Propagation of solar disturbances and heliospheric storms

In this paper, we review solar disturbances (solar flares) and their propagation towards the earth and to the heliosphere. For solar flares, we consider that a photospheric dynamo supplies the power and that high speed streams are caused by the basic solar wind (modified by the solar magnetic field), not from coronal holes. These new views allow us to predict the occurrence of solar flares and the 27-day recurrent storms more accurately than in the past. It is suggested that the explosive aspect of solar flares, the phenomenon, called ‘diparition brusques (DB)’, is the source of coronal mass ejections (CMEs)/magnetic clouds (MCs) and of heliospheric disturbances, namely heliospheric storms. It is also suggested that some CMEs have a magnetically helical structure, which are rooted at the sun. For the inner heliospheric storms, a simple method, called the HAF method, is used to study the propagation of solar disturbances and tested by various simultaneous space probes, such as IMP, HELIOS A, and B for the inner heliosphere. For the middle heliosphere, the same method is tested at a distance 7 au with the Pioneer 11 data; the result is satisfactory. The method is further extended to 100 au in an early 2004; thus, it is possible to envisage the whole heliospheric disturbances over 200 days.

[1]  Lou‐Chuang Lee,et al.  The basic solar wind speed distribution and its sunspot cycle variations , 2023, Frontiers in Astronomy and Space Sciences.

[2]  Q. Hu,et al.  Whether Small Flux Ropes and Magnetic Clouds Have the Same Origin: A Statistical Study of Small Flux Ropes in Different Types of Solar Wind , 2020, The Astrophysical Journal.

[3]  Lou‐Chuang Lee,et al.  On the explosive nature of auroral substorms and solar flares: The electric current approach , 2019, Journal of Atmospheric and Solar-Terrestrial Physics.

[4]  M. Tokumaru,et al.  Comparison of Cylindrical Interplanetary Flux-Rope Model Fitting with Different Boundary Pitch-Angle Treatments , 2019, Solar Physics.

[5]  S. Poedts,et al.  The Magnetic Morphology of Magnetic Clouds: Multi-spacecraft Investigation of Twisted and Writhed Coronal Mass Ejections , 2019, The Astrophysical Journal.

[6]  R. Lepping,et al.  A comparison between the geoeffectiveness of north‐south and south‐north magnetic clouds and an associated prediction , 2017 .

[7]  R. Lepping,et al.  Average Magnetic Field Magnitude Profiles of Wind Magnetic Clouds as a Function of Closest Approach to the Clouds’ Axes and Comparison to Model , 2016 .

[8]  T. Howard,et al.  THE FORMATION AND LAUNCH OF A CORONAL MASS EJECTION FLUX ROPE: A NARRATIVE BASED ON OBSERVATIONS , 2014 .

[9]  P. Démoulin,et al.  In situ properties of small and large flux ropes in the solar wind , 2014, 1408.5520.

[10]  A. Vourlidas,et al.  Three-Dimensional Evolution of Flux-Rope CMEs and Its Relation to the Local Orientation of the Heliospheric Current Sheet , 2013, 1312.0458.

[11]  R. Skoug,et al.  WEAKEST SOLAR WIND OF THE SPACE AGE AND THE CURRENT “MINI” SOLAR MAXIMUM , 2013 .

[12]  P. Démoulin,et al.  Global axis shape of magnetic clouds deduced from the distribution of their local axis orientation , 2013, 1305.4039.

[13]  P. Hess,et al.  A Comparative Study of Coronal Mass Ejections with and Without Magnetic Cloud Structure near the Earth: Are All Interplanetary CMEs Flux Ropes? , 2013 .

[14]  P. Démoulin,et al.  Dynamical evolution of a magnetic cloud from the Sun to 5.4 AU , 2011, 1108.0951.

[15]  N. Lugaz,et al.  Numerical Modeling of Interplanetary Coronal Mass Ejections and Comparison with Heliospheric Images , 2010, 1008.5394.

[16]  S. Akasofu,et al.  A New Morphology of Solar Activity and Recurrent Geomagnetic Disturbances: The Late-Declining Phase of the Sunspot Cycle , 2005 .

[17]  D. Odstrcil,et al.  Three‐dimensional MHD simulation of a loop‐like magnetic cloud in the solar wind , 2002 .

[18]  Craig E. Deforest,et al.  The origin and development of the May 1997 magnetic cloud , 2000 .

[19]  M. Dryer.  Interplanetary studies: Propagation of disturbances between the Sun and the magnetosphere , 1994 .

[20]  H. Zirin,et al.  Vector magnetic field changes associated with X-class flares , 1994 .

[21]  S. Akasofu,et al.  The sunspot cycle variations of the neutral line on the source surface , 1989 .

[22]  S. Wu,et al.  Magnetohydrodynamics of atmospheric transients. IV - Nonplane two-dimensional analyses of energy conversion and magnetic field evolution. [during corona following solar flare] , 1982 .

[23]  K. Hakamada,et al.  Simulation of three-dimensional solar wind disturbances and resulting geomagnetic storms , 1982 .

[24]  F. Mariani,et al.  Magnetic loop behind an interplanetary shock: Voyager, Helios and IMP-8 observations , 1981 .

[25]  D. Covey,et al.  Magnetic field configuration of the heliosphere in interstellar space , 1981 .

[26]  S. Akasofu,et al.  A study of the propagation of solar particles in interplanetary space - the center-limb effect of the magnitude of cosmic-ray storms and of geomagnetic storms. , 1965 .

[27]  K. Marubashi.  Interplanetary magnetic flux ropes observed by the pioneer venus orbiter , 1991 .

[28]  S. Akasofu,et al.  A first generation numerical geomagnetic storm prediction scheme , 1986 .

[29]  S. Wu,et al.  Magnetohydrodynamics of atmospheric transients. II - Two-dimensional numerical results for a model solar corona , 1978 .