TY - JOUR
T1 - RELATIONSHIP between CHROMOSPHERIC EVAPORATION and MAGNETIC FIELD TOPOLOGY in AN M-CLASS SOLAR FLARE
AU - Sadykov, Viacheslav M.
AU - Kosovichev, Alexander G.
AU - Sharykin, Ivan N.
AU - Zimovets, Ivan V.
AU - Dominguez, Santiago Vargas
N1 - Funding Information:
The BBSO operation is supported by NJIT, US NSF AGS-1250818, and NASA NNX13AG14G grants, and the NST operation is partly supported by the Korea Astronomy and Space Science Institute and Seoul National University and by the strategic priority research program of CAS with grant No. XDB09000000. IRIS is a NASA small explorer mission developed and operated by LMSAL with mission operations executed at the NASA Ames Research Center and major contributions to downlink communications funded by ESA and the Norwegian Space Centre. The authors thank NASAs SDO HMI team for the availability of the high-quality scientific data. The authors also thank the anonymous referee for valuable comments. The work was partially supported by NASA grants NNX14AB68G, NNX14AB70G, and NNX11AO736; NSF grant AGS-1250818; RFBR grants 15-32-21078 and 16-32-00462; and an NJIT grant.
Publisher Copyright:
© 2016. The American Astronomical Society. All rights reserved.
PY - 2016/9/1
Y1 - 2016/9/1
N2 - 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 Hα 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.
AB - 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 Hα 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.
KW - Sun: UV radiation
KW - Sun: activity
KW - Sun: chromosphere
KW - Sun: flares
KW - Sun: magnetic fields
KW - techniques: spectroscopic
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U2 - 10.3847/0004-637X/828/1/4
DO - 10.3847/0004-637X/828/1/4
M3 - Article
AN - SCOPUS:84987788948
SN - 0004-637X
VL - 828
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 4
ER -