ELECTROMAGNETIC WAVES NEAR THE PROTON CYCLOTRON FREQUENCY:<i>STEREO</i>OBSERVATIONS

Jian, L. K.; Wei, H. Y.; Russell, C. T.; Luhmann, J. G.; Klecker, B.; Omidi, N.; Isenberg, Philip A.; Goldstein, M. L.; Figueroa-Viñas, A.; Blanco‐Cano, X.

doi:10.1088/0004-637x/786/2/123

Cited by 76 publications

(102 citation statements)

References 75 publications

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“…The resonant activity is at a slightly lower frequency than f sc -,meaning that the wave either has a lower frequency, has a higher phase speed, or is propagating at a slightly oblique angle to the background magnetic field in the plasma frame. This is consistent with previous results from Jian et al (2009Jian et al ( , 2010Jian et al ( , 2014.…”

Section: Case Studysupporting

confidence: 94%

“…The most commonly observed coherent waves close to ion scales in the solar wind are ion-cyclotron waves, which can be found in individual wave packets lasting just a few minutes (Jian et al 2009), or in "cyclotron wave storms" lasting many hours (Jian et al 2014). Cyclotron waves seen in the solar wind frame are left-hand-polarized electromagnetic plasma waves with frequencies close to the proton gyrofrequency in the plasma frame and wavevectors often close to the local magnetic field direction (quasi-parallel).…”

Section: Introductionmentioning

confidence: 99%

“…Cyclotron waves seen in the solar wind frame are left-hand-polarized electromagnetic plasma waves with frequencies close to the proton gyrofrequency in the plasma frame and wavevectors often close to the local magnetic field direction (quasi-parallel). Surveys of STEREO and MESSENGER spacecraft data have been used to identify and study ion-cyclotron-wave storms (Jian et al 2010(Jian et al , 2014, although a complete description of how and why such storms happen is currently lacking.…”

Section: Introductionmentioning

confidence: 99%

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A Proton-Cyclotron Wave Storm Generated by Unstable Proton Distribution Functions in the Solar Wind

Wicks

Alexander

Stevens

et al. 2016

ApJ

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We use audification of 0.092 s cadence magnetometer data from the Wind spacecraft to identify waves with amplitudes 0.1 > nT nearthe ion gyrofrequency (∼0.1 Hz) with duration longer than 1 hr during 2008. We present one of the most common types of event for a case study and find it to be a proton-cyclotron wave storm, coinciding with highly radial magnetic field and a suprathermal proton beam close in density to the core distribution itself. Using linear Vlasov analysis, we conclude that the long-duration, large-amplitude waves are generated by the instability of the proton distribution function. The origin of the beam is unknown, but the radial field period is found in the trailing edge of a fast solar wind stream and resembles other events thought to be caused by magnetic field footpoint motion or interchange reconnection between coronal holes and closed field lines in the corona.

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Section: Case Studysupporting

confidence: 94%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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A Proton-Cyclotron Wave Storm Generated by Unstable Proton Distribution Functions in the Solar Wind

Wicks

Alexander

Stevens

et al. 2016

ApJ

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“…The review of Hollweg & Isenberg The parallel propagating, circularly polarized ion cyclotron mode required for the proton heating was also discussed by Jian et al (2009Jian et al ( , 2014. Detailed studies on the quasi-perpendicular kinetic slow mode and of their effects on the velocity distribution functions and proton heating still remain to be carried out with appropriate wave and particle observations in situ in the solar wind; these may eventually come from the Solar Orbiter mission.…”

Section: Heating Mechanismsmentioning

confidence: 99%

Kinetic Slow Mode in the Solar Wind and Its Possible Role in Turbulence Dissipation and Ion Heating

