the Creative Commons Attribution 4.0 License.
the Creative Commons Attribution 4.0 License.
Impact of solar cycle on the non-linearity of the relationship between the solar wind parameters and geomagnetic conditions
Abstract. Solar wind and its transients drive the dynamics of Earth’s magnetosphere. Interplanetary coronal mass ejections (ICMEs) induce the largest variations in the near-Earth space, but significant geomagnetic activity can also be driven by high-speed streams (HSSs) and stream interaction regions (SIRs). Solar wind – magnetosphere interaction may lead to fluctuations in the inner magnetosphere and, hence, impact the electrons in the outer radiation belt. In this study, we use mutual information from information theory to study the change in the statistical dependence between solar wind parameters and inner magnetospheric indices including ultra low frequency (ULF) waves in the Pc5 range and electrons in the outer radiation belt during solar cycle 23 (1998–2008). Unlike Pearson correlation coefficient, mutual information can be used to investigate non-linear statistical dependencies between different parameters. We calculate linear and non-linear correlation coefficients separately for each year during solar cycle 23 and define the non-linearity with the ratio between the linear and non-linear correlation coefficients. We find that the non-linearity between solar wind speed and electron flux index is higher during solar maximum when most of the geomagnetic activity is driven by ICMEs, while the non-linearity decreases during the declining phase, when a larger portion of the geomagnetic activity is driven by HSSs and SIRs. On the other hand, IMF Bz and solar wind electric field Ey = VswBz have smaller non-linearity with the geomagnetic indices during time periods of stronger geomagnetic activity.
To investigate further if the change of the ratio of ICMEs and SIRs/HSSs as the driver of geomagnetic activity is the possible cause of the changes in the non-linearity during the solar cycle, we calculate the correlation coefficients separately during ICMEs, HSSs/SIRs and quiet solar wind. We find that non-linearity for solar wind speed and inner magnetospheric electron flux and ULF wave indices is smallest and correlations (both linear and non-linear) highest and therefore, the non-linearity is the lowest during the quiet time, while other studied solar wind parameters correlate better either during HSSs or ICMEs. These results show that the selected time period (phase of the solar cycle, dominant driver of the geomagnetic activity during the selected time) for the correlation analysis can significantly impact the results. Results also indicate that during ICMEs the solar wind – magnetosphere coupling becomes more non-linear for the majority of the studied solar wind–magnetospheric index parameter pairs (velocity, density, dynamic pressure) but IMF Bz and solar wind electric field Ey = VswBz have smaller non-linearity during time periods of stronger geomagnetic activity.
- Preprint
(2433 KB) - Metadata XML
- BibTeX
- EndNote
Status: open (until 08 Jun 2024)
-
RC1: 'Comment on angeo-2024-3', Anonymous Referee #1, 29 Apr 2024
reply
Review of “Impact of solar cycle on the non-linearity of the relationship between the solar wind parameters and geomagnetic conditions” by Hoilijoki, Kilpua, Osmane, Turc, Savola, Lipsanen, George and Kalliokoski
This paper covers geomagnetic activity at the Earth and their interplanetary causes over a solar cycle. Studies like this have been done since the 1980s and all of the physical findings presented here have been noted before. As far as I can tell there is nothing particularly new here. If the authors feel that there is a point or two that is new, please focus on those one or two points and shorten the paper considerably.
The referencing is inadequate. References lack coverage over particularly well-developed magnetospheric areas. If included, the authors/readers will note that the conclusions the paper draws are not informative or even worse, incorrect.
Data sets. The data sets for ICMEs, CIRs and ULF waves should be given in Appendices and should be verified as being correct by the authors. This should be a stand-alone paper and the authors are responsible for the accuracy of their data sets.
I cannot recommend this paper for publication in anything resembling its current form.
Comments on Abstract
Abstract line 3 and elsewhere. “SIRs” everywhere should be called “CIRs” as in the discovery paper and naming in GRL, 3, 3, 137-140, 1976. The name “Corotating Interaction Regions” had to do with the shape of the interaction region as it comes outward from the Sun. There was no implication that it had to reappear 27 days later. Please read the paper.
Lines 5-7. It has been well established that magnetospheric relativistic electron enhancements are primarily found during the declining phase of the solar cycle where high speed solar winds coming from coronal holes impact the magnetosphere (Quant.Model. Magne. Proc., Geophys. Monogr. Ser., 21, edited by W. Olsen, p. 21, AGU, Washington, D. C. 1979; JGR, 111, A07S01, doi:10.1029/2005JA011273, 2006). The mechanism is acceleration of substorm ~90-100 keV electrons by chorus waves (GRL 25, 3011, 1998). The substorms are caused by IMF Bsouth components of Alfvén waves embedded in the high speed streams (PSS, 35, 405, 1987; GRL, 41, 1876, 2014; ApJ, 799:39, 2015 doi:10.1088/0004-637X/799/1/39; Ext. Ev. Geosp., 373-400, https://doi.org/10.1016/B978-0-12-812700-1.00014-5, 2018). This scenario is believed to be the main mechanism for the cause of enhanced relativistic electrons in the magnetosphere. This is not mentioned in the abstract, only the effect of PC5 pulsations. Balance should be given to this paper and a statement about the relationship between chorus and relativistic electrons should be mentioned in the abstract. Since chorus and ULF waves are competing mechanisms (see the JGR 2006 paper) for relativistic electron acceleration, your abstract should make some conclusions on this issue.
