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Solar and interplanetary activities of isolated and non-isolated coronal mass ejections

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Abstract

We report our results on comparison of two halo Coronal Mass Ejections (CME) associated with X-class flares of similar strength (X1.4) but quite different in CME speed and acceleration, similar geo-effectiveness but quite different in Solar Energetic Particle (SEP) intensity. CME1 (non-isolated) was associated with a double event in X-ray flare and it was preceded by another fast halo CME of speed = 2684 km/s (pre-CME) associated with X-ray flare class X5.4 by 1 h from the same location. Since this pre-CME was more eastern, interaction with CME1 and hitting the earth were not possible. This event (CME1) has not suffered the cannibalism since pre-CME has faster speed than post-CME. Pre-CME plays a very important role in increasing the intensity of SEP and Forbush Decrease (FD) by providing energetic seed particles. So, the seed population is the major difference between these two selected events. CME2 (isolated) was a single event. We would like to address on the kinds of physical conditions related to such CMEs and their associated activities. Their associated activities such as, type II bursts, SEP, geomagnetic storm and FD are compared. The following results are obtained from the analysis. (1) The CME leading edge height at the start of metric/DH type II bursts are ~2 R⊙/~4 R⊙ for CME1, but ~2 R⊙/~2.75 R⊙ for CME2. (2) Peak intensity of SEP event associated with the two CMEs are quite different: 6530 pfu for CME1, but 96 pfu for CME2. (3) The Forbush decrease occurred with a minimum decrease of 9.98% in magnitude for CME1, but 6.90% for CME2. (4) These two events produced similar intense geomagnetic storms of intensity of Dst index ~−130 nT. (5) The maximum southward magnetic fields corresponding to Interplanetary CME (ICME) of these two events are nearly the same, but there is difference in Sheath Bz maximum (−14.2, −6.9 nT). (6) The time-line chart of the associated activities of two CMEs show some difference in the time delay between the onsets of activities with respect to the onset of flare/CME.

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Acknowledgements

We gratefully acknowledge the open data policy of the SOHO/LASCO CME team, Solar Geophysical Data team, WDC, Kyoto team, OMNI team. The CME catalogue used is generated and maintained by the Centre for Solar Physics and Space Weather, The Catholic University of America in cooperation with the Naval Research Laboratory and NASA. SOHO is a project of international cooperation between ESA and NASA. This work is supported by the BK21 plus program through the National Research Foundation (NRF) funded by the Ministry of Education of Korea, Basic Science Research Program through the NRF funded by the Ministry of Education (NRF-2016R1A2B4013131) and NRF of Korea Grant funded by the Korean Government (NRF-2013M1A3A3A02042232).

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Authors and Affiliations

  1. Department of Physics, TRP Engineering College (SRM Group), Irungalur, Tiruchirappalli, Tamilnadu, 621105, India

    M. Bendict Lawrance

  2. Department of Physics, Arul Anandar College, Karumathur, Madurai District, Tamilnadu, 625514, India

    A. Shanmugaraju

  3. School of Space Research, Kyung Hee University, Yongin, Seoul, 446-701, Republic of Korea

    Y.-J. Moon

  4. School of Physics, Madurai Kamaraj University, Madurai, Tamilnadu, 625021, India

    S. Umapathy

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  1. M. Bendict Lawrance
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  2. A. Shanmugaraju
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  4. S. Umapathy
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Correspondence to M. Bendict Lawrance.

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Bendict Lawrance, M., Shanmugaraju, A., Moon, YJ. et al. Solar and interplanetary activities of isolated and non-isolated coronal mass ejections. Indian J Phys 91, 711–720 (2017). https://doi.org/10.1007/s12648-017-0966-6

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