E-Print Archive

There are 2658 abstracts currently viewable.
There is a problem with some abstracts that became corrupted following database issues. These will be restored as soon as possible.


Search:

Advanced Search
Options
Main Page Add New E-Print Submitter
Information
Feedback
News Help/FAQ About Preferences
Manage Key Phrase
Notification
Dynamics of Coronal Bright Points as seen by Sun Watcher using Active Pixel System detector and Image Processing (SWAP), Atmospheric Imaging Assembly AIA), and Helioseismic and Magnetic Imager (HMI) View all abstracts by submitter

Chandrahekhar Kalugodu   Submitted: 2012-06-05 04:48

The extit{Sun Watcher using Active Pixel system detector and Image Processing}(SWAP) on board the extit{PRoject for OnBoard Autonomy odash 2} (PROBA odash 2) spacecraft provides images of the solar corona in EUV channel centered at 174 AA. These data, together with extit{Atmospheric Imaging Assembly} (AIA) and the extit{Helioseismic and Magnetic Imager} (HMI) on board extit{Solar Dynamics Observatory} (SDO), are used to study the dynamics of coronal bright points. The evolution of the magnetic polarities and associated changes in morphology are studied using magnetograms and multi-wavelength imaging. The morphology of the bright points seen in low-resolution SWAP images and high-resolution AIA images show different structures, whereas the intensity variations with time show similar trends in both SWAP 174 and AIA 171 channels. We observe that bright points are seen in EUV channels corresponding to a magnetic-flux of the order of 1018 Mx. We find that there exists a good correlation between total emission from the bright point in several UV odash EUV channels and total unsigned photospheric magnetic flux above certain thresholds. The bright points also show periodic brightenings and we have attempted to find the oscillation periods in bright points and their connection to magnetic flux changes. The observed periods are generally long (10 odash 25 minutes) and there is an indication that the intensity oscillations may be generated by repeated magnetic reconnection.

Authors: K. Chandrashekhar, S. Krishna Prasad, D. Banerjee, B. Ravindra, Daniel B. Seaton
Projects: None

Publication Status: Accepted for publication in Solar Physics
Last Modified: 2012-06-05 10:40
Go to main E-Print page  Solar Coronal Loops Resolved by Hinode and SDO  Determination of the acceleration region size in a loop-structured solar flare   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
Internal-cycle variation of solar differential rotation
The standard flare model in three dimensions III. Slip-running reconnection properties
Global axis shape of magnetic clouds deduced from the distribution of their local axis orientation
Fine-scale Structures of Flux Ropes Tracked by Erupting Material
The influence of numerical resolution on coronal density in hydrodynamic models of impulsive heating
Spectral diagnostics with the SDO EVE flare lines
A revised radiometric calibration for the Hinode/EIS instrument
Disturbances in the U.S. electric grid associated with geomagnetic activity
Origin of Macrospicule and Jet in Polar Corona by A Small-scale Kinked Flux-Tube
Spatially Resolved Microwave Observations of Multiple Periodicities in a Flaring Loop
Changes in quasi-periodic variations of solar photospheric fields: precursor to the deep solar minimum in the cycle 23?
Pathways of large-scale magnetic couplings between coronal events
Superflares on Solar-Type Stars Observed with Kepler II. Photometric Variability of Superflare-Generating Stars : A Signature of Stellar Rotation and Starspots
A Challenging Solar Eruptive Event of 18 November 2003 and the Causes of the 20 November Geomagnetic Superstorm. I. Unusual History of an Eruptive Filament
Hi-C & AIA observations of transverse MHD waves in active regions
Geometric properties of acoustic waves generated by a point source in the solar-like interior: effects of acoustic cutoff frequency
Study of Failed CME Core Associated with Asymmetric Filament Eruption
Simulation of the Observed Coronal Kink Instability and Its Implications for the SDO/AIA
Investigating Two Successive Flux Rope Eruptions In A Solar Active Region
Observations of intensity oscillations in a prominence-like cool loop system as observed by SDO/AIA: evidence of multiple harmonics of fast magnetoacoustic waves

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