skip to main content

SciTech ConnectSciTech Connect

Title: Confined partial filament eruption and its reformation within a stable magnetic flux rope

We present observations of a confined partial eruption of a filament on 2012 August 4, which restores its initial shape within ≈2 hr after eruption. From the Global Oscillation Network Group Hα observations, we find that the filament plasma turns into dynamic motion at around 11:20 UT from the middle part of the filament toward the northwest direction with an average speed of ≈105 km s{sup –1}. A little brightening underneath the filament possibly shows the signature of low-altitude reconnection below the filament eruptive part. In Solar Dynamics Observatory/Atmospheric Imaging Assembly 171 Å images, we observe an activation of right-handed helically twisted magnetic flux rope that contains the filament material and confines it during its dynamical motion. The motion of cool filament plasma stops after traveling a distance of ≈215 Mm toward the northwest from the point of eruption. The plasma moves partly toward the right foot point of the flux rope, while most of the plasma returns after 12:20 UT toward the left foot point with an average speed of ≈60 km s{sup –1} to reform the filament within the same stable magnetic structure. On the basis of the filament internal fine structure and its position relative to themore » photospheric magnetic fields, we find filament chirality to be sinistral, while the activated enveloping flux rope shows a clear right-handed twist. Thus, this dynamic event is an apparent example of one-to-one correspondence between the filament chirality (sinistral) and the enveloping flux rope helicity (positive). From the coronal magnetic field decay index, n, calculation near the flux rope axis, it is evident that the whole filament axis lies within the domain of stability (i.e., n < 1), which provides the filament stability despite strong disturbances at its eastern foot point.« less
Authors:
; ;  [1] ; ;  [2] ;  [3] ;  [4] ;  [5]
  1. Aryabhatta Research Institute of Observational Sciences (ARIES), Manora Peak, Nainital 263 002, Uttarakhand (India)
  2. Department of Physics, Indian Institute of Technology (Banaras Hindu University), Varanasi 221005 (India)
  3. Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation, Russian Academy of Sciences, Troitsk, Moscow (Russian Federation)
  4. Department of Physics, D.S.B. Campus, Kumaun University, Nainital 263 002, Uttarakhand (India)
  5. California State University Northridge, 18111 Nordhoff Street, Northridge, CA 91330 (United States)
Publication Date:
OSTI Identifier:
22356880
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal; Journal Volume: 787; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ALTITUDE; CHIRALITY; DECAY; DISTANCE; DISTURBANCES; ERUPTION; FINE STRUCTURE; HELICITY; MAGNETIC FIELDS; MAGNETIC FLUX; OSCILLATIONS; PLASMA FILAMENT; STABILITY; SUN; VELOCITY