scholarly journals Solar Variation and Super Geomagnetic Storm Event during March 10-31, 2015

2019 ◽  
Vol 9 (1) ◽  
pp. 2469-2472
Keyword(s):  
Magnetic Field ◽  
Solar Cycle ◽  
Geomagnetic Storm ◽  
Space Weather ◽  
Solar Flares ◽  
Storm Event ◽  
Earth Magnetic Field ◽  
Solar Cycle 24 ◽  
Cycle 24

CMEs and solar flares are important solar ejections which are the cause of storm in Heliosphere. These ejections are producing a change in Earth magnetic field. In this paper we have studied heliospheric disturbance of solar cycle 24 during period from 10 March to 31 March 2015. We observed that a huge explosion of magnetic field and plasma from the Sun’s corona on 15 March 2015 and associated solar flares have disturbed space weather towards earth causes strongest geomagnetic storm on 17 March 2015. We found that Dst value reached to its minimum is -223 nT and a FDs during the period on 17 March 2015.

Geomagnetic Consequences of Interacting CMEs of June 13-14, 2012

2017 ◽  
Vol 13 (S335) ◽  
pp. 65-68
Author(s):  
Nandita Srivastava ◽  
Zavkiddin Mirtoshev ◽  
Wageesh Mishra
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Solar Cycle ◽  
Geomagnetic Storm ◽  
Solar Wind Plasma ◽  
Single Step ◽  
Solar Cycle 24 ◽  
In Situ Observations ◽  
Cycle 24

AbstractWe have studied the consequences of interacting coronal mass ejections (CMEs) of June 13-14, 2012 which were directed towards Earth and caused a moderate geomagnetic storm with Dst index ~ −86 nT. We analysed the in-situ observations of the solar wind plasma and magnetic field parameters obtained from the OMNI database for these CMEs. The in-situ observations show that the interacting CMEs arrive at Earth with the strongest (~ 150 nT) Sudden Storm Commencement (SSC) of the solar cycle 24. We compared these interacting CMEs to a similar interaction event which occurred during November 9-10, 2012. This occurred in the same phase of the solar cycle 24 but resulted in an intense geomagnetic storm (Dst ~ −108 nT), as reported by Mishra et al. (2015). Our analysis shows that in the June event, the interaction led to a merged structure at 1 AU while in the case of November 2012 event, the interacted CMEs arrived as two distinct structures at 1 AU. The geomagnetic signatures of the two cases reveal that both resulted in a single step geomagnetic storm.

Seasonal behavior of H component during solar cycle 24

2021 ◽  
Author(s):  
Yasmina Bouderba ◽  
Ener Aganou ◽  
Abdenaceur Lemgharbi
Keyword(s):  
Solar Activity ◽  
Solar Cycle ◽  
Horizontal Component ◽  
Low Latitude ◽  
Seasonal Behavior ◽  
The Earth ◽  
Earth Magnetic Field ◽  
Solar Cycle 24 ◽  
Minimum Solar Activity ◽  
Cycle 24

<p>In this work we will show the behavior of the horizontal component H of the Earth Magnetic Field (EMF) along the seasons during the period of solar cycle 24 lasting from 2009 to 2019. By means of  continuous measurements of geomagnetic components (X, Y) of the EMF, we compute the horizontal component H at the Earth’s surface. The data are recorded with a time resolution of one minute at Tamanrasset observatory in Algeria at the geographical coordinates of 22.79° North and 5.53° East. These data are available from the INTERMAGNET network. We find that the variation in amplitude of the hourly average of H component at low latitude changes from a season to another and it is greater at the maximum solar activity than at the minimum solar activity.</p><p><strong>Keywords:</strong> Solar cycle 24, Season, Horizontal component H. </p>

scholarly journals Source-region characteristics of anemone active regions in the ascending phase of solar cycle 24

2020 ◽  
Vol 642 ◽  
pp. A233
Author(s):  
R. Sharma ◽  
C. Cid
Keyword(s):  
Magnetic Field ◽  
Solar Cycle ◽  
Minimum Distance ◽  
Source Region ◽  
Coronal Holes ◽  
Active Regions ◽  
Yearly Average ◽  
Solar Cycle 24 ◽  
Cycle 24 ◽  
Rise Phase

Context. Active regions in close proximity to coronal holes, also known as anemone regions, are the best candidates for studying the interaction between closed and open magnetic field topologies at the Sun. Statistical investigation of their source-region characteristics can provide vital clues regarding their possible association with energetic events, relevant from space weather perspectives. Aims. The main goal of our study is to understand the distinct properties of flaring and non-flaring anemone active regions and their host coronal holes, by examining spatial and magnetic field distributions during the rise phase of the solar cycle, in the years 2011–2014. Methods. Anemone regions were identified from the minimum-distance threshold, estimated using the data available in the online catalogs for on-disk active regions and coronal holes. Along with the source-region area and magnetic field characteristics, associated filament and flare cases were also located. Regions with and without flare events were further selected for a detailed statistical examination to understand the major properties of the energetic events, both eruptive and confined, at the anemone-type active regions. Results. Identified anemone regions showed weak asymmetry in their spatial distribution over the solar disk, with yearly average independent from mean sunspot number trend, during the rise phase of solar cycle 24. With the progression in solar cycle, the area and minimum-distance parameters indicated a decreasing trend in their magnitudes, while the magnetic field characteristics indicated an increase in their estimated magnitudes. More than half of the regions in our database had an association with a filament structure, and nearly a third were linked with a magnetic reconnection (flare) event. Anemone regions with and without flares had clear distinctions in their source-region characteristics evident from the distribution of their properties and density analysis. The key differences included larger area and magnetic field magnitudes for flaring anemone regions, along with smaller distances between the centers of the active region and its host coronal hole.

