June 19, 2024

Langmuir-Slow Extraordinary Mode Magnetic Signature Observations with Parker Solar Probe by A. Larosa et al

Krasnoselskikh, V., Voshchepynets, A., and Maksimovic, M.: 2019, ApJ, 51. https://ui.adsabs.harvard.edu/abs/2019ApJ…879…51K/abstract.

General view of the plasma conditions on May 27, 2020. From leading to bottom: the magnetic field from MAG; spectrogram of the V1-V2 dipole voltage from RFS (with color-bar at the top); peak frequency of the L-SE bursts observed by TDS; energetic electron counts from EPI-Lo.
Conclusions.
The first ever unambiguous magnetic signatures of the beam created Langumir-Slow Extraordinary modes have been observed by Parker Solar Probe. The density changes play undoubtedly an important function in this phenomenon however an essential element that is missing out on here are the details of the beam plasma interaction and how the energy of the beam can effect the observations.
Based upon a recent paper: Larosa, A., et al., Langmuir-Slow Extraordinary Mode Magnetic Signature Observations with Parker Solar Probe, 2022, ApJ, 95. DOI:10.3847/ 1538-4357/ ac4e85.
Referrals:.

Observation of a magnetic signature in a L-SE wave. On the left, from leading to bottom: waveform of the potential distinction of the PSP antennas 1 and 2; waveform of the search-coil magnetometer high frequency coil. The vertical rushed line shows the location of the plasma frequency as examined from the thermal sound data.
The rare magnetic signatures were observed in a truly inhomogeneous plasma environment and were preceded by a type III radio burst. The events were likewise connected with strong electrical fields. An electron beam was present as anticipated (see Figure 2.).
The link in between the magnetic signature, the electric field and the refractive index of the waves can be gotten from the linearized Vlasov-Maxwell system as revealed in referral 1. A drop in the refractive index increases the magnitude of the magnetic part of the waves and boosts the opportunity of observing it above the sound level.
The reflections of the Langmuir waves due to density fluctuations can result in the transformation of electrostatic to electro-magnetic energy and discuss the formation of type III bursts (see referral 3). The observations of the magnetic signatures of the Langmuir-Slow Extraordinary Modes and their link to the density fluctuations are incredibly pertinent to the plasma emission problem. The systems of improvement of electrostatic waves onto SE and Ordinary waves are both associated to the density fluctuations.

Larosa, A., Dudok de Wit, T., Krasnoselskikh, et al. 2022, ApJ, 95. https://ui.adsabs.harvard.edu/abs/2022ApJ…927…95L/abstract.

Malaspina, D.M., Cairns, I.H., and Ergun, R.E.: 2011, Geophys. 38, L13101.https:// ui.adsabs.harvard.edu/abs/2011GeoRL..3813101M/abstract.

Langmuir-Slow remarkable mode (L-SE) waves have actually been consistently observed in the Solar wind and in Earths electron foreshock because the early age of the area exploration. The typically accepted scenario is that L-SE waves are mode-converted to easily propagating electro-magnetic emission at the plasma frequency. Observation of a magnetic signature in a L-SE wave. The link in between the magnetic signature, the electric field and the refractive index of the waves can be gotten from the linearized Vlasov-Maxwell system as shown in reference 1. The mechanisms of change of electrostatic waves onto SE and Ordinary waves are both related to the density changes.

Langmuir-Slow remarkable mode (L-SE) waves have been regularly observed in the Solar wind and in Earths electron foreshock because the early age of the area exploration. They are intimately connected to the plasma emission system for the type III and type II radio emissions. The typically accepted situation is that L-SE waves are mode-converted to easily propagating electro-magnetic emission at the plasma frequency. However, the information of the mode conversion are disputed. A magnetic part for the L-SE was expected from the polarization homes of the electric field, however never determined till just recently by the Parker Solar Probe (see Figure 1).