The radial diffusion model is not described in detail. What does it assume, incoherent wave-particle interactions or coherent ones? Please state in the abstract.
Lines 10-12, “non-linearity” results. Please state what this mean in physical terms. Interpret the phrase: “the non-linearity decreases during the declining phase, when a larger portion of the geomagnetic activity is driven by HSSs and CIRs”. Is the implication: in the declining phase the geomagnetic activity is driven by HSSs and CIRs”? If so this has been discovered before and this is nothing new. See the second paragraph above. “Most of the geomagnetic activity is driven by ICMEs” is also well, well known. This goes back to JGR, 99 A4, 5771, 1994 and has been verified by others many, many times already.
Line 14 Ey = Vsw Bz correlation results with magnetic storms has been shown in many, many publications before. One of the first is the 1994 paper stated previously. There is nothing new here.
Lines 15-16. The geoeffectiveness of ICMEs, HSSs and CIRs for SC23 have been studied and reported before. Two good examples are: JGR 112, A10102, doi:10.1029/2007JA012321, 2007; JGR 113, A05221, doi:10.1029/2007JA012744, 2008. What new information has your study produced, if any?
Lines 16-17. “the nonlinearity for solar wind and magnetospheric electron flux and ULF wave indices is smallest… and correlations highest” is not new. Please see the second paragraph in this section.
Lines 19-20. “These results show that the selected time period (phase of the solar cycle, dominant driver of the geomagnetic activity during the selected time) for the correlation analysis can significantly impact the results”. This has been known for a long time. Please delete.
Lines 20-24. What does this mean physically and is there any new findings here?
Comments, Main Part of Text
Line 25. A better reference is JGR, 99, A4, 5771-5792, 1994. Add this here.
Lines 29-30 and elsewhere. SIRs should be changed to CIRs everywhere in the paper and the GRL 1976 reference should be added on line 30.
Line 31, “weak and moderate geomagnetic activity”. JGR 100, A11, 21727-21733, 1995 should be added to the references.
Line 32. The JGR 1994 reference should be added here. Also a more recent reference on intense magnetic storms: JGRSP 124, 3926-3948, 2019 https://doi.org/10.1029/2018JA026425.
Lines 35-37. These last two sentences should be deleted.
Line 37. For “magnetospheric current changes” a better reference is JGR 73, 17, 5549-5559, 1968. For “ionospheric current changes” a better reference is JSWSC, 2021, 11, 23 https://doi.org/10.1051/swsc/2021001.
Lines 39-40 needs references. For “high energy particle fluxes” see some of the references given previously. For “plasma wave activity” add the references JGR, 82, 32, 5112-5128, 1977 and JGR 106, A7, 13,165–13,178, 2001. And the waves are “chorus” and not generally unknown waves. Please be specific.
Line 41. A more recent reference should be added here: ApJ 946:17, 2023 https://doi.org/10.3847/1538-4357/acb143. It should be noted that solar wind energy is both stored and then released and also directly injected. So your sentence needs revision.
Lines 41-43 needs a reference. The discovery paper is JGR 76, 16, 3587-3611, 1971. Most people standardly state that the substorm electron energies range from ~10 to 100 keV, not up to “hundreds of keVs”. Please correct.
Line 44. Add above chorus references to “wave modes” and add the GRL 1998 reference to “accelerate them up to relativistic (MeV) energies”
Line 46. For ULF waves add the references Springer Nature Switz 2020, Ency. Sol. Ear. Geophys. https://doi.org/10.1007/978-3-030-10475-7_156-1 and JGR 111, A07S01, doi:10.1029/2005JA011273, 2006.
Line 48. Please state the assumptions of the radial diffusion model. Is it coherent or incoherent wave-particle interactions? For fast radial diffusion the assumption must be coherent interactions. There is actually no evidence for coherence in ULF ground observations.
Lines 66-74. This section is inaccurate and is dated. ULF wave activity is believed to be substorm related and the substorms are caused by IMF Bz fluctuation in high speed streams. See the JGR 2006 review paper mentioned before. For substorms during high speed streams see the JGR 1995 paper mentioned before. In parallel with this, the substorms inject ANISOTROPIC ~10 to 100 keV electrons (Wave Inst. Spa Plas. 55-62, 1979, D. Reidel), which in turn generate chorus, which is believed to accelerate the high energy portion of the electrons to relativistic energies. This should be mentioned here as well.
Lines 76-78. This sentence gives no physical meaning. Please delete.
Lines 89-81. It has been shown in the JGR 1994 and the JGR 2008 papers that it is IMF Bsouth that causes geomagnetic storms. What does your statement of “more non linear” mean in this context? Does it add any new information?
Lines 82-83. This “more linear during solar max of Kp and VBs” is just saying that large southward IMF is causing magnetic storms during solar max. This is again nothing new.
Citation: https://doi.org/10.5194/angeo-2024-3-RC1
Viewed
HTML | XML | Total | BibTeX | EndNote | |
---|---|---|---|---|---|
88 | 27 | 8 | 123 | 7 | 6 |
- HTML: 88
- PDF: 27
- XML: 8
- Total: 123
- BibTeX: 7
- EndNote: 6
Viewed (geographical distribution)
Country | # | Views | % |
---|
Total: | 0 |
HTML: | 0 |
PDF: | 0 |
XML: | 0 |
- 1