The Solar Internetwork. III. Unipolar versus Bipolar Flux Appearance

Gošić, Milan; Rubio, L. R. Bellot; Cheung, Mark C. M.; Suárez, D. Orozco; Katsukawa, Y.; Iniesta, J. C. del Toro

doi:10.3847/1538-4357/ac37be

Cited by 16 publications

(29 citation statements)

References 65 publications

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“…However, the morphology of the emerging fields resembles that of ephemeral regions. Therefore, the fields analyzed here support the idea of a continuous flux and size distribution of magnetic elements in the solar IN (Gošić 2015).…”

Section: Discussionsupporting

confidence: 81%

“…It brings much larger flux features to the surface with upflows of up to −1 km s −1 . Magnetic elements continue appearing in this region for the next ∼ 60 minutes, which is not uncommon for IN fields (Gošić 2015;Gošić et al 2016). The strongest flux patches in this cluster can be identified and tracked for the entire duration of the magnetogram sequence, despite interacting with other magnetic elements.…”

Section: Criteria For Identificationmentioning

confidence: 76%

“…Moreover, the majority of elements that constitute the clusters-those with fluxes below 10 18 Mx-, would be invisible to instruments with modest spatial resolution such as the Michelson Doppler Imager aboard the SOHO satellite (Scherrer et al 1995) and HMI. However, taking into account that the total flux inside the emerging region (all three clusters combined) is 8.8×10 18 Mx at maximum, and that the morphology of the newly emerged flux features resembles that of ERs, we conclude that most likely there is no difference between ERs and clusters of IN elements, and that they all are part of a continuous flux and size distribution of magnetic elements in the QS (Gošić 2015). This idea is consistent with the conclusions of Parnell et al (2009).…”

Section: Criteria For Identificationmentioning

confidence: 81%

“…These loops may also emerge as a group of mixed-polarity patches within a relatively small region (see e.g. Wang 1988, Harvey & Martin 1973, Title 2000, Hagenaar 2001, Gošić 2015, forming clusters of IN magnetic elements with typical total fluxes between 10 18 and 10 19 Mx.…”

Section: Introductionmentioning

confidence: 99%

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Emergence of internetwork magnetic fields through the solar atmosphere

Gošić,

De Pontieu,

Rubio

et al. 2021

Preprint

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Internetwork (IN) magnetic fields are highly dynamic, short-lived magnetic structures that populate the interior of supergranular cells. Since they emerge all over the Sun, these small-scale fields bring a substantial amount of flux, and therefore energy, to the solar surface. Because of this, IN fields are crucial for understanding the quiet Sun (QS) magnetism. However, they are weak and produce very small polarization signals, which is the reason why their properties and impact on the energetics and dynamics of the solar atmosphere are poorly known. Here we use coordinated, high-resolution, multiwavelength observations obtained with the Swedish 1-m Solar Telescope (SST) and the Interface Region Imaging Spectrograph (IRIS) to follow the evolution of IN magnetic loops as they emerge into the photosphere and reach the chromosphere and transition region. We studied in this paper three flux emergence events having total unsigned magnetic fluxes of 1.9×10 18 , 2.5×10 18 , and 5.3 × 10 18 Mx. The footpoints of the emerging IN bipoles are clearly seen to appear in the photosphere and to rise up through the solar atmosphere, as observed in Fe I 6173 Å and Mg I b 2 5173 Å magnetograms, respectively. For the first time, our polarimetric measurements taken in the chromospheric Ca II 8542 Å line provide direct observational evidence that IN fields are capable of reaching the chromosphere. Moreover, using IRIS data, we study the effects of these weak fields on the heating of the chromosphere and transition region.

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Section: Discussionsupporting

confidence: 81%

Section: Criteria For Identificationmentioning

confidence: 76%

Section: Criteria For Identificationmentioning

confidence: 81%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Emergence of internetwork magnetic fields through the solar atmosphere

Gošić,

De Pontieu,

Rubio

et al. 2021

Preprint

View full text Add to dashboard Cite

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“…However, we cannot rule out the possibility that we are partly also seeing weak fields that were present earlier (Lamb et al 2008(Lamb et al , 2010, as discussed in Gošić et al (2016). These could become concentrated by the shuffling motions due to the EG and, hence, visible.…”

Section: Discussionmentioning

confidence: 85%

On the Magnetic Nature of an Exploding Granule as Revealed by Sunrise/IMaX

Guglielmino,

Pillet,

Cobo

et al. 2020

Preprint

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We study the photospheric evolution of an exploding granule observed in the quiet Sun at high spatial (∼ 0. ′′ 3) and temporal (31.5 s) resolution by the imaging magnetograph Sunrise/IMaX in June 2009. These observations show that the exploding granule is cospatial to a magnetic flux emergence event occurring at mesogranular scale (up to ∼ 12 Mm 2 area). Using a modified version of the SIR code for inverting the IMaX spectropolarimetric measurements, we obtain information about the magnetic configuration of this photospheric feature. In particular, we find evidence of highly inclined emerging fields in the structure, carrying a magnetic flux content up to ∼ 4 × 10 18 Mx. The balance between gas and magnetic pressure in the region of flux emergence, compared with a very quiet region of the Sun, indicates that the additional pressure carried by the emerging flux increases by about 5% the total pressure and appears to allow the granulation to be modified, as predicted by numerical simulations. The overall characteristics suggest that a multi-polar structure emerges into the photosphere, resembling an almost horizontal flux sheet. This seems to be associated with exploding granules. Finally, we discuss the origin of such flux emergence events.

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Small-Scale Dynamos: From Idealized Models to Solar and Stellar Applications

et al. 2023

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In this article we review small-scale dynamo processes that are responsible for magnetic field generation on scales comparable to and smaller than the energy carrying scales of turbulence. We provide a review of critical observation of quiet Sun magnetism, which have provided strong support for the operation of a small-scale dynamo in the solar photosphere and convection zone. After a review of basic concepts we focus on numerical studies of kinematic growth and non-linear saturation in idealized setups, with special emphasis on the role of the magnetic Prandtl number for dynamo onset and saturation. Moving towards astrophysical applications we review convective dynamo setups that focus on the deep convection zone and the photospheres of solar-like stars. We review the critical ingredients for stellar convection setups and discuss their application to the Sun and solar-like stars including comparison against available observations.

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The Solar Internetwork. III. Unipolar versus Bipolar Flux Appearance

Cited by 16 publications

References 65 publications

Emergence of internetwork magnetic fields through the solar atmosphere

Emergence of internetwork magnetic fields through the solar atmosphere

On the Magnetic Nature of an Exploding Granule as Revealed by Sunrise/IMaX

Small-Scale Dynamos: From Idealized Models to Solar and Stellar Applications

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