Studying Extreme Ultraviolet Wave Transients With a Digital Laboratory: Direct Comparison of Extreme Ultraviolet Wave Observations to Global Magnetohydrodynamic Simulations

Downs, Cooper; Roussev, I. I.; Holst, B. van der; Lugaz, Noé; Соколов, И. В.; Gombosi, T. I.

doi:10.1088/0004-637x/728/1/2

Cited by 92 publications

(70 citation statements)

References 53 publications

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…Irrespective of their initial speeds or deceleration profiles, these waves ended up travelling within a rather narrow speed range of 180-380 km s −1 which is consistent with the fast mode speed over the quiet Sun (e.g., Wang, 2000;Wu et al, 2001;Cohen et al, 2009;Schmidt and Ofman, 2010;Downs et al, 2011;Zhao et al, 2011). Therefore, the kinematics of the observed waves are consistent with fast-mode waves.…”

Section: Kinematics Amplitudes and Dispersionsupporting

confidence: 66%

See 1 more Smart Citation

On the Nature and Genesis of EUV Waves: A Synthesis of Observations from SOHO, STEREO, SDO, and Hinode (Invited Review)

2012

View full text Add to dashboard Cite

A major, albeit serendipitous, discovery of the SOlar and Heliospheric Observatory mission was the observation by the Extreme Ultraviolet Telescope (EIT) of large-scale Extreme Ultraviolet (EUV) intensity fronts propagating over a significant fraction of the Sun's surface. These so-called EIT or EUV waves are associated with eruptive phenomena and have been studied intensely. However, their wave nature has been challenged by non-wave (or pseudo-wave) interpretations and the subject remains under debate. A string of recent solar missions has provided a wealth of detailed EUV observations of these waves bringing us closer to resolving their nature. With this review, we gather the current state-of-art knowledge in the field and synthesize it into a picture of an EUV wave driven by the lateral expansion of the CME. This picture can account for both wave and pseudo-wave interpretations of the observations, thus resolving the controversy over the nature of EUV waves to a large degree but not completely. We close with a discussion of several remaining open questions in the field of EUV waves research.

show abstract

Section: Kinematics Amplitudes and Dispersionsupporting

confidence: 66%

“…As we will discuss in Section 12, this is not the complete picture. The two fronts exist, they are observed, and recent theoretical work sheds a much clearer light in this hybrid view (Downs et al, 2011).…”

Section: Introductionmentioning

confidence: 96%

On the Nature and Genesis of EUV Waves: A Synthesis of Observations from SOHO, STEREO, SDO, and Hinode (Invited Review)

2012

View full text Add to dashboard Cite

show abstract

“…The outer front has a fast-mode wave nature driven by the eruption, which has been simulated in previous studies (e.g., Wu et al 2001;Cohen et al 2009;Downs et al 2011Downs et al , 2012. The intensity increase in the EUV bands is caused by adiabatic compression, which can be seen as a density increase region in the 3D configuration image (red surface).…”

Section: Type I: Direct Connectionsupporting

confidence: 52%

A Numerical Study of Long-Range Magnetic Impacts During Coronal Mass Ejections

Jin

Schrijver

Cheung

et al. 2016

ApJ

View full text Add to dashboard Cite

With the global view and high-cadence observations from Solar Dynamics Observatory/Atmospheric Imaging Assembly and Solar TErrestrial RElations Observatory, many spatially separated solar eruptive events appear to be coupled. However, the mechanisms for "sympathetic" events are still largely unknown. In this study, we investigate the impact of an erupting flux rope on surrounding solar structures through large-scale magnetic coupling. We build a realistic environment of the solar corona on 2011 February 15 using a global magnetohydrodynamics model and initiate coronal mass ejections (CMEs) in active region 11158 by inserting Gibson-Low analytical flux ropes. We show that a CME's impact on the surrounding structures depends not only on the magnetic strength of these structures and their distance to the source region, but also on the interaction between the CME and the large-scale magnetic field. Within the CME expansion domain where the flux rope field directly interacts with the solar structures, expansion-induced reconnection often modifies the overlying field, thereby increasing the decay index. This effect may provide a primary coupling mechanism underlying the sympathetic eruptions. The magnitude of the impact is found to depend on the orientation of the erupting flux rope, with the largest impacts occurring when the flux rope is favorably oriented for reconnecting with the surrounding regions. Outside the CME expansion domain, the influence of the CME is mainly through field line compression or post-eruption relaxation. Based on our numerical experiments, we discuss a way to quantify the eruption impact, which could be useful for forecasting purposes.

