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Using the Parker Solar Probe data taken in the inner heliosphere, weinvestigate the power and spatial anisotropy of magnetic-field spectra atkinetic scales (i.e., around sub-ion scales) in solar wind turbulence in theinner heliosphere. We find that strong anisotropy of magnetic spectra occurs atkinetic scales with the strongest power in the perpendicular direction withrespect to the local magnetic field (forming an angle theta_B with the meanflow velocity). The spectral index of magnetic spectra varies from -3.2 to -5.8when the angle theta_B changes from 90 to 180 (or 0) deg, indicating thatstrong anisotropy of the spectral indices occurs at kinetic scales in the solarwind turbulence. Using a diagnosis based on the magnetic helicity, we show thatthe anisotropy of the spectral indices can be explained by the nature of theplasma modes that carry the cascade at kinetic scales. We discuss our findingsin light of existing theories and current development in the field.

Anisotropy of Magnetic Field Spectra at Kinetic Scales of Solar Wind Turbulence as Revealed by Parker Solar Probe in the Inner Heliosphere