Physics of auroral phenomena : proceedings of the 39th annual seminar, Apatity, 29 February-4 March, 2016 / [ed. board: N. V. Semenova, A. G. Yahnin]. - Апатиты : Издательство Кольского научного центра РАН, 2016. - 167 с. : ил., табл.

Proton acceleration in the solarflare >Ф 2 N-i *r w CORONAS F 1 - re<v i § o 31 16 2 1 -I Л “ 1 1 I 1 1 6 :3 0 28 .10.2003. 3- 2 - 1 4 16 :3 3 1 6 :3 6 UT 1 1 :0 0 11:03 1 1 :0 6 1 1 :0 9 U T 1 9 :3 3 1 9 :3 9 19 :4 3 1 9 :5 4 UT Figure 3. The flares gamma-ray according CORONAS F data. The proton flux from the flare that occurred on the eastern part of solar disk (Fig. 2 below), can not reach the GOES spacecraft, moving along the magnetic field lines. At the propagation without collisions, the protons in the interplanetary medium must drift across the magnetic field with the solar wind velocity. Consequently, the particle drift lead to delay the arrival of the protons front to Earth AU/Vsw 3-4 days. In reality (Fig. 2) the delay of protons front from the eastern flares relative to the solar flare is about 3-5 hours. This rapid transfer of protons across the magnetic field may be associated with turbulent diffusion across the magnetic field. Proton flux from the eastern flares, unlike the flux of western flares arises slowly as it should be because o f diffusion. Its typical front duration is about a day. The particle flux directed along the magnetic field line and across the lines is recorded for several days after the end of the flare. That is the flux with the velocity directed along the magnetic field, which decreases by several orders of magnitude, but the diffusion flux velocity of the protons across the magnetic field increases. This behavior is characteristic for protons including the relativistic proton. The measurements on neutron monitors have shown [9- 11] that the so-called prompt component of relativistic protons has a strong anisotropy (magnetic field proton velocity vector is parallel to the lines of the spiral of Archimedes), but the delayed component with an isotropic velocity distribution begins to register in 20-30 minutes. Such a scenario should take place, if the front of the beam of accelerated protons caused the development of plasma turbulence, and then the following particles are scattered in this turbulence. The proton flux becomes isotropic, and its propagation velocity along the field lines decreases. Currently we do not have sufficient information about the development of turbulent processes in the solar wind. Our working hypothesis can be stated as follows. Streams of protons from the flare that occurred on the eastern limb (Fig, 2 below), can not reach the device located at the GOES Earth, moving along the magnetic field lines. At the propagation without collisions, the protons in the interplanetary medium, where the Larmor radius is much smaller then AU, must drift across the magnetic field with the solar wind velocity. The narrow beam of proton front of a western flare moves to the Earth with the particle velocity. The beam caused the development of turbulence, and particle scattering with magnetic fluctuations dramatically increased. The transfer of particles along the field becomes diffusion and its velocity decreases, but the diffusion across the field increases. The velocity of propagation across the field on the long flux front of the eastern flares also rises. As a result, the front of proton fluxes from the eastern flares can move across the magnetic field lines faster then the solar wind. Formulated scheme is in good agreement with measured data, but the detailed investigation of the dynamics of solar cosmic rays requires careful observation and theoretical analysis. The difference of forms of the proton pulses that arrived from the western limb and from the disc center flares can be clearly seen in Fig. 4. This is a rare case when the two proton events occurred with an interval of two days in different active regions of the Sun. At right side of the figure the fronts of arrival of protons and X-ray pulses are presented in an extended time-scalc. The event 06/01/2014 7:30 is appeared just after a start of very weak X-ray flare pulse C2.1. Such weak flares occurring on the visible disc of the Sun never generate large streams of protons. The C2.1 06/01/2014 flare according to the RHESSI data belongs to the active region AO l 1936. It is located on the limb (S15W89). Apparently, X-rays are generated mainly on the back side of the sun. The recorded X-rays might arrive along the Sun surface. Most of X-ray could be screened by the chromosphere. Apparently, the flare C2.1 intensity is greatly underestimated. Protons from this western flare have begun to register in - 20 min after the start of the flare. The proton flux of the C2.1 flare demonstrates a steep front, typical for the large proton pulses of western flares. Fast collision-free flux of protons from C2.1 flare could come to Earth from the back side of the Sun along the magnetic lines of the Archimedes spiral. The flare X I.2 is produced by S12W08 active region near the Sun center little bit shifted to the West. The accelerated protons from this flare appear with 1.5 hours delay and possesses front about 10 hours. The front is not as long as for the proton fluxes generated by flares that appeared in the far West. The same character of diffuse flux of delayed protons from the western and eastern flares in the interplanetary space and the different forms of the proton flux fronts of western and eastern flares are particularly well illustrated by the single flares accompaniment by very long proton fluxes (Fig. 5). No distinctions are observed in the decaying parts of proton pulses that generated by the western and eastern flares. There is no reason to suppose that the mechanism of propagation of protons in the interplanetary medium of the decaying part of the proton pulses is 63