Table 1
Basic model parameters and derived quantities.
Model | M⋆ | Menv | L⋆ | ![]() |
xbox | tavg | R⋆,smin | Teff,smin | log gsmin | Ppuls | |
---|---|---|---|---|---|---|---|---|---|---|---|
(M⊙) | (M⋆) | (L⊙) | (R⊙) | (yr) | (R⊙) | (K) | cgs | (d) | |||
st28gm06n051 | 1.0 | 0.182 | 6933 | 6373 | 1558 | 48.27 | 328 | 2907 | −0.598 | 459 | |
st28gm05n056 | 1.0 | 0.399 | 5085 | 3173 | 1263 | 60.20 | 293 | 2848 | −0.498 | 390 | Shock, Sect. 5 |
st28gm05n032 | 1.5 | 0.256 | 6936 | 6373 | 1263 | 24.93 | 280 | 3149 | −0.286 | 256 | |
st35gm04n048 | 5.0 | 0.110 | 40914 | 6373 | 1929 | 26.58 | 623 | 3288 | −0.456 | 523 | Rebound, Sect. 4 |
st35gm04n045 | 5.0 | 0.092 | 41336 | 6373 | 1929 | 20.91 | 597 | 3368 | −0.419 | 516 | Plume, Sect. 3 |
st34gm02n002 | 8.0 | 0.277 | 41675 | 7653 | 1626 | 23.17 | 602 | 3359 | −0.223 | 314 |
Notes. The table shows the model name (composed of “s,” referring to the gravitational potential, “t” for “temperature” followed by two digits indicating the approximate effective temperature, “g” for “gravity” followed by “m” for “minus” and two digits indicating the approximate logarithm of the surface gravity, and “n” for “number” with the model counter); the current stellar mass, M⋆, used for prescribing the gravitational potential; the envelope mass, Menv, derived from integrating the mass density of all grid cells within the computational box; the average emitted luminosity, L⋆; the grid dimensions, ; the edge length of the cubical computational box, xbox; the time, tavg, used for averaging the remaining quantities in this table; the average approximate stellar radius, R⋆,smin, taken as the radial position of the innermost photospheric entropy minimum (see Ahmad et al. 2023); the average approximate effective temperature, Teff,smin; the logarithm of the average approximate surface gravity, log gsmin; the pulsation period, Ppuls; and a comment about the levitation mechanism that we used the model as a reference for. The first three models (with M⋆ = 1 and 1.5 M⊙) are examples of the scenario of darkening due to cool post-shock gas (see Sect. 5). The 5 M⊙ model st35gm04n048 shows a prominent dimming event due to a convective rebound (we present in Sect. 4). The remaining two models (with M⋆ = 5 and 8 M⊙) show dark patches due to plumes (see Sect. 3).
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