2017
DOI: 10.3847/1538-4357/aa7466
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Abstract: Before using three-dimensional (3D) magneto-hydrodynamical (MHD) simulations of the solar photosphere in the determination of elemental abundances, one has to ensure that the correct amount of magnetic flux is present in the simulations. The presence of magnetic flux modifies the thermal structure of the solar photosphere, which affects abundance determinations and the solar spectral irradiance. The amount of magnetic flux in the solar photosphere also constrains any possible heating in the outer solar atmosph… Show more

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Cited by 8 publications
(5 citation statements)
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References 65 publications
(97 reference statements)
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“…A degraded data set (rebinned and point-spread function (PSF)-convolved to approximate the Hinode resolution) yields similar values. This is within a factor 2 of the observationally based quiet-Sun values of Khomenko et al (2005) or Beck et al (2017). On the other hand, in the BPS, < B >= 48 G in the photosphere.…”
Section: Methodssupporting
confidence: 72%
“…More recent work by Beck et al (2017) have quoted a value of 35 G as the average magnetic flux density of the quiet Sun region. Comparing it with the cases that we study in this paper, this would coincide with a model intermediate to Sun-v10 and Sun-v50, for which the average height of plasma-β=1 layer would correspond to around z = 900 km.…”
Section: Limitations Of the Current Study And Future Outlookmentioning
confidence: 99%
“…The magnetic connectivity is to a large extent deterministic and can only provide closed MFLs between opposite-polarity FPs, but HMI cannot detect diffuse weak magnetic flux below a certain level because of its spatial and spectral resolution. Photospheric highresolution observations of internetwork quiet Sun magnetism reveal a large amount of magnetic flux that is beyond the detection capabilities of the HMI (Lites et al 2008;Beck & Rezaei 2009;Beck et al 2017). However, a connection between the outer penumbra and weak magnetic flux favors a siphon flow scenario even more because of the resulting small field strength at the outer foot points.…”
Section: Limitations Of the Current Studymentioning
confidence: 99%
“…The magnetic connectivity is to a largest extent deterministic and can only provide closed MFLs between opposite-polarity FPs, but HMI cannot detect diffuse weak magnetic flux below a certain level because of its spatial and spectral resolution. Photospheric high-resolution observations of internetwork quiet Sun magnetism reveal a large amount of magnetic flux that is beyond HMI's detection capabilities (Lites et al 2008;Beck & Rezaei 2009;Beck et al 2017). A connection between the outer penumbra and weak magnetic flux favors, however, a siphon flow scenario even more because of the resulting small field strength at the outer foot points.…”
Section: Limitations Of the Current Studymentioning
confidence: 99%
“…The pair of Fe i infrared lines at 15 648 and 15 652 Å has been extensively used in the literature for polarimetric measurements since the early 1990s. Among many other works, we have the series of works entitled Infrared lines as probes of solar magnetic features that started with Muglach & Solanki (1992), or the publications of, for instance, Mathew et al (2003), Khomenko et al (2005), Bello González et al (2013), and Beck et al (2017.…”
Section: Appendix A: Fe I 15652874 åmentioning
confidence: 99%