Table 1
Initial parameters.
| Model | Halo | Initial stellar disk | Gas | Bar parameters | |||||||||||||||
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| Type | M h | a h | Type | M d | R d | z d | M gas | R gas | z gas | h | r b | ε b | |||||||
| 1010 M⊙ | kpc | 1010 M⊙ | kpc | kpc | 1010 M⊙ | kpc | kpc | Gyr | kpc | ||||||||||
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| RA | rigid/iso | 5.8 | 5 | rigid/exp | 2 | 3 | 0.3 | 2 | 6 | 0.2 | – | – | – | ||||||
| RA- | rigid/iso | 5.8 | 5 | rigid/exp | 2 | 3 | 0.3 | 2 | 6 | 0.2 | – | – | - | ||||||
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| RB | rigid/iso | 5.8 | 5 | rigid/exp | 2 | 3 | 0.3 | 2 | 6 | 0.2 | 0.2 | 5 | 0.1 | ||||||
| RBm02 | rigid/iso | 5.8 | 5 | rigid/exp | 2 | 3 | 0.3 | 0.2 | 6 | 0.2 | 0.2 | 5 | 0.1 | ||||||
| RB- | rigid/iso | 5.8 | 5 | rigid/exp | 2 | 3 | 0.3 | 2 | 6 | 0.2 | 0.2 | 5 | 0.1 | ||||||
| RBh05 | rigid/iso | 5.8 | 5 | rigid/exp | 2 | 3 | 0.3 | 2 | 6 | 0.2 | 0.5 | 5 | 0.1 | ||||||
| RBh1 | rigid/iso | 5.8 | 5 | rigid/exp | 2 | 3 | 0.3 | 2 | 6 | 0.2 | 1 | 5 | 0.1 | ||||||
| RBe02 | rigid/iso | 5.8 | 5 | rigid/exp | 2 | 3 | 0.3 | 2 | 6 | 0.2 | 0.5 | 5 | 0.2 | ||||||
| RBe05 | rigid/iso | 5.8 | 5 | rigid/exp | 2 | 3 | 0.3 | 2 | 6 | 0.2 | 0.5 | 5 | 0.5 | ||||||
| RBe1 | rigid/iso | 5.8 | 5 | rigid/exp | 2 | 3 | 0.3 | 2 | 6 | 0.2 | 0.5 | 5 | 1.0 | ||||||
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| LB | live/plum | 10 | 10 | live/M-N | 2 | 3 | 0.3 | 2 | 6 | 0.2 | – | – | – | ||||||
| LB- | live/plum | 10 | 10 | live/M-N | 2 | 3 | 0.3 | 2 | 6 | 0.2 | – | – | – | ||||||
Notes. Mh is the halo mass; ah is the halo scale length; Md, Rd, zd are the initial stellar disk mass, radial scale length and vertical scale height respectively; Mgas, Rgas, zgas are the initial stellar disk mass, radial scale length and vertical scale hight respectively; rb is the bar size; εb is the bar potential amplitude; h is the bar growth timescale in models with a rigid bar potential. Models marked by minus include no converging flow criterion in the star-formation prescription. First section of the table shows the model with no bar imposed in the disk (axisymmetric potential); the second section presents models with a rigid potential of bar; and the last section shows the parameters of the self-consistent simulations that have live halos and an initial stellar disk. For simulations with a rigid potential, we adopted an isothermal dark matter (iso) distribution and exponential (exp) stellar disk; for self-consistent simulations we used Plummer (plum) sphere for dark matter halo and Miyamoto-Nagai (M-N) initial stellar disk.
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