SH052-06
Whistler wave properties and their occurrence during the Parker Solar Probe's 1st and 2nd encounter

Wednesday, 16 December 2020: 10:42
Virtual
vamsee Krishna Jagarlamudi1,2, Thierry Dudok de Wit3, Clara Froment4, Vladimir Krasnoselskikh5, Andrea Larosa5, David Malaspina6, Oleksiy V Agapitov7, Laura Bercic8, Karine Issautier9, Matthieu Kretzschmar10, Mingzhe Liu9, Michel Moncuquet9, Stuart D Bale11, Anthony W Case12, Justin Christophe Kasper13, Davin Larson14, Kelly E Korreck12, Michael Louis Stevens12 and Phyllis L Whittlesey14, (1)IAPS-INAF, Rome, Italy, (2)LPC2E, Orleans, France, (3)LPC2E, CNRS and University of Orléans, Orléans, France, (4)University of Oslo, Institute of Theoretical Astrophysics, Oslo, Norway, (5)Laboratoire de Physique et Chimie de l'Environnement et de l'Espace, Orléans Cedex 2, France, (6)University of Colorado, Astrophysical and Planetary Sciences Department, Boulder, CO, United States, (7)Space Science Laboratory, UCB, Berkeley, CA, United States, (8)LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université Paris Diderot, Sorbonne Paris Cité, Meudon, France, (9)LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université de Paris, Meudon, France, (10)CNRS and University of Orléans, LPC2E, Orléans, France, (11)University of California Berkeley, Space Sciences Laboratory, Berkeley, CA, United States, (12)Smithsonian Astrophysical Observatory, Cambridge, MA, United States, (13)University of Michigan, Climate and Space Sciences and Engineering, Ann Arbor, MI, United States, (14)Space Sciences Laboratory, University of California Berkeley, Berkeley, CA, United States
Recorded Presentation
Abstract:
We present the analysis of narrow-band whistler wave signatures observed between the lower-hybrid and half of the electron cyclotron frequency during the 1st and 2nd encounters of Parker Solar Probe (PSP). These whistlers are identified using the band-pass filter data from the Digital Fields Board on the PSP. We find that nearly 85% of the whistlers are observed for less than three seconds consecutively, the probability of occurrence of long-consecutive (> 60 s) whistler intervals are rare. Using both the peak and mean band-pass filter data we show that whistler waves occur intermittently and the majority of the whistlers are of low amplitudes and occur for a short period (< 0.1 s). We investigate the dependence of the occurrence of whistlers and their amplitudes with respect to different proton and electron plasma parameters and with respect to magnetic field deflections. Several of the observed whistler features are in line with the previous Helios observations. We infer that the slower the velocity of the wind is, the higher the occurrence of whistlers is.
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