E-Print Archive

There are 3813 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
Extending Counter-Streaming Motion from an Active Region Filament to Sunspot Light Bridge View all abstracts by submitter

Haimin Wang   Submitted: 2017-12-19 21:15

We analyze the high-resolution observations from the 1.6m telescope at Big Bear Solar Observatory that cover an active region filament. Counter-streaming motions are clearly observed in the filament. The northern end of the counter-streaming motions extends to a light bridge, forming a spectacular circulation pattern around a sunspot, with clockwise motion in the blue wing and counterclockwise motion in the red wing as observed in Hα off-bands. The apparent speed of the flow is around 10 to 60 km s-1 in the filament, decreasing to 5 to 20 km s-1 in the light bridge. The most intriguing results are the magnetic structure and the counter-streaming motions in the light bridge. Similar to those in the filament, magnetic fields show a dominant transverse component in the light bridge. However, the filament is located between opposite magnetic polarities, while the light bridge is between strong fields of the same polarity. We analyze the power of oscillations with the image sequences of constructed Dopplergrams, and find that the filament's counter-streaming motion is due to physical mass motion along fibrils, while the light bridge's counter-streaming motion is due to oscillation in the direction along the line-of-sight. The oscillation power peaks around 4 minutes. However, the section of the light bridge next to the filament also contains a component of the extension of the filament in combination with the oscillation, indicating that some strands of the filament are extended to and rooted in that part of the light bridge.

Authors: Haimin Wang, Rui Liu, Qin Li, Chang Liu, Na Deng, Yan Xu, Ju Jing, Yuming Wang, Wenda Cao
Projects: BBSO/NST,SDO-HMI

Publication Status: ApJ Letters, Accepted
Last Modified: 2017-12-20 10:32
Go to main E-Print page  Active Region Photospheric Magnetic Properties Derived from Line-of-sight and Radial Fields  A Hydrodynamic Model of Alfv?nic Wave Heating in a Coronal Loop and its Chromospheric Footpoints  Edit Entry  Download Preprint  Submitter's Homepage 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 density compression ratio of shock fronts associated with coronal mass ejections
Evolution of Photospheric Flow and Magnetic Fields Associated with The 2015 June 22 M6.5 Flare
Spatially inhomogeneous acceleration of electrons in solar flares
Probing Twisted Magnetic Field Using Microwave Observations in an M Class Solar Flare on 11 February, 2014
The origin, early evolution and predictability of solar eruptions
Polar Field Correction for HMI Line-of-Sight Synoptic Data
Relationship between Intensity of White-Light Flares and Proton Flux of Solar Energetic Particles
Spectroscopic Observations of a Current Sheet in a Solar Flare
IRIS Observations of Spicules and Structures Near the Solar Limb
Strong Transverse Photosphere Magnetic Fields and Twist in Light Bridge Dividing Delta Sunspot of Active Region 12673
Simultaneous observation of a flux rope eruption and magnetic reconnection during an X-class solar flare
Spectroscopic diagnostics of the non-Maxwellian κ-distributions using SDO/EVE observations of the 2012 March 7 X-class flare
Transient rotation of photospheric vector magnetic fields associated with a solar flare
Three-dimensional Forward-fit Modeling of the Hard X-Ray and Microwave Emissions of the 2015 June 22 M6.5 Flare
Center-to-Limb Variability of Hot Coronal EUV Emissions During Solar Flares
A time dependent relation between EUV solar flare light-curves from lines with differing formation temperatures
Understanding Breaks in Flare X-Ray Spectra: Evaluation of a Cospatial Collisional Return-current Model
Solar energetic particles and radio burst emission
A quasi-periodic fast-propagating magnetosonic wave associated with the eruption of a magnetic flux rope
Two-step solar filament eruptions

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