Solar wind spatial scales in and comparisons of hourly Wind and ACE plasma and magnetic field data

King, J. H.; Papitashvili, N. E.

doi:10.1029/2004ja010649

Cited by 1,176 publications

(1,099 citation statements)

References 17 publications

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“…This paper is a continuation of our previous paper [Yermolaev et al, 2012b], and we use the same databases (OMNI data of interplanetary plasma and magnetic field parameters (see http://omniweb.gsfc.nasa.gov) [King and Papitashvili, 2004] and measurements of Dst index (see http://wdc.kugi.kyoto-u.ac.jp/index.html for the period of 1976-2000)) and the same method of classification of large-scale solar wind streams (see our catalog of large-scale interplanetary events for 1976-2000 on the web site ftp://www.iki.rssi.ru/pub/ omni [Yermolaev et al, 2009]). We analyze separately 798 moderate (with −100nT < Dst min ≤ −50 nT) and strong (Dst min ≤ −100 nT) magnetic storms.…”

Section: Methodsmentioning

confidence: 99%

Influence of the interplanetary driver type on the durations of the main and recovery phases of magnetic storms

et al. 2014

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We study the durations of the main and recovery phases of magnetic storms induced by different types of large‐scale solar‐wind streams (Sheath, magnetic cloud (MC), Ejecta, and corotating interaction region (CIR)) on the basis of OMNI data for 1976–2000. The durations of both the main and recovery phases depend on the type of interplanetary drivers. On average, the duration of the main phase of storms induced by compressed regions (CIR and Sheath) is shorter than for MC and Ejecta, while the duration of the recovery phase of CIR‐ and Sheath‐induced storms is longer. Analysis of the durations of individual storms shows that the durations of the main and recovery phases anticorrelate for CIR‐ and Sheath‐induced storms and there is no dependence between them for (MC + Ejecta)‐induced storms.

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Section: Methodsmentioning

confidence: 99%

Influence of the interplanetary driver type on the durations of the main and recovery phases of magnetic storms

et al. 2014

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“…We use the 1 h interplanetary plasma and magnetic field data of OMNI database [King and Papitashvili, 2004] as a basis for our investigations. We made our own data archive including OMNI data and calculated (using OMNI data) additional parameters.…”

Section: Methodsmentioning

confidence: 99%

Dynamics of large‐scale solar wind streams obtained by the double superposed epoch analysis

et al. 2015

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Using the OMNI data for period 1976-2000 we investigate the temporal profiles of 20 plasma and field parameters in the disturbed large-scale types of solar wind (SW): CIR, ICME (both MC and Ejecta) and Sheath as well as the interplanetary shock (IS). To take into account the different durations of SW types we use the double superposed epoch analysis (DSEA) method: re-scaling the duration of the interval for all types in such a manner that, respectively, beginning and end for all intervals of selected type coincide. As the analyzed SW types can interact with each other and change parameters as a result of such interaction, we investigate separately 8 sequences of SW types: (1) CIR, (2) IS/CIR, (3) Ejecta, (4) Sheath/Ejecta, (5) IS/Sheath/Ejecta, (6) MC, (7) Sheath/MC, and ( 8) IS/Sheath/MC. The main conclusion is that the behavior of parameters in Sheath and in CIR are very similar both qualitatively and quantitatively. Both the high-speed stream (HSS) and the fast ICME play a role of pistons which push the plasma located ahead them. The increase of speed in HSS and ICME leads at first to formation of compression regions (CIR and Sheath, respectively), and then to IS. The occurrence of compression regions and IS increases the probability of growth of magnetospheric activity.

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“…The second panel shows sunspot number. The third panel shows the unsigned open solar flux (OSF), calculated from 4πAU 2 |B R |, where AU is the Earth-Sun distance and B R is the daily mean radial magnetic field from the OMNI dataset (King and Papitashvili, 2005). The bottom panel shows the HCS index, a useful parameter for quantifying any tilt and the warped nature of the heliospheric current sheet (in other studies often quantified by tilt angle).…”

Section: The 22-year Solar Cycle Variationsmentioning

confidence: 99%

The 22-Year Hale Cycle in Cosmic Ray Flux – Evidence for Direct Heliospheric Modulation

2013

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The ability to predict times of greater galactic cosmic ray (GCR) fluxes is important for reducing the hazards caused by these particles to satellite communications, aviation, or astronauts. The 11-year solar cycle variation in cosmic rays is highly correlated with the strength of the heliospheric magnetic field. Differences in GCR flux during alternate solar cycles yield a 22-year cycle, known as the Hale Cycle, which is thought to be due to different particle drift patterns when the northern solar pole has predominantly positive (denoted a qA>0 cycle) or negative (qA<0) polarities. This results in the onset of the peak cosmic ray flux at Earth occurring earlier during qA>0 cycles than for qA<0 cycles and hence the peak being more domed for qA>0 and more sharply peaked for qA<0. In this study, we demonstrate that properties of the large-scale heliospheric magnetic field are different during the declining phase of the qA<0 and qA>0 solar cycles, when the difference in GCR flux is most apparent. This suggests that particle drifts may not be the sole mechanism responsible for the Hale Cycle in GCR flux at Earth. However, it is also demonstrated that these polarity-dependent heliospheric differences are evident during the space-age but much less clear in earlier data: using geomagnetic reconstructions, it is shown that for the period of 1905 -1965, alternate polarities do not give as significant a difference during the declining phase of the solar cycle. Thus we suggest that the 22-year cycle in cosmic ray flux is at least partly the result of direct modulation by the heliospheric magnetic field and that this effect may be primarily limited to the grand solar maximum of the space-age.

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Solar wind spatial scales in and comparisons of hourly Wind and ACE plasma and magnetic field data

Cited by 1,176 publications

References 17 publications

Influence of the interplanetary driver type on the durations of the main and recovery phases of magnetic storms

Influence of the interplanetary driver type on the durations of the main and recovery phases of magnetic storms

Dynamics of large‐scale solar wind streams obtained by the double superposed epoch analysis

The 22-Year Hale Cycle in Cosmic Ray Flux – Evidence for Direct Heliospheric Modulation

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