Suppression of photospheric velocity fluctuations in strongly magnetic O stars in radiation-magnetohydrodynamic simulations

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Table 2

Horizontally time-averaged values of R_phot, T_eff, log(g), and T₀ (estimated temperature where magnetic and gas pressure are equal to each other) for all the models in this study.

Model	R_phot (R₀)	T_eff (kK)	log(g) (cm s⁻²)	T₀ (kK)
0 G	1.24	39.98	3.75	—
Radial 1 kG	1.22	40.37	3.76	61.69
Radial 10 kG	1.22	40.05	3.76	193.56
Radial 20 kG	1.25	40.39	3.75	278.66
Horiz. 1 kG	1.30	38.95	3.71	61.41
Horiz.10 kG	1.49	36.86	3.59	196.66
Horiz. 20 kG	1.49	37.97	3.59	286.43

Notes. The models initialised with a uniform radial magnetic field exhibit properties similar to the non-magnetic case, while those with a sufficiently strong horizontal magnetic field show significant deviations from the non-magnetic scenario.

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