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| Content Provider | Springer Nature Link |
|---|---|
| Author | Kurt, Viktoriya G. Yushkov, B. Yu. Belov, A. V. |
| Copyright Year | 2010 |
| Abstract | Based on our analysis of the data fromthe global network of neutronmonitors for several events, we have found the times of the first increases in count rate at individual stations that precede the main solar cosmic-ray enhancement. The onset time of proton acceleration at the Sun has been determined from the appearance of a broad gamma-ray line with its maximum near 70 MeV that is generated during the decay of neutral pions, which, in turn, are produced when protons with energies above 300 MeV interact with the solar atmosphere. The time of the first recording of energetic protons at the Earth is delayed relative to the time at which these protons appeared at the Sun by 60–300 s, i.e., by a value comparable to the difference between the direct photon and particle propagation times. At least two conclusions follow from the existence of such “precursors”. First, the protons begin to escape from the solar atmosphere into interplanetary space immediately after their acceleration. Second, some of the protons traverse a path shorter than the nominal length of interplanetary magnetic field lines. |
| Starting Page | 520 |
| Ending Page | 530 |
| Page Count | 11 |
| File Format | |
| ISSN | 10637737 |
| Journal | Astronomy Letters |
| Volume Number | 36 |
| Issue Number | 7 |
| e-ISSN | 15626873 |
| Language | English |
| Publisher | SP MAIK Nauka/Interperiodica |
| Publisher Date | 2010-07-08 |
| Publisher Place | Dordrecht |
| Access Restriction | One Nation One Subscription (ONOS) |
| Subject Keyword | solar flares gamma-ray emission solar cosmic rays energetic protons neutron monitors Astrophysics and Astroparticles Astronomy, Observations and Techniques |
| Content Type | Text |
| Resource Type | Article |
| Subject | Astronomy and Astrophysics Space and Planetary Science |
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