Interplanetary magnetic fields, their fluctuations, and cosmic ray variations

Barouch, Eytan; Sari, J. W.

doi:10.1029/ja081i007p01453

Cited by 13 publications

(2 citation statements)

References 24 publications

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“…All the above points are in agreement with the summary of Forbush decrease characteristics presented by Barouch and Burlaga [1975] and Barouch and Sari [1976] on the basis of a statistical study.…”

Section: From (1) and (5) We See That The Diffusion Coefficient Depensupporting

confidence: 90%

Average properties of cosmic ray diffusion in solar wind streams

Morfill¹,

Richter²,

Scholer³

1979

J. Geophys. Res

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Applying a superposed epoch analysis to the Mariner 5 plasma and magnetic field observations of 13 corotating high speed solar wind streams, we obtain the average azimuthal distribution of all relevant parameters of the background interplanetary medium, as well as those of superimposed Alfvén waves. Using these measurements in model calculations allows us to determine the radial and azimuthal variation of the background and fluctuation parameters between 1 and 5 AU, and thus to calculate the cosmic ray diffusion coefficient κ from the plasma and field properties. The calculation of κ assumes that quasi‐linear wave‐particle interaction theory is applicable, and that the Alfvén waves responsible for the scattering are propagating in the azimuthally varying solar wind according to geometrical optics. The consequences of these calculations regarding the occurrence of solar wind stream associated Forbush decreases are discussed.

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Section: From (1) and (5) We See That The Diffusion Coefficient Depensupporting

confidence: 90%

Average properties of cosmic ray diffusion in solar wind streams

Morfill¹,

Richter²,

Scholer³

1979

J. Geophys. Res

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“…Barouch and Burlaga [11] found that the individual magnetic enhancements are generally associated with depressions in cosmic ray intensity, and Barouch and Sari [12] have further demonstrated that these depressions are not related to turbulence or random motions in the field and only the large-scale features of interplanetary magnetic fields are important. However, Nishida [13] has emphasized the importance of scattering by the turbulent magnetic field in producing the transient modulation.…”

Section: Introductionmentioning

confidence: 96%

Interplanetary magnetic clouds and cosmic ray modulation

Mishra

Mishra²

2007

Astrophysics

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We studied the cosmic ray intensity variation due to interplanetary magnetic clouds during an unusual class of low amplitude anisotropic wave train events. The low amplitude anisotropic wave train events in cosmic ray intensity have been identified using the data of ground based Deep River neutron monitor and studied during the period 1981-1994. Even though the occurrence of low amplitude anisotropic wave trains does not depend on the onset of interplanetary magnetic clouds, but the possibility of occurrence of these events cannot be overlooked during the periods of the interplanetary magnetic cloud events. It is observed that the solar wind velocity remains higher (> 300) than normal and the interplanetary magnetic field B remains lower than normal on the onset of the interplanetary magnetic cloud during the passage of low amplitude wave trains. It is also noted that the proton density remains significantly low during high solar wind velocity, which is expected. The north south component of interplanetary magnetic field Bz turns southward to one day before the arrival of cloud and remains in the southward direction after the arrival of a cloud. During these events the cosmic ray intensity is found to increase with increase of solar wind velocity. The superposed epoch analysis of cosmic ray intensity for these events during the onset of interplanetary magnetic clouds reveals that the decrease in cosmic ray intensity starts not at the onset of the cloud but after a few days. The cosmic ray intensity increases on arrival of the magnetic cloud and decreases gradually after the passage of the magnetic cloud.

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Solar Wind and Interplanetary Medium

Svalgaard¹

1977

Illustrated Glossary for Solar and Solar-Terrestrial Physics

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Interplanetary magnetic fields, their fluctuations, and cosmic ray variations

Cited by 13 publications

References 24 publications

Average properties of cosmic ray diffusion in solar wind streams

Average properties of cosmic ray diffusion in solar wind streams

Interplanetary magnetic clouds and cosmic ray modulation

Solar Wind and Interplanetary Medium

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