Transparency of a magnetic cloud boundary for cosmic rays

Petukhov, I. S.; Petukhov, S. I.

doi:10.3103/s1062873813050456

Cited by 3 publications

(3 citation statements)

References 2 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…According to the kinematic approximation, the speed of Lagrangian particle flow persists that can be used for the calculation of a MC dynamic [7]. The approximation validity is based on: 1) the influence of the force-free magnetic field to the MC dynamic is negligible ( ⃗ × ⃗ ⃗⃗ ≪ 1); 2) the kinetic energy of the particle flow significantly exceeds the thermal energy ( 2 = 2 / 2 ).…”

Section: Modelmentioning

confidence: 99%

See 1 more Smart Citation

Forbush-decrease in a Magnetic Cloud

Petukhov¹

2016

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

View full text Add to dashboard Cite

Calculation of cosmic ray intensity in a magnetic cloud is realized. It is supposed that the magnetic cloud near the Sun has the shape of a torus segment with typical structure of the magnetic field (magnetic field rope). The magnetic cloud is located in the coronal mass ejection having distribution of movement velocity by radius. The subsequent propagation of ejection in interplanetary space is determined on the basis of kinematic model. The magnetic field is determined by the freezing-in condition. It is supposed that the cosmic ray intensity in a magnetic cloud is determined by the large-scale electromagnetic field. The zero and first moments of distribution function of cosmic ray with different energies are calculated. It is revealed influence of the regions connecting a magnetic cloud to the Sun on cosmic ray intensity. Comparison of calculation results with measurements is shown.

show abstract

Section: Modelmentioning

confidence: 99%

“…Forbush-decrease in a Magnetic Cloud Petukhov I.S., Petukhov S.I. 7 The results of the analysis of CR density and anisotropy with hardness 10 GV ( = 9…”

Section: Pos(icrc2015)186mentioning

confidence: 99%

Forbush-decrease in a Magnetic Cloud

Petukhov¹

2016

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

View full text Add to dashboard Cite

show abstract

“…We investigate FD in a MC having a MFR with a toroidal structure. Earlier we presented the calculation results of the CR flux entering into the torus segment through the lateral surface from the surrounding space (Petukhov & Petukhov, , ) and the calculation results of the FD amplitude and vector anisotropy for one type of MC (Petukhova et al, ). We compared the calculation results of the FD amplitude and the vector anisotropy with the measurements for the event on 27 July 2004 and found the dependence between the recovery time of the CR intensity and the MC orientation.…”

Section: Introductionmentioning

confidence: 99%

Image of Forbush Decrease in a Magnetic Cloud by Three Moments of Cosmic Ray Distribution Function

Petukhova

Petukhov

2019

JGR Space Physics

Self Cite

View full text Add to dashboard Cite

The time dynamics of the cosmic ray distribution function in a magnetic cloud is calculated. The magnetic cloud has the form of a torus segment with the force‐free magnetic field structure at the initial moment. The subsequent propagation of the magnetic cloud in interplanetary space is determined by inertial description. The magnetic field is determined by the frozen‐in condition. When calculating the particle distribution function, the electromagnetic field of the magnetic cloud is taken into account, with the scattering of particles not being taken into account. Relations between the particle distribution function and its three moments (particle density and unidirectional and bidirectional anisotropies) are derived. It is established that cosmic ray losses at the regions connecting the magnetic cloud with the Sun determine the amplitude of the second step of Forbush decrease. The time dependence of the Forbush decrease characteristics on magnetic cloud type is determined. The calculation results of the particle density and unidirectional anisotropy generally correspond to measurements. The referred results show a prominent role of the magnetic field structure in the time dynamics of the Forbush decrease.

show abstract

Properties of a cosmic ray flux crossing the magnetic cloud-solar wind interface

Petukhov

2015

Bull. Russ. Acad. Sci. Phys.

View full text Add to dashboard Cite

Transparency of a magnetic cloud boundary for cosmic rays

Cited by 3 publications

References 2 publications

Forbush-decrease in a Magnetic Cloud

Forbush-decrease in a Magnetic Cloud

Image of Forbush Decrease in a Magnetic Cloud by Three Moments of Cosmic Ray Distribution Function

Properties of a cosmic ray flux crossing the magnetic cloud-solar wind interface

Contact Info

Product

Resources

About