SDO
2018-2019 ApJ2018, 864, L4; 2018, 868,
L33; 2019, 884, 34formed, and they would resemble the prominence
formationmodels (Pneuman 1983; Kaneko & Yokoyama 2015).
How-ever, the condensation remains for only a short time, and
thenrains down to the chromosphere when the dips are broken bythe
successive MR. In this Letter, we show that the MR and
thecondensation cannot be treated separately, but that
plasmacondensation naturally arises during the MR process.
The authors are indebted to the SDO team for providing thedata.
The work is supported by the National Foundations ofChina
(11673034, 11533008, 11790304, and 11773039), andKey Programs of
the Chinese Academy of Sciences (QYZDJ-SSW-SLH050). L.C. received
funding from the EuropeanUnion’s Horizon 2020 Research and
Innovation Programmeunder the Marie Sklodowska-Curie grant
agreement No.707837. This project supported by the Specialized
ResearchFund for Shandong Provincial Key Laboratory.
ORCID iDs
Leping Li https://orcid.org/0000-0001-5776-056XChun Xia
https://orcid.org/0000-0002-7153-4304Hongqiang Song
https://orcid.org/0000-0001-5705-661X
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Figure 6. Schematic diagrams of the MR and coronal condensation.
In (a)–(c),the gray thick lines denote the solar limb. The green,
blue, and green-blue linesseparately show the magnetic field lines
of loops L1, L2, L3, and L4, whosedirections are marked by the red
arrows. In (a), the green arrow denotes the dipof loops L1 and also
the moving direction. In (b) and (c), the purple stars showthe MR
between loops L1 and L2. The green, yellow, and red patches
indicatethe AIA 171 Å, 131 Å, and 304 Åplasma, respectively.
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The Astrophysical Journal Letters, 864:L4 (7pp), 2018 September
1 Li et al.
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