I9: SolarGeoMag

> Read the articles connected to the project.

Improving Solar and Geo-dynamo predictability: towards advanced integrated data assimilation techniques

 

  • The main goal of the project is to improve our physical understanding, and our capability to predict, the long-term magnetic activity of the Sun and the Earth. This understanding is based on the analysis of 3D simulations that are parameterized and implemented in low dimensional models amenable to data assimilation experiments.

    Three-dimensional, self-consistent numerical simulations of solar and Earth interior magnetic field generation have made tremendous progress over the past 15 years, due to the dramatic increase in computational power.

     

    full 3D simulation of the Sun

    Full 3-D simulation of the Sun. Shown is the radial normalized velocity from the Sun’s core r=0 up to its surface at 99% Rsol (Alvan et al. 2015, Brun et al. 2016 in prep). Note the busy surface convective patterns and the excitation of internal gravito-inertial waves by the turbulent convective flows.

     

     

    Solar rotation profile in the meridional plane as computed with ASH code in Alvan et al. 2015.

    Solar rotation profile in the meridional plane as computed with ASH code in Alvan et al. 2015. Note the strong outer differential rotation and the fast transition (so-called tachocline) to inner core solid-body rotation (Alvan et al. 2015).

     

    Magnetic field lines within a three-dimensional simulation of the solar dynamo computed with ASH code

    Magnetic field lines within a three-dimensional simulation of the solar dynamo computed with ASH code (after Augustson et al., ApJ, 2015)

    butterfly diagram

    Butterfly diagram from a cyclic numerical simulation of the solar dynamo (Augustson et al., 2015). Note the equatorward propagation of the dynamo wave at mid/low latitude and the period of minima between cycle 11 and 16.

    Solar Wind computed from a Wilcox Observatory magnetogram during cycle 22 using PLUTO code (Reville, Brun et al. 2015). Field lines are coded with Br amplitude and the grey shade corresponds to the Alfven surface, beyond which the wind speed is super-Alfvenic.

    Solar Wind computed from a Wilcox Observatory magnetogram during cycle 22 using PLUTO code (Reville, Brun et al. 2015). Field lines are coded with Br amplitude and the grey shade corresponds to the Alfven surface, beyond which the wind speed is super-Alfvenic.

     

    In parallel advanced data assimilation pipelines have been implemented in geo and solar magnetohydrodynamics (MHD) to better constrain the short-term evolution of the magnetic field B. However, predictions of the long-term magnetic variations on the Earth and the Sun are intractable with 3-D simulations. This imposes to develop more conceptual, lower dimensional models in order to support (by objective comparison with data) our 3-D studies of the origin of the long-terms variations of B, such as rare and irregular polarity reversals, or solar grand minima. Our group has developed such models (of the mean-field flux transport type) together with a variational assimilation scheme to predict solar activity over one solar cycle (11 yr). We propose here to improve these models, and to propose new models, to be able to characterize the long term behavior of the Earth and the Sun.

    The questions that we address are :

    • What are the physical mechanisms responsible for the long-term magnetic variability of the Sun and the Earth?
    • What is the predictability of the low-frequency/rare events such as solar minima and geomagnetic reversals?
    • Can we make robust forecasts of these events using, eg., partly simplified (parameterized) models?

    These questions, whose answers must rely on the available observational evidence, can be cast in the general framework of data assimilation. Utilizing data assimilation techniques to study the long-term behaviour of the magnetism of the Sun and the Earth is currently out of reach if one wishes to resort to high-resolution 3-D models based on first-principles (the cost of assimilation is 10 to 100 times that of a single model integration).

    Our goal is to analyze complex, 3-D simulations of the solar- and geo-dynamo in order to extract the fundamental mechanisms which control the long-term magnetic variability of these objects, and to test these mechanisms against observations by placing them at the core of conceptual models of moderate size well-suited for data assimilation. These observations include systematic sunspot count since the early 1600s for the Sun (encompassing the Maunder minimum) and geomagnetic intensity for the past 2 Myr (covering 5 reversals of polarity).

  •  

    POSITION NAME SURNAME LABORATORY NAME GRADE, EMPLOYER
    WP leader Alexandre Fournier IPGP Professor (IPGP)
    WP co-leader A. Sacha Brun AIM Senior researcher (CEA)
    WP member Ching Pui Hung IPGP / AIM Post-doctoral researcher
    WP member Laurène Jouve IRAP / AIM Maître de conférences (U Toulouse)
    WP member Gauthier Hulot IPGP Senior Researcher (CNRS)
    WP member Thomas Gastine IPGP Junior Researcher (CNRS)

  • WP1 3D simulations of the solar and Geodynamo

    The goal of this task is to identify the key physical processes controlling the long-term behavior of the geo- and solar magnetic fields, through the detailed analysis of three-dimensional simulations of these systems. For the geodynamo simulations, we conducted during year 1 a series of preliminary runs to explore the sensitivity of the geomagnetic pole location to the vigor of convection, as an indicator of the possibility for a given simulation to lead to a geomagnetic reversal (see annual report 2016 for details). At the beginning of year 2, we increased the vigor even more, and obtained a multipolar solution, ie one that does not bear any resemblance with the geodynamo (characterized by a dipole-dominated field, which occasionally reverses). The solution remained multipolar, never returning to a dipole dominated state.

