E-Print Archive

There are 3882 abstracts currently viewable.


Search:

Advanced Search
Options
Main Page Add New E-Print Submitter
Information
Feedback
News Help/FAQ About Preferences
Manage Key Phrase
Notification
Evolution of Photospheric Flow and Magnetic Fields Associated with The 2015 June 22 M6.5 Flare View all abstracts by submitter

Jiasheng Wang   Submitted: 2018-01-16 10:12

The evolution of photospheric flow and magnetic fields before and after flares can provide important information regarding the flare triggering and back reaction processes. However, such studies on the flow field are rare due to the paucity of high-resolution observations covering the entire flaring period. Here we study the structural evolution of penumbra and shear flows associated with the 2015 June 22 M6.5 flare in NOAA AR 12371, using high-resolution imaging observation in the TiO band taken by the 1.6 m Goode Solar Telescope at Big Bear Solar Observatory, with the aid of the differential affine velocity estimator method for flow tracking. The accompanied photospheric vector magnetic field changes are also analyzed using data from the Helioseismic and Magnetic Imager. As a result, we found, for a penumbral segment in the negative field adjacent to the magnetic polarity inversion line (PIL), an enhancement of penumbral flows (up to an unusually high value of ~2 km s-1) and extension of penumbral fibrils after the first peak of the flare hard X-ray (HXR) emission. We also found an area at the PIL, which is co-spatial with a precursor brightening kernel, exhibits a gradual increase of shear flow velocity (up to ~0.9 km s-1) after the flare. The enhancing penumbral and shear flow regions are also accompanied by an increase of horizontal field and a decrease of magnetic inclination angle(measured from the solar surface). These results are discussed in the context of the theory of back reaction of coronal restructuring on the photosphere as a result of flare energy release.

Authors: Jiasheng Wang, Chang Liu, Na deng, Haimin Wang
Projects: BBSO/NST

Publication Status: accepted
Last Modified: 2018-01-16 11:09
Go to main E-Print page  The density compression ratio of shock fronts associated with coronal mass ejections  Spatially inhomogeneous acceleration of electrons in solar flares  Edit Entry  Download Preprint  Delete Entry 

Key
Go to main E-Print pageGo to main E-Print page.
Previous AbstractPrevious Abstract.
Next AbstractNext Abstract.
Download PreprintDownload Preprint.
Submitter's HomepageSubmitters Homepage.
Edit EntryEdit Entry.
View All Abstracts By SubmitterView all abstracts by submitter.
Delete AbstractDelete abstract.

Latest Entries
The origin of the modulation of the radio emission from the solar corona by a fast magnetoacoustic wave
Indirect solar wind measurements using archival cometary tail observations
Helium abundance and speed difference between helium ions and protons in the solar wind from coronal holes, active regions, and quiet Sun
Always a Farm Boy
Effect of transport coefficients on excitation of flare-induced standing slow-mode waves in coronal loops
Study of Three-dimensional Magnetic Structure and the Successive Eruptive Nature of Active Region 12371
Statistical study of magnetic non-potential measures in confined and eruptive flares
Quasi-periodic Counter-propagating Fast Magnetosonic Wave Trains from Neighboring Flares: SDO/AIA Observations and 3D MHD Modeling
Negative flare in the He I 10830 Å line in facula
Time resolved spectroscopic observations of an M-dwarf flare star EV Lac during a flare
Two Episodes of Magnetic Reconnections During a Confined Circular-ribbon Flare
Enhanced stellar activity for slow antisolar differential rotation?
Quasi-periodic pulsations in the most powerful solar flare of Cycle 24
GONG Catalog of Solar Filament Oscillations Near Solar Maximum
Chromospheric response during the precursor and the main phase of a B6.4 flare on August 20, 2005
Unambiguous Evidence of Coronal Implosions During Solar Eruptions and Flares
Two Types of Long-duration Quasi-static Evolution of Solar Filaments
Oscillations of cometary tails: a vortex shedding phenomenon?
Observations of Running Penumbral Waves Emerging in a Sunspot
Reconnection in the Post-Impulsive Phase of Solar Flares

Related Pages
MSU Solar Physics.
Max Millennium Science Mail Archive.
Max Millennium Message of the Day Mail Archive.
Max Millennium Flare Catalog

Archive Maintainer
Alisdair Davey



© 2003 Solar Physics Group - Montana State University