The effect of variations in the magnetic field direction from turbulence on kinetic-scale instabilities

Opie, Simon; Verscharen, Daniel; Chen, C.H.K.; Owen, Christopher J.; Isenberg, Philip A.

doi:10.1051/0004-6361/202345965

Cited by 2 publications

(3 citation statements)

References 55 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…We see that most of the data points are located at the red-patch area with 0.5 < T ⊥ /T ∥ < 1 and 0.7 < β ∥ < 2. In general, the proton temperature anisotropy in our observations in the fast streams is constrained by the MM instability (solid black line) and the OF instability (dashed black line), which is consistent with previous studies (e.g., Hellinger et al 2006;Bale et al 2009;Chen et al 2016;Opie et al 2023).…”

Section: Data Setsupporting

confidence: 92%

“…The time resolution of the magnetic field data is 0.125 s in the normal mode. Following Opie et al (2022), Opie et al (2023), we average the magnetic field over each 1 s VDF measurement interval from SWA-PAS, so that the magnetic field data and the ion data have the same sampling time sequence.…”

Section: Data Setmentioning

confidence: 99%

“…Based on the data from SolO, the plasma conditions for proton temperature-anisotropy-driven MM and OF instabilities to occur in the solar wind are investigated by Opie et al (2022), Opie et al (2023). It is evident that a large number of data points are well beyond the instability threshold (i.e., Figure 2 in Opie et al 2022;and Figure 1 in Opie et al 2023).…”

Section: Data Setmentioning

confidence: 99%

See 2 more Smart Citations

Temperature Intermittent Structures in the Fast Solar Wind

Wang,

Song

et al. 2024

ApJ

View full text Add to dashboard Cite

In the solar wind turbulence, proton temperature fluctuations are highly intermittent, especially at small scales in the inertial range. This phenomenon may contain information about solar wind intermittent heating. However, the physical nature of the temperature intermittency is not yet clear. Based on the measurements from Solar Orbiter between 2020 September and 2022 September, we identify 185 temperature intermittent structures at the scale of 24 s with well-defined minimum variance direction in the fast solar wind and study the nature and kinetic effects of them. According to the variations of proton temperature, the intermittent structures are classified into four types, including temperature bump, step, dip, and chain. When considering the magnetic field configuration together with other plasma properties, we find that, among the bump cases, 46 of them are linear magnetic holes (LMHs) that are mainly related to mirror-mode (MM) instability, and 43 of them are current sheets (CSs) with local temperature enhancement. The step cases are found to be associated with shock-like structures (13 cases) and tangential discontinuities (eight cases) that separate two different parcels of plasma. For the dip cases, 21 of them could be associated with the MM instability, and the rest of the 16 ones may prefer soliton scenario. The 38 chain cases are identified as compressive vortex-like structures and a mixture of LMHs and CSs. These results will help to further understand the intermittent dissipation process in the solar wind turbulence.

show abstract

Section: Data Setsupporting

confidence: 92%

Section: Data Setmentioning

confidence: 99%

Section: Data Setmentioning

confidence: 99%

See 1 more Smart Citation

Temperature Intermittent Structures in the Fast Solar Wind

Wang,

Song

et al. 2024

ApJ

View full text Add to dashboard Cite

show abstract

Isolation and phase-space energization analysis of the instabilities in collisionless shocks

et al. 2023

View full text Add to dashboard Cite

We analyse the generation of kinetic instabilities and their effect on the energization of ions in non-relativistic, oblique collisionless shocks using a 3D-3V (three spatial with three velocity components) simulation by dHybridR, a hybrid particle-in-cell code. At sufficiently high Mach number, quasi-perpendicular and oblique shocks can experience rippling of the shock surface caused by kinetic instabilities arising from free energy in the ion velocity distribution due to the combination of the incoming ion beam and the population of ions reflected at the shock front. To understand the role of the ripple on particle energization, we devise a new instability isolation method to identify the unstable modes underlying the ripple and interpret the results in terms of the governing kinetic instability. We generate velocity-space signatures using the field–particle correlation technique to look at energy transfer in phase space from the isolated instability driving the shock ripple, providing a viewpoint on the different dynamics of distinct populations of ions in phase space. Together, the field–particle correlation technique and our new instability isolation method provide a unique viewpoint on the different dynamics of distinct populations of ions in phase space and allow us to completely characterize the energetics of the collisionless shock under investigation.

show abstract

The effect of variations in the magnetic field direction from turbulence on kinetic-scale instabilities

Cited by 2 publications

References 55 publications

Temperature Intermittent Structures in the Fast Solar Wind

Temperature Intermittent Structures in the Fast Solar Wind

Isolation and phase-space energization analysis of the instabilities in collisionless shocks

Contact Info

Product

Resources

About