摘要

Dynamic spectra are widely used in radio astronomy for processing observation data to characterize time-frequency distribution of the received emission total power. The paper presents a data processing technique which extends capabilities of such a time-frequency analysis through involving information on the phase difference between signals from sub-antennas composed of elements of the radio telescope antenna system. Dynamic phase spectra, which represent time-frequency dependences of the cross-spectrum phase for two signals, are formed by means of interferometric processing algorithms to be then used jointly with the conventional dynamic power spectra. The technique has been implemented at the UTR-2 radio telescope and used for several years for visual detection of the sought radio emission, recognition of false signals received by the antenna side lobes, and for discrimination of radio bursts observed within the main beam. The use of two pairs of antennas with noncollinear baselines makes it possible to determine the emission direction of arrival for each point on the time-frequency plane. The efficiency of the technique as applied to different types of radio emission are illustrated by examples of processing observational data for the Sun, Saturn and flare stars.