Subarcsecond Imaging of a Solar Active Region Filament With ALMA and IRIS

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Fältnamn	Indikatorer	Metadata
000		03316naa a2200457 4500
001		oai:DiVA.org:su-207227
003		SwePub
008		220711s2022 \| \|\|\|\|\|\|\|\|\|\|\|000 \|\|eng\|
024	7	a https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-2072272 URI
024	7	a https://doi.org/10.3389/fspas.2022.8981152 DOI
040		a (SwePub)su
041		a engb eng
042		9 SwePub
072	7	a ref2 swepub-contenttype
072	7	a art2 swepub-publicationtype
100	1	a Da Silva Santos, J. M.4 aut
245	1 0	a Subarcsecond Imaging of a Solar Active Region Filament With ALMA and IRIS
264		c 2022-05-23
264	1	b Frontiers Media SA,c 2022
338		a print2 rdacarrier
520		a Quiescent filaments appear as absorption features on the solar disk when observed in chromospheric lines and at continuum wavelengths in the millimeter (mm) range. Active region (AR) filaments are their small-scale, low-altitude analogues, but they could not be resolved in previous mm observations. This spectral diagnostic can provide insight into the details of the formation and physical properties of their fine threads, which are still not fully understood. Here, we shed light on the thermal structure of an AR filament using high-resolution brightness temperature (Tb) maps taken with ALMA Band 6 complemented by simultaneous IRIS near-UV spectra, Hinode/SOT photospheric magnetograms, and SDO/AIA extreme-UV images. Some of the dark threads visible in the AIA 304 Å passband and in the core of Mg ii resonance lines have dark (Tb << 5,000 K) counterparts in the 1.25 mm maps, but their visibility significantly varies across the filament spine and in time. These opacity changes are possibly related to variations in temperature and electron density in filament fine structures. The coolest Tb values (<< 5,000 K) coincide with regions of low integrated intensity in the Mg ii h and k lines. ALMA Band 3 maps taken after the Band 6 ones do not clearly show the filament structure, contrary to the expectation that the contrast should increase at longer wavelengths based on previous observations of quiescent filaments. The ALMA maps are not consistent with isothermal conditions, but the temporal evolution of the filament may partly account for this.
650	7	a NATURVETENSKAPx Fysikx Astronomi, astrofysik och kosmologi0 (SwePub)103052 hsv//swe
650	7	a NATURAL SCIENCESx Physical Sciencesx Astronomy, Astrophysics and Cosmology0 (SwePub)103052 hsv//eng
653		a Sun
653		a radio
653		a ultraviolet
653		a chromosphere
653		a active regions
653		a filaments
653		a prominences
700	1	a White, S. M.4 aut
700	1	a Reardon, K.4 aut
700	1	a Cauzzi, G.4 aut
700	1	a Gunár, S.4 aut
700	1	a Heinzel, P.4 aut
700	1	a Leenaarts, Jorritu Stockholms universitet,Institutionen för astronomi4 aut0 (Swepub:su)jleen
710	2	a Stockholms universitetb Institutionen för astronomi4 org
773	0	t Frontiers in Astronomy and Space Sciencesd : Frontiers Media SAg 9q 9x 2296-987X
856	4	u https://doi.org/10.3389/fspas.2022.898115y Fulltext
856	4 8	u https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-207227
856	4 8	u https://doi.org/10.3389/fspas.2022.898115

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Av lärosätet: Stockholms universitet

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