Eruption of a Bifurcated Solar Filament

Zhu, Chunming; Alexander, David
January 2014
Solar Physics;Jan2014, Vol. 289 Issue 1, p279
Academic Journal
We study the partial eruption of a solar filament observed by the Solar Dynamics Observatory (SDO) and the Solar TErrestrial RElations Observatory-Ahead (STEREO-A) spacecraft on 9 May 2012. This filament was located in Active Region NOAA 11475 and consisted of two distinct branches, separated in height above the active region’s primary polarity-inversion line. For two days prior to the filament eruption, several threads of filament material were observed to connect the lower branch to the upper branch with evidence of a transfer of mass along them. The eruption commenced as a slow rise of the upper branch that began at 9 May 2012 23:40 UT, with the main eruption occurring half an hour later, producing a coronal mass ejection (CME). During the eruption, the upper branch was observed to rotate approximately 120 degrees in a counter-clockwise direction. We suggest that the mass transfer events also comprised a transfer of magnetic flux that led the upper branch of the filament to lose equilibrium as a result of a helical kink instability or torus instability.


Related Articles

  • The Topology and Behavior of Magnetic Fields Emerging at the Solar Photosphere. Lites, B. W. // Space Science Reviews;Dec2008, Vol. 144 Issue 1-4, p197 

    The nature of flux emerging through the surface layers of the Sun is examined in the light of new high-resolution magnetic field observations from the Hinode space mission. The combination of vector magnetic field data and visible-light imaging from Hinode support the hypothesis that active...

  • Bimodal Distribution of Magnetic Fields and Areas of Sunspots. Tlatov, Andrey G.; Pevtsov, Alexei A. // Solar Physics;Apr2014, Vol. 289 Issue 4, p1143 

    We applied automatic identification of sunspot umbrae and penumbrae to daily observations from the Helioseismic Magnetic Imager (HMI) on board the Solar Dynamics Observatory (SDO) to study their magnetic flux density ( B) and area ( A). The results confirm an already known logarithmic...

  • Subsurface Vorticity of Flaring versus Flare-Quiet Active Regions. Komm, R.; Ferguson, R.; Hill, F.; Barnes, G.; Leka, K. // Solar Physics;Feb2011, Vol. 268 Issue 2, p389 

    We apply discriminant analysis to 1023 active regions and their subsurface-flow parameters, such as vorticity and kinetic helicity density, with the goal of distinguishing between flaring and non-flaring active regions. We derive synoptic subsurface flows by analyzing GONG high-resolution...

  • Signatures of Emerging Subsurface Structures in Acoustic Power Maps of the Sun. Hartlep, T.; Kosovichev, A.; Zhao, J.; Mansour, N. // Solar Physics;Feb2011, Vol. 268 Issue 2, p321 

    We show that under certain conditions, subsurface structures in the solar interior can alter the average acoustic power observed at the photosphere above them. By using numerical simulations of wave propagation, we show that this effect is large enough for it to be potentially used for detecting...

  • Properties of Magnetic Neutral Line Gradients and Formation of Filaments. Karachik, Nina V.; Pevtsov, Alexei A. // Solar Physics;Mar2014, Vol. 289 Issue 3, p821 

    We investigate the gradients of magnetic fields across neutral lines (NLs) and compare their properties for NLs with and without chromospheric filaments. Our results show that there is a range of preferred magnetic field gradients where the filament formation is enhanced. On the other hand, a...

  • Fast approximate radiative transfer method for visualizing the fine structure of prominences in the hydrogen Hα line. Heinzel, P.; Gunár, S.; Anzer, U. // Astronomy & Astrophysics / Astronomie et Astrophysique;Jul2015, Vol. 579, p1 

    Aims. We present a novel approximate radiative transfer method developed to visualize 3D whole-prominence models with multiple fine structures using the hydrogen Hα spectral line. Methods. This method employs a fast line-of-sight synthesis of the Hα line profiles through the whole 3D...

  • Evolving Photospheric Flux Concentrations and Filament Dynamic Changes. Schmieder, B.; Aulanier, G.; Mein, P.; Ariste, A. Ló pez // Solar Physics;Nov2006, Vol. 238 Issue 2, p245 

    We analyze the role of weak photospheric flux concentrations that evolve in a filament channel, in the triggering of dynamic changes in the shape of a filament. The high polarimetric sensitivity of THEMIS allowed us to detect weak flux concentrations (few Gauss) associated with the filament...

  • Onset of the Kelvin-Helmholtz instability in partially ionized magnetic flux tubes. Martínez-Gómez, D.; Soler, R.; Terradas, J. // Astronomy & Astrophysics / Astronomie et Astrophysique;Jun2015, Vol. 578, p1 

    Context. Recent observations of solar prominences show the presence of turbulent flows that may be caused by Kelvin-Helmholtz instabilites (KHI). However, the observed flow velocities are below the classical threshold for the onset of KHI in fully ionized plasmas. Aims. We investigate the effect...

  • Sunspot Structure and Dynamics. Weiss, N. // Space Science Reviews;May2006, Vol. 124 Issue 1-4, p13 

    Sunspots are the most prominent magnetic features on the Sun but it is only within the last few years that the intricate structure of their magnetic fields has been resolved. In the penumbra the fields in bright and dark filaments differ in inclination by 30°. The field in the bright...


Read the Article


Sorry, but this item is not currently available from your library.

Try another library?
Sign out of this library

Other Topics