Cme sun
Pro Research Analysisby 
Searched over 200M research papers for "cme sun"
Understanding Coronal Mass Ejections (CMEs) and Their Impact on Earth
Introduction to Coronal Mass Ejections (CMEs)
Coronal Mass Ejections (CMEs) are significant solar phenomena characterized by the expulsion of large quantities of plasma and magnetic flux from the Sun's corona into space. These events are crucial in understanding solar and interplanetary dynamics due to their potential to cause severe space weather effects on Earth4 6.
Pre-CME Sun: Magnetic Structures and Eruption Triggers
CMEs originate in regions of the Sun with closed magnetic field structures, such as active regions, filament regions, and transequatorial interconnection regions. The evolution of these magnetic structures, influenced by photospheric motions like convection and differential rotation, leads to the eruption of CMEs. Pre-eruption indicators include small-scale energetic signatures such as nonthermal radio bursts and compact soft X-ray brightenings1.
Predicting CME Arrival: Data Integration and Machine Learning
Accurate prediction of CME arrival times is essential to mitigate their impact on Earth's technological systems. The CMETNet ensemble learning approach integrates data from solar cycles 23 and 24, including CME features, solar wind parameters, and images from the SOHO/LASCO C2 coronagraph. This method has shown improved prediction accuracy, with a Pearson correlation coefficient of 0.83 and a mean absolute error of 9.75 hours2.
Thermodynamic Properties and Evolution of CMEs
The internal thermodynamic properties of CMEs, such as the polytropic index, heating/cooling rates, and forces acting within the CME, can be estimated using models like the Flux Rope Internal State (FRIS) model. Studies have shown that CMEs are in a heat-releasing state throughout their journey from the Sun to Earth, with the Lorentz force and thermal pressure force playing significant roles in their expansion3.
Observations and Tracking of CMEs
CMEs are observed using various instruments, including the SOHO, TRACE, Wind, ACE, STEREO, and SDO spacecraft. These observations have enhanced our understanding of CME origins, development, and their contribution to space weather. Instruments like the LASCO coronagraphs and STEREO spacecraft provide continuous imaging and tracking of CMEs across the inner heliosphere, allowing for detailed analysis of their three-dimensional properties and internal structures4 7.
CME Propagation and Interaction Effects
The propagation of CMEs from the Sun to Earth involves complex interactions with the solar wind and other CMEs. For instance, a fast CME associated with an intense flare can undergo rapid acceleration and expansion, overcoming the drag exerted by the ambient solar wind. Interaction with preceding slow CMEs can increase turbulence levels, affecting the CME's speed and expansion5.
Advances in Understanding CME Dynamics
Recent advances in the study of CMEs have focused on their three-dimensional configuration, internal magnetic field structures, and the physical processes governing their evolution. Observations from missions like the Parker Solar Probe and STEREO have provided insights into the internal structure of CMEs, revealing features such as loops within the CME flux rope channel7 8.
Conclusion
CMEs are complex solar phenomena with significant implications for space weather and Earth's technological systems. Advances in observational techniques and predictive models have improved our understanding of CME origins, propagation, and impact. Continued research and data integration are essential for enhancing our ability to predict and mitigate the effects of CMEs on Earth.
Sources and full results
Most relevant research papers on this topic
The Pre-CME Sun
Pre-eruption evolution of closed magnetic structures on the Sun, including electron acceleration and plasma heating, can lead to coronal mass ejections.
Highly CitedProbing the Thermodynamic State of a Coronal Mass Ejection (CME) Up to 1 AU
The 2010 April 3 flux rope CME is in a heat-releasing state throughout its journey from the Sun to Earth, with the Lorentz force hindering its expansion and thermal pressure force contributing.
Coronal Mass Ejections: Observations
Recent studies using spacecraft and ground-based instruments have improved our understanding of coronal mass ejections (CMEs) and their contribution to severe space weather at Earth.
Highly CitedAn Intense Flare–CME Event in 2015: Propagation and Interaction Effects Between the Sun and Earth’s Orbit
The fast coronal mass ejection associated with the intense X2.7 flare in 2015 propagated at a speed of 800 km/s between the Sun and 1 AU, overcame solar wind drag, and increased turbulence levels in the inner heliosphere.
Earth-affecting solar transients: a review of progresses in solar cycle 24
In the last decade, advances in solar research have improved our understanding of Earth-affecting solar transients, enabling more accurate predictions and mitigation strategies for advanced technologies.
Literature ReviewInternal Structure of the 2019 April 2 CME
The PSP/WISPR instrument reveals two bright and dark linear features in the 2019 April 2 CME, suggesting two independent flux rope structures within the overall CME outline.
On the three-dimensional configuration of coronal mass ejections
Structured CMEs arise from pre-existing small scale loop systems, with their white-light topology primarily dependent on the orientation and position of their source region's neutral line on the solar disk.
Highly CitedPhysics of erupting solar flux ropes: Coronal mass ejections (CMEs)—Recent advances in theory and observation
Recent advances in theory and observation of CMEs reveal that the physical mechanisms responsible for solar eruptions are primarily driven by magnetic fields in the solar wind, with a strong influence on the Earth's ionosphere.
The Physical Processes of CME/ICME Evolution
CMEs and their interplanetary counterparts undergo complex physical processes during their journey through the solar wind, influencing space weather forecasts.
Highly Cited