Inference of the magnetic field in spicules
from spectropolarimetry of He I D$_\mathsf{3}$

Ariste, A. López; Casini, R.

doi:10.1051/0004-6361:20042214

Cited by 48 publications

(28 citation statements)

References 15 publications

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“…Such a distance off-limb corresponds to the low spicular region, as proven by the broadening of the spectral features in Ba ii (when compared to on-disk profiles, as seen in the following figures of this paper, the central peak broadens almost 10%, from a Gaussian fit with FWHM of 110 mÅ on disk to 123 mÅ off disk). This broadening is characteristic of spicules (Krat & Krat 1971;López Ariste & Casini 2005;Trujillo Bueno et al 2005) and is considered as non-thermal in nature. The polarization pattern in Fig.…”

Section: Stokes Q Profilesmentioning

confidence: 99%

Variability of the polarization profiles of the Ba II D₂ line in the solar atmosphere

Ariste¹,

Ramos

Sainz

et al. 2009

A&A

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Context. Resonance-scattering polarization and the Hanle effect are powerful but seldom exploited probes into the magnetism of the quiet solar atmosphere. They are also very interesting checks of the quantum theory of atomic polarization. The Ba ii D 2 line has been known for more than 20 years as presenting a conspicuous signal of resonance scattering polarization thanks to its atomic configuration and the presence of five different isotopes of Ba, two of which present a hyperfine structure. Aims.A model that considers most of the known ingredients of the atomic polarization of Ba ii related to the formation of the D 2 line was presented in 2007. We intend to observe all the variability of the Stokes profiles of this line in conditions of resonance scattering to verify the general validity of the model and to ascertain the use of the model for magnetic field diagnostics in the quiet solar chromosphere and in spicules. Methods. The new CCD cameras at THEMIS and the recently commissioned tip-tilt tracking system gave us the opportunity to perform the required observations with unprecedented precision and reliability, resulting in data ready to confront the present theory. Results. The Stokes Q profiles, both off-limb and on disk, appear to verify this theory in qualitative terms. The observed departures in terms of overall signal amplitude and relative ratios among the three spectral features point to a refinement of the theory for quantitative purposes, perhaps including radiative-transfer effects. We observed, on the other hand, anomalous Stokes V profiles in the absence of Zeeman effect that remain unexplained. Conclusions. The qualitative agreement between the theory and the observations encourages an increased effort to also match the observations from a quantitative point of view, including the observed anomalous Stokes V profiles.

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Section: Stokes Q Profilesmentioning

confidence: 99%

Variability of the polarization profiles of the Ba II D₂ line in the solar atmosphere

Ariste¹,

Ramos

Sainz

et al. 2009

A&A

Self Cite

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“…Levens et al (2016) investigated the magnetic field in and around prominence bubbles finding increases in the inferred magnetic field strength in these regions, which the authors interpret as being consistent with the bubble being formed by emerging magnetic flux. This is the first attempt at such measurements and aspects of the results support the ideas behind bubble formation, but cautions has to be taken due to the relatively large space of parameters where solutions to the inversions exist (López Ariste and Casini 2005).…”

Section: Prominence Bubblesmentioning

confidence: 83%

The magnetic Rayleigh–Taylor instability in solar prominences

Hillier

2017

Rev. Mod. Plasma Phys.

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The magnetic Rayleigh-Taylor instability is a fundamental instability of many astrophysical systems, and recent observations are consistent with this instability developing in solar prominences. Prominences are cool, dense clouds of plasma that form in the solar corona that display a wide range of dynamics of a multitude of spatial and temporal scales, and two different phenomena that have been discovered to occur in prominences can be understood as resulting from the Rayleigh-Taylor instability. The first is that of plumes that rise through quiescent prominences from low density bubbles that form below them. The second is that of a prominence eruption that fragments as the material falls back to the solar surface. To identify these events as the magnetic Rayleigh-Taylor instability, a wide range of theoretical work, both numerical and analytical has been performed, though alternative explanations do exist. For both of these sets of observations, determining that they are created by the magnetic Rayleigh-Taylor instability has meant that the linear instability conditions and nonlinear dynamics can be used to make estimates of the magnetic field strength. There are strong connections between these phenomena and those in a number of other astro, space and plasma systems, making these observations very important for our understanding of the role of the RayleighTaylor instability in magnetised systems.

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“…They point out, however, that significantly stronger fields could also be present (as indicated by larger Stokes-V signals detected during another observing run). The possibility of magnetic fields significantly larger than 10 G was also tentatively suggested by the He I D 3 measurements of López Ariste & Casini (2005), although these spicules emanated from active plage. More detailed spectropolarimetric observations of spicules in the He I D 3 multiplet were carried out by Ramelli et al (2006), who found B≈10 G in quiet Sun and B≈50 G in more active areas.…”

Section: Introductionmentioning

confidence: 64%

The Magnetic Field of Solar Spicules

Centeno

Bueno

Ramos

2009

Magnetic Coupling Between the Interior and Atmosphere of the Sun

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Summary. Determining the magnetic field of solar spicules is vital for developing adequate models of these plasma jets, which are thought to play a key role in the thermal, dynamic, and magnetic structure of the chromosphere. Here we report on magnetic spicule properties in a very quiet region of the off-limb solar atmosphere, as inferred from new spectropolarimetric observations in the He I 10830Å triplet. We have used a novel inversion code for Stokes profiles caused by the joint action of atomic level polarization and the Hanle and Zeeman effects (HAZEL) to interpret the observations. Magnetic fields as strong as 40 G were unambiguously detected in a very localized area of the slit, which may represent a possible lower value of the field strength of organized network spicules.

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Inference of the magnetic field in spicules from spectropolarimetry of He I D$_\mathsf{3}$

Cited by 48 publications

References 15 publications

Variability of the polarization profiles of the Ba II D₂ line in the solar atmosphere

Variability of the polarization profiles of the Ba II D₂ line in the solar atmosphere

The magnetic Rayleigh–Taylor instability in solar prominences

The Magnetic Field of Solar Spicules

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Inference of the magnetic field in spicules from spectropolarimetry of He I D$_\mathsf{3}$

Cited by 48 publications

References 15 publications

Variability of the polarization profiles of the Ba II D2 line in the solar atmosphere

Variability of the polarization profiles of the Ba II D2 line in the solar atmosphere

The magnetic Rayleigh–Taylor instability in solar prominences

The Magnetic Field of Solar Spicules

Contact Info

Product

Resources

About

Variability of the polarization profiles of the Ba II D₂ line in the solar atmosphere

Variability of the polarization profiles of the Ba II D₂ line in the solar atmosphere