The Solar Internetwork. Ii. Flux Appearance and Disappearance Rates

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

doi:10.3847/0004-637x/820/1/35

Cited by 42 publications

(50 citation statements)

References 23 publications

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“…As discussed above, the total instantaneous flux distribution in birth events shows that features born by appearance have lower values of flux on average. Whereas, the maximum flux in a feature born by appearance reached in the course of its life is roughly a factor of nearly 1.5 − 1.6 larger than its flux at birth (see also Gošić et al 2016). Consequently, features born by appearance events display a larger relative contribution to the total flux when the maximum flux is counted.…”

Section: Unipolar Interactionsmentioning

confidence: 97%

“…4.3 has been carried out by Lamb et al (2008) based on SOHO MDI magneto-graph data, and by Zhou et al (2010); Wang et al (2012); Lamb et al (2013); Gošić et al (2014Gošić et al ( , 2016 based on Hinode/SOT/NFI data. Their approach differs somewhat from ours in the definition of the events and the type of data used and partly also in the aims of the studies.…”

Section: Discussionmentioning

confidence: 99%

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Statistical evolution of quiet-Sun small-scale magnetic features using Sunrise observations

Anusha¹,

Solanki²,

Hirzberger³

et al. 2017

A&A

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The evolution of small magnetic features in quiet regions of the Sun provides a unique window to probing solar magnetoconvection. Here we analyze small scale magnetic features in the quiet Sun, using the high resolution, seeing-free observations from the Sunrise balloon borne solar observatory. Our aim is to understand the contribution of different physical processes, such as splitting, merging, emergence and cancellation of magnetic fields to the rearrangement, addition and removal of magnetic flux in the photosphere. We employ a statistical approach for the analysis and the evolution studies are carried out using a feature tracking technique. In this paper we provide a detailed description of the feature tracking algorithm that we have newly developed and we present the results of a statistical study of several physical quantities. The results on the fractions of the flux in the emergence, appearance, splitting, merging, disappearance and cancellation qualitatively agrees with other recent studies (see e.g., Lamb et al. 2008Lamb et al. , 2013. To summarize, the total flux gained in unipolar appearance is an order of magnitude larger than the total flux gained in emergence. On the other hand, the bi-polar cancellation contributes nearly an equal amount to the loss of magnetic flux as unipolar disappearance. The total flux lost in cancellation is nearly 6 − 8 times larger than the total flux gained in emergence. One big difference between our study and previous similar studies is that thanks to the higher spatial resolution of Sunrise we can track features with fluxes as low as 9 × 10 14 Mx. This flux is nearly an order of magnitude lower than the smallest fluxes of the features tracked in the highest resolution previous studies based on Hinode data. The area and flux of the magnetic features follow power-law type distribution, while the lifetimes show either power-law or exponential type distribution depending on the exact definitions used to define various birth and death events. We also statistically determine the evolution of the flux within the features in the course of their lifetime, finding that this evolution depends very strongly on the birth and death process that the features undergo.

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Section: Unipolar Interactionsmentioning

confidence: 97%

Section: Discussionmentioning

confidence: 99%

Statistical evolution of quiet-Sun small-scale magnetic features using Sunrise observations

Anusha¹,

Solanki²,

Hirzberger³

et al. 2017

A&A

View full text Add to dashboard Cite

show abstract

“…This leads to a higher estimation of the FER. Gošić et al (2016) have estimated that accounting for reappeared features decreases the FER by nearly 10%. If we assume the same amount of decrease in the FER from the reappeared features in our dataset, then we finally obtain an FER of 1100 Mx cm −2 day −1 .…”

Section: Uncertaintiesmentioning

confidence: 99%

“…The current estimates of the FER in the IN vary over a wide range, which include: 10 24 Mx day −1 (Zirin 1987), 3.7 × 10 24 Mx day −1 (120 Mx cm −2 day −1 , Gošić et al 2016) and 3.8 × 10…”

Section: Introductionmentioning

confidence: 99%

“…By considering all the magnetic features (smallscale features and active regions), Thornton & Parnell (2011) To estimate the FER, Zirin (1987) and Thornton & Parnell (2011) considered features with fluxes ≥ 10 16 Mx, while Zhou et al (2013) and Gošić et al (2016) included features with fluxes as low as 6 × 10 15 Mx and 6.5 × 10 15 Mx (M. Gošić, priv. comm.…”

Section: Introductionmentioning

confidence: 99%

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Estimation of the Magnetic Flux Emergence Rate in the Quiet Sun from Sunrise Data

Smitha

Anusha

Solanki

et al. 2017

ApJS

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Small-scale internetwork (IN) features are thought to be the major source of fresh magnetic flux in the quiet Sun. During its first science flight in 2009, the balloon-borne observatory Sunrise captured images of the magnetic fields in the quiet Sun at a high spatial resolution. Using these data we measure the rate at which the IN features bring magnetic flux to the solar surface. In a previous paper it was found that the lowest magnetic flux in small-scale features detected using the Sunrise observations is 9 × 10 14 Mx. This is nearly an order of magnitude smaller than the smallest fluxes of features detected in observations from Hinode satellite. In this paper, we compute the flux emergence rate (FER) by accounting for such small fluxes, which was not possible before Sunrise. By tracking the features with fluxes in the range 10 15 − 10 18 Mx, we measure an FER of 1100 Mx cm −2 day −1 . The smaller features with fluxes ≤ 10 16 Mx are found to be the dominant contributors to the solar magnetic flux. The FER found here is an order of magnitude higher than the rate from the Hinode, obtained with a similar feature tracking technique. A wider comparison with the literature shows, however, that the exact technique of determining the rate of the appearance of new flux can lead to results that differ by up to two orders of magnitude, even when applied to similar data. The causes of this discrepancy are discussed and first qualitative explanations proposed.

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Polarimetric Observations of the Sun

Suárez

2019

Astrophysics and Space Science Library

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The Solar Internetwork. Ii. Flux Appearance and Disappearance Rates

Cited by 42 publications

References 23 publications

Statistical evolution of quiet-Sun small-scale magnetic features using Sunrise observations

Statistical evolution of quiet-Sun small-scale magnetic features using Sunrise observations

Estimation of the Magnetic Flux Emergence Rate in the Quiet Sun from Sunrise Data

Polarimetric Observations of the Sun

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