Numerical Simulation of Coronal Waves Interacting with Coronal Holes. II. Dependence on Alfvén Speed Inside the Coronal Hole

Piantschitsch, Isabell; Vršnak, Bojan; Hanslmeier, A.; Lemmerer, Birgit; Veronig, Astrid; Hernandez-Perez, Aaron; Čalogović, Jaša

doi:10.3847/1538-4357/aab709

Cited by 13 publications

(6 citation statements)

References 40 publications

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“…Both interfaces represent a sharp change in the local fast-mode phase speed and are natural sites for wave reflection and refraction. This is consistent with previous modeling work (e.g., Schmidt & Ofman 2010 and more recently Piantschitsch et al 2017Piantschitsch et al , 2018aPiantschitsch et al , 2018b and observations of phase speed changes and reflection (e.g., Long et al 2008;Veronig et al 2008;Gopalswamy et al 2009;Olmedo et al 2012;Kienreich et al 2013;Liu et al 2018). The streamer disturbance also resembles the large-scale rarefaction and interaction with an EUV wave described by Kwon et al (2013).…”

Section: The Simulated Euv Wavesupporting

confidence: 91%

Validation of Global EUV Wave MHD Simulations and Observational Techniques

Downs

Warmuth

Long³

et al. 2021

ApJ

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Global EUV waves remain a controversial phenomenon more than 20 yr after their discovery by SOHO/EIT. Although consensus is growing in the community that they are most likely large-amplitude waves or shocks, the wide variety of observations and techniques used to identify and analyze them have led to disagreements regarding their physical properties and interpretation. Here, we use a 3D magnetohydrodynamic (MHD) model of the solar corona to simulate an EUV wave event on 2009 February 13 to enable a detailed validation of the various commonly used detection and analysis techniques of global EUV waves. The simulated event exhibits comparable behavior to that of a real EUV wave event, with similar kinematic behavior and plasma parameter evolution. The kinematics of the wave are estimated via visual identification and profile analysis, with both approaches providing comparable results. We find that projection effects can affect the derived kinematics of the wave, due to the variation in fast-mode wave speed with height in the corona. Coronal seismology techniques typically used for estimates of the coronal magnetic field are also tested and found to estimate fast-mode speeds comparable to those of the model. Plasma density and temperature variations of the wave front are also derived using a regularized inversion approach and found to be consistent with observed wave events. These results indicate that global waves are best interpreted as large-amplitude waves and that they can be used to probe the coronal medium using well-defined analysis techniques.

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Section: The Simulated Euv Wavesupporting

confidence: 91%

Validation of Global EUV Wave MHD Simulations and Observational Techniques

Downs

Warmuth

Long³

et al. 2021

ApJ

Self Cite

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“…Observational studies of the interaction of the EUV waves with the CHs are scarce, but the appearance of the secondary waves is found to be a pretty frequent phenomenon when the waves interact with CHs or ARs (Wang, 2000;Gopalswamy et al, 2009;Liu et al, 2019). These observational findings were verified by numerical simulation (Piantschitsch et al, 2017(Piantschitsch et al, , 2018aAfanasyev & Zhukov, 2018). In accordance with these observational and simulation wave-like features confidently confirm the interpretation that it is a fast-mode magnetohydrodynamic (MHD) wave.…”

Section: Discussionsupporting

confidence: 66%

Total reflection of a flare-driven quasi-periodic EUV wave train at a coronal hole boundary

Zhou,

Shen,

Tang

et al. 2021

Preprint

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The reflection, refraction, and transmission of large-scale extreme ultraviolet (EUV) waves (collectively, secondary waves) have been observed during their interactions with coronal structures such as active regions (ARs) and coronal holes (CHs). However, the effect of the total reflection of EUV waves has not been reported in the literature. Here, we present the first unambiguous observational evidence of the total reflection of a quasi-periodic EUV wave train during its interaction with a polar CH. The event occurred in NOAA AR 12473, located close to the southeast limb of the solar disk, and was characterized by a jet-like CME. In this study, we focus in particular on the driving mechanism s of the quasi-periodic wave train and the total reflection effect at the CH boundary. We find that the periods of the incident and the reflected wave trains are both about 100 seconds. The excitation of the quasi-periodic wave train was possibly due to the intermittent energy release in the associated flare since its period is similar to that of the quasi-periodic pulsations in the associated flare. Our observational results showed that the reflection of the wave train at the boundary of the CH was a total reflection because the measured incidence and critical angles satisfy the theory of total reflection, i.e., the incidence angle is less than the critical angle.

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“…Now the MHD wave propagation and its interaction with a region of lower density such as a CH is solved numerically by using the standard ideal MHD equations (see Piantschitsch et al 2017Piantschitsch et al , 2018a. An initial Gaussian linear perturbation is introduced into the system and the evolution of this fluctuation is followed in time, see Fig.…”

Section: Numerical Experiments In the Linear Regimementioning

confidence: 99%

A new method for estimating global coronal wave properties based on their interaction with solar coronal holes

Piantschitsch

Terradas

Temmer

2020

A&A

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Among the effects of interactions between global coronal waves (CWs) and coronal holes (CHs) is the formation of reflected and transmitted waves. Observations of such events provide us with measurements of different CW parameters, such as phase speed and intensity amplitudes. However, several of these parameters are provided with only intermediate observational quality, whereas other parameters, such as the phase speed of transmitted waves, can hardly be observed in general. We present a new method to estimate crucial CW parameters, such as density and phase speed of reflected as well as transmitted waves, Mach numbers and density values of the CH’s interior, by using analytical expressions in combination with the most basic and most accessible observational measurements available. The transmission and reflection coefficients were derived from linear theory and used to calculate estimations for phase speeds of incoming, reflected, and transmitted waves. The obtained analytical expressions were validated by performing numerical simulations of CWs interacting with CHs. This new method enables us to determine in a fast and straightforward way reliable CW and CH parameters from basic observational measurements which provides a powerful tool to better understand the observed interaction effects between CWs and CHs.

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Numerical Simulation of Coronal Waves Interacting with Coronal Holes. II. Dependence on Alfvén Speed Inside the Coronal Hole

Cited by 13 publications

References 40 publications

Validation of Global EUV Wave MHD Simulations and Observational Techniques

Validation of Global EUV Wave MHD Simulations and Observational Techniques

Total reflection of a flare-driven quasi-periodic EUV wave train at a coronal hole boundary

A new method for estimating global coronal wave properties based on their interaction with solar coronal holes

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