Ohmic Dissipation in Mini-Neptunes

• Published in: arXiv.org 2017-09
• Main Authors: Bonan Pu, Valencia, Diana
• Format: Article
• Language: English
• Subjects: Atmospheric models; Energy dissipation; Heating; Magnetic induction; Ohmic dissipation; Planetary composition; Planetary magnetic fields; Planetary mass; Planets; Thermal evolution
• ISSN: 2331-8422
• DOI: 10.48550/arxiv.1709.01642

In the presence of a magnetic field and weakly ionizing winds, ohmic dissipation is expected to take place in the envelopes of Jovian and lower-mass planets alike. While the process has been investigated on the former, there have been no studies done on mini-Neptunes so far. From structure and thermal evolution models, we determine that the required energy deposition for halting the contraction of mini-Neptunes increases with planetary mass and envelope fraction. Scaled to the insolation power, the ohmic heating needed is small \(\sim10^{-5}\) -- orders of magnitude lower than for exo-Jupiters \(\sim 10^{-2}\). Conversely, from solving the magnetic induction equation, we find that ohmic energy is dissipated more readily for lower-mass planets and those with larger envelope fractions. Combining these two trends, we find that ohmic dissipation in hot mini-Neptunes is strong enough to inflate their radii (\(\sim 10^{15}\) W for \(T_{eq}=1400K\)). The implication is that the radii of hot mini-Neptunes may be attributed in part to ohmic heating. Thus, there is a trade-off between ohmic dissipation and H/He content for hot mini-Neptunes, adding a new degeneracy for the interpretation of the composition of such planets. In addition, ohmic dissipation would make mini-Neptunes more vulnerable to atmospheric evaporation.