On the Dynamics of the Largest Active Region of the Solar Cycle 24

2017 ◽  
Vol 13 (S335) ◽  
pp. 32-35
Author(s):  
Ranadeep Sarkar ◽  
Nandita Srivastava ◽  
Sajal Kumar Dhara
Keyword(s):  
Magnetic Field ◽  
Solar Cycle ◽  
Active Region ◽  
Comparative Study ◽  
Lorentz Force ◽  
Sunspot Group ◽  
Solar Dynamics Observatory ◽  
Solar Cycle 24 ◽  
Solar Dynamics ◽  
Cycle 24

AbstractWe have studied the dynamics of the solar active region (AR) NOAA 12192 using full-disc continuum images and the vector magnetograms observed by the Helioseismic and Magnetic Imager (HMI) onboard Solar Dynamics Observatory (SDO). AR 12192 is the largest region of the solar cycle 24. It underwent a noticeable growth and produced 6 X-class, 22 M-class and 53 C-class flares during its disc passage. But the most peculiar fact of this AR is that it was associated with only one CME in spite of producing several X-class flares. In this work, we present the area evolution of this giant sunspot group during the first three rotations when it appeared as AR 12172, AR 12192 and AR 12209, respectively. We have also attempted to make a comparative study of the flare-related photospheric magnetic field and Lorentz force changes for both the eruptive and non-eruptive flares produced by AR 12192.

Solar flares, CMEs and solar energetic particle events during solar cycle 24

2018 ◽  
Vol 61 (2) ◽  
pp. 777-785 ◽  
Author(s):  
Bimal Pande ◽  
Seema Pande ◽  
Ramesh Chandra ◽  
Mahesh Chandra Mathpal
Keyword(s):  
Solar Cycle ◽  
Solar Flares ◽  
Energetic Particle ◽  
Solar Energetic Particle ◽  
Solar Energetic Particle Events ◽  
Solar Cycle 24 ◽  
Cycle 24

scholarly journals Study of Geomagnetic Storms, Interplanetary Magnetic Field and Solar Wind

2019 ◽  
Vol 14 (1) ◽  
Author(s):  
Chandrasekhar Bhoj ◽  
Lalan Prasad
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Solar Cycle ◽  
Interplanetary Magnetic Field ◽  
Correlation Coefficient ◽  
Geomagnetic Storms ◽  
Solar Cycle 24 ◽  
Time Periods ◽  
Cycle 24 ◽  
The Imf

The aim of this paper is to investigate the association of the geomagnetic storms with the IMF for solar cycle 24. Result of the present analysis shows that IMF is geoeffective parameter but its impact varies in accordance with different time periods. The correlation coefficient between Dst and IMF found to be -0.6 for solar cycle 24.

scholarly journals Study of Geomagnetic Storms, Interplanetary Magnetic Field and Solar Wind

2019 ◽  
Vol 14 (1) ◽  
Author(s):  
Chandrasekhar Bhoj ◽  
Lalan Prasad
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Solar Cycle ◽  
Interplanetary Magnetic Field ◽  
Correlation Coefficient ◽  
Geomagnetic Storms ◽  
Solar Cycle 24 ◽  
Time Periods ◽  
Cycle 24 ◽  
The Imf

The aim of this paper is to investigate the association of the geomagnetic storms with the IMF for solar cycle 24. Result of the present analysis shows that IMF is geoeffective parameter but its impact varies in accordance with different time periods. The correlation coefficient between Dst and IMF found to be -0.6 for solar cycle 24

scholarly journals Descriptive study of X-class flares released in the year 2014, during the double peak of SC-24

2015 ◽  
Vol 11 (S320) ◽  
pp. 330-332
Author(s):  
Ahmed A. Hady ◽  
Marwa H. Mostafa ◽  
Susan W. Samwel
Keyword(s):  
Data Analysis ◽  
Solar Cycle ◽  
Solar Flares ◽  
Descriptive Study ◽  
Energetic Particles ◽  
Main Peak ◽  
Solar Cycles ◽  
Double Peak ◽  
Solar Cycle 24 ◽  
Cycle 24

AbstractDuring the declining phase of the Solar cycle 24, a new peak appeared on January 7, 2014. The release of x-class flares, with the high energetic particles, were found to be more intense than that occurred during the main peak of the same cycle. Few X-class flares were released, lately, during the year 2014. We note that during the last 5 solar cycles, a new peak has appeared, releasing high energetic particles and X-class solar flares, which are called the secondary peak or the double peak of solar cycle. The aim of this descriptive study is to follow the morphological and magnetic changes of the active region before, during, and after the production of X-class flares according to data analysis. Furthermore, the causes of the release of such eruptive storms have been discussed for the period, year 2014, during the double peak of the solar cycle 24.

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