Solar Flares and Geomagnetic Storms (Data collection and analysis (original) (raw)
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Geomagnetic storm dependence on the solar flare class
We compare published results on flare-storm dependences and discuss possible sources of the discrepancy. We analyze following sources of difference: (1) different intervals of observations, (2) different statistics and (3) different methods of event identification and comparison. Our analysis shows that magnitude of geomagnetic storms is likely to be independent on X-ray class of solar flares.
A Study of Solar Flare Effects on the Geomagnetic Field Components during Solar Cycles 23 and 24
Atmosphere
In this paper, we investigated the impact of solar flares on the horizontal (H), eastward (Y) and vertical (Z) components of the geomagnetic field during solar cycles 23 and 24 (SC23/24) using data of magnetometer measurements on the sunlit side of the Earth. We examined the relation between sunspot number and solar flare occurrence of various classes during both cycles. During SC23/24, we obtained correlation coefficient of 0.93/0.97, 0.96/0.96 and 0.60/0.56 for C-class, M-class and X-class flare, respectively. The three components of the geomagnetic field reached a peak a few minutes after the solar flare occurrence. Generally, the magnetic crochet of the H component was negative between the mid-latitudes and Low-latitudes in both hemispheres and positive at low latitudes. By contrast, the analysis of the latitudinal variation of the Y and Z components showed that unlike the H component, their patterns of variations were not coherent in latitude. The peak amplitude of solar flare ...
Does geomagnetic storm magnitude depend on solar flare importance?
Cosmic Research, 2009
In order to predict space weather effects, solar flares are often used as precursors of magnetic storms on the Earth. In particular, possible relation between the solar flare importance and magnetic storm intensity is discussed in some papers. However, published results contradict each other. We compare the published results on the flare-storm dependence and discuss possible causes of this disagreement: (1) different intervals of observation, (2) differing statistics, and (3) different methods of identification of events and their comparison. Our analysis has shown that the fact of occurrence and the magnitude of a geomagnetic storm cannot be determined, generally, using only the solar flare importance. However, analyzing additional information on the coronal mass ejection ( CME ), associated with the geomagnetic storm, one can offer an algorithm for the storm magnitude prediction on the basis of flare importance. PACS: 94.30 Lr, 96.50 Uv, 96.60 qe, 96.60 ph
Statistical Study of Nine Months Distribution of Solar Flares
International Letters of Chemistry, Physics and Astronomy, 2014
Solar flare is one of the solar activities that take place in the outermost layer of the corona. Solar flares can heat the material to several million degrees in just a few minutes and at the same time they release the numerous amount of energy. It is believed that a change of magnetic field lines potentially creates the solar flares. The objectives of the study are to identify and compare the types of solar flares (in X-Ray) region and to improve understanding of solar flares. Data are taken from the NOAA website, from the United States Department of Commerce, NOAA, Space Weather Prediction Center (SPWC). Solar radio flux readings were merged together with the three classes and a total of nine graphs were plotted. In illustrating the relationship of solar radio flux and solar flares, it can be explained by studying the range values of flux corresponding to flares values. From this case study, it was found that the minimum value of solar radio flux in order for the flares to occur i...
An Analysis of Sources and Predictability of Geomagnetic Storms
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Solar transient eruptions are the main cause of interplanetary-magnetospheric disturbances leading to the phenomena known as geomagnetic storms. Eruptive solar events such as coronal mass ejections (CMEs) are currently considered the main cause of geomagnetic storms (GMS). GMS are strong perturbations of the Earth’s magnetic field that can affect space-borne and ground-based technological systems. The solar-terrestrial impact on modern technological systems is commonly known as Space Weather. Part of the research study described in this thesis was to investigate and establish a relationship between GMS (periods with Dst ≤ −50 nT) and their associated solar and interplanetary (IP) properties during solar cycle (SC) 23. Solar and IP geoeffective properties associated with or without CMEs were investigated and used to qualitatively characterise both intense and moderate storms. The results of this analysis specifically provide an estimate of the main sources of GMS during an average 11...
International Letters of Chemistry, Physics and Astronomy, 2015
This paper is highlighted on the duration of time for the Coronal Mass Ejections (CMEs) to occur related to solar flare event and the class of solar burst type III that present within the two phenomenon. It is important to understand the evaluations of solar flare until CMEs mean to be appearing and know the basic characterization of solar radio burst type III. It can be observed that CME is even larger than the sun itself. At certain period of time, when the Sun launches billons tones of electrically conducting gas plasma into the space at millions of miles per hours it is assigned that CMEs begin to launch. The data on 23rd of April was selected whereby; solar radio burst type 3 was detected (about 17:36 UT – 17:44 UT). At 17:40 solar flare with a radio burst and CMEs were produced by the sun. Associated with this event, current condition of solar wind speed is 359.5 km/sec with density of 6.0 protons/ and sunspot number are 118. Those at the high latitude have a chance of aurora ...
