Speaker
Description
In recent decades, flux-transport-dynamo models have emerged as a promising and crucial framework for understanding the dynamics of the Sun's magnetic field and solar cycle (Choudhuri et al. (1995); Dikpati et al. (2009); Wang et al. (1991)). Their importance lies in their ability to reproduce key features of the solar cycle and provide valuable insights into the Sun's magnetic field behaviour.
In the present communication, we show how by applying spatial truncation on the axisymmetric mean-field dynamo model, two coupled differential equations can be deduced. Then, we employ the solutions of these equations obtained by homotopy and Poincaré–Lindstedt perturbation methods (Chadou et al.(2024)), to propose a new model that describes the true mean magnetic field of the sun.
An interesting breakthrough that emerged from our analysis is that when confronted with the measurements of the sun’s mean line-of-sight field, our model allows us to reconstruct important parameters linked to other solar indicators, suggesting that the key to the underlying dynamics of the sun’s magnetic field lies in the sun-as-a-star magnetic field measurements.
References
Chadou, I., Belhadi, Z., Becheker, K., Zaidi, A., and Bekli, M. R. (2024). Solar magnetic cycles as a van der pol-duffing oscillator: new insights. Monthly Notices of the Royal Astronomical Society, 527(4):10416–10424.
Choudhuri, A. R., Sch¨ussler, M., and Dikpati, M. (1995). Astronomy Astrophysics, 303:L29.
Dikpati, M., Gilman, P. A., Cally, P. S., and Miesch, M. S. (2009). Axisymmetric mhd instabilities in solar/stellar tachoclines. The Astrophysical Journal, 692(2):1421.
Wang, Y.-M., Sheeley Jr., N. R., and Nash, A. G. (1991). The Astrophysical Journal, 383:431.
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