Parametrization of spatial-energy distributions of H+ and O+ ions of the ring current on the main phase of magnetic storms

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Based on the results of measurements near the equatorial plane a fluxes and energy spectra of H+ and O+ ions of the magnetosphere’s ring current by the OGO-3, Explorer 45, AMPTE/CCE, and Van Allen Probes (A and B) satellites, a systematic analysis of spatial distributions of the energy density for these ions on the main phase of magnetic storms was carried out. Twelve storms of different strength were considered, with max|Dst| from 64 to 307 nT. The radial profile of the ring current ions energy density is characterized by the maximum (Lm) and by the ratio of the energy densities of the ions and the magnetic field at this maximum (βm), and at L > Lm this profile is approximated by the function w(L) = w0exp(–L/L0). Quantitative dependences of the parameter Lm on the Dst index and MLT, and also the dependences of the parameters βm, w0 and L0 on the Dst, MLT and Lm, are obtained. These dependences are different for H+ and O+ ions, as well as for ions of low (E < 60 keV) and higher energies. It has been established that in a narrow inner region of the ring current near its maximum in the nighttime hemisphere of the magnetosphere, the ring current asymmetry is much smaller (especially for O+ ions) than at L > Lm. It was found that with increasing L, the asymmetry of the ring current by MLT increases significantly, with H+ ions concentrated at near 18 MLT, and O+ ions at near 24 MLT. It is shown that for O+ ions with E ~ 1–300 keV, βm ∝ Lm–9; this result shows that a deeper penetration of hot plasma into a geomagnetic trap, during strong storms, requires not only a stronger electric field of convection, but also a significant preliminary accumulation and acceleration of ions (especially O+ ions) in the sources of the ring current.

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Sobre autores

A. Kovtyukh

Lomonosov Moscow State University

Autor responsável pela correspondência
Email: kovtyukhas@mail.ru

Skobeltsyn Institute of Nuclear Physics

Rússia, Moscow

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2. Fig. 1. Position of the maximum energy density of CT ions (Lm) in the main phase of different storms depending on |Dst| (a) and MLT (b).

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3. Fig. 2. Ratios of the ion energy density at the CT maximum to the local magnetic field pressure (βm) as a function of |Dst| (a), MLT (b), and Lm (c). Thin lines are root-mean-square power-law approximations of these data.

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4. Fig. 3. Radial profiles of the energy density (w) of H++O+ ions with E ~ 1–300 keV (thin lines) and with E ~ 1–60 keV (dashed lines) for the outer part of the RC during the main phase of various storms.

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5. Fig. 4. Distributions of the parameter w0 of the outer edge of the CT depending on |Dst| (a), MLT (b) and Lm (c). These results relate to the energy density of H++O+ ions and were obtained at the end of the main phase of the storms (except for point 8). The thin lines show the root-mean-square power approximations of these distributions for ions of low (dashed line) and high energies.

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6. Fig. 5. Distributions of the L0 parameter of the outer part of the CT depending on |Dst| (a), MLT (b), and Lm (c). These results relate to the energy density of H++O+ ions with E ~ 1–300 keV and were obtained at the end of the main phase of the storms. The thin lines show the root-mean-square approximations of these distributions.

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7. Fig. 6. Distributions of the parameters w0 and L0 by MLT, constructed separately for H+ and O+ ions.

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8. Fig. 7. Comparison of expressions (4) and (5) obtained for a simple model of CT ion convection (see text).

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9. Fig. 8. Changes in the average values ​​of energy density 〈wH+〉 and 〈wO+〉 (left side of the figure) and the ratio 〈wO+〉/〈wH+〉 (right side of the figure) with an increase in MLT from 18 to 24 h. The beginning of each vector corresponds to 18 MLT, and its end (arrow) to 24 MLT. Thick, thin and dotted vectors correspond to L = 4, 5 and 6.

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