The role and contribution of magnetic fields, characterized via their magnetic flux, to the statistical structuring of the solar atmosphere

Li, K. J.; Xu, J. C.; Wen, Feng

doi:10.1038/s41598-022-20094-x

Cited by 5 publications

(1 citation statement)

References 47 publications

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“…An accepted understanding among solar and stellar scientists is that the 11-year variations in global activity observed in the Sun are coherent and connected with the 22-year magnetic cycle. These cycles have been extensively studied and correlated with a synchronized behavior of the solar atmospheric layers (i.e., photosphere, chromosphere, and corona Hathaway 2015; Li et al 2022). In order to approach a better magnetic understanding of other stars, stellar researchers have conjugated a set of multiple techniques to overcome the difficulties generated by the lack of quality and quantity data, if compared with the solar counterpart (see review by, Reiners 2012).…”

Section: Introductionmentioning

confidence: 99%

Far beyond the Sun − II. Probing the stellar magnetism of the young Sun ι Horologii from the photosphere to its corona

Amazo-Gómez

Alvarado‐Gómez

Poppenhaeger

et al. 2023

Monthly Notices of the Royal Astronomical Society

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A comprehensive multi-wavelength campaign has been carried out to probe stellar activity and variability in the young Sun-like star ι-Horologii. We present the results from long-term spectropolarimetric monitoring of the system by using the ultra-stable spectropolarimeter/velocimeter HARPS at the ESO 3.6-m telescope. Additionally, we included high-precision photometry from the NASA Transiting Exoplanet Survey Satellite (TESS) and observations in the far- and near-ultraviolet spectral regions using the STIS instrument on the NASA/ESA Hubble Space Telescope (HST). The high-quality dataset allows a robust characterisation of the star’s rotation period, as well as a probe of the variability using a range of spectroscopic and photometric activity proxies. By analyzing the gradient of the power spectra (GPS) in the TESS lightcurves we constrained the faculae-to-spot driver ratio ($\rm S_{fac}/S_{spot}$) to 0.510±0.023, which indicates that the stellar surface is spot dominated during the time of the observations. We compared the photospheric activity properties derived from the GPS method with a magnetic field map of the star derived using Zeeman-Doppler imaging (ZDI) from simultaneous spectropolarimetric data for the first time. Different stellar activity proxies enable a more complete interpretation of the observed variability. For example, we observed enhanced emission in the HST transition line diagnostics C iv and C iii, suggesting a flaring event. From the analysis of TESS data acquired simultaneously with the HST data, we investigate the photometric variability at the precise moment that the emission increased and derive correlations between different observables, probing the star from its photosphere to its corona.

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Section: Introductionmentioning

confidence: 99%

Far beyond the Sun − II. Probing the stellar magnetism of the young Sun ι Horologii from the photosphere to its corona

Amazo-Gómez

Alvarado‐Gómez

Poppenhaeger

et al. 2023

Monthly Notices of the Royal Astronomical Society

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Study on the relation of the solar coronal rotation with magnetic field structures

Xiang,

Zhao,

Deng

et al. 2023

Sci Rep

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Daily solar spectral irradiances (SSIs) at the spectral intervals 1–40, 116–264 and 950–1600 nm and four categories of solar small-scale magnetic elements ($$MF_{no}$$ M F no , $$MF_{anti}$$ M F anti , $$MF_{tran}$$ M F tran and $$MF_{in}$$ M F in ) are used to study the temporal variation of coronal rotation and investigate the relation of the coronal rotation with magnetic field structures through continuous wavelet transform and Pearson correlation analysis. The results reveal the contributions of different magnetic structures to the temporal variation of the rotation for the coronal atmosphere during different phases of the solar cycle. During the solar maximum, the temporal variation of rotation for the coronal plasma atmosphere is mainly dominated by the small-scale magnetic elements of $$MF_{anti}$$ M F anti ; whereas during the epochs of the relatively weak solar activity, it is controlled by the joint effect of the small-scale magnetic elements of both $$MF_{anti}$$ M F anti and $$MF_{in}$$ M F in . The weaker the solar activity, the stronger the effect of $$MF_{in}$$ M F in would be. Furthermore, this study presents an explanation for the inconsistent results for the coronal rotation issue among the previous studies, and also reveals the reason why the coronal atmosphere rotates faster than the lower photosphere.

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The quiet chromosphere: differential rotation

Wan

Wen

2023

Monthly Notices of the Royal Astronomical Society

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The solar chromosphere was daily observed in the Ca ii K line at the Mount Wilson Observatory from 1915 August to 1985 July. A digitized data base was created, which includes synoptical maps of the chromosphere in Ca ii intensity from Carrington rotations 827 to 1764. We have used the data base to investigate rotation and its differential of the chromosphere and the quiet chromosphere. The chromosphere is found to rotate faster than sunspots, but the difference in their rotation rates decreases with decreasing latitude, and near the equator they rotate at nearly the same speed. The chromosphere is obviously faster than the quiet photosphere and slightly faster than the quiet chromosphere at low latitudes, but slightly slower than the quiet chromosphere at middle latitudes. The differential degree of the rotation rate at low latitudes, ranging from largest to smallest in order, is found to be: sunspots, the chromosphere, the quiet photosphere, and the quiet chromosphere. The differential of the rotation rate is found to be different in different solar cycles for the chromosphere and the quiet chromosphere. Helioseismology observations suggest that these findings are plausible.

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The role and contribution of magnetic fields, characterized via their magnetic flux, to the statistical structuring of the solar atmosphere

Cited by 5 publications

References 47 publications

Far beyond the Sun − II. Probing the stellar magnetism of the young Sun ι Horologii from the photosphere to its corona

Far beyond the Sun − II. Probing the stellar magnetism of the young Sun ι Horologii from the photosphere to its corona

Study on the relation of the solar coronal rotation with magnetic field structures

The quiet chromosphere: differential rotation

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