scholarly journals THE ROLE OF ACTIVE REGION CORONAL MAGNETIC FIELD IN DETERMINING CORONAL MASS EJECTION PROPAGATION DIRECTION

2015 ◽  
Vol 814 (1) ◽  
pp. 80 ◽  
Author(s):  
Rui Wang ◽  
Ying D. Liu ◽  
Xinghua Dai ◽  
Zhongwei Yang ◽  
Chong Huang ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Active Region ◽  
Coronal Mass Ejection ◽  
Coronal Magnetic Field ◽  
Propagation Direction ◽  
Mass Ejection

scholarly journals The exceptional aspects of the confined X-class flares of solar active region 2192

2015 ◽  
Vol 11 (S320) ◽  
pp. 60-63
Author(s):  
Julia K. Thalmann ◽  
Yang Su ◽  
Manuela Temmer ◽  
Astrid M. Veronig
Keyword(s):  
Magnetic Field ◽  
Active Region ◽  
Large Scale ◽  
Coronal Magnetic Field ◽  
Active Region Noaa ◽  
High Energies ◽  
The Past ◽  
Large Scale Magnetic Field ◽  
High Level ◽  
Mass Ejection

AbstractDuring late October 2014, active region NOAA 2192 caused an unusual high level of solar activity, within an otherwise weak solar cycle. While crossing the solar disk, during a period of 11 days, it was the source of 114 flares of GOES class C1.0 and larger, including 29 M- and 6 X-flares. Surprisingly, none of the major flares (GOES class M5.0 and larger) was accompanied by a coronal mass ejection, contrary to statistical tendencies found in the past. From modeling the coronal magnetic field of NOAA 2192 and its surrounding, we suspect that the cause of the confined character of the flares is the strong surrounding and overlying large-scale magnetic field. Furthermore, we find evidence for multiple magnetic reconnection processes within a single flare, during which electrons were accelerated to unusual high energies.

Effects of optimisation parameters on data-driven magnetofrictional modelling 

2021 ◽  
Author(s):  
Anshu Kumari ◽  
Daniel Price ◽  
Emilia Kilpua ◽  
Jens Pomoell ◽  
Farhad Daei
Keyword(s):  
Magnetic Field ◽  
Active Region ◽  
Large Scale ◽  
Magnetic Energy ◽  
Flux Rope ◽  
Coronal Magnetic Field ◽  
Early Evolution ◽  
Data Driven ◽  
Magnetic Field Magnitude ◽  
Mass Ejection

<p>The solar coronal magnetic field plays an important role in the formation, evolution, and dynamics of small and large-scale structures in the corona. Estimation of the coronal magnetic field, the ultimate driver of space weather, particularly in the ‘low’ and ‘middle’ corona, is presently limited due to practical difficulties. Data-driven time-dependent magnetofrictional modelling (TMFM) of active region magnetic fields has been proven as a tool to observe and study the corona. In this work, we present a detailed study of data-driven TMFM of active region 12473 to trace the early evolution of the flux rope related to the coronal mass ejection that occurred on 28 December 2015. Non-inductive electric field component in the photosphere is critical for energizing and introducing twist to the coronal magnetic field, thereby allowing unstable configurations to be formed. We estimate this component using an approach based on optimizing the injection of magnetic energy. We study the effects of these optimisation parameters on the data driven coronal simulations. By varying the free optimisation parameters, we explore the changes in flux rope formation and their early evolution, as well other parameters, e.g. axial flux, magnetic field magnitude.</p>

scholarly journals Photospheric magnetic field of an eroded-by-solar-wind coronal mass ejection

2016 ◽  
Vol 12 (S327) ◽  
pp. 67-70
Author(s):  
J. Palacios ◽  
C. Cid ◽  
E. Saiz ◽  
A. Guerrero
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Coronal Mass Ejection ◽  
Coronal Hole ◽  
Interplanetary Medium ◽  
Flux Rope ◽  
Magnetic Characteristics ◽  
Interplanetary Coronal Mass Ejection ◽  
Fast Wind ◽  
Mass Ejection

AbstractWe have investigated the case of a coronal mass ejection that was eroded by the fast wind of a coronal hole in the interplanetary medium. When a solar ejection takes place close to a coronal hole, the flux rope magnetic topology of the coronal mass ejection (CME) may become misshapen at 1 AU as a result of the interaction. Detailed analysis of this event reveals erosion of the interplanetary coronal mass ejection (ICME) magnetic field. In this communication, we study the photospheric magnetic roots of the coronal hole and the coronal mass ejection area with HMI/SDO magnetograms to define their magnetic characteristics.

scholarly journals Dependence of Coronal Mass Ejection Properties on Their Solar Source Active Region Characteristics and Associated Flare Reconnection Flux

2018 ◽  
Vol 865 (1) ◽  
pp. 4 ◽  
Author(s):  
Sanchita Pal ◽  
Dibyendu Nandy ◽  
Nandita Srivastava ◽  
Nat Gopalswamy ◽  
Suman Panda
Keyword(s):  
Active Region ◽  
Coronal Mass Ejection ◽  
Solar Source ◽  
Mass Ejection

Modeling the magnetic structure of CMEs in the inner heliosphere based on data-driven time-dependent simulations of active region evolution

2021 ◽  
Author(s):  
Jens Pomoell ◽  
Emilia Kilpua ◽  
Daniel Price ◽  
Eleanna Asvestari ◽  
Ranadeep Sarkar ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Active Region ◽  
Magnetic Structure ◽  
Interplanetary Space ◽  
Coronal Magnetic Field ◽  
Time Dependent ◽  
Data Driven ◽  
Dependent Data ◽  
Heliospheric Physics ◽  
The Magnetic Field

<p>Characterizing the detailed structure of the magnetic field in the active corona is of crucial importance for determining the chain of events from the formation to the destabilisation and subsequent eruption and propagation of coronal structures in the heliosphere. A comprehensive methodology to address these dynamic processes is needed in order to advance our capabilities to predict the properties of coronal mass ejections (CMEs) in interplanetary space and thereby for increasing the accuracy of space weather predictions. A promising toolset to provide the key missing information on the magnetic structure of CMEs are time-dependent data-driven simulations of active region magnetic fields. This methodology permits self-consistent modeling of the evolution of the coronal magnetic field from the emergence of flux to the birth of the eruption and beyond. </p><p>In this presentation, we discuss our modeling efforts in which time-dependent data-driven coronal modeling together with heliospheric physics-based modeling are employed to study and characterize CMEs, in particular their magnetic structure, at various stages in their evolution from the Sun to Earth. </p>

Focused transport of energetic particles along magnetic field lines draped around a coronal mass ejection

1992 ◽  
Vol 97 (A2) ◽  
pp. 1597 ◽  
Author(s):  
L. C. Tan ◽  
G. M. Mason ◽  
M. A. Lee ◽  
B. Klecker ◽  
F. M. Ipavich
Keyword(s):  
Magnetic Field ◽  
Coronal Mass Ejection ◽  
Energetic Particles ◽  
Field Lines ◽  
Mass Ejection
Sign in / Sign up

Export Citation Format

Share Document