Development of Coronal Field and Solar Wind Components for MHD Interplanetary Simulations

Authors: Ljubomir Nikolic, Larisa Trichtchenko

Abstract:

The connection between solar activity and adverse phenomena in the Earth’s environment that can affect space and ground based technologies has spurred interest in Space Weather (SW) research. A great effort has been put on the development of suitable models that can provide advanced forecast of SW events. With the progress in computational technology, it is becoming possible to develop operational large scale physics based models which can incorporate the most important physical processes and domains of the Sun-Earth system. In order to enhance our SW prediction capabilities we are developing advanced numerical tools. With operational requirements in mind, our goal is to develop a modular simulation framework of propagation of the disturbances from the Sun through interplanetary space to the Earth. Here, we report and discuss on the development of coronal field and solar wind components for a large scale MHD code. The model for these components is based on a potential field source surface model and an empirical Wang-Sheeley-Arge solar wind relation. 

Keywords: Space weather, numerical modeling, coronal field, solar wind.

Digital Object Identifier (DOI): doi.org/10.5281/zenodo.1062642

References:

[1] E. N. Parker, "Suprathermal particle generation in the solar corona," Astrophys. J., vol. 128, p. 677, 1958.
[2] R. Tousey, "The solar corona," in Space research XIII, eds. M. J. Rycroft and S. K. Runcorn, Akademie-Verlag, Berlin, 1973, p. 713.
[3] H. Koskinen, and T. Pulkkinen, "State of the art space weather modelling and proposed ESA strategy," SPEE-WP310-TN, 1998.
[4] National Space Weather Program Implementation Plan, FCM-P31-2000, US, 2002.
[5] National Space Weather Program Strategic Plan, FCM-P30-2010, US, 2010.
[6] Space Weather Canada, Natural Resources Canada. http://www.spaceweather.ca
[7] C. N. Arge, and V. J. Pizzo, "Improvement in the prediction of solar wind conditions using near-real time solar magnetic field updates," Journal of Geophys. Res., vol. 105, p. 465, 2000.
[8] C. N. Arge, D. Odstrcil, V. J. Pizzo, and L. R. Mayer, "Improved method for specifying solar wind speed near the Sun," Solar Wind Ten, Conference Proceedings, vol. 679, p. 190, 2003.
[9] C. D. Fry et al., "Forecasting solar wind structures and shock arrival times using an ensemble of models," J. Geophys. Res. vol. 108, p. 1070, 2003.
[10] Z. Smith, M. Dryer, E. Ort, and W. Murtagh, "Performance of interplanetary shock prediction models," J. Atmos. Sol.-Terr. Phy., vol. 62, p. 1265, 2000.
[11] D. Odstrcil et al., "Initial coupling of coronal and heliospheric numerical magnetohydrodynamic codes," J. Atmos. Sol.-Terr. Phy., vol. 66, p. 1311, 2004.
[12] V. J. Pizzo et al., "Wang-Sheeley-Arge-Enlil cone model transitions to operations," Space Weather, vol. 9, p. S03004, 2011.
[13] M. D. Altschuler, and G. Newkirk , "Magnetic field and the structure of the solar corona," Sol. Phys., vol. 9, p. 131, 1969.
[14] M. D. Altschuler et al., "High resolution mapping of the magnetic field of the solar corona," Sol. Phys., vol. 51, p. 345, 1977.
[15] P. Riley et al., "A comparison between global magnetohydrodynamic and potential field source surface model results," Astrophys. J., vol. 653, p. 1510, 2006.
[16] K. H. Schatten, "Current sheet magnetic model for the solar corona," Cosmic Electrodynamics, vol. 2, p. 232, 1971.
[17] P. MacNeice, "Validation of community models: 2. Development of a baseline using Wang-Sheeley-Arge model," Space Weather, vol. 7, p. S12002, 2009.
[18] National Solar Observatory, Global Oscillation Network Group. http://gong.nso.edu/
[19] NASA. http://heasarc.gsfc.nasa.gov/fitsio/
[20] G. T'oth, B. van der Holst, and Z. Huang, "Obtaining potential field solution with spherical harmonics and finite differences," Astrophysical Journal, vol. 732, a. 102, 2011.
[21] Advanced Composition Explorer (ACE). http://www.srl.caltech.edu/ACE/