E-Print Archive

There are 3928 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
Flux Rope Breaking and Formation of a Rotating Blowout Jet View all abstracts by submitter

Navin Chandra Joshi   Submitted: 2018-02-07 06:40

We analyzed a small flux rope eruption converted into a helical blowout jet in a fan-spine configuration using multi-wavelength observations taken by SDO, which occurred near the limb on 2016 January 9. In our study, first, we estimated the fan-spine magnetic configuration with the potential field calculation and found a sinistral small filament inside it. The filament along with the flux rope erupted upward and interacted with the surrounding fan- spine magnetic configuration, where the flux rope breaks in the middle section. We observed compact brightening, flare ribbons and post-flare loops underneath the erupting filament. The northern section of the flux rope reconnected with the surrounding positive polarity, while the southern section straightened. Next, we observed the untwisting motion of the southern leg, which was transformed into a rotating helical blowout jet. The sign of the helicity of the mini-filament matches the one of the rotating jet. This is consistent with the jet models presented by Adams et al. (2014) and Sterling et al. (2015). We focused on the fine thread structure of the rotating jet and traced three blobs with the speed of 60-120 km s-1, while the radial speed of the jet is approx 400 km s-1. The untwisting motion of the jet accelerated plasma upward along the collimated outer spine field lines, and it finally evolved into a narrow coronal mass ejection at the height of approx 9 Rsun . On the basis of the detailed analysis, we discussed clear evidence of the scenario of the breaking of the flux rope and the formation of the helical blowout jet in the fan-spine magnetic configuration.

Authors: Navin Chandra Joshi, Naoto Nishizuka, Boris Filippov, Tetsuya Magara, Andrey G. Tlatov
Projects: GOES X-rays,RHESSI,SDO-AIA,SDO-HMI,SoHO-LASCO

Publication Status: Accepted for publication in MNRAS Journal
Last Modified: 2018-02-08 16:19
Go to main E-Print page  Identification of multiple hard X-ray sources in solar flares: A Bayesian analysis of the February 20 2002 event  On-Orbit Performance of the Helioseismic and Magnetic Imager Instrument onboard the Solar Dynamics Observatory  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
Diagnostic Analysis of the Solar Proton Flares of September 2017 by Their Radio Bursts
Densities Probed by Coronal Type III Radio Burst Imaging
The Minimum Energy Principle Applied to Parker's Coronal Braiding and Nanoflaring Scenario
Eruptions from quiet Sun coronal bright points. I. Observations
Evolution of the transverse density structure of oscillating coronal loops inferred by forward modelling of EUV intensity
Non-stationary quasi-periodic pulsations in solar and stellar flares
Lost and found sunquake in the 6 September 2011 flare caused by beam electrons
Nonkinematic solar dynamo models with double-cell meridional circulation
Solar Kinetic Energy and Cross Helicity Spectra
Collective Study of Polar Crown Filaments in the Past Four Solar Cycles
Highly Ionized Calcium and Argon X-ray Spectra from a Large Solar Flare
Detecting the solar new magnetic flux regions on the base of vector magnetograms
A Truly Global EUV Wave From the SOL2017-09-10 X8.2 Solar Flare-CME Eruption
ALTERNATIVE ZEBRA-STRUCTURE MODELS IN SOLAR RADIO EMISSION
Photospheric Shear Flows in Solar Active Regions and Their Relation to Flare Occurrence
Linear Polarization Features in the Quiet-Sun Photosphere: Structure and Dynamics
Solar Microflares Observed by SphinX and RHESSI
Two Kinds of Dynamic Behavior in a Quiescent Prominence Observed by the NVST
Resistively-limited current sheet implosions in planar anti-parallel (1D) and null-point containing (2D) magnetic field geometries
Is It Small-scale Weak Magnetic Activity That Effectively Heats the Upper Solar Atmosphere?

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