A study on the solar coronal dynamics during the post-maxima phase of the solar cycle 24 using S-band radio signals from the Indian Mars Orbiter Mission

Radio signals from India's Mars Orbiter Mission (MOM) have been used to study turbulence in the solar plasma during the post-maximum phase of solar cycle 24. S-band (2.29 GHz) radio carrier downlink signals from MOM were received at the Indian Deep Space Network, Bangalore, and frequency residuals were spectrally analysed to obtain coronal turbulence spectra at heliocentric distances ranging between 4 and 20 R-circle dot, corresponding to coronal regions where the solar wind is primarily accelerated. The frequency fluctuation spectrum relates to the turbulence regime in the near-Sun region. The turbulence power spectrum (the temporal spectrum of frequency fluctuations) at smaller heliocentric distances (<10 R-circle dot) reveals flattening in lower-frequency regions, with a spectral index alpha(f) similar to 0.3-0.5, which corresponds to the solar wind acceleration region. For larger heliocentric distances (>10 R-circle dot), the curve steepens with a spectral index alpha(f) similar to 0.7-0.8, a value close to 2/3 and indicative of a developed Kolmogorov-type turbulence spectrum. The findings are consistent with earlier results. Plausible explanations to support the theory of coronal heating by magnetohydrodynamic waves and the acceleration of the solar wind are presented. An insight into the feeble maximum of solar cycle 24 is discussed.

Automated summary

Radio signals from India's Mars Orbiter Mission were used to study turbulence in the solar plasma, and the corresponding turbulence power spectrum was obtained. These findings are important for understanding the mechanisms of solar wind acceleration and coronal heating.