  Solar and interplanetary radio bursts can reflect the existence and motion of
energetic electrons and are therefore a kind of vital phenomenon in solar
activities. The present study reported a solar radio burst (SRB) event observed
by Parker Solar Probe (PSP) in its 8th orbital encounter phase, and it lasted
about 20 hours in a frequency range of 0.5-15 MHz, called the type IV-like SRB.
This type IV-like SRB consists of a series of numerous spikes with the
center-frequency drifting slowly from ~5 MHz to ~1 MHz, and each individual
spike appears a much faster frequency drifting and has a narrow frequency range
of a few MHz and short duration of a few minutes. Based on the empirical models
of the solar atmosphere adopted commonly, combining the in-situ measurement by
PSP, we propose that these small-scale spikes were generated by a group of
solitary kinetic Alfv\'en waves (SKAWs) in a magnetic loop accompanying coronal
mass ejection (CME) and moving outwards, in which the frequency drifting of
individual spike is caused by the SKAW's propagation and the center-frequency
drifting may be attributed to the motion of the magnetic loop.
