Evidence for the Oscillating Two Stream Instability and Spatial Collapse of Langmuir Waves in a Solar Type Iii Radio Burst

Thejappa, G.; MacDowall, R. J.; Bergamo, M.; Papadopoulos, K.

doi:10.1088/2041-8205/747/1/l1

Cited by 61 publications

(44 citation statements)

References 41 publications

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“…This type of streaming instability arises in stellar atmospheres, since the stellar plasmas are predominantly electron-proton type. A specific example for this instability is an electron-precipitation related phenomenon in solar chromosphere [1], and also the presence of oscillating TSI in a solar type III radio bursts [2] is a strong experimental support for our theoretical calculation which shows a greater growth rate of TSI in the photosphere. The very important point presented by them is the spatial damping of Langmuir waves induced by the TSI, which is also our conclusion that these waves are damped out in coronal plasma which heats the ions.…”

Section: Introductionsupporting

confidence: 69%

Two Stream Instability as a Source of Coronal Heating

Soosaleon¹,

Jose²

2015

IJAA

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Recent observation of oscillating the two stream instability (TSI) in a solar type III radio bursts and spatial damping of Langmuir oscillations has made this instability as an important candidate to understand the coronal heating problem. This instability has been studied by several authors for cold plasma found to be stable for high frequencies (greater than plasma frequency ω p ). In this paper, we prove that this instability is unstable for warm plasma for higher frequencies (greater than plasma frequency ω p ) and much suitable to study the solar coronal heating problem. We have derived a general dispersion relation for warm plasma and discussed the various methods analyzing the instability conditions. Also, we derived an expression for the growth rate of TSI and analyzed the growth rate for photospheric and coronal plasmas. A very promising result is that the ion temperature is the source of this instability and shifts the growth rate to high frequency region, while the electron temperature does the reverse. TSI shows a high growth rate for a wide frequency range for photosphere plasma, suggesting that the electron precipitation by magnetic reconnection current, acceleration by flares, may be source of TSI in the photosphere. But for corona, these waves are damped to accelerate the ions and further growing of such instability is prohibited due to the high conductivity in coronal plasma. The TSI is a common instability; the theory can be easily modifiable for multi-ion plasmas and will be a useful tool to analyze all the astrophysical problems and industrial devices, too.

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Section: Introductionsupporting

confidence: 69%

Two Stream Instability as a Source of Coronal Heating

Soosaleon¹,

Jose²

2015

IJAA

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“…Thejappa et al (2012a) had reported the observations of the X component of this wave packet and had shown that it is characterized by (1) a spectrum consisting of (a) a resonant peak at the local electron plasma frequency, f pe , (b) Stokes peak at a frequency slightly lower than f pe , (c) anti-Stokes peak at a frequency slightly higher than f pe , and (d) low-frequency enhancement corresponding to ion sound fluctuations, which satisfy the resonance conditions of oscillating two-stream instability (OTSI); and by (2) peak intensity, which is well above the thresholds for OTSI, supersonic collapse and formation of collapsing envelope soliton. Thejappa et al (2012b) have for the first time applied the trispectral analysis technique on this wave packet and showed that its spectral components are coupled to each other with a high degree of phase coherency.…”

Section: Discussionmentioning

confidence: 99%

“…The in situ wave measurements have shown some signatures of the ESD in type III bursts (Lin et al, 1986;Gurnett et al, 1993;Hospodarsky and Gurnett, 1995;Thejappa and MacDowall, 1998;Thejappa et al, 2003;Henri et al, 2009). The high time resolution observations from the Fast Envelope Sampler (FES) of the ULYSSES/URAP experiment have provided some evidence for the strong Langmuir turbulence processes in type III burst sources (Kellogg et al, 1992;Thejappa et al, 1993Thejappa et al, , 1996Thejappa et al, , 1999MacDowall, 1998, 2004).…”

