Cosmic Ray Streaming--I EFFECT OF ALFVEN WAVES ON PARTICLES

Skilling, John

doi:10.1093/mnras/172.3.557

Cited by 490 publications

(334 citation statements)

References 0 publications

Supporting

Mentioning

324

Contrasting

Unclassified

Order By: Relevance

“…Stochastic acceleration can also result from resonant pitch-angle scattering from Alfven waves with wavelengths of the order of the particle gyroradius. To accelerate particles these waves must propagate both parallel and antiparallel to the average magnetic field [Skilling, 1975]. Other modes of stochastic acceleration, called magnetic pumping and transit-time damping, occur through interaction with magnetosonic waves whose wavelengths are much longer than the particle gyroradius [Kulsrud and Ferrari, 1971;Melrose, 1980;and Achterberg, 1981 ].…”

Section: A Stochastic Accelerationmentioning

confidence: 99%

Particle acceleration in solar flares

Mandzhavidze

Ramaty

1993

Nuclear Physics B - Proceedings Supplements

View full text Add to dashboard Cite

Section: A Stochastic Accelerationmentioning

confidence: 99%

Particle acceleration in solar flares

Mandzhavidze

Ramaty

1993

Nuclear Physics B - Proceedings Supplements

View full text Add to dashboard Cite

“…To accelerate paticles these waves must propagate both parallel and anti-parallel to the average magnetic field (Skilling 1975). Other modes of stochastic acceleration, called magnetic pumping and transit-time damping, occur through interaction with magnetosonic waves whose wavelengths are much longer than the particle gyroradius (Kulsrud and Ferrari 1971, Melrose 1980, Achterbera 1981.…”

Section: A Stochas Tic Accelerationmentioning

confidence: 99%

The Acceleration and Propagation of Solar Flare Energetic Particles

1985

View full text Add to dashboard Cite

“…The quest for understanding what kind of instability could lead to the right conditions is still open. The resonant instability induced by CR streaming leads to estimate E M ∼ 10 3 − 10 4 GeV [23,24], still well below the knee: this is due to its resonant nature that fixes the saturation at δ B/B ∼ 1 [22,38,32,33,34]. Non-resonant modes, largely studied in Refs.…”

Section: Introductionmentioning

confidence: 99%

On the cosmic ray spectrum from type II Supernovae expanding in their red giant presupernova wind

Cardillo¹,

Amato²,

Blasi³

2016

Proceedings of the 34th International Cosmic Ray Conference — PoS(ICRC2015)

View full text Add to dashboard Cite

One of the most important challenges for the largely accepted idea that Galactic CRs are accelerated in SNR shocks is the maximum energy at which particles can be accelerated. The resonant streaming instability, long invoked for magnetic field amplification at shocks, can not provide sufficiently high fields and efficient enough scattering so as to ensure particle acceleration up to the knee. Here we discuss the non-resonant version of this instability which, with its faster growth and larger value of the amplified field, increases the achievable maximum energy. Because of their higher explosion rate, we focus on type II SNe expanding in their red supergiant wind and we find that the transition between Ejecta Dominated (ED) and Sedov-Taylor (ST) phases takes place at very early times. In this environment, the accelerated particle spectrum shows no high energy exponential cut-off but a spectral break at the maximum energy (E M ). Moreover, the maximum energy of protons can easily reach PeV energies. With this model, we tried to fit KASCADEGrande and ARGO -YBJ data but failed to find a parameter combination that can explain both data sets. We discuss the different scenarios implied by the two data sets.

show abstract

Cosmic Ray Streaming--I EFFECT OF ALFVEN WAVES ON PARTICLES

Cited by 490 publications

References 0 publications

Particle acceleration in solar flares

Particle acceleration in solar flares

The Acceleration and Propagation of Solar Flare Energetic Particles

On the cosmic ray spectrum from type II Supernovae expanding in their red giant presupernova wind

Contact Info

Product

Resources

About