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Linking the Sun to the Heliosphere Using Composition Data and Modelling

A Test Case with a Coronal Jet

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Abstract

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 1 AU.

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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Data Availability

The Hinode/EIS data are freely available through the European Hinode Data Cente: http://sdc.uio.no/sdc/.

STEREO and SDO/AIA data are available through the MEDOC datacenter: https://idoc-medoc.ias.u-psud.fr/sitools/client-user/index.html?project=Medoc-Solar-Portal.

GONG synoptic maps: ftp://gong2.nso.edu/oQR/zqs/201008/mrzqs100802/mrzqs100802t1154c2099_034.fits.gz.

SDO/HMI radial field synoptic map: http://jsoc.stanford.edu/data/hmi/synoptic/hmi.Synoptic_Mr_small.2099.fits.

Code Availability

The CHIANTI and ChiantiPy atomic database and software for the EUV diagnostic analysisFootnote 6 are freely available through SolarSoft: https://www.lmsal.com/solarsoft/.

The PFSS extrapolations are based on an IDL implementation of the current-free case of the formula presented in Zhao and Hoeksema (1993). Our results are comparable to those obtained with the PFSS package provided in SolarSoft: https://www.lmsal.com/~derosa/pfsspack/.

The Adaptively Refined MHD Solver (ARMS; DeVore and Antiochos 2008) is a proprietary research code designed for massively parallel high-performance computing clusters such as the NASA Center for Climate Simulation. For queries about the ARMS simulation data herein or the IDL post-processing analysis routines, please contact blynch@berkeley.edu. For queries about ARMS, including obtaining the source code, please contact c.richard.devore@nasa.gov.

FIPLCR finds the optimal linear combination of EUV spectral lines for calculating the FIP bias using the LCR method: https://git.ias.u-psud.fr/nzambran/fiplcr.

Notes

  1. ftp://gong2.nso.edu/oQR/zqs/201008/mrzqs100802/mrzqs100802t1154c2099_034.fits.gz

  2. http://jsoc.stanford.edu/data/hmi/synoptic/hmi.Synoptic_Mr_small.2099.fits.

  3. For an overview http://hmi.stanford.edu/hminuggets/?p=1689.

  4. https://www.adas.ac.uk; https://open.adas.ac.uk.

  5. We use Monte-Carlo simulations to simulate noisy radiances by adding Gaussian random perturbations with a 20% standard deviation assuming that this would be a typical error bar one would obtain for the radiances of EIS observations. From these noisy observations computed assuming different relative FIP biases we obtain \(P(f_{p} \mid f_{i})\), the probability distribution of the real relative FIP bias of the plasma \(f_{p}\) knowing that we have obtained a measured (inferred) relative FIP bias \(f_{i}\).

  6. http://www.chiantidatabase.org/.

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Acknowledgements

This collaborative work was made with the support of the International Space Science Institute through its International Team program (Team 418). S.P. acknowledges the funding by CNES through the MEDOC data and operations center. S.P. is grateful to Dr. Hans-Peter Doerr for the discussion on images co-registration. B.J.L. was supported in part by NASA grants 80NSSC18K0645, 80NSSC18K1553, and 80NSSC20K1448. J.M.L. was supported by the NASA Heliophysics Guest Investigator (80HQTR19T0029) and Supporting Research Programs (80HQTR20T0076), and by Basic Research Funds of the Office of Naval Research. I.C. acknowledges DFG-grant WI 3211/5-1. G.D.Z. acknowledges support from STFC (UK) via the consolidated grants to the atomic astrophysics group at DAMTP, University of Cambridge (ST/P000665/1. and ST/T000481/1). T.W. acknowledges financial support by DLR-grants 50 OC 1701 and 50 OC 2101 and DFG-grant WI 3211/5-1. Y.J.R. acknowledges support from the Rackham Merit Fellowship at the University of Michigan, the Newkirk Fellowship at the High Altitude Observatory, and Future Faculty Leaders Fellowship at the Center for Astrophysics. S.T.L. acknowledges support from NASA grants: NNX16AP03H, NNX16AH01G, and 80NSSC20K1063; NSF Grants: 1460170 and AGS 1358268; and DOD Grant: N00173-14-1-G904. R.F.W-S. acknowledges DLR grant 50OT1702 and DFG grant WI 2139/11-1. G.P. has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (grant agreement No. 724326). CHIANTI is a collaborative project involving George Ma-son University, the University of Michigan, the NASA Goddard Space Flight Centre (USA) and the University of Cambridge (UK). Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as domestic partner and NASA and UKSA as international partners. It is operated by these agencies in co-operation with ESA and NSC (Norway). “Courtesy of NASA/SDO and the AIA, EVE, and HMI science teams.” The EUVI images are supplied courtesy of the STEREO Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI) team.

Funding

This work was supported by the International Space Science Institute through its International Team program.

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Authors and Affiliations

  1. Institut d’Astrophysique Spatiale, CNRS-Université Paris-Saclay, 91405, Orsay, France

    Susanna Parenti & Natalia Zambrana Prado

  2. Institute for Astrophysics, University of Göttingen, Friedrich-Hund-Platz 1, 37077, Göttingen, Germany

    Iulia Chifu

  3. Max-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, 37077, Göttingen, Germany

    Iulia Chifu & Thomas Wiegelmann

  4. DAMTP, Centre for Mathematical Sciences, University of Cambridge, Wilberforce Road, Cambridge, CB3 0WA, UK

    Giulio Del Zanna

  5. Department of Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, MI, 48109, USA

    Justin Edmondson, Aleida Higginson & Susan T. Lepri

  6. RAL Space, UKRI STFC Rutherford Appleton Laboratory, Harwell, Didcot, OX11 0QX, UK

    Alessandra Giunta

  7. Institute of Theoretical Astrophysics, University of Oslo, P.O. Box 1029 Blindern, 0315, Oslo, Norway

    Viggo H. Hansteen

  8. Space Science Division, Code 7684, Naval Research Laboratory, Washington, DC, 20375, USA

    J. Martin Laming

  9. Space Sciences Laboratory, University of California–Berkeley, Berkeley, CA, 94720, USA

    Benjamin J. Lynch

  10. Center for Astrophysics, Harvard University, 60 Garden Street, Cambridge, MA, 02138, USA

    Yeimy J. Rivera

  11. International Space Science Institute, Hallerstrasse 6, 3012, Bern, Switzerland

    Rudolf von Steiger

  12. Physikalisches Institut, University of Bern, Sidlerstrasse 5, 3012, Bern, Switzerland

    Rudolf von Steiger

  13. Institute of Experimental and Applied Physics, University of Kiel, Leibnizstrasse 11, 24118, Kiel, Germany

    Robert F. Wimmer-Schweingruber

  14. Centre for mathematical Plasma Astrophysics, Department of Mathematics, KU Leuven, Celestijnenlaan 200B bus 2400, 3001, Leuven, Belgium

    Gabriel Pelouze

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  1. Susanna Parenti
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  2. Iulia Chifu
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  3. Giulio Del Zanna
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Correspondence to Susanna Parenti.

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Parenti, S., Chifu, I., Del Zanna, G. et al. Linking the Sun to the Heliosphere Using Composition Data and Modelling. Space Sci Rev 217, 78 (2021). https://doi.org/10.1007/s11214-021-00856-1

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