# Solar wind turbulence at kinetic scales inside 1 AU: HELIOS revisited

Vamsee Krishna Jagarlamudi, Olga Alexandrova, Thierry Dudok de Wit, Milan Maksimovic

► To cite this version:

Vamsee Krishna Jagarlamudi, Olga Alexandrova, Thierry Dudok de Wit, Milan Maksimovic. Solar wind turbulence at kinetic scales inside 1 AU: HELIOS revisited. 20th EGU General Assembly, 2018, Vienne, Austria. pp.9438. insu-03566332

HAL Id: insu-03566332

https://insu.hal.science/insu-03566332

Submitted on 11 Feb 2022

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# Solar wind turbulence at kinetic scales inside 1 AU: HELIOS revisited

Vamsee krishna Jagarlamudi (1), Olga Alexandrova (2), Thierry Dudok de Wit (3), and Milan Maksimovic (4)

(1) LPC2E, LESIA - Observatoire de Paris, France (vjagarla@cnrs-orleans.fr), (2) LESIA - Observatoire de Paris (olga.alexandrova@obspm.fr), (3) University of Orléans, LPC2E (ddwit@cnrs-orleans.fr), (4) LESIA - Observatoire de Paris (milan.maksimovic@obspm.fr)

We use Search Coil Magnetometer data on Helios 1 in 1975 to study the radial evolution of solar wind magnetic field turbulence in the kinetic range, at scales smaller than the ion characteristic scales. Helios being a closest mission to Sun till date offers a unique opportunity to study turbulence in different regions of the inner Heliosphere. The magnetic spectra from 7Hz and up to ~680 Hz has been studied. We see the signatures of quasi-parallel whistlers waves in the magnetic spectra at a fraction of the local electron cyclotron frequency. We relate the presence of whistlers and their evolution with radial distance to different physical parameters such as solar wind type, plasma beta and features of the electron distribution functions.