THE 2011 FEBRUARY 15 X2 FLARE, RIBBONS, CORONAL FRONT, AND MASS EJECTION: INTERPRETING THE THREE-DIMENSIONAL VIEWS FROM THESOLAR DYNAMICS OBSERVATORYANDSTEREOGUIDED BY MAGNETOHYDRODYNAMIC FLUX-ROPE MODELING

AbstractWe report observations of a filament eruption, two-ribbon flare, and coronal mass ejection (CME) that occurred in Active Region NOAA 10898 on 6 July 2006. The filament was located South of a strong sunspot that dominated the region. In the evolution leading up to the eruption, and for some time after it, a counter-clockwise rotation of the sunspot of about 30 degrees was observed. We suggest that the rotation triggered the eruption by progressively expanding the magnetic field above the filament. To test this scenario, we study the effect of twisting the initially potential field overlying a pre-existing flux rope, using three-dimensional zero–β MHD simulations. We consider a magnetic configuration whose photospheric flux distribution and coronal structure is guided by the observations and a potential field extrapolation. We find that the twisting leads to the expansion of the overlying field. As a consequence of the progressively reduced magnetic tension, the flux rope quasi-statically adapts to the changed environmental field, rising slowly. Once the tension is sufficiently reduced, a distinct second phase of evolution occurs where the flux rope enters an unstable regime characterized by a strong acceleration. Our simulation thus suggests a new mechanism for the triggering of eruptions in the vicinity of rotating sunspots.

Download Full-text

Evolution of the 5 January 2005 CMEs associated with eruptive filaments in inner heliosphere

Proceedings of the International Astronomical Union ◽

10.1017/s1743921313011691 ◽

2013 ◽

Vol 8 (S300) ◽

pp. 491-492 ◽

Cited By ~ 1

Author(s):

Rahul Sharma ◽

Nandita Srivastava ◽

Bernard V. Jackson ◽

D. Chakrabarty ◽

Nolan Luckett ◽

...

Keyword(s):

Three Dimensional ◽

Flux Rope ◽

Recovery Phase ◽

Magnetic Clouds ◽

Reconstruction Technique ◽

Solar Mass ◽

Magnetic Structures ◽

Solar Mass Ejection Imager ◽

Mass Ejection ◽

Filament Plasma

AbstractOn 5 January 2005, SoHO/LASCO observed two CMEs associated with eruptive filaments with different initial velocities and acceleration. The second CME accelerates much faster than the previous and the resulting interaction has been revealed in in-situ spacecraft measurements by the presence of magnetic holes at the border of the two distinct magnetic clouds. At their interface region, these magnetic clouds have embedded filament plasma that shows complex magnetic structures with a distinct magnetic flux rope configuration; these have been modeled by the Grad - Shafranov reconstruction technique. The geomagnetic consequences of these structures have been associated with substorms in recovery phase of a storm and detailed analysis is presented in Sharma et al. (2013). In the present paper, we highlight the comparison of shape and extent of two filament plasma remnants in magnetic clouds as revealed by three - dimensional (3D) reconstruction and analysis from the Solar Mass Ejection Imager (SMEI) data. The results provide an overview of the two eruptive filaments on 5 January 2005 and their interplanetary propagation.

Download Full-text

Observations for the Role of Flux rope Eruption in a Geoeffective Solar Flare

JOURNAL OF ADVANCES IN PHYSICS ◽

10.24297/jap.v4i2.6965 ◽

2014 ◽

Vol 4 (2) ◽

pp. 555-564

Author(s):

A.M Aslam

Keyword(s):

