North-south asymmetry of the heliosphere from cosmic-ray observations

Krymsky, G. F.; Krivoshapkin, P. A.; Mamrukova, V. P.; Gerasimova, S. K.

doi:10.1134/s1063773709050077

Cited by 11 publications

(2 citation statements)

References 4 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…It is obtained that the FD model in which the MC has a form of the expansion cylinder in general correspondences with intensity measurements of CRs in some events [5]. The calculation results of FDs based on the model of the piston of a shock wave generated by a sharp speed jump of the solar wind are presented in [6]. The calculated FDs have the hard spectrum observed during the periods of solar minimum activity.…”

Section: Introductionsupporting

confidence: 52%

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: Introductionsupporting

confidence: 52%

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

“…Various periods have been found, 3.7 years (Vizoso & Ballester 1990), periods between 9 and 12 years (Chang 2008), 43.25, 8.65 and 1.44 years (Ballester, Oliver & Carbonell 2005) and a time scale of 12 cycles (Li et al 2009). Signatures of the solar hemispheric asymmetry has been claimed in solar wind speed (Zieger & Mursula 1998) and the cosmic rays (Krymsky et al 2009). Ballester, Oliver & Carbonell (2005) have not found an 11 year period in the normalized north-south asymmetry index.…”

Section: Introductionmentioning

confidence: 99%

Phase Relationships of Solar Hemispheric Toroidal and Poloidal Cycles

Muraközy

2016

ApJ

View full text Add to dashboard Cite

The solar northern and southern hemispheres exhibit differences between the intensities and time profiles of the activity cycles. The time variation of these properties has been studied in a previous article on the data of Cycles 12-23. The hemispheric phase lags exhibited a characteristic variation: the leading role has been exchanged between the hemispheres by four cycles. The present work extends the investigation of this variation with the data of Schwabe and Staudacher in Cycles 1-4 and 7-10 as well as Spörer's data in cycle 11. The previously found variation can not be clearly recognized using the data of Staudacher, Schwabe and Spörer. However, it is more interesting that the phase lags of the reversals of the magnetic fields at the poles follow the same variation as that of the hemispheric cycles in Cycles 12-23, i.e. in four cyles one of the hemispheres leads and the leading role jumps to the opposite hemisphere in the next four cycles.This means that this variation is a long term property of the entire solar dynamo mechanism, both the toroidal and poloidal fields, that hints at an unidentified component of the process responsible for the long term memory.

show abstract