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Time Scale of the Largest Imaginable Magnetic Storm : Volume 20, Issue 1 (08/01/2013)

By Vasyliūnas, V. M.

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Book Id: WPLBN0003988415
Format Type: PDF Article :
File Size: Pages 5
Reproduction Date: 2015

Title: Time Scale of the Largest Imaginable Magnetic Storm : Volume 20, Issue 1 (08/01/2013)  
Author: Vasyliūnas, V. M.
Volume: Vol. 20, Issue 1
Language: English
Subject: Science, Nonlinear, Processes
Collections: Periodicals: Journal and Magazine Collection (Contemporary), Copernicus GmbH
Historic
Publication Date:
2013
Publisher: Copernicus Gmbh, Göttingen, Germany
Member Page: Copernicus Publications

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Vasyliūnas, V. M. (2013). Time Scale of the Largest Imaginable Magnetic Storm : Volume 20, Issue 1 (08/01/2013). Retrieved from http://hawaiilibrary.net/


Description
Description: Max-Planck-Institut für Sonnensystemforschung, 37191 Katlenburg-Lindau, Germany. The depression of the horizontal magnetic field at Earth's equator for the largest imaginable magnetic storm has been estimated (Vasyliūnas, 2011a) as −Dst ~ 2500 nT, from the assumption that the total pressure in the magnetosphere (plasma plus magnetic field perturbation) is limited, in order of magnitude, by the minimum pressure of Earth's dipole field at the location of each flux tube. The obvious related question is how long it would take the solar wind to supply the energy content of this largest storm. The maximum rate of energy input from the solar wind to the magnetosphere can be evaluated on the basis either of magnetotail stress balance or of polar cap potential saturation, giving an estimate of the time required to build up the largest storm, which (for solar-wind and magnetospheric parameter values typical of observed superstorms) is roughly between ~2 and ~6 h.

Summary
Time scale of the largest imaginable magnetic storm

Excerpt
Gonzalez, W. D.: A unified view of solar wind-magnetosphere coupling functions, Planet. Space Sci., 38, 627–632, 1990.; Carovillano, R. L. and Siscoe, G. L.: Energy and momentum theorems in magnetospheric dynamics, Rev. Geophys. Space Phys., 11, 289–353, 1973.; Dal Lago, A., Gonzalez, W. D., Balmaceda, L. A., Vieira, L. E. A., Echer, E., Guarnieri, F. L., Santos, J., da Silva, M. R., de Lucas, A., Clúa de Gonzalez, A. L., Schwenn, R., and Schuch, N. J.: % The 17–22 October (1999) solar-interplanetary-geomagnetic event: Very intense geomagnetic storm associated with a pressure balance between interplanetary coronal mass ejection and a high-speed stream, J. Geophys. Res., 111, A07S14, doi:10.1029/2005JA011394, 2006.; Echer, E., Gonzalez, W. D., and Tsurutani, B. T.: Interplanetary conditions leading to superintense geomagnetic storms (Dst ≤ −250 nT) during solar cycle 23, Geophys. Res. Lett., 35, L06S03, doi:10.1029/2007GL031755, 2008.; Gonzalez, W. D. and Mozer, F. S.: A quantitative model for the potential resulting from reconnection with an arbitrary interplanetary magnetic field, J. Geophys. Res., 79, 4186–4194, 1974.; Gonzalez, W. D., Tsurutani, B. T., Gonzalez, A. L. C., Smith, E. J., Tang, F., and Akasofu, S.-I.: Solar wind-magnetosphere coupling during intense magnetic storms (1978–1979), J. Geophys. Res., 94, 8835–8851, 1989.; Gonzalez, W. D., Joselyn, J. A., Kamide, Y., Kroehl, H. W., Rostoker, G., Tsurutani, B. T., and Vasyli{\=u}nas, V. M.: What is a geomagnetic storm?, J. Geophys. Res., 99, 5771–5792, 1994.; Gonzalez, W. D., Echer, E., Tsurutani, B. T., Clúa de Gonzalez, A. L., and Dal Lago, A.: Interplanetary origin of intense, superintense and extreme geomagnetic storms, Space Sci. Rev., 158, 69–89, doi:10.1007/s11214-010-9715-2, 2011.; Hairston, M. R., Drake, K. A., and Skoug, R.: Saturation of the ionospheric polar cap potential during the October–November 2003 superstorms, J. Geophys. Res., 110, A09S26, doi:10.1029/2004JA010864, 2005.; Siscoe, G. L. and Cummings, W. D.: On the cause of geomagnetic bays, Planet. Space Sci., 17 1795–1802, 1969.; Siscoe, G. L. and Crooker, N. U.: A theoretical relation between DST and the solar wind merging electric field, Geophys. Res. Lett., 1, 17–19, 1974.; Hill, T. W., Dessler, A. J., and Wolf, R. A.: Mercury and Mars: The role of ionospheric conductivity in the acceleration of magnetospheric particles, Geophys. Res. Lett., 3, 429–432, 1976.; Kan, J. R. and Lee, L. C.: Energy coupling function and solar wind-magnetosphere dynamo, Geophys. Res. Lett, 6, 577–580, 1979.; Kan, J. R., Lee, L. C. and Akasofu, S.-I.: The energy coupling function and the power generated by the solar wind-magnetosphere dynamo, Planet. Space Sci., 28, 823–825, 1980.; Kivelson, M. G. and Ridley, A. J.: Saturation of the polar cap potential: Inference from Alfvén wing arguments, J. Geophys. Res., 113, A05214, doi:10.1029/2007JA012302, 2008.; Koskinen, H. E. J. and Tanskanen, E. I.: Magnetospheric energy budget and the epsilon parameter, J. Geophys. Res., 107, 1415, doi:10.1029/2002JA009283, 2002.; Shepherd, S. G.: Polar cap potential saturation: Observations, theory, and modeling, J. Atmos. Solar-Terr. Phys., 69

 

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