RELATIONSHIP BETWEEN CHROMOSPHERIC EVAPORATION AND MAGNETIC FIELD TOPOLOGY IN AN M-CLASS SOLAR FLARE

ABSTRACT Chromospheric evaporation is observed as Doppler blueshift during solar flares. It plays a key role in the dynamics and energetics of solar flares; however, its mechanism is still unknown. In this paper, we present a detailed analysis of spatially resolved multi-wavelength observations of c...

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Bibliographic Details
Published in:The Astrophysical journal 2016-09, Vol.828 (1), p.4-4
Main Authors: Sadykov, Viacheslav M, Kosovichev, Alexander G, Sharykin, Ivan N, Zimovets, Ivan V, Dominguez, Santiago Vargas
Format: Article
Language:English
Subjects:
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
CHROMOSPHERE
Delay
EVAPORATION
Flares
INTERFACES
LAYERS
MAGNETIC FIELDS
Magnetic properties
PLASMA
RED SHIFT
RESOLUTION
Ribbons
SOLAR FLARES
SPATIAL DISTRIBUTION
SPECTROMETERS
SUN
Sun: activity
Sun: chromosphere
Sun: flares
Sun: magnetic fields
Sun: UV radiation
techniques: spectroscopic
TELESCOPES
Topology
ULTRAVIOLET RADIATION
WAVELENGTHS
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Summary:ABSTRACT Chromospheric evaporation is observed as Doppler blueshift during solar flares. It plays a key role in the dynamics and energetics of solar flares; however, its mechanism is still unknown. In this paper, we present a detailed analysis of spatially resolved multi-wavelength observations of chromospheric evaporation during an M 1.0-class solar flare (SOL2014-06-12T21:12) using data from NASA's Interface Region Imaging Spectrograph and HMI/SDO (the Helioseismic and Magnetic Imager on board the Solar Dynamics Observatory), and high-resolution observations from VIS/NST (the Visible Imaging Spectrometer at the New Solar Telescope). The results show that the averaged over the flare region Fe xxi blueshift of the hot (107 K) evaporating plasma is delayed relative to the C ii redshift of the relatively cold (104 K) chromospheric plasma by about one minute. The spatial distribution of the delays is not uniform across the region and can be as long as two minutes in several zones. Using vector magnetograms from HMI, we reconstruct the magnetic field topology and the quasi-separatrix layer, and find that the blueshift delay regions as well as the H flare ribbons are connected to the region of the magnetic polarity inversion line (PIL) and an expanding flux rope via a system of low-lying loop arcades with a height of 4.5 Mm. As a result, the chromospheric evaporation may be driven by the energy release in the vicinity of PIL, and has the observed properties due to a local magnetic field topology.
ISSN:0004-637X
1538-4357
DOI:10.3847/0004-637X/828/1/4