We address the problem of early diagnostics of geomagnetic storms based on the use of models of coordinates of movements of centers of solar coronal mass ejections (CME) and observations of their angular positions obtained from space monitoring systems. We propose a method for early diagnostics of geomagnetic storms, introduce a function to predict the distance between Earth and CME centers, and establish a decision-making procedure. We give an example of calculating the distance prediction function and implement the diagnostic decision-making procedure based on coordinate models and model observations of angular positions of CME centers. We determine the efficiency of the decision-making procedure for the algorithm for early diagnostics of geomagnetic storms.

We address the problem of early diagnostics of geomagnetic storms based on the use of models of coordinates of movements of centers of solar coronal mass ejections (CME) and observations of their angular positions obtained from space monitoring systems. We propose a method for early diagnostics of geomagnetic storms, introduce a function to predict the distance between Earth and CME centers, and establish a decision-making procedure. We give an example of calculating the distance prediction function and implement the diagnostic decision-making procedure based on coordinate models and model observations of angular positions of CME centers. We determine the efficiency of the decision-making procedure for the algorithm for early diagnostics of geomagnetic storms.

We calculate the angular distribution of cosmic rays at a given point of the heliosphere under the assumption that the incoming flux from outer space is isotropic. The static magnetic field is shown to cause no anisotropy provided that the observation point is situated out of the trapped particle area. We consider a coronal ejection model in the form of a static cylinder with an axial homogeneous magnetic field inside. We calculate angular distribution samples in the trapped particle area (inside the cylinder) and show that there is a certain cone of directions with a reduced flux. For the same model with the moving cylinder, the angular distribution samples are calculated for different positions of the observation point outside the cylinder. Anisotropy of order of the ejection to light velocity ratio is shown to arise. The calculated samples are in qualitative agreement with URAGAN muon hodoscope data.

No abstract

We calculate the angular distribution of cosmic rays at a given point of the heliosphere under the assumption that the incoming flux from outer space is isotropic. The static magnetic field is shown to cause no anisotropy provided that the observation point is situated out of the trapped particle area. We consider a coronal ejection model in the form of a static cylinder with an axial homogeneous magnetic field inside. We calculate angular distribution samples in the trapped particle area (inside the cylinder) and show that there is a certain cone of directions with a reduced flux. For the same model with the moving cylinder, the angular distribution samples are calculated for different positions of the observation point outside the cylinder. Anisotropy of order of the ejection to light velocity ratio is shown to arise. The calculated samples are in qualitative agreement with URAGAN muon hodoscope data.