Solar wind dispersion quantity measuring method and device, electronic equipment and medium

Abstract

A solar wind dispersion quantity measuring method based on pulsar signals is applied to the technical field of deep space exploration and comprises the following steps: S1, selecting a pulsar with known standard dispersion quantity for observation according to the position of the sun; S2, receiving a pulsar signal after superposition of solar wind dispersion; S3, searching the current dispersion quantity of the signal; and S4, calculating the dispersion quantity of the solar wind according to the standard dispersion quantity and the current dispersion quantity of the signal. The invention further provides a solar wind dispersion quantity measuring device, electronic equipment and a medium. By measuring the dispersion quantity of the pulsar signal and inverting the dispersion quantity of the pulsar signal according to the characteristics of the solar wind, the near-distance solar wind dispersion quantity measurement of the sun is realized.

Description

technical field [0001] The present disclosure relates to the technical field of deep space exploration, and in particular to a method, device, electronic equipment and medium for measuring solar wind dispersion based on pulsar signals. Background technique [0002] With the successful implementation of the lunar exploration project, my country's deep space exploration has begun. Affected by solar activities such as the solar wind and the corona, the wireless communication environment in deep space is very complicated. A large number of irregularly charged particles in the solar wind will cause radio signals to flicker. Especially during the SCO period, the earth, the sun, and the deep space probe are roughly on the same straight line. When the sun-earth-probe angle (SEP) is small or when the sun is in an active cycle, the deep space Null detectors may experience intermittent or even complete loss of communication. The influence of the solar wind on radio signals also refle...

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Problems solved by technology

[0003] The traditional method of observing the solar wind using ordinary radio sources, because the signal has no phase information, can only measure intensity scintillation, and cannot directly measure group delay and dispersion. When the angle between the sun-earth-radio source is relatively large The phenomenon of saturation will also appear in the hour, so this method is not suitable for the observation of the perihelion

Although the downlink signals of deep space probes can be used to observe time delay, phase scintillation (Doppler scintillation) and spectrum expansion, etc., but because there are very few deep space probes, and the downlink signal frequency is single (currently mainly concentrated in the X frequency band) , The bandwidth is narrow, and the observation of the solar wind is very limited

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