Solar Flare ◽

Flux Rope ◽

Magnetic Configuration ◽

Solar Dynamics Observatory ◽

Multi Wavelength ◽

Solar Dynamics ◽

Halo Coronal Mass Ejection ◽

Mass Ejection ◽

The Waves

On September 24, 2011 a solar flare of M 7.1 class was released from the Sun. The flare was observed by most of the space and ground based observatories in various wavebands. We have carried out a study of this flare to understand its causes on Sun and impact on earth. The flare was released from NOAA active region AR 11302 at 12:33 UT. Although the region had already produced many M class flares and one X- class flare before this flare, the magnetic configuration was not relaxed and still continued to evolve as seen from HMI observations. From the Solar Dynamics Observatory (SDO) multi-wavelength (131 Ã…, 171 Ã…, 304 Ã… and 1600Ã…) observations we identified that a rapidly rising flux rope triggered the flare although HMI observations revealed that magnetic configuration did not undergo a much pronounced change. The flare was associated with a halo Coronal Mass Ejection (CME) as recorded by LASCO/SOHO Observations. The flare associated CME was effective in causing an intense geomagnetic storm with minimum Dst index -103 nT. A radio burst of type II was also recorded by the WAVES/WIND. In the present study attempt is made to study the nature of coupling between solar transients and geospace.

Download Full-text

Flux Rope Model of the 2003 October 28–30 Coronal Mass Ejection and Interplanetary Coronal Mass Ejection

The Astrophysical Journal ◽

10.1086/500822 ◽

2006 ◽

Vol 642 (1) ◽

pp. 541-553 ◽

Cited By ~ 32

Author(s):

J. Krall ◽

V. B. Yurchyshyn ◽

S. Slinker ◽

R. M. Skoug ◽

J. Chen

Keyword(s):

Coronal Mass Ejection ◽

Flux Rope ◽

Interplanetary Coronal Mass Ejection ◽

Mass Ejection

Download Full-text

Three-dimensional MHD modeling of the solar wind structures associated with 13 December 2006 coronal mass ejection

Journal of Geophysical Research Atmospheres ◽

10.1029/2009ja014167 ◽

2009 ◽

Vol 114 (A10) ◽

pp. n/a-n/a ◽

Cited By ~ 40

Author(s):

R. Kataoka ◽

T. Ebisuzaki ◽

K. Kusano ◽

D. Shiota ◽

S. Inoue ◽

...

Keyword(s):

Solar Wind ◽

Coronal Mass Ejection ◽

Three Dimensional ◽

Mhd Modeling ◽

Mass Ejection

Download Full-text

The Formation of a Cavity in a 3D Flux Rope

Proceedings of the International Astronomical Union ◽

10.1017/s1743921313010880 ◽

2013 ◽

Vol 8 (S300) ◽

pp. 147-150 ◽

Cited By ~ 1

Author(s):

Donald Schmit ◽

Sarah Gibson

Keyword(s):

Ad Hoc ◽

Numerical Models ◽

Dimensional Space ◽

Three Dimensional ◽

Flux Rope ◽

Multiple Structures ◽

Field Lines ◽

Hydrostatic Balance ◽

Distinct Field ◽

Three Dimensional Space

AbstractThere are currently no three dimensional numerical models which describe the magnetic and energetic formation of prominences self-consistently. Consequently, there has not been significant progress made in understanding the connection between the dense prominence plasma and the coronal cavity. We have taken an ad-hoc approach to understanding the energetic implications of the magnetic models of prominence structure. We extract one dimensional magnetic field lines from a 3D MHD model of a flux rope and solve for hydrostatic balance along these field lines incorporating field-aligned thermal conduction, uniform heating, and radiative losses. The 1D hydrostatic solutions for density and temperature are then mapped back into three dimensional space, which allows us to consider the projection of multiple structures. We find that the 3D flux rope is composed of several distinct field line types. A majority of the flux rope interior field lines are twisted but not dipped. These field lines are density-reduced relative to unsheared arcade field lines. We suggest the cavity may form along these short interior field lines which are surrounded by a sheath of dipped field lines. This geometric arrangement would create a cavity on top of a prominence, but the two structures would not share field lines or plasma.

Download Full-text

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

Proceedings of the International Astronomical Union ◽

10.1017/s1743921317001077 ◽

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.

Download Full-text