Spectroscopic investigations of a filament reconnecting with coronal loops during a two-ribbon solar flare

Result code in IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F25%3A00637038" target="_blank" >RIV/67985815:_____/25:00637038 - isvavai.cz</a>

Result on the web

<a href="https://hdl.handle.net/11104/0368001" target="_blank" >https://hdl.handle.net/11104/0368001</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/202554011" target="_blank" >10.1051/0004-6361/202554011</a>

Result language

angličtina

Original language name

Spectroscopic investigations of a filament reconnecting with coronal loops during a two-ribbon solar flare

Original language description

In the standard 2D model of eruption, the eruption of a magnetic flux rope is associated with magnetic reconnection occurring beneath it. However, in 3D, additional reconnection geometries are possible, in particular the AR-RF, where external reconnection involving the overlying arcades (A) and erupting flux rope (R) turns into another arcade and a flare loop (F). This process results in the drifting of the legs of the erupting flux rope. Aims. We investigate spectroscopic signatures of such AR-RF reconnection occurring in an erupting filament reconnecting with coronal arcades during a weak B3.2-class two-ribbon flare. Methods. We examined the evolution of the erupting filament eruption using imaging observations by the Atmospheric Imaging Assembly (AIA) as well as both imaging and spectroscopic observations by the Interface Region Imaging Spectrograph (IRIS). Results. As the filament rises into the corona, it reconnects with the surrounding arcade of coronal loops with localized brightenings, resulting in the disappearance of the coronal loops and formation of a hot flux rope, showing a slipping motion of its footpoints that extends to the previous footpoints of the coronal loops (AR-RF reconnection), as was predicted by the 3D extensions to the standard solar flare model. These brightenings are accompanied by the presence of strong blueshifts in both the IRIS Si IV and Mg II lines, up to approximate to 200 km s(-1). The lines are also extremely wide, with nonthermal widths above 100 km s(-1). Furthermore, a strongly non-Gaussian profile of the most blueshifted component is detected at the start of the AR-RF reconnection, indicating the presence of accelerated particles and magnetohydrodynamic turbulence, and associated with the appearance of hot plasma in the AIA 94 Å passband. Results. For the first time, an observation has been reported in which the IRIS slit successfully captures AR-RF reconnection between a filament and overlying arcades, resulting in strong blueshifts and very broad line profiles.

Czech name

—

Czech description

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Type

J_imp - Article in a specialist periodical, which is included in the Web of Science database

CEP classification

—

OECD FORD branch

10308 - Astronomy (including astrophysics,space science)

Project

Result was created during the realization of more than one project. More information in the Projects tab.

Continuities

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Publication year

2025

Confidentiality

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Name of the periodical

Astronomy & Astrophysics

ISSN

0004-6361

e-ISSN

1432-0746

Volume of the periodical

698

Issue of the periodical within the volume

June

Country of publishing house

FR - FRANCE

Number of pages

14

Pages from-to

A301

UT code for WoS article

001512479700015

EID of the result in the Scopus database

2-s2.0-105009010987