Long-lived recurrent fluxes of energetic ions from solar coronal holes

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Abstract

The results of studying the relative abundances and energy spectra of 4He, C, O, and Fe suprathermal ions in particle fluxes from long-lived near-equatorial coronal holes are presented. It was found that the ion energy spectra had a power or exponential form and, in a number of events, increased particle fluxes were observed in the region of ion energies (~0.2–1.5 MeV/nucleon), creating a fracture in the spectra, which may be due to additional ions accelerated beyond 1 au.

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About the authors

M. A. Zeldovich

Lomonosov Moscow State University

Author for correspondence.
Email: ms.zeldovich@mail.ru
Russian Federation, Moscow

Yu. I. Logachev

Lomonosov Moscow State University

Email: ms.zeldovich@mail.ru
Russian Federation, Moscow

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2. Fig. 1. Relative content of solar wind thermal ions He/O (solid rhombuses), C/O (solid triangles), and Fe/O (solid circles) and suprathermal ions He/O (grey rhombuses), C/O (empty triangles), and Fe/O (empty circles) with energies of 0. 04-0.08 MeV/nucleon in the particle fluxes from the long-lived CH1 CD [12] at 29 solar revolutions since the beginning of its existence (38 solar revolutions) as a function of the maximum solar wind velocity from this CD, according to [14]

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3. Fig. 2. Energy spectra of suprathermal 4He ions accelerated in recurrent particle streams from the long-lived CH1 CD studied here [12] (a) at four different revolutions of its existence: 1) No. 19 18-19/12/2007, 2) No. 15 3/9/2007, 3) No. 14 7/8/2007, 4) No. 12 14-15/6/2007. Energy spectra of suprathermal 4He (rhombuses), C (grey triangles), O (empty triangles) and Fe (black circles) ions in the ion fluxes from KD at the 14th turn of CH2 [12] existence (b) observed on 15-16.08.2008

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