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Magnetized Winds of M-type Stars and Star–Planet Magnetic Interactions: Uncertainties and Modeling Strategy

  • Authors: Victor Réville, Jamie M. Jasinski, Marco Velli, Antoine Strugarek, Allan Sacha Brun, Neil Murphy, Leonardo H. Regoli, Alexis P. Rouillard, Jacobo Varela

Victor Réville et al 2024 The Astrophysical Journal 976 .

  • Provider: AAS Journals

Caption: Figure 5.

Illustration of the energy balance in our simulations according to Equations (10)–(11). Red lines correspond to the kinetic energy luminosity while dark blue lines correspond to the radiated energy. The sum is shown in black and corresponds to the expected input energy in light blue. Dashed lines are used when the turbulence correlation length scale λ = 0.01. The target mass-loss rate (expressed in kinetic luminosity) is given by the horizontal dark line, with the reported uncertainties of Figure 1 in red shades.

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