Magnetic Field Geometry and Composition Variation in Slow Solar Winds: The Case of Sulfur

Kuroda, Natsuha; Laming, J. Martin

doi:10.3847/1538-4357/ab8870

Cited by 10 publications

(10 citation statements)

References 53 publications

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“…213 Å,Fe IX 188.497 Å,Fe X 184.536 Å,Fe XI 188.216 Å,Fe XI 188.299 Å,Fe XII 195.119 Å,Fe XII 203.72 Å,Fe XIII 202.044 Å,Fe XIII 203.826 Å,Fe XIV 264.787 Å,Fe XV 284.16 Å,and Fe XVI 262.984 Å. 3 Si X 258.37 Å and S X 264.22 Å. studies, it lies close to the boundary between low and high FIP elements, and it has been suggested that it can exhibit both low and high FIP behaviour (Reames 2018;Kuroda & Laming 2020). Ideally another element with a higher FIP would be used, but emission lines from other high FIP elements are challenging to measure with Hinode/EIS (Feldman et al 2009).…”

Section: Coronal Compositionmentioning

confidence: 94%

Directly comparing coronal and solar wind elemental fractionation

Stansby

Baker

Brooks

et al. 2020

A&A

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Context. As the solar wind propagates through the heliosphere, dynamical processes irreversibly erase the signatures of the near–Sun heating and acceleration processes. The elemental fractionation of the solar wind should not change during transit, however, making it an ideal tracer of these processes. Aims. We aim to verify directly if the solar wind elemental fractionation is reflective of the coronal source region fractionation, both within and across different solar wind source regions. Methods. A backmapping scheme was used to predict where solar wind measured by the Advanced Composition Explorer (ACE) originated in the corona. The coronal composition measured by the Hinode Extreme ultraviolet Imaging Spectrometer (EIS) at the source regions was then compared with the in situ solar wind composition. Results. On hourly timescales, there is no apparent correlation between coronal and solar wind composition. In contrast, the distribution of fractionation values within individual source regions is similar in both the corona and solar wind, but distributions between different sources have a significant overlap. Conclusions. The matching distributions directly verify that elemental composition is conserved as the plasma travels from the corona to the solar wind, further validating it as a tracer of heating and acceleration processes. The overlap of fractionation values between sources means it is not possible to identify solar wind source regions solely by comparing solar wind and coronal composition measurements, but a comparison can be used to verify consistency with predicted spacecraft-corona connections.

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Section: Coronal Compositionmentioning

confidence: 94%

Directly comparing coronal and solar wind elemental fractionation

Stansby

Baker

Brooks

et al. 2020

A&A

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“…In the open field, S behaves more like a low FIP element, while in closed field it more closely resembles a high FIP element. The reasons for this have been previously discussed (Laming et al, 2019;Kuroda and Laming, 2020) (Reames, 2018). It is curious then that CO1 appears to exhibit abundances more appropriate to a closed loop than to open field (see Fig.…”

Section: Modelling the Fip Biasmentioning

confidence: 89%

“…The wave angular frequency is taken to be the resonant frequency for each loop, assuming that the Alfvén waves have a coronal origin. For each model we give two fractionations, one arising solely from the ponderomotive force as would be revealed by spectroscopy of emissions from close to the solar surface, and a second incorporating also the effects on abundances of the conservation of the first adiabatic invariant in the expanding magnetic field lines (Laming et al, 2017(Laming et al, , 2019Kuroda and Laming, 2020), as would be detected in-situ. We assume (as before) that the plasma becomes collisionless at a density of ∼ 10 6 cm −3 , which in this open field region occurs at a radius of about 2.5 R .…”

Section: Modelling the Fip Biasmentioning

confidence: 99%

Linking the Sun to the Heliosphere Using Composition Data and Modelling

et al. 2021

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Our understanding of the formation and evolution of the corona and the heliosphere is linked to our capability of properly interpret the data from remote sensing and in-situ observations. In this respect, being able to correctly connect in-situ observations with their source regions on the Sun is the key for solving this problem. In this work we aim at testing a diagnostics method for this connectivity.This paper makes use of a coronal jet observed on 2010 August 2nd in active region 11092 as a test for our connectivity method. This combines solar EUV and in-situ data together with magnetic field extrapolation, large scale MHD modeling and FIP (First Ionization Potential) bias modeling to provide a global picture from the source region of the jet to its possible signatures at 1AU.Our data analysis reveals the presence of outflow areas near the jet which are within open magnetic flux regions and which present FIP bias consistent with the FIP model results. In our picture, one of these open areas is the candidate jet source. Using a back-mapping technique we identified the arrival time of this solar plasma at the ACE spacecraft. The in-situ data show signatures of changes in the plasma and magnetic field parameters, with FIP bias consistent with the possible passage of the jet material.Our results highlight the importance of remote sensing and in-situ coordinated observations as a key to solve the connectivity problem. We discuss our results in view of the recent Solar Orbiter launch which is currently providing such unique data.

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“…Sulfur lies on the boundary between low-and high-FIP elements and shows variable behavior that is sometimes consistent with one group or the other. In some theoretical models this depends on the open or closed topology of the magnetic field (Laming et al 2019;Kuroda & Laming 2020), making it a useful diagnostic regardless (Brooks & Yardley 2021b).…”

Section: Atomic Data and Analysis Methodsmentioning

confidence: 99%

Plasma Composition Measurements in an Active Region from Solar Orbiter/SPICE and Hinode/EIS

Brooks

Janvier

Baker

et al. 2022

ApJ

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A key goal of the Solar Orbiter mission is to connect elemental abundance measurements of the solar wind enveloping the spacecraft with extreme-UV (EUV) spectroscopic observations of their solar sources, but this is not an easy exercise. Observations from previous missions have revealed a highly complex picture of spatial and temporal variations of elemental abundances in the solar corona. We have used coordinated observations from Hinode and Solar Orbiter to attempt new abundance measurements with the Spectral Imaging of the Coronal Environment (SPICE) instrument, and benchmark them against standard analyses from the EUV Imaging Spectrometer (EIS). We use observations of several solar features in active region (AR) 12781 taken from an Earth-facing view by EIS on 2020 November 10, and SPICE data obtained one week later on 2020 November 17, when the AR had rotated into the Solar Orbiter field of view. We identify a range of spectral lines that are useful for determining the transition region and low-coronal-temperature structure with SPICE, and demonstrate that SPICE measurements are able to differentiate between photospheric and coronal magnesium/neon abundances. The combination of SPICE and EIS is able to establish the atmospheric composition structure of a fan loop/outflow area at the AR edge. We also discuss the problem of resolving the degree of elemental fractionation with SPICE, which is more challenging without further constraints on the temperature structure, and comment on what that can tell us about the sources of the solar wind and solar energetic particles.

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Magnetic Field Geometry and Composition Variation in Slow Solar Winds: The Case of Sulfur

Cited by 10 publications

References 53 publications

Directly comparing coronal and solar wind elemental fractionation

Directly comparing coronal and solar wind elemental fractionation

Linking the Sun to the Heliosphere Using Composition Data and Modelling

Plasma Composition Measurements in an Active Region from Solar Orbiter/SPICE and Hinode/EIS

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