Asymmetries in asymptotic giant branch stars and their winds - I. From 3D RHD models to synthetic observables

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Volume 690 (October 2024)

A&A, 690 (2024) A162

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Table 1.

Stellar properties of models included in this study.

Designation	Pulsation period (d)	M_⋆ (M_⊙)	R_⋆ (au )	L_⋆ (L_⊙)	T_eff (K)
`st28gm06n052`^(a)	545	1.0	1.65	7030	2806 K
`st28gm06n056`^(a)	390	1.0	1.36	5085	2848 K
`M2n315u6`^(b)	490	1.5	1.67	6498	2730 K
Point source ^(c)	N/A	N/A	1.65	6975	2800 K

Additional model parameters

	Snapshot time (yr)	Box size (au)	Number of cells	Includes dust

`st28gm06n052`	29.95	29.8³	679³	Yes
`st28gm06n056`	22.02, 22.18, 22.34	7.3³	317³	No
`M2n315u6`	361.64	46.8 ^(d)	98 ^(d)	No ^(e)

Notes.

^(a)

Stellar mass, radius, bolometric luminosity, effective temperatures are all simulation time averages as computed with CO⁵BOLD.

^(b)

This model is from 1D DARWIN simulations and the snapshot was chosen to have luminosity and radius close to the CO⁵BOLD model star. The effective temperature is given by Stefan-Boltzmann’s law.

^(c)

Point source refers to input stellar parameters for the RADMC-3D test star. Radius and temperature are input values, the luminosity comes from Stefan-Boltzmann’s law.

^(d)

The size and number of cells of the DARWIN model refer to a 1D radial structure (centre to outer edge). The 1D model also uses a self-adaptive grid, concentrating points in critical regions.

^(e)

The original DARWIN model contains dust that is not included in this study.

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