Study of coronal mass ejections with solar activity and geomagnetic index
In the present study we have investigated the some statistical properties such as occurrence rate, speed of halo partial halo CMEs and all type of CMEs observed during the periods 1996 to 2014 by using solar heliospheric observatory (SOHO) and large angle spectrometric coronagraph (LASCO) data. We investigate the relationship between coronal mass ejection (CMEs), Sunspot number (Rz) and geomagnetic index Ap variations of long term basis. The 650 halo, 1692 partial halo, and 24641 all CMEs which include halo and partial halo event have been observed for the solar cycle 23 to ascending phase of recent solar cycle 24,(years 1996 to 2014). It has been found that the positively correlated between linear speed (Km \sec) all CMEs, halo event CMEs, PHalo event CMES, with sunspot number and geomagnetic index. We found that the rate of occurrence of CMEs is good correlated with sunspot number (Rz) and geomagnetic index (Ap). Keyword-Coronal mass ejection, Sunspot number geomagnetic index, linear speed, halo, partial halo event and correlation coefficient. Introduction-When coronal mass ejections (CMEs) erupt from the sun, high speed particles and strong magnetic field can hurl earthward thus causing a significant impact on the near Earth space environment (geomagnetic storms) such as adverse effects on satellites and communications, electric power, pipelines etc. numerous severe storms occur during the maximum phase of the solar cycle and they are mostly associated with CMEs (Gopalswamy et. al. 2007, Zhane et al. 2007). Disturbances of the near Earth environment are measured by various parameters, such as Ap (Bartels et al. 1939). Coronal mass ejections CMEs are important sources of solar variability from the point of view of plasma and magnetic field. The CMEs remove billions of tons of magnetized plasma from the sun and dump them into sun and the earth connected space once every day during solar minimum and several times per day during solar maximum. The coronal mass ejection are the most energetic events in the heliosphere and are widely recognized as being responsible for production of large disturbances in solar wind, sunspot and geomagnetic. Yashiro et al. (2003) have studied the properties of (CMEs) observed with large angle and spectrometric coronagraphs (LASCO) on board solar and heliospheric observatory (SOHO). Gopalswamy et at. (2003a) have described the solar cycle variation of different properties of CMEs such as average, median speeds, daily occurrence rate and latitude of solar sources for the periods 1996 to 2003.The measured properties of CMEs include their angular widths, speeds, acceleration masses and energies occurrence rate, locations relation to the solar disk have been also discussed by many researches St Cycer et al. 2003, Weeb 2002. The occurrence rate per day of all
Correlation between speeds of coronal mass ejections and the intensity of geomagnetic storms
Space Weather, 2004
We studied the relationship between the projected speed of coronal mass ejections (CMEs), determined from a sequence of Solar and Heliospheric Observatory/Large Angle and Spectrometric Coronagraph Experiment (SOHO/LASCO) images, and the hourly averaged magnitude of the Bz component of the magnetic field in an interplanetary ejecta, as measured by the Advanced Composition Explorer (ACE) magnetometer in the Geocentric Solar Magnetospheric Coordinate System (GSM). For CMEs that originate at the central part of the solar disk we found that the intensity of Bz is correlated with the projected speed of the CME, Vp. The relationship is more pronounced for very fast ejecta (Vp > 1200 km/s), while slower events display larger scatter. We also present data which support earlier conclusions about the correlation of Bz and the Dst index of geomagnetic activity. A possible application of the results to space weather forecasting is discussed.
Factors of geomagnetic storms during the solar cycles 23 and 24: A comparative statistical study
Scientific Research and Essays
The solar sources of 884 geomagnetic storms have been studied for the solar cycles 23 and 24 (1996-2019), regardless of their size ranges; using the Kp index and the NOAA G criteria (minor to extreme storms). It claims from our investigation that fast solar wind streams (HSSWs) is the main factor of small (G1) and medium (G2) storms and occur mostly on the descending phase of the solar cycle. Fast solar wind has contributed to about 59% of G1 storms; 50% of G2; 29% G3; and 10% G4 storm. Large storms (G3 to G5) are the effects of coronal mass ejections (CMEs) and they are observed mainly during the maximum and the descending phases of the solar cycle. About 10% of G1 storms, 26% of G2 storms, 59% of G3 (strong) storms, 87% of G4 (severe) storms, and 100% of G5 (extreme) storms were the effect of CMEs. Magnetic clouds contributed 11% of G1 storms, 15% of G2 storms, 9% of G3 storms, and 3% of G4 storms. A comparative statistical occurrence shows that the number of storms decreased during solar cycle 24 when compared with the solar cycle 23. These results showed that the magnetospheric energy transfer decreased in solar cycle 24 and that the magnetosphere was under the influence of intense solar magnetic fields in solar cycle 23. The phenomenon observed in these investigations highlight a drop in solar plasma geoeffectiveness since the long minimum that followed the solar cycle 23.
American Based Research Journal, 2019
Coronal Mass Ejections (CMEs) are the drastic solar events in which huge amount of solar plasma materials are ejected into the heliosphere from the sun and are mainly responsible to generate large disturbances in solar wind plasma parameters and geomagnetic storms in the geomagnetic field. We have studied geomagnetic storms, (Dst ≤-90nT) observed during the period of 1997-2012 with Coronal Mass Ejections and disturbances in solar wind plasma parameters (velocity). We have inferred that most of the geomagnetic storms are associated with halo and partial-halo Coronal Mass Ejections (CMEs). The association rate of halo and partial halo coronal mass ejections are found 75 % and 25 % respectively. Further, we have concluded that geomagnetic storms are closely associated with the disturbances in solar wind plasma parameters. We have determined a positive correlation between the magnitudes of geomagnetic storms and speed of CMEs with correlation coefficient 0.26. Further Positive co-relation has been found between the speed of CMEs and peak velocity of jump in solar wind plasma velocity. Statistically calculated co-relation coefficient is 0.31 between these two events. Again there is a Positive co-relation has been found between the speed of CMEs and magnitude of jump in solar wind plasma velocity with correlation coefficient 0.20. Furthermore, we observe the positive correlation between the magnitude of geomagnetic storms and the peak value of JSWV events and statistically calculated co-relation coefficient is 0.42 between these two events. We have concluded that geomagnetic storms are mainly caused by Coronal Mass Ejections and disturbances in solar wind plasma parameters that they generate.