Narita

Marsch

2015

ApJ

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The solar wind is permeated by various kinds of fluctuations ranging broadly in scales from those of the solar corona and inner heliosphere down to the local ion and electron plasma kinetic scales. The question of what rules the dissipation of magnetohydrodynamic (MHD) turbulence in the solar wind has not conclusively been answered, but remains a key research topic of space plasma physics. Here we propose a new dissipation mechanism, the proton Landau damping of the quasi-perpendicular kinetic slow mode. This mode is linked to the oblique MHD slow mode, yet has shorter wavelengths going down to the proton inertial length. The kinetic slow mode can be separated from the kinetic Alfvén mode by the Alfvén resonance parameter, the proton Landau resonance parameter, the magnetic compressibility, and the electric field polarization. Numerical simulations and in situ observations indicate that the MHD turbulent cascade preferably transfers energy in the direction perpendicular to the background magnetic field. If the kinetic slow mode is also generated and replenished by the energy cascade, this mode can lead to both perpendicular and parallel heating of the protons.

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“…However, remote sensing close to the sun and in-situ observations at <0.3 AU of fast solar wind reveal that for ions T ⊥ > T || . This anisotropy has been attributed as indirect evidence for the presence of ion-cyclotron waves, as it has been suggested that resonant absorption of ion cyclotron waves heats and accelerates the ions in the solar wind (e.g., Axford & McKenzie 1992;Tu & Marsch 1997;Li et al 1999;Ofman et al 2001;Hollweg & Isenberg 2002;Jian et al 2014;Omidi et al 2014). Furthermore, observations by Helios, ACE, Wind, and Ulysses show that magnetic fluctuations in fast solar wind streams can be fitted by simple power laws in the inertia range and steeper spectrum in the dissipation range, providing clues on the possible heating mechanism (e.g., Bavassano et al 1982;Goldstein et al 1995;Podesta et al 2006;Vasquez et al 2007;Salem et al 2009).…”

Section: Introductionmentioning

confidence: 99%

Ion Heating in Inhomogeneous Expanding Solar Wind Plasma: The Role of Parallel and Oblique Ion-Cyclotron Waves

Ozak¹,

Ofman²,

Viñas³

2015

ApJ

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Remote sensing observations of coronal holes show that heavy ions are hotter than protons and their temperature is anisotropic. In-situ observations of fast solar wind streams provide direct evidence for turbulent Alfvén wave spectrum, left-hand polarized ion-cyclotron waves, and He ++ -proton drift in the solar wind plasma, which can produce temperature anisotropies by resonant absorption and perpendicular heating of the ions. Furthermore, the solar wind is expected to be inhomogeneous on decreasing scales approaching the Sun. We study the heating of solar wind ions in inhomogeneous plasma with a 2.5D hybrid code. We include the expansion of the solar wind in an inhomogeneous plasma background, combined with the effects of a turbulent wave spectrum of Alfvénic fluctuations and initial ion-proton drifts. We study the influence of these effects on the perpendicular ion heating and cooling and on the spectrum of the magnetic fluctuations in the inhomogeneous background wind. We find that inhomogeneities in the plasma lead to enhanced heating compared to the homogenous solar wind, and the generation of significant power of oblique waves in the solar wind plasma. The cooling effect due to the expansion is not significant for super-Alfvénic drifts, and is diminished further when we include an inhomogeneous background density. We reproduce the ion temperature anisotropy seen in observations and previous models, which is present regardless of the perpendicular cooling due to solar wind expansion. We conclude that small scale inhomogeneities in the inner heliosphere can significantly affect resonant wave ion heating.

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ELECTROMAGNETIC WAVES NEAR THE PROTON CYCLOTRON FREQUENCY:STEREOOBSERVATIONS

Cited by 76 publications

References 75 publications

A Proton-Cyclotron Wave Storm Generated by Unstable Proton Distribution Functions in the Solar Wind

A Proton-Cyclotron Wave Storm Generated by Unstable Proton Distribution Functions in the Solar Wind

Kinetic Slow Mode in the Solar Wind and Its Possible Role in Turbulence Dissipation and Ion Heating

Ion Heating in Inhomogeneous Expanding Solar Wind Plasma: The Role of Parallel and Oblique Ion-Cyclotron Waves

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