  Context. To investigate the source of a type III radio burst storm during
encounter 2 of NASA's Parker Solar Probe (PSP) mission.
  Aims. It was observed that in encounter 2 of NASA's Parker Solar Probe
mission there was a large amount of radio activity, and in particular a noise
storm of frequent, small type III bursts from 31st March to 6th April 2019. Our
aim is to investigate the source of these small and frequent bursts.
  Methods. In order to do this, we analysed data from the Hinode EUV Imaging
Spectrometer (EIS), PSP FIELDS, and the Solar Dynamics Observatory (SDO)
Atmospheric Imaging Assembly (AIA). We studied the behaviour of active region
12737, whose emergence and evolution coincides with the timing of the radio
noise storm and determined the possible origins of the electron beams within
the active region. To do this, we probe the dynamics, Doppler velocity,
non-thermal velocity, FIP bias, densities, and carry out magnetic modelling.
  Results. We demonstrate that although the active region on the disk produces
no significant flares, its evolution indicates it is a source of the electron
beams causing the radio storm. They most likely originate from the area at the
edge of the active region that shows strong blue-shifted plasma. We demonstrate
that as the active region grows and expands, the area of the blue-shifted
region at the edge increases, which is also consistent with the increasing area
where large-scale or expanding magnetic field lines from our modelling are
anchored. This expansion is most significant between 1 and 4 April 2019,
coinciding with the onset of the type III storm and the decrease of the
individual burst's peak frequency, indicating the height at which the peak
radiation is emitted increases as the active region evolves.
