Solar-like oscillations in stars with expanding convective cores.
Grid of models.
Blazej L. Popielski

The models in my grid are characterized by three parameters:
All models were calculated for PopI chemical abundance: X=0.7, Z=0.02. I adopted EOS2001 equation of state and OPAL opacity tables. Further details may be found in Popielski&Dziembowski (2005).

Ranges for mass (M) and large frequency separations (D) were chosen to cover most of evolutionary models with expanding convective core. Table below shows the grid in M (columns) and D (rows).

1.2 1.3 1.5 1.7
93.8 M2a
91.0 M2b M3b
81.6 M2c M3c M5c
74.5 M2d M3d M5d M7d
53.6 M3e M5e M7e
42.3 M7f

For each pair (M, D) four models were calculated adopting various mixing recipes: LY, SC, OV1 and OV2. The picture below shows all SC and OV1 models on an HR diagram. Only two scenarios are shown for clarity. All figures may be downloaded in postscript format, with use of accompanying links.

HR diagram for SC and OV1 models.(ps)
Some standard stellar parameters for all the models may be found in the Table below. These are central hydrogen abundance (Xc), core radius relative to the stellar radius (xcc), mass fraction in the core (mcc), evolutionary status of the core (dmcc: + expanding, - contracting, 0 no core). For each model two data files are available: spectrum and small separation.

LY SC
Xc xcc mcc dmcc data Xc xcc mcc dmcc data
M2a 0.291 0.046 0.021 + spec
ssep		 0.304 0.048 0.022 + spec ssep
M2b 0.248 0.048 0.024 + spec ssep 0.276 0.051 0.029 + spec ssep 
M2c 0.083 0.047 0.036 - spec ssep  0.143 0.054 0.047 - spec ssep 
M2d 0.000 0.000 0.000 0 spec ssep  0.005 0.014 0.028 - spec ssep 
M3b 0.474 0.085 0.034 + spec ssep  0.479 0.086 0.036 + spec ssep 
M3c 0.323 0.095 0.053 + spec ssep  0.335 0.097 0.055 + spec ssep 
M3d 0.206 0.096 0.059 - spec ssep  0.223 0.099 0.052 - spec ssep 
M3e 0.000 0.000 0.000 0 spec ssep  0.000 0.000 0.000 0 spec ssep 
M5c 0.565 0.083 0.079 + spec ssep  0.565 0.084 0.080 + spec ssep 
M5d 0.466 0.079 0.085 + spec ssep  0.467 0.079 0.087 + spec ssep 
M5e 0.065 0.050 0.064 - spec ssep  0.091 0.052 0.070 - spec ssep 
M7d 0.539 0.095 0.111 + spec ssep  0.546 0.096 0.112 + spec ssep 
M7e 0