  The interpretation of solar radio bursts observed by Parker Solar Probe (PSP)
in the encounter phase plays a key role in understanding intrinsic properties
of the emission mechanism in the solar corona. Lower time-frequency resolution
of the PSP receiver can be overcome by simultaneous ground-based observations
using more advanced antennas and receivers. In this paper we present such
observations for which the active active region 12765, begetter of type III, J,
and U solar bursts, was within sight of ground-based instruments and behind the
solar limb of the PSP spacecraft. We used a subarray of the Giant Ukrainian
Radio Telescope (GURT) to get the spectral properties of radio bursts at the
frequency range of 8-80 MHz, as well as the PSP radio instruments with a
bandwidth of 10.5 kHz - 19.2 MHz, during solar observations on June 5, 2020. We
directly detected the radio events initiated by the active region behind the
solar limb of the PSP spacecraft, using special conditions in the solar corona,
due to the absence of active regions from the PSP side. Following the
generation mechanism of solar radio emission, we refined the density model for
the solar corona above the active region 12765 responsible for the radio
bursts. Based on the PSP spacecraft position near the Sun and delays of radio
waves between space- and ground-based records, we found the corresponding radio
responses on the PSP spectrogram. The absence of sunspots from the PSP side
contributes to the propagation of radio waves from a dense loop of the Sun to
quiet regions with low densities, through which PSP instruments can detect the
radiation.
