Cycling Changes in the Amplitudes of the 27-Day Variation of the Galactic Cosmic Ray Intensity
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We study quasi-periodical changes in the amplitudes of the 27-day variation of the galactic cosmic ray (GCR) intensity, and the parameters of solar wind and solar activity. We have recently found quasi-periodicity of three to four Carrington rotation periods (3 – 4 CRP) in the amplitudes of the 27-day variation of the GCR intensity (Gil and Alania in J. Atmos. Solar-Terr. Phys. 73, 294, 2011). A similar recurrence is recognized in parameters of solar activity (sunspot number, solar radio flux) and solar wind (components of the interplanetary magnetic field, solar wind velocity). We believe that the 3 – 4 CRP periodicity, among other periodicities, observed in the amplitudes of the 27-day variation of the GCR intensity is caused by a specific cycling structure of the Sun’s magnetic field, which may originate from the turbulent nature of the solar dynamo.
KeywordsCosmic rays Solar dynamo 27-days variation of the GCR intensity Sun’s differential roatation
Various periodicities in the temporal changes of the galactic cosmic ray (GCR) intensity have been studied rather intensively up to the present time. We mention here only a few representative papers published in the last decade, e.g., Mursula, Zieger, and Vilppola (2003), Mavromichalaki et al. (2003), Ruzmaikin, Cadavid, and Lawrence (2008), Kudela (2009), Ma, Han, and Yin (2009), Chowdhury, Khan, and Ray (2010), Sabbah and Kudela (2011), and references therein. The periodicities of the GCR intensity at first approximation can be divided into three groups: long-, intermediate- (mid-), and short-term quasi-periodicities (see, e.g., Chowdhury, Khan, and Ray 2010). We mainly study features of the mid-term periodicities (∼27 days) connected with the Sun’s rotation (e.g., Gil and Alania, 2001, 2010). Recently we found (Gil and Alania 2011) a clear recurrence in the temporal changes of the amplitudes of the 27-day variation of the GCR intensity, and in parameters of solar activity (SA) and solar wind. Namely, we recognized a significant recurrence with a duration of three to four Carrington rotations (3 – 4 CRP) as a new type of quasi-periodic variation. We assume that the observed quasi-periodic variability with a 3 – 4 CRP recurrence is related to the cycling structure of the solar magnetic field resulting from the turbulent solar dynamo. Our purpose in this paper is to study features of the 3 – 4 CRP cycling of the 27-day variations of the GCR intensity, and the solar activity and solar wind parameters.
2 Data and Methods
We use the daily data of the Kiel neutron monitor ( http://22.214.171.124/kiel/ , from years 1958 – 2009), the solar wind velocity (SWV), strength and components (B, Bx, By, Bz) of the interplanetary magnetic field (IMF; http://omniweb.gsfc.nasa.gov/ , from 1973 – 2010), sunspot numbers (SSNs), and solar radio flux (SRF; http://spidr.ngdc.noaa.gov/spidr/ , from 1958 – 2010). We also use the data of neutron monitors Potchefstroom, Oulu, and Rome in the period 1980 – 1981, and Moscow, Oulu, and Apatity in the period 1996 – 1998.
3 Results and Discussion
Let us assume that there is no relationship between the possible 3 – 4 CRP features and the 27-day variation of the GCR intensity. In this case we can postulate that there exist different sources for the 3 – 4 CRP cycling structure and the 27-day variation of the GCR intensity; these two phenomena are independent and both are sporadic. We could observe the 3 – 4 CRP cycling only in the amplitudes of the 27-day variations of the GCR intensity and other parameters of solar activity and solar wind, but we have no direct observations of the 3 – 4 CRP cycling structure in the solar magnetic field. For both cases either the 27-day variation of the GCR intensity/or the 3 – 4 CRP cycling recognized in the 27-day variation of the GCR intensity is used as an indicator. However, we can compare the length of the time intervals without 3 – 4 CRP cyclic changes to those when recurrent changes are present. Let us consider the time interval 1973 – 2009, which is significantly longer than the duration of the 3 – 4 CRP and the 27-day variation of the GCR intensity. Taking into account that the 27-day variation of the GCR intensity (including some base values of its amplitude) exists for practically the whole period (at first approximation), the length of the time intervals with the 3 – 4 CRP cyclic changes in the amplitudes of the 27-day variation of the GCR intensity equals ∼46%. Perhaps this feature can help us to better understand the processes taking place on the Sun.
As we have mentioned, the 3 – 4 CRP cycling has a rather sporadic character. It can exist for as long as two years, but after that it disappears, to emerge again after a few rotations. We suppose that the cycling is a universal property of solar activity connected with the solar dynamo – sometimes disturbed by other processes, not very clearly visible, but still existing.
Generally, when proposing any new pattern (e.g., the 3 – 4 CRP structure of the magnetic field on the Sun), one must try to disprove a proposed model or to recommend other possible models. However, we could not find a more appropriate model. Thus, we accept a possible existence of the 3 – 4 CRP cycling structure of the Sun’s magnetic field as a working hypothesis. In the temporal changes of the amplitudes of the 27-day variation of the GCR intensity, besides fluctuations of duration of 3 – 4 CRP, one clearly observes cycling structures with longer duration as well.
We identify a relatively clearly established quasi-recurrence with duration of three to four Carrington rotation periods (3 – 4 CRP) in the temporal changes of the amplitudes of the 27-day variations of the GCR intensity, and parameters of solar activity (sunspot number, 10.7 cm solar radio flux) and solar wind (components of the interplanetary magnetic field, solar wind velocity).
We assume that the 3 – 4 CRP cycling structure is created by processes connected with the turbulent solar magnetic dynamo.
The authors thank the referee and editors, who helped us to improve the paper; the investigators of the websites http://spidr.ngdc.noaa.gov/spidr/ , http://omniweb.gsfc.nasa.gov/ , and http://cr0.izmiran.rssi.ru ; and the researchers of the Kiel, Potchefstroom, Oulu, Apatity, Moscow, and Rome neutron monitors for allowing us to use their data.
This article is distributed under the terms of the Creative Commons Attribution License which permits any use, distribution, and reproduction in any medium, provided the original author(s) and the source are credited.
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