     

     

    WP2 Design of an operational tool for the prediction of solar activity

     

    UnivEarthS Labex funded Post-doc Ching-Pui Hung kept on making considerable development for this WP, which is the one that is likely to have the broader impact. We have at our disposal an assimilation tool whose backbone is a mean-field model of the solar dynamo and which can convincingly estimate the time-dependent deep circulation within the Sun, based on the observation of sunspots and surface magnetograms. Proof-of-concept experiments were carried out for the most part in 2016 and reported in the 2016 scientific report; their detailed analysis and their comparison with the state of the art appeared in the Astrophysical Journal (Hung et al., accepted for publication,
    http://arxiv.org/abs/1710.02114)

     

    WP3 Long-term predictability of geomagnetic reversals (and long-term variability of the solar dynamo)

     

    The start of this WP3 is contingent, for the most part, upon the completion of WP1. With respect to this line of research, and independently of actual support from UnivEarthS, a collaboration with Dr Matthias Morzfeld of the University of Arizona led to a paper describing the testbed one can use for that task, stressing in particular the importance
    of the concept of coarse predictions (Morzfeld et al., Physics of the Earth and Planetary Interiors, 2017). Since WP1 has not been completed yet, we have to defer the start of WP3 for what regards the geomagnetic field.

     

  • C. P. Hung, A. S. Brun, A. Fournier, L. Jouve, O. Talagrand, and M. Zakari, Variational estimation of the large scale time dependent meridional circulation in the Sun: proofs of concept with a solar mean field solar dynamo model, accepted for publication in the Astrophysical Journal. 2017.
    http://arxiv.org/abs/1710.02114

     

    C. P. Hung, A. S. Brun, A. Fournier, L. Jouve, O. Talagrand, and M. Zakari , Estimating the Solar Meridional Flow and Predicting the 11-yr Cycle Using Advanced Variational Data Assimilation Techniques, Space Weather of the Heliosphere: Processes and Forecasts, Proceedings IAU Symposium No. 335, 2017, Claire Foullon & Olga Malandraki, ed.

     

    Coarse predictions of dipole reversals by low-dimensional modeling and data assimilation, by M. Morzfeld, A.Fournier, and G. Hulot, 262, 8-27, 2017. doi: 10.1016/j.pepi.2016.10.007 (in connection with WP2)

     

    Sandpile models and solar flares: eigenfunction decomposition for data assimilation, by A. Strugarek, A. S. Brun, P.Charbonneau and N. Vilmer, Space Weather of the Heliosphere: Processes and Forecasts, Proceedings IAU Symposium No. 335, 2017, Claire Foullon & Olga Malandraki, ed. Submitted

     

    Hung, C.P., Jouve, L., Brun, A.S., Fournier, A., and Talagrand O., Estimating the deep solar meridional circulation using magnetic observations and a dynamo model: a variational approach,The Astrophysical Journal, 814, 151 (21 pp), 2015. doi:10.1088/0004-637X/814/2/151

     

    Svanda, M., Brun, A.S., Roudier, T., Jouve, L., Polar cap magnetic field reversals during solar grand minima: could pores play a role?, Astronomy and Astrophysics, 586, A123 (11 pp), 2016.
    10.1051/0004-6361/201527314

     

    Brun, A.S., Browning, M.K., Dikpati, M., Hotta, H., Strugarek, A., Recent Advances on Solar Global Magnetism and Variability, Space Science Reviews, 196, 101 (35 pp), 2015

     

    Réville, V., Brun, A.S., Strugarek, A., et al., From Solar to Stellar Corona: The Role of Wind, Rotation, and Magnetism, The Astrophysical Journal, 814, 99 (9 pp), 2015
    10.1088/0004-637X/814/2/99

     

    Alvan, L., Strugarek, A., Brun, A.S., Mathis, S., Garcia, R.A., Characterizing the propagation of gravity waves in 3D nonlinear simulations of solar-like stars, Astronomy and Astrophysics, 581, A112 (13 pp), 2015.

    10.1051/0004-6361/201526250

     

    Augustson, K., Brun, A.S., Miesch, M., Toomre, J., Grand Minima and Equatorward Propagation in a Cycling Stellar Convective Dynamo, The Astrophysical Journal, 809, 149 (25 pp), 2015

    10.1088/0004-637X/809/2/149