Bursty magnetic reconnection under slow shock‐generated whistler waves

W., Z.; Wu, Liang-neng; Li, L. J.; Wang, L. C.

doi:10.1002/2014ja020190

Cited by 5 publications

(3 citation statements)

References 25 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The whistler waves, in contrast, can affect the electron dynamics inside the EDR and therefore may contribute to the reconnection triggering. In fact, previous numerical simulations [Birn et al, 2001;Drake et al, 2008;Goldman et al, 2014;Ma et al, 2014] and laboratory experiments [Ji et al, 2004] also emphasize the role of whistlers in facilitating reconnection processes. Apart from the whistlerdriven anomalous resistivity, the electron inertia term can also affect magnetic reconnection inside the EDR.…”

Section: Summary and Discussionmentioning

confidence: 90%

MMS observations of whistler waves in electron diffusion region

Cao

et al. 2017

Geophysical Research Letters

View full text Add to dashboard Cite

Whistler waves that can produce anomalous resistivity by affecting electrons' motion have been suggested as one of the mechanisms responsible for magnetic reconnection in the electron diffusion region (EDR). Such type of waves, however, has rarely been observed inside the EDR so far. In this study, we report such an observation by Magnetospheric Multiscale (MMS) mission. We find large‐amplitude whistler waves propagating away from the X line with a very small wave‐normal angle. These waves are probably generated by the perpendicular temperature anisotropy of the ~300 eV electrons inside the EDR, according to our analysis of dispersion relation and cyclotron resonance condition; they significantly affect the electron‐scale dynamics of magnetic reconnection and thus support previous simulations.

show abstract

Section: Summary and Discussionmentioning

confidence: 90%

MMS observations of whistler waves in electron diffusion region

Cao

et al. 2017

Geophysical Research Letters

View full text Add to dashboard Cite

show abstract

“…Star formation (Norman and Heyvaerts, 1985;Marchand et al, 2019;Wurster et al, 2021), solar atmosphere and the solar wind at Earth distance (Galtier and Buchlin, 2007;González-Morales et al, 2019), dynamo action (Mininni et al, 2002(Mininni et al, , 2005Gómez et al, 2010) and the Earth and planetary magnetospheres (Liu et al, 2013;Dorelli et al, 2015;Xie et al, 2015;Tóth et al, 2016), are only some of the frameworks and science cases tackled in the literature employing the Hall-MHD model. Several studies have also shown that the Hall term enhances the rate of magnetic reconnection (Wang et al, 2001;Morales et al, 2005;Ma et al, 2014;Ma et al, 2018), though there is an ongoing discussion on the role of the Hall current in the emergence of magnetic structures (Mininni et al, 2007). In particular, claims are made that the Hall effect may help amplifying the large-scale magnetic field (Mininni et al, 2005) and the emergence of self-organized structures (Numata et al, 2004;Ohsaki, 2006), while some authors argue it helps instead with the generation of small-scale structures and filaments (Rheinhardt and Geppert, 2002;Miura and Araki, 2014;Martin et al, 2013).…”

Section: Hall-mhd Description Of Plasmasmentioning

confidence: 99%

Scaling Laws for the Energy Transfer in Space Plasma Turbulence

Marino,

Sorriso-Valvo

2023

Preprint

View full text Add to dashboard Cite

One characteristic trait of space plasmas is the multi-scale dynamics resulting from non-linear transfers and conversions of various forms of energy. Routinely evidenced in a range from the large-scale solar structures down to the characteristic scales of ions and electrons, turbulence is a major cross-scale energy transfer mechanism in space plasmas. At intermediate scales, the fate of the energy in the outer space is mainly determined by the interplay of turbulent motions and propagating waves. More mechanisms are advocated to account for the transfer and conversion of energy, including magnetic reconnection, emission of radiation and particle energization, all contributing to make the dynamical state of solar and heliospheric plasmas difficult to predict. The characterization of the energy transfer in space plasmas benefited from numerous robotic missions. However, together with breakthrough technologies, novel theoretical developments and methodologies for the analysis of data played a crucial role in advancing our understanding of how energy is transferred across the scales in the space. In recent decades, several scaling laws were obtained providing effective ways to model the energy flux in turbulent plasmas. Under certain assumptions, these relations enabled to utilize reduced knowledge (in terms of degrees of freedom) of the fields from spacecraft observations to obtain direct estimates of the energy transfer rates (and not only) in the interplanetary space, also in the proximity of the Sun and planets. Starting from the first third-order exact law for the magnetohydrodynamics by Politano and Pouquet (1998), we present a detailed review of the main scaling laws for the energy transfer in plasma turbulence and their application, presenting theoretical, numerical and observational milestones of what has become one of the main approaches for the characterization of turbulent dynamics and energetics in space plasmas. Copyright permission for the seminar banner granted by [ESA/ATG medialab](https://www.esa.int/ESA_Multimedia/Images/2020/06/Solar_Orbiter_reaches_first_perihelion).

show abstract

“…In the outflow region or the ideal MHD region, the ejected velocity of the reconnected magnetic flux must be less than the local Alfvén velocity because of the frozen-in condition, which suggests that the Alfvén wave controls the rate of the magnetic reconnection. With the inclusion of the Hall effect in MHD, the whistler wave can be generated [1].…”

Section: Introductionmentioning

confidence: 99%

Generation of Alfvén wave energy during magnetic reconnection in Hall MHD

Wang

2017

Plasma Sci. Technol.

View full text Add to dashboard Cite

The effect of the reconnection rate on the generation of Alfvén wave energy is systematically investigated using Hall magnetohydrodynamics (MHD). It is well known that a decrease in magnetic energy is proportional to the reconnection rate. It is found that an instantaneous increase in Alfvén wave energy in unit Alfvén time is the square dependence on the reconnection rate. The converted Alfvén wave energy is strongly enhanced due to the large increase in the reconnection rate in Hall MHD. For solar-terrestrial plasmas, the maximum converted Alfvén wave energy in unit Alfvén time with the Hall effect can be over 50 times higher than that without the Hall effect during magnetic reconnection.

show abstract

Bursty magnetic reconnection under slow shock‐generated whistler waves

Cited by 5 publications

References 25 publications

MMS observations of whistler waves in electron diffusion region

MMS observations of whistler waves in electron diffusion region

Scaling Laws for the Energy Transfer in Space Plasma Turbulence

Generation of Alfvén wave energy during magnetic reconnection in Hall MHD

Contact Info

Product

Resources

About