Effects of electromagnetic fluctuations in plasmas on solar neutrino fluxes

Eunseok Hwang, Dukjae Jang, Kiwan Park, Motohiko Kusakabe, Toshitaka Kajino, A. Baha Balantekin, Tomoyuki Maruyama, Youngshin Kwon, Kyujin Kwak, Myung-Ki Cheoun

Submitted on 2 November 2022


We explore the effects of electromagnetic (EM) fluctuations in plasmas on solar neutrino fluxes exploiting the fluctuation-dissipation theorem. We find that the EM spectrum in the solar core is enhanced by the EM fluctuations due to the high density of the Sun, which increases the radiation energy density and pressure. By the EM fluctuations involving the modified radiation formula, the central temperature decreases when the central pressure of the Sun is fixed. With a help of the empirical relation between central temperature and neutrino fluxes deduced from the numerical solar models, we present the change in each of the solar neutrino fluxes by the EM fluctuations. We also discuss the enhanced radiation pressure and energy density by the EM fluctuations for other astronomical objects.


Subjects: Astrophysics - Solar and Stellar Astrophysics; Astrophysics - High Energy Astrophysical Phenomena; Nuclear Theory; Physics - Plasma Physics


EM spectrum in the solar center. Red-solid and blue-dashed lines denote $S_{\rm EM}(\omega)$ and $S_{\rm BB}(\omega)$, respectively. The vertical dashed line indicates the peak intensity region of $\omega = 2.8 T_c$ where $T_c$ denoted the central temperature of the Sun. The density and temperature in the center is adopted as $\rho_c = 6.38 \times 10^{8}\,{\rm keV}^4\ (= 1.48 \times 10^2\,{\rm g/cm^3}\ {\rm in\ cgs\ unit)}$, and $T_c=1.34\,{\rm keV}\ (=1.56\times10^7\,{\rm K})$, respectively \cite{bahcall1988}. Nuclear mass fractions are taken from the SSM \cite{bahcall1988}.