreases, phase velocity increases. New formed Langmuir wave may interact with Whistler wave. Besides, in scattering process Langmuir wave vector turns toward magnetic field [15]. Hence we can calculate wave number moreover still calculate Langmuir's Wkll by (5) and (6) to replace approximately new Langmuir wave after scattering.Coupling equation of l+ w - t process is Eq. (11). Angular radius of the souree takes 2'.In the corona, because of Qe<sight line direction of source is 3×109 cm, electron density with radial direction is taken approximately 6×Newkirk's value [17]. For convenience, we take the source as a column perpendicular to Photosphere surface.According to former formula, we have calculated spectrum of type IVdm radio burst on Aug. 2, 0330, 1972 (Fig. 3). It is seen from Fig. 3 that spectrum of numerical calculation coincides roughly with that of observation. By comparision with each other, we obtain a nont