Variations in the X-ray Intensity of the Solar Corona and Heating of the Coronal Plasma in the Context of the Quantum Th
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Variations in the X-ray Intensity of the Solar Corona and Heating of the Coronal Plasma in the Context of the Quantum Theory of Photon Pairs I. K. Mirzoevaa, * and S. G. Chefranovb a
b
Space Research Institute, Russian Academy of Sciences, Moscow, 117997 Russia Obukhov Institute of Atmospheric Physics, Russian Academy of Sciences, Moscow, 119017 Russia *e-mail: [email protected] Received February 21, 2018
Abstract―Data obtained in the framework of the INTERBALL–Tail Probe (1995–2000) and RHESSI (from 2002 to the present) projects have revealed variations in the X-ray intensity of the solar corona in the photon energy range of 2−15 keV during the period of the quiet Sun. Previously, a hypothesis was proposed that this phenomenon could be associated with the effect of coronal heating. In the present study, a new mechanism of coronal plasma heating is proposed on the basis of the experimental data and the quantum theory of photon pairs that are produced from vacuum in the course of the Universe’s expansion. A similar mechanism based on the splitting of photon pairs in the interplanetary and intergalactic space is also proposed to explain the observed microwave background radiation. DOI: 10.1134/S1063780X18100094
1. INTRODUCTION In the previous studies [1–3], variations in the intensity of solar X-ray emission in the photon energy range from 2 to 15 keV during the period of the quiet Sun were investigated. The phenomenon of a decrease in the intensity of solar emission in narrow subranges of the X-ray spectrum in the photon energy range of 2−15 keV was revealed in 2005 [1] by analyzing the data of the INTERBALL–Tail Probe project. Further, this phenomenon was confirmed by the data of the RHESSI project. In [2, 3], the total range of soft X-ray (SXR) emission from 3 to 11 keV was divided into narrow subranges of width 1 keV, i.e., the X-ray spectrum was separately analyzed in the following subranges: 3– 4, 4–5, 5–6, 6–7, 7–8, 8–9, 9–10, and 10–11 keV. Such a partition of the spectrum made it possible to observe a drop (in some cases, an increase) in the X-ray intensity of microflares and thermal background radiation of the solar corona. In some cases, the maximum drop in the X-ray intensity was shifted toward harder spectral range. Detailed analysis of the observational data revealed the subranges in which the X-ray intensity most often decreased: these are the subranges of 3–4 and 4–5 keV and, in some cases, the subranges of 7–8 and 8–9 keV. Along with this drop, an increase in the X-ray intensity was also observed in the spectral subrange of 10–11 keV compared to the other subranges in the total spectral range of 3–16 keV.
Let us consider an example of an atypical energy spectrum of the thermal X-ray background of the solar corona [3]. Figure 1 shows almost quiet thermal X-ray background of the solar corona recorded during 7 min on March 10, 2003. In the figure, one can see the above-mentioned drop in the X-ray intensity in the subrange of 3–4 keV and, simultaneously, an increase in the intensity in the
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