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Propagation of Fast Coronal Mass Ejections and Shock Waves Associated with Type II Radio-Burst Emission: An Analytic Study

  • OBSERVATIONS AND MODELLING OF THE INNER HELIOSPHERE
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Abstract

Coronal mass ejections (CMEs) are large-scale eruptive events in the solar corona. Once they are expelled into the interplanetary (IP) medium, they propagate outwards and “evolve” interacting with the solar wind. Fast CMEs associated with IP shocks are a critical subject for space weather investigations. We present an analytic model to study the heliocentric evolution of fast CME/shock events and their association with type II radio-burst emissions. The propagation model assumes an early stage where the CME acts as a piston driving a shock wave; beyond this point the CME decelerates, tending to match the ambient solar wind speed and its shock decays. We use the shock speed evolution to reproduce type II radio-burst emissions. We analyse four fast CME halo events that were associated with kilometric type II radio bursts, and in-situ measurements of IP shock and CME signatures. The results show good agreement with the dynamic spectra of the type II frequency drifts and the in-situ measurements. This suggests that, in general, IP shocks associated with fast CMEs evolve as blast waves approaching 1 AU, implying that the CMEs do not drive their shocks any further at this heliocentric range.

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Acknowledgements

P. Corona-Romero thanks CONACyT for the doctoral grant. J.A. Gonzalez-Esparza thanks for partial funding by projects DGAPA-PAPIIT (IN105310) and CONACyT (152471). E. Aguilar-Rodriguez thanks DGAPA-PAPIIT project (grant IN109112) and CONACyT project (grant 101625). The authors want to thank the referee, whose comments helped to significantly improve the presentation of this work.

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  1. MEXART, Instituto de Geofisica, Unidad Michoacan, Universidad Nacional Autonoma de Mexico, antigua carretera a Patzcuaro # 8701 Ex-Hda. San Jose de la Huerta, Morelia, Michoacan, 58089, Mexico

    P. Corona-Romero, J. A. Gonzalez-Esparza & E. Aguilar-Rodriguez

  2. Posgrado en Ciencias de la Tierra, Universidad Nacional Autonoma de Mexico, Circuito de la investigacion Cientifica s/n, Ciudad Universitaria, Delegacion Coyoacan, 04510, Mexico City, Mexico

    P. Corona-Romero

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Observations and Modelling of the Inner Heliosphere

Guest Editors: Mario M. Bisi, Richard A. Harrison and Noé Lugaz

Appendix

Appendix

1.1 A.1 Polytropic MHD Jump Relations

Polytropic MHD jump relations are the specific jump relations used in this work; for a more general solution see Petrinec and Russell (1997), Equations (14), (15) and (16). The downstream variables (subindex 2) are related with their upstream counterparts (subindex 1) according to

(19)
(20)
(21)

In Equations (19), (20) and (21) we have used

To obtain Equations (19), (20) and (21) we assume that the normal to the shock is radial at the shock front.

1.2 A.2 Velocity Coplanarity

The velocity coplanarity is commonly used to approximate the shock velocity by applying the mass conservation at the shock reference frame. If a shock wave propagates with a velocity v sh through an ambient solar wind with density ρ 1 and velocity v 1, the shock wave velocity shall fulfil ρ 1(v sh−v 1)=ρ 2(v sh−v 2), where the subindex 2 indicates the downstream values. Thus, solving for v sh:

$$ \mathbf{v}_{\mathrm{sh}} = \frac{\rho_2\mathbf{v}_2 - \rho_1\mathbf{v}_1}{\rho_2 - \rho_1} . $$
(22)

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Corona-Romero, P., Gonzalez-Esparza, J.A. & Aguilar-Rodriguez, E. Propagation of Fast Coronal Mass Ejections and Shock Waves Associated with Type II Radio-Burst Emission: An Analytic Study. Sol Phys 285, 391–410 (2013). https://doi.org/10.1007/s11207-012-0103-9

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