Fundamentals of Differences Between Quasi-Stationary and Sporadic Solar Wind Flows in Earth's Orbit

The stable existence of 4 coronal holes on the solar surface is shown, which during two Carrington revolutions CR2081 and CR2082 emit four stable quasi-stationary SW (solar wind) flows towards the Earth. The position of the neutral line of the IMF (interplanetary magnetic field) CR 2081 and CR 2082 also remains stable. For quasi-stationary SW flows, the maximum velocity Vmax weakly depends on the corresponding magnetic field B at the moment of time, the value of which at the Earth's orbit is in the range of ≈ (2–8) nT. For sporadic SW, Vmax increases more than twice, with B (IMF strength modulus) values in the range of large values from ≈ 15 nT to ≈ 52 nT. Thus, measuring the value of “B” at the moment of registration, the value of Vmax allows us to understand in advance whether the observed SW flow is quasi-stationary or sporadic. Predict whether the observed SW flow is of the quasi-stationary or sporadic type.