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AIM: Large amplitude narrowband obliquely propagating whistler-mode waves atfrequencies of ~0.2 fce (electron cyclotron frequency) are commonly observed at1 AU, and are most consistent with the whistler heat flux fan instability. Wewant to determine whether similar whistler-mode waves occur inside 0.2 AU, andhow their properties compare to those at 1 AU.  METHODS: We utilize the waveform capture data from the Parker Solar ProbeFields instrument to develop a data base of narrowband whistler waves. TheSWEAP instrument, in conjunction with the quasi-thermal noise measurement formFields, provides the electron heat flux, beta, and other electron parameters.  RESULTS: Parker Solar Probe observations inside ~0.3 AU show that the wavesare more intermittent than at 1 AU, and are often interspersed withelectrostatic whistler/Bernstein waves at higher frequencies. This is likelydue to the more variable solar wind observed closer to the Sun. The whistlersusually occur within regions when the magnetic field is more variable and oftenwith small increases in the solar wind speed. The near-sun whistler-mode wavesare also narrowband and large amplitude, and associated with beta greater than1. Wave angles are sometimes highly oblique (near the resonance cone), butangles have been determined for only a small fraction of the events. Theassociation with heat flux and beta is generally consistent with the whistlerfan instability although there are intervals where the heat flux issignificantly lower than the instability limit. Strong scattering of strahlenergy electrons is seen in association with the waves, providing evidence thatthe waves regulate the electron heat flux..

Narrowband oblique whistler-mode waves: Comparing properties observed by Parker Solar Probe at <0.2 AU and STEREO at 1 AU