\begin{document}$ \nu_H $\end{document}) in the MeV mass range using solar neutrino experiments is presented. \begin{document}$ \nu_H $\end{document}, with masses ranging from a few MeV up to approximately 15 MeV, can be produced in the Sun through 8B decay and subsequently decays into \begin{document}$ \nu_e e^+ e^- $\end{document}. Its flux and lifetime strongly depend on the mixing parameter \begin{document}$ |U_{eH}|^2 $\end{document} and mass \begin{document}$ m_{\nu_H} $\end{document}. The \begin{document}$ \nu_H $\end{document} signal can be detected via its decay products, either the \begin{document}$ e^+e^- $\end{document} pair or \begin{document}$ \nu_e $\end{document}, depending on whether \begin{document}$ \nu_H $\end{document} decays inside or outside the detector. Expected signal yields for both detection methods (detecting \begin{document}$ e^+e^- $\end{document} or \begin{document}$ \nu_e $\end{document} signal) are presented across the full \begin{document}$ |U_{eH}|^2 $\end{document} and \begin{document}$ m_{\nu_H} $\end{document} parameter spaces. These two methods are found to be complementary in different regions of the \begin{document}$ |U_{eH}|^2 $\end{document} and \begin{document}$ m_{\nu_H} $\end{document} phase spaces. By combining both approaches, we anticipate observing at least a handful of signal events across most of the parameter space of \begin{document}$ 10^{-6} \lt |U_{eH}|^2 \lt 1 $\end{document} and 2 MeV \begin{document}$ \lt m_{\nu_H} \lt $\end{document} 15 MeV, assuming a 500-ton solar neutrino experiment operating for one year. Key variables, such as the energy spectra of \begin{document}$ \nu_e $\end{document} or \begin{document}$ e^+e^- $\end{document} and \begin{document}$ \nu_e $\end{document} solar angle, are also discussed to help distinguish the signal from major backgrounds, such as solar neutrino events."> Extending the sensitivity of heavy sterile neutrino searches with solar neutrino experiments -
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