Atmospheric losses of N+ and O+ under the extreme solar conditions during geomagnetic reversals

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According to the widespread concept, the magnetosphere shields the planet's atmosphere from erosion caused by the solar wind. We have previously shown that during geomagnetic polarity reversals, when the magnetic field weakens to about 10 % of the present one, its shielding is still effective. This conclusion was obtained for quiet periods of solar activity. However, since the duration of a geomagnetic reversal can cover several thousand years, during which many extreme events can occur, changes in solar parameters such as solar wind pressure and EUV-flux should be considered. At high EUV-flux, the concentrations of nitrogen and oxygen, as well as their losses, increase in the Earth's upper atmosphere. We have considered the most significant mechanisms of heavy ion escape from Earth's atmosphere and estimated their losses within the framework of a semi-empirical model. The results show that a weak geomagnetic field and strong solar activity lead to a change in the dominant escape mechanism and to significant atmospheric losses of preferentially lighter isotopes.

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Sobre autores

O. Tsareva

Space Research Institute

Autor responsável pela correspondência
Email: olga8.92@mail.ru
Rússia, Moscow

A. Cannell

USP

Email: olga8.92@mail.ru

Institute of Advanced Studies (Human Evolution)

Brasil, São Paulo

N. Levashov

Space Research Institute; Lomonosov MSU

Email: olga8.92@mail.ru

Faculty of Physics

Rússia, Moscow; Moscow

H. Malova

Space Research Institute; Lomonosov MSU

Email: olga8.92@mail.ru

Scobeltsyn Institute of Nuclear Physics

Rússia, Moscow; Moscow

V. Popov

Space Research Institute; Lomonosov MSU; National Research University “Higher School of Economics”

Email: olga8.92@mail.ru

Faculty of Physics

Rússia, Moscow; Moscow; Moscow

L. Zelenyi

Space Research Institute; Lomonosov MSU

Email: olga8.92@mail.ru

Scobeltsyn Institute of Nuclear Physics

Rússia, Moscow; Moscow

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2. Fig. 1. (a) – frequency of geomagnetic reversals in the Phanerozoic era and their modeled values (dashed), for which data are missing [5]. (b) – percentage and mass of atmospheric oxygen O2 [7]; (c) – secular changes in nitrogen isotope ratios δ15N with an average value of +2.0±0.3‰ (dashed line) [8]. The average long-term trend is shown by the black curve and the uncertainty region around it. The symbol δ expresses the change in isotope ratios between the sample and the standard: δX = (Rsample/ Rstandart – 1) . 1000 ‰, where R is the ratio of the heavy/light isotope of element X

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3. Fig. 2. (a) – oxygen O+ (solid) and nitrogen N+ (dashed) ion density profiles, (b) – temperature and (c) – exobase height obtained from the theoretical model [14] similar to the GAIT model [21], under different conditions of solar EUV flux (normalized to the modern average solar flux of ~1×EUV, which is a solar flux of EUV ≈ 5.1 mW/m2)

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4. Fig. 3. Fractionation (separation) coefficient of nitrogen (dashed) and oxygen (solid) isotopes due to SW-induced losses, depending on EUV flux (at SW pressure Psw0 = 1.4 nPa and in the absence of intrinsic magnetic field BTot = 0 μT)

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5. Fig. 4. Oxygen O+ (solid) and nitrogen N+ (dashed) ion loss rates as a function of solar EUV flux: (a) – contribution of each dissipation mechanism for a quadrupole magnetic field with μT and at SW pressure of 1.4 nPa; (b, c) – total O+ and N+ loss rates for different magnetic field strengths and configurations at 1.4 nPa and 30 nPa

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6. Fig. 5. Oxygen O+ (solid) and nitrogen N+ (dashed) ion loss rates for a quadrupole magnetic field with μT (thin) and = 0. 25 μT (thick) as a function of SW pressure

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