Propagation of Solar and Galactic Cosmic Rays of Low Energies in Interplanetary Medium

Vernov, S. N.; Chudakov, A. E.; Vakulov, P. V.; Gorchakov, E. V.; Kontor, N. N.; Logachev, Yu. I.; Lyubimov, G. P.; Pereslegina, N. V.; Timofeev, G.A.

doi:10.1007/978-94-010-3278-0_5

Cited by 22 publications

(16 citation statements)

References 4 publications

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“…The slowing ratio of the shock (defined as the ratio of the observed speed at 1 AU to the average transit speed) was 0.76; the slowing ratio of the flare ejecta was 0.68. Similar (e.g., Hundhausen, 1972;Hirshberg et al, 1972) and larger (e.g., Gosling et al, 1968;Vernov et al, 1970;Dryer, 1974) interplanetary decelerations have been reported for other interplanetary disturbances. Vernov et al (1970), Dryer (1974 and others have suggested that shock wave disturbances propagating through the solar wind often exhibit a power law behavior, i.e., v (r) = Vo (r0/r)",…”

Section: Discussionmentioning

confidence: 61%

Direct observations of a flare related coronal and solar wind disturbance

et al. 1975

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Numerous mass ejections from the Sun have been detected with orbiting coronagraphs.Here for the first time we document and discuss the direct association ofa coronagraph observed mass ejection, which followed a 2B flare, with a large interplanetary shock wave disturbance observed at 1 AU. Estimates of the mass (2.4 • 1016 g) and energy content (1.1 • 1032 erg) of the coronal disturbance are in reasonably good agreement with estimates of the mass and energy content of the solar wind disturbance at 1 AU. The energy estimates as well as the transit time of the disturbance are also in good agreement with numerical models of shock wave propagation in the solar wind.

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Section: Discussionmentioning

confidence: 61%

Direct observations of a flare related coronal and solar wind disturbance

et al. 1975

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“…It will be seen at once that all of the events showing acceleration occurred when this rate was `10, and that none of the shocks which occurred when the ambient rate was <10 showed an increase in the number of particles greater than 1 Mev at the time of the shock. It then appears that for these events the action of interplanetary shocks will not accelerate protons from the solar wind energies, (of order 1 KeV), to energies of order 1 Mev contrary to the suggestion of Vernov (1969). In column eight of Table I we note whether the detection of the shock was immediately followed by a decrease in particle flux below the previous ambient level, of the type noted by Van Allen and Press.…”

Section: Resultsmentioning

confidence: 70%

“…As the particles originated at the sun simultaneously with the shock, the average particle on the outward side of the shock before it passed the spacecraft would be expected to have higher energy than the average particle on the sunward side, as a result of collisions with the shock. Such acceleration has been suggested by Vernov et al (1969), in connection with socalled "Storm Particle Events". The increases discussed here, of duration about 1030 seconds, are not to be identified with such events.…”

Section: Introductionmentioning

confidence: 99%

Acceleration of protons by interplanetary shocks

Ogilvie¹,

Arens²

1971

J. Geophys. Res.

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Short‐duration increases in particle flux at 1‐Mev energy, detected by Explorer 34 just before the time of passage of interplanetary shocks are discussed. The effect is interpreted as particle acceleration associated with the shocks; most of the increase is found to be consistent in many ways with the idea of energy gain by successive reflection between the earth's bow shock and the interplanetary shock. Other mechanisms are not excluded, however. From the small sample observed, it appears that shocks occurring when the interplanetary magnetic field at the observer's position does not intersect the earth's bow shock did not show particle flux increases, and that the particles accelerated to 1 Mev by the observed shocks did not come from solar wind energies, but rather from solar particles in the hundred‐kev energy region which were available in the medium.

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“…. 1962;Rao et al 1967;Ogilvie and Arens, 1968;et al, 1970et al, . Sarris ca t al., 1975Ipavich et il., 1975).…”

Section: Resultsmentioning

confidence: 99%

The radial variation of corotating energetic particle streams in the inner and outer solar system

Hollebeke¹,

McDonald²,

Trainor³

et al. 1978

J. Geophys. Res.

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The radial gradient of long-lived, corotating energetic particle .treams is measured using observations of .9-2.2 MeV protons from Helios 1 and 2 between .3 All and 1 AU, IMP 7 at 1 AU, Pioneer 11 at 3.8 All and Pioneer 10 between 9 All and 10 AU. These studies cover several time periods from mid-1973 to mid-1976. A positive gradient of 11 -3507 per All is found between .3 All and 1 AU. Between 1 All and some 3-5 AU, the gradient is variable with an average value of 100% per Ali which is consistent with the earlier statistical results obtained from the IMP 7 and Pioneer 11 data. A comparison between measurements at 9 AU and 24 AU shows a negative gradient which is variable from -40 to -100% per AU. Possible solar latitudinal effects on these gradient studies are also discussed. Using solar wind and magnetic field data from Helios 1 between 1 All and .3 AU, the relation between corotating energetic particle events in the inner solar system and the interplanetary medium is examined. It is found that the energetic particles are contained inside the high speed solar wind stream in a region adjacent to the interaction region t,etw-!en low speed and high speed streams.

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Propagation of Solar and Galactic Cosmic Rays of Low Energies in Interplanetary Medium

Cited by 22 publications

References 4 publications

Direct observations of a flare related coronal and solar wind disturbance

Direct observations of a flare related coronal and solar wind disturbance

Acceleration of protons by interplanetary shocks

The radial variation of corotating energetic particle streams in the inner and outer solar system

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