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>Brief communication: Lower-bound estimates for residence time of energy in the atmospheres of Venus, Mars and Titan
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Brief communication: Lower-bound estimates for residence time of energy in the atmospheres of Venus, Mars and Titan
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机译：Brief communication: Lower-bound estimates for residence time of energy in the atmospheres of Venus, Mars and Titan
The residence time of energy in a planetary atmosphere, τ , which was recently introduced and computed for the Earth's atmosphere ( Osácar et al. , 2020 ) , is here extended to the atmospheres of Venus, Mars and Titan. τ is the timescale for the energy transport across the atmosphere. In the cases of Venus, Mars and Titan, these computations are lower bounds due to a lack of some energy data. If the analogy between τ and the solar Kelvin–Helmholtz scale is assumed, then τ would also be the time the atmosphere needs to return to equilibrium after a global thermal perturbation.
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