Section: Published By Copernicus Publications On Behalf Of the Europementioning

confidence: 99%

“…The high time resolution observations from the Fast Envelope Sampler (FES) of the ULYSSES/URAP experiment have provided some evidence for the strong Langmuir turbulence processes in type III burst sources (Kellogg et al, 1992;Thejappa et al, 1993Thejappa et al, , 1996Thejappa et al, , 1999MacDowall, 1998, 2004). Thejappa et al (2012a) had reported the high time resolution observations of a Langmuir wave packet obtained by the X-antenna of the STEREO spacecraft, and had shown that this wave packet satisfies the threshold conditions for OTSI, supersonic collapse as well as formation of collapsing envelope soliton, and its spectrum contains the signatures of OTSI, namely, the peaks corresponding to the beam-generated Langmuir waves, Stokes and anti-Stokes modes and ion sound waves, with frequencies and wave numbers satisfying the matching rules of the four-wave interaction. For the first time, Thejappa et al (2012b) had applied the trispectral analysis technique on this wave packet and had shown that its spectral components are coupled to each other with a high degree of phase coherency (high tricoherence).…”

Section: Published By Copernicus Publications On Behalf Of the Europementioning

confidence: 99%

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Evidence for four- and three-wave interactions in solar type III radio emissions

2013

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The high time resolution observations obtained by the STEREO/WAVES experiment show that in the source regions of solar type III radio bursts, Langmuir waves often occur as intense localized wave packets with short durations of only few ms. One of these wave packets shows that it is a three-dimensional field structure with W_Ln_eT_e ~ 10⁻³, where W_L is the peak energy density, and n_e and T_e are the electron density and temperature, respectively. For this wave packet, the conditions of the oscillating two-stream instability (OTSI) and supersonic collapse are satisfied within the error range of determination of main parameters. The density cavity, observed during this wave packet indicates that its depth, width and temporal coincidence are consistent with those of a caviton, generated by the ponderomotive force of the collapsing wave packet. The spectrum of each of the parallel and perpendicular components of the wave packet contains a primary peak at f_pe, two secondary peaks at f_pe ± f_S and a low-frequency enhancement below f_S, which, as indicated by the frequency and wave number resonance conditions, and the fast Fourier transform (FFT)-based tricoherence spectral peak at (f_pe, f_pe, f_pe + f_S, f_pe − f_S), are coupled to each other by the OTSI type of four-wave interaction (f_pe is the local electron plasma frequency and f_S is the frequency of ion sound waves). In addition to the primary peak at f_pe, each of these spectra also contains a peak at 2f_pe, which as indicated by the frequency and wave number resonance conditions, and the wavelet-based bicoherence spectral peak at (f_pe, f_pe), appears to correspond to the second harmonic electromagnetic waves generated as a result of coalescence of oppositely propagating sidebands excited by the OTSI. Thus, these observations for the first time provide combined evidence that (1) the OTSI and related strong turbulence processes play a significant role in the stabilization of the electron beam, (2) the coalescence of the oppositely propagating up- and down-shifted daughter Langmuir waves excited by the OTSI probably is the emission mechanism of the second harmonic radiation, and (3) the Langmuir collapse follows the route of OTSI in some of the type III radio bursts

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“…There has been a number of recent works claiming to observe Langmuir wave collapse in the solar wind (e.g. Thejappa et al, 2012Thejappa et al, , 2013. However, other studies have analysed the same events but using all three components of the electric field (Graham et al, 2012b,a) and find that the electric field is too weak for wave collapse to occur.…”

Section: Langmuir Wavesmentioning

confidence: 99%

A review of solar type III radio bursts

Reid

Ratcliffe

2014

Res. Astron. Astrophys.

339

217

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Solar type III radio bursts are an important diagnostic tool in the understanding of solar accelerated electron beams. They are a signature of propagating beams of nonthermal electrons in the solar atmosphere and the solar system. Consequently, they provide information on electron acceleration and transport, and the conditions of the background ambient plasma they travel through. We review the observational properties of type III bursts with an emphasis on recent results and how each property can help identify attributes of electron beams and the ambient background plasma. We also review some of the theoretical aspects of type III radio bursts and cover a number of numerical efforts that simulate electron beam transport through the solar corona and the heliosphere.

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Evidence for the Oscillating Two Stream Instability and Spatial Collapse of Langmuir Waves in a Solar Type Iii Radio Burst

Cited by 61 publications

References 41 publications

Two Stream Instability as a Source of Coronal Heating

Two Stream Instability as a Source of Coronal Heating

Evidence for four- and three-wave interactions in solar type III radio emissions

A review of solar type III radio bursts

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