show abstract

“…Currently, the most sophisticated numerical models used are 3D, time-dependent thermodynamic MHD simulations (Downs et al, 2011(Downs et al, , 2012. Such models can produce synthesized observables that can be directly compared with actual observations (see right panel in Figure 41).…”

Section: Small-scale Ejectamentioning

confidence: 99%

“…The models consistently show that the fast outer front is a fast-mode MHD wave (or shock), while there is a larger diversity for the interpretation of the inner front. The latter is variously attributed to plasma compression due to the erupting/expanding CME (Cohen et al, 2009;Downs et al, 2011), a compression front associated with a current shell , a slow-mode wave (Wu et al, 2005), a quite complex combination of slow-mode shocks and velocity vortices , or due to a wave launched by the collision between the flow behind the flux rope and the flux rope itself (Pomoell et al, 2008).…”

Section: Hybrid Modelsmentioning

confidence: 99%

Large-scale Globally Propagating Coronal Waves

Warmuth

2015

Living Rev. Sol. Phys.

169

140

View full text Add to dashboard Cite

Large-scale, globally propagating wave-like disturbances have been observed in the solar chromosphere and by inference in the corona since the 1960s. However, detailed analysis of these phenomena has only been conducted since the late 1990s. This was prompted by the availability of high-cadence coronal imaging data from numerous spaced-based instruments, which routinely show spectacular globally propagating bright fronts. Coronal waves, as these perturbations are usually referred to, have now been observed in a wide range of spectral channels, yielding a wealth of information. Many findings have supported the "classical" interpretation of the disturbances: fast-mode MHD waves or shocks that are propagating in the solar corona. However, observations that seemed inconsistent with this picture have stimulated the development of alternative models in which "pseudo waves" are generated by magnetic reconfiguration in the framework of an expanding coronal mass ejection. This has resulted in a vigorous debate on the physical nature of these disturbances. This review focuses on demonstrating how the numerous observational findings of the last one and a half decades can be used to constrain our models of large-scale coronal waves, and how a coherent physical understanding of these disturbances is finally emerging. Article RevisionsLiving Reviews supports two ways of keeping its articles up-to-date:Fast-track revision. A fast-track revision provides the author with the opportunity to add short notices of current research results, trends and developments, or important publications to the article. A fast-track revision is refereed by the responsible subject editor. If an article has undergone a fast-track revision, a summary of changes will be listed here.Major update. A major update will include substantial changes and additions and is subject to full external refereeing. It is published with a new publication number.For detailed documentation of an article's evolution, please refer to the history document of the article's online version at http://dx

show abstract

Studying Extreme Ultraviolet Wave Transients With a Digital Laboratory: Direct Comparison of Extreme Ultraviolet Wave Observations to Global Magnetohydrodynamic Simulations

Cited by 92 publications

References 53 publications

On the Nature and Genesis of EUV Waves: A Synthesis of Observations from SOHO, STEREO, SDO, and Hinode (Invited Review)

On the Nature and Genesis of EUV Waves: A Synthesis of Observations from SOHO, STEREO, SDO, and Hinode (Invited Review)

A Numerical Study of Long-Range Magnetic Impacts During Coronal Mass Ejections

Large-scale Globally Propagating Coronal Waves

Contact Info

Product

Resources

About