Magnetic Maps of Prominences from Full Stokes Analysis of the He
                    <scp>i</scp>
                    D3 Line

Casini, R.; Ariste, A. López; Tomczyk, S.; Lites, B. W.

doi:10.1086/380496

Cited by 163 publications

(171 citation statements)

References 20 publications

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“…If the dense plasma is truly suspended in magnetic dips, the existing correlation between the opacity and the field strength may provide additional information for understanding current physical mechanisms for suspending the prominence material. Interestingly, we do not detect any abrupt changes in the prominence field strength contrary to the results of Casini et al (2003).…”

Section: Discussioncontrasting

confidence: 99%

“…In particular, we found that the field vector is about 77 • inclined with respect to the solar vertical. This result is between the values reported by, e.g., Leroy (1989) and Bommier et al (1994), with inclinations of about 60 • from the local vertical, and those reported by Casini et al (2003), mostly horizontal fields.…”

Section: Discussionsupporting

confidence: 64%

“…The first one differs from previous findings. For instance, Leroy (1989), Bommier et al (1994), and Casini et al (2003) report angles below 30 • . In contrast, the second solution, χ † = 156 • , implies an acute angle of 24 • , in line with previous measurements.…”

Section: Discussionmentioning

confidence: 99%

“…For instance, spectropolarimetric observations in the He i D3 multiplet at 587.6 nm have greatly contributed to the understanding of the magnetic field configuration in prominences (Athay et al 1983;Querfeld et al 1985;Casini et al 2003).…”

Section: Introductionmentioning

confidence: 99%

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The magnetic field configuration of a solar prominence inferred from spectropolarimetric observations in the He i 10 830 Å triplet

Suárez

Ramos

Bueno

2014

A&A

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Context. Determining the magnetic field vector in quiescent solar prominences is possible by interpreting the Hanle and Zeeman effects in spectral lines. However, observational measurements are scarce and lack high spatial resolution. Aims. We determine the magnetic field vector configuration along a quiescent solar prominence by interpreting spectropolarimetric Results. For the most probable magnetic field vector configuration, the analysis depicts a mean field strength of 7 gauss. We do not find local variations in the field strength except that the field is, on average, lower in the prominence body than in the prominence feet, where the field strength reaches ∼25 gauss. The averaged magnetic field inclination with respect to the local vertical is ∼77 • . The acute angle of the magnetic field vector with the prominence main axis is 24 • for the sinistral chirality case and 58 • for the dextral chirality. These inferences are in rough agreement with previous results obtained from the analysis of data acquired with lower spatial resolutions.

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Section: Discussioncontrasting

confidence: 99%

Section: Discussionsupporting

confidence: 64%

Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The magnetic field configuration of a solar prominence inferred from spectropolarimetric observations in the He i 10 830 Å triplet

Suárez

Ramos

Bueno

2014

A&A

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“…One of the advantages of the multiplets is that the absorption of these lines is usually negligible in quiet regions, so that any absorption can be regarded as due to a levitating cloud at a certain height, which greatly simplifies the solution of the radiative transfer equation for polarized radiation SahalBrechot et al 1977;Trujillo Bueno & Asensio Ramos 2007). In particular, these spectral lines have been widely used for the study of solar prominences and filaments (e.g., Bommier et al 1981;Casini et al 2003;Merenda et al 2006;Orozco Suárez et al 2014;Martínez González et al 2015), the reconstruction of magnetic fields in flux emerging regions (Solanki et al 2003;Xu et al 2010) and in chromospheric spicules (e.g., López Ariste & Casini 2005;Centeno et al 2010;Martínez González et al 2012;Orozco Suárez et al 2015).…”

Section: Introductionmentioning

confidence: 99%

Active Region Filaments Might Harbor Weak Magnetic Fields

Baso

González

Ramos

2016

ApJ

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Recent spectropolarimetric observations of active region filaments have revealed polarization profiles with signatures typical of the strong field Zeeman regime. The conspicuous absence in those observations of scattering polarization and Hanle effect signatures was then pointed out by some authors. This was interpreted as either a signature of mixed "turbulent" field components or as a result of optical thickness. In this article, we present a natural scenario to explain these Zeeman-only spectropolarimetric observations of active region (AR) filaments. We propose a two-component model, one on top of the other. Both components have horizontal fields, with the azimuth difference between them being close to 90°. The component that lies lower in the atmosphere is permeated by a strong field of the order of 600 G, while the upper component has much weaker fields, of the order of 10 G. The ensuing scattering polarization signatures of the individual components have opposite signs, so its combination along the line of sight reduces-and even can cancel out-the Hanle signatures, giving rise to an apparent Zeeman-only profile. This model is also applicable to other chromospheric structures seen in absorption above ARs.

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Scientific objectives and capabilities of the Coronal Solar Magnetism Observatory

et al. 2016

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Magnetic influences increase in importance in the solar atmosphere from the photosphere out into the corona, yet our ability to routinely measure magnetic fields in the outer solar atmosphere is lacking. We describe the scientific objectives and capabilities of the COronal Solar Magnetism Observatory (COSMO), a proposed synoptic facility designed to measure magnetic fields and plasma properties in the large‐scale solar atmosphere. COSMO comprises a suite of three instruments chosen to enable the study of the solar atmosphere as a coupled system: (1) a coronagraph with a 1.5 m aperture to measure the magnetic field, temperature, density, and dynamics of the corona; (2) an instrument for diagnostics of chromospheric and prominence magnetic fields and plasma properties; and (3) a white light K‐coronagraph to measure the density structure and dynamics of the corona and coronal mass ejections. COSMO will provide a unique combination of magnetic field, density, temperature, and velocity observations in the corona and chromosphere that have the potential to transform our understanding of fundamental physical processes in the solar atmosphere and their role in the origins of solar variability and space weather.

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Magnetic Maps of Prominences from Full Stokes Analysis of the He i D3 Line

Cited by 163 publications

References 20 publications

The magnetic field configuration of a solar prominence inferred from spectropolarimetric observations in the He i 10 830 Å triplet

The magnetic field configuration of a solar prominence inferred from spectropolarimetric observations in the He i 10 830 Å triplet

Active Region Filaments Might Harbor Weak Magnetic Fields

Scientific objectives and capabilities of the Coronal Solar Magnetism Observatory

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