Well-defined EUV wave associated with a CME-driven shock

¹ Universidade do Vale do Paraíba – UNIVAP, Av. Shishima Hifumi, 2911 Urbanova, São José dos Campos, SP, Brazil
e-mail: rfldoug@gmail.com
² NAT – Núcleo de Astrofísica Teórica, Universidade Cruzeiro do Sul, Rua Galvão Bueno, 868 Liberdade, São Paulo, SP, Brazil
e-mail: caiuslucius@gmail.com

Received: 26 December 2016
Accepted: 9 January 2018

Abstract

Aims. We report on a well-defined EUV wave observed by the Extreme Ultraviolet Imager (EUVI) on board the Solar Terrestrial Relations Observatory (STEREO) and the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO). The event was accompanied by a shock wave driven by a halo CME observed by the Large Angle and Spectrometric Coronagraph (LASCO-C2/C3) on board the Solar and Heliospheric Observatory (SOHO), as evidenced by the occurrence of type II bursts in the metric and dekameter-hectometric wavelength ranges. We investigated the kinematics of the EUV wave front and the radio source with the purpose of verifying the association between the EUV wave and the shock wave.

Methods. The EUV wave fronts were determined from the SDO/AIA images by means of two appropriate directions (slices). The heights (radial propagation) of the EUV wave observed by STEREO/EUVI and of the radio source associated with the shock wave were compared considering the whole bandwidth of the harmonic lane of the radio emission, whereas the speed of the shock was estimated using the lowest frequencies of the harmonic lane associated with the undisturbed corona, using an appropriate multiple of the Newkirk (1961, ApJ, 133, 983) density model and taking into account the H/F frequency ratio f_H∕f_F = 2. The speed of the radio source associated with the interplanetary shock was determined using the Mann et al. (1999, A&A, 348, 614) density model.

Results. The EUV wave fronts determined from the SDO/AIA images revealed the coexistence of two types of EUV waves, a fast one with a speed of ~560 km s⁻¹, and a slower one with a speed of ~250 km s⁻¹, which corresponds approximately to one-third of the average speed of the radio source (~680 km s⁻¹). The radio signature of the interplanetary shock revealed an almost constant speed of ~930 km s⁻¹, consistent with the linear speed of the halo CME (950 km s⁻¹) and with the values found for the accelerating coronal shock (~535–823 km s⁻¹), taking into account the gap between the radio emissions.