  AIM: Large amplitude narrowband obliquely propagating whistler-mode waves at
frequencies of ~0.2 fce (electron cyclotron frequency) are commonly observed at
1 AU, and are most consistent with the whistler heat flux fan instability. We
want to determine whether similar whistler-mode waves occur inside 0.2 AU, and
how their properties compare to those at 1 AU.
  METHODS: We utilize the waveform capture data from the Parker Solar Probe
Fields instrument to develop a data base of narrowband whistler waves. The
SWEAP instrument, in conjunction with the quasi-thermal noise measurement form
Fields, provides the electron heat flux, beta, and other electron parameters.
  RESULTS: Parker Solar Probe observations inside ~0.3 AU show that the waves
are more intermittent than at 1 AU, and are often interspersed with
electrostatic whistler/Bernstein waves at higher frequencies. This is likely
due to the more variable solar wind observed closer to the Sun. The whistlers
usually occur within regions when the magnetic field is more variable and often
with small increases in the solar wind speed. The near-sun whistler-mode waves
are also narrowband and large amplitude, and associated with beta greater than
1. Wave angles are sometimes highly oblique (near the resonance cone), but
angles have been determined for only a small fraction of the events. The
association with heat flux and beta is generally consistent with the whistler
fan instability although there are intervals where the heat flux is
significantly lower than the instability limit. Strong scattering of strahl
energy electrons is seen in association with the waves, providing evidence that
the waves regulate the electron heat flux..
