2019
DOI: 10.3847/1538-4357/ab2635
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Properties of the Umbral Filament Observed in Active Region NOAA 12529

Abstract: Recent observations of the solar photosphere revealed the presence of elongated filamentary bright structures inside sunspot umbrae, called umbral filaments (UFs). These features differ in morphology, magnetic configuration, and evolution from light bridges that are usually observed to intrude in sunspots. To characterize an UF observed in the umbra of the giant leading sunspot of active region NOAA 12529, we analyze high-resolution observations taken in the photosphere with the spectropolarimeter aboard the H… Show more

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Cited by 23 publications
(31 citation statements)
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“…The continuum contrast in a large quiet-Sun region increases from 6.5%, 6.2%, and 6.3% for the three original maps to 13.9%, 12.8%, and 13% in the deconvolved maps, respectively. These values are similar to those obtained in previous works (Quintero Noda et al 2015Guglielmino et al 2019).…”
Section: Sdo/hmi and Hinode/sp Datasetssupporting
confidence: 92%
See 1 more Smart Citation
“…The continuum contrast in a large quiet-Sun region increases from 6.5%, 6.2%, and 6.3% for the three original maps to 13.9%, 12.8%, and 13% in the deconvolved maps, respectively. These values are similar to those obtained in previous works (Quintero Noda et al 2015Guglielmino et al 2019).…”
Section: Sdo/hmi and Hinode/sp Datasetssupporting
confidence: 92%
“…We normalized these measurements by the average intensity in the continuum of the Fe i 630.2 nm line pair in a large quiet-Sun region placed in the upper part of the Hinode/SP FOV. We also corrected the perturbation introduced by the point spread function (PSF) of the telescope by applying the regularization method proposed by Ruiz Cobo & Asensio Ramos (2013) and used in Quintero Noda et al (2015Noda et al ( , 2016, Guglielmino et al (2018Guglielmino et al ( , 2019. This method is based on a principal component decomposition of the Stokes profiles.…”
Section: Sdo/hmi and Hinode/sp Datasetsmentioning
confidence: 99%
“…And a strong horizontal magnetic field is predicted to exist along the penumbral filament. As for umbral filaments, they are unusual elongated filamentary bright structures with strong horizontal fields within sunspot umbrae, and are interpreted as the photospheric manifestation of a flux rope hanging above the umbra (Guglielmino et al 2019).…”
Section: Introductionmentioning
confidence: 99%
“…Inside the dark sunspots, many small-scale structures with inhomogeneous brightness have been studied, such as umbral dots (Beckers & Schröter 1968;Sobotka et al 1997;Riethmüller et al 2008;Goodarzi et al 2018), light bridges (Muller 1979;Lites et al 1991;Sobotka et al 1994;Leka 1997;Berger & Berdyugina 2003;Katsukawa et al 2007a;Rouppe van der Voort et al 2010;Lagg et al 2014;Felipe et al 2017;Wang et al 2018;Durán et al 2020), penumbral filaments (Muller 1973;Schlichenmaier et al 1998;Scharmer et al 2002;Ichimoto et al 2007; Movies associated to Figs. 1, 2, and 4 are available at https:// www.aanda.org 2007; Su et al 2010;Tiwari et al 2013), and umbral filaments (Kleint & Sainz Dalda 2013;Guglielmino et al 2017Guglielmino et al , 2019. Umbral dots are bright dot-like features embedded in the umbral background, and their number rapidly increases with decreasing diameter (Sobotka et al 1997).…”
Section: Introductionmentioning
confidence: 99%
“…This Evershed flow (see Solanki 2003 for a review) was detected more than a century ago (Evershed 1909). In the past decade, there have been a few reports of peculiar flows directed toward the umbra (Kleint & Sainz Dalda 2013;Louis et al 2014;Siu-Tapia et al 2017;Guglielmino et al 2017Guglielmino et al , 2019Louis et al 2020). These socalled counter Evershed flows (CEFs) have also been observed in one magnetohydrodynamic (MHD) simulation (Siu-Tapia et al 2018).…”
Section: Introductionmentioning
confidence: 99%