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Table 1:

Characteristics of the dynamic atmospheric models for pulsating, C-rich AGB stars used for the modelling (for a detailed description see text and DMA3).

Model: 		W S M
$L_\star$ [$L_{\odot}$] 7000 10 000 7000
$M_\star$ [$M_{\odot}$] 1.0 1.0 1.5
$T_\star$ [K] 2800 2600 2600
[Fe/H] [dex] 0.0 0.0 0.0
C/O by number 1.4 1.4 1.4
$R_{\star }$ [$R_{\odot}$] 355 493 412
  [AU] 1.65 2.29 1.92
log $g_\star$   -0.66 -0.94 -0.61
P [d] 390 490 490
$\Delta u_{\rm p}$ [km s-1] 2 4 6
$f_{\rm L}$   1.0 2.0 1.5
$\Delta m_{\rm bol}$ [mag] 0.21 0.86 1.07

$\langle\dot M\rangle$ 		[ $M_{\odot}\ $yr-1] - $4.3\times 10^{-6}$ $2.5 \times 10^{-6}$
$\langle u \rangle$ [km s-1] - 15 7.5
$\langle f_{\rm c}$$\rangle$   - 0.28 0.40

Notes. Listed are (i) parameters of the hydrostatic initial model; (ii) quantities derivable from these parameters; (iii) attributes of the inner boundary (piston) used to simulate the pulsating stellar interior as well as the resulting bolometric amplitude  $\Delta m_{\rm bol}$; and (iv) properties of the resulting wind. The notation was adopted from previous papers (DMA3, DMA4): P,  $\Delta u_{\rm p}$ - period and velocity amplitude of the piston at the inner boundary; $f_{\rm L}$ - free parameter to adjust the luminosity amplitude at the inner boundary; $\langle\dot M\rangle$, $\langle u \rangle$ - mean mass loss rate and outflow velocity at the outer boundary; $\langle f_{\rm c}$$\rangle$ - mean degree of condensation of carbon into dust at the outer boundary. The radial coordinates in this work are plotted in units of the corresponding stellar radii $R_{\star }$ of the hydrostatic initial models, calculated from their luminosities $L_\star$ and temperatures $T_\star$ (as given in the table) via the relation $L_\star$ = 4$\pi$$R_\star^2$ $\sigma$$T_\star^4$.


Source LaTeX | All tables | In the text

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