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Exploring the common origins of the Forbush decrease phenomenon caused by the interplanetary counterpart of coronal mass ejections or corotating interaction regions

Anil Raghav1,*, Zubair Shaikh2, Disha Misal1, Gopika Rajan1, Wageesh Mishra3,6, S. Kasthurirangan1, Ankush Bhaskar4,7, Nitinkumar Bijewar1, Abhishek Johri5 et al.

Geeta Vichare2

  • 1University Department of Physics, University of Mumbai, Vidyanagari, Santacruz (E), Mumbai-400098, India
  • 2Indian Institute of Geomagnetism (IIG), New Panvel, Navi Mumbai-410218, India
  • 3University of Science and Technology of China, Hefei 230027, China
  • 4Heliophysics Science Division, NASA/Goddard Space Flight Center, Greenbelt, Maryland 20771, USA
  • 5Centre for Basic Sciences, Pt. Ravishankar Shukla University, Raipur 492 010, India
  • 6Max Planck Institute for Solar System Research, Göttingen D-37077, Germany
  • 7The Catholic University of America, 620 Michigan Ave NE, Washington, DC 20064, USA

  • *Corresponding author. raghavanil1984@gmail.com
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Phys. Rev. D 101, 062003 – Published 24 March, 2020

DOI: https://doi.org/10.1103/PhysRevD.101.062003

Abstract

The interplanetary counterpart of coronal mass ejections (ICMEs) and the interaction regions of slow-fast solar wind (CIRs) have both been known as potential drivers of Forbush decrease (FD). However, reported studies often take an independent approach for investigating FD caused by ICMEs and CIRs, since both the structures show different signature in in-situ observations. In this paper, we explore the common origin of the FD profile caused by these two large scale structures, within the framework of a diffusion-convection model. As a case study, we present one event of each type, in both of which, the solar wind is the most prominent driver. Possible extensions of this model could incorporate other parameters such as magnetic field strength, turbulence, etc which influence the observed FD features. This attempt could help to resolve the complex problem of the diversity in observed FD profiles.

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Phys. Rev. D 101, 062003– Published 24 March, 2020
  • Received 26 June 2019
  • Accepted 18 February 2020
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