Emergence of Small-Scale Magnetic Loops in the Quiet-Sun Internetwork

By Rebecca Centeno, Héctor Socas-Navarro, B. Lites, M. Kubo, Z. Frank, R. Shine, T. Tarbell, A. Title, K. Ichimoto, S. Tsuneta and 4 more. 2007

169 citations recorded by the source corpus.

We study the emergence of magnetic flux at very small spatial scales (less than 2'') in the quiet-Sun internetwork. To this aim, a time series of spectropolarimetric maps was taken at disk center using the instrument SP/SOT on board Hinode. The LTE inversion of the full Stokes vector measured in the Fe I 6301 and 6302 Å lines allows us to retrieve the magnetic flux and topology in the region of study. In the example presented here, the magnetic flux emerges within a granular structure. The horizontal magnetic field appears prior to any significant amount of vertical field. As time goes on, the traces of the horizontal field disappear, while the vertical dipoles drift—carried by the plasma motions—toward the surrounding intergranular lanes. These events take place within typical granulation timescales.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/0858f4643b3289999fbbbc89b8cf8aa233c3bcbf

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Citations in the corpus

Solar Surface Emerging Flux Regions: A Comparative Study of Radiative MHD Modeling and Hinode SOT Observations (2008, background): “Whereas Centeno et al. (2007) and Orozco Suárez et al. (2008) studied flux emergence in a quiet Sun environment, Ishikawa et al. (2008) and Otsuji et al. (2007) examined flux emergence in a plage region and near sunspot penumbrae, respectively.”
The Horizontal Magnetic Flux of the Quiet-Sun Internetwork as Observed with the Hinode Spectro-Polarimeter (2008, background): “Ser. 154, The Tenth Cambridge Workshop on Cools Stars, Stellar Systems and the Sun, ed.”
Magnetic Flux Transport at the Solar Surface (2014, background): “The toroidal field concentrated there becomes buoyantly unstable once it reaches a critical strength and a part of it, thought to be in the form of magnetic flux tubes, rises through the convection zone until it reaches the solar surface (Parker 1955; Choudhuri and Gilman 1987; Schüssler et al.…”
The magnetic field in the solar atmosphere (2014, background): “Most commonly, loop footpoints move apart almost linearly with time (Centeno et al. 2007).”
The Magnetic Landscape of the Sun's Polar Region (2008, background): “The transient horizontal magnetic field discovered in the polar region appears to have properties similar to those found in the quiet Sun and in active regions (Lites et al. 2008; Centeno et al. 2007; Orozco Suárez et al. 2007a; Ishikawa et al. 2008; Ishikawa & Tsuneta 2009).”
Solar Fine-Scale Structures. I. Spicules and Other Small-Scale, Jet-Like Events at the Chromospheric Level: Observations and Physical Parameters (2012, methodology): “Recently, Centeno et al. (2007) using observations obtained with Solar Optical Telescope Spectropolarimeter (SOT/SP) on board the Hinode spacecraft presented clear evidence of an emerging IN magnetic loop showing strong horizontal magnetic signal and traces of vertical opposite polarities on each…”
ORBITAL MOTION OF HR 8799 b, c, d USING HUBBLE SPACE TELESCOPE DATA FROM 1998: CONSTRAINTS ON INCLINATION, ECCENTRICITY, AND STABILITY (2011, background): “The idea of a small-scale turbulent dynamo operating in the quiet sun photosphere received strong observational support when turbulent magnetic ﬁelds were discovered with with Hinode instruments (Centeno et al. 2007; Lites et al. 2008; Orozco Suarez et al. 2008; Sch¨ussler & V¨ogler 2008).”
SIMULATION OF THE FORMATION OF A SOLAR ACTIVE REGION (2010, result): “…lines have been undulated by their interaction with the convective downflows as is consistent with observations (see e.g. Pariat et al. 2004; Cheung et al. 2007; Centeno et al. 2007; Mart́ınez González et al. 2007; Mart́ınez González & Bellot Rubio 2009; Cheung et al. 2008; Ishikawa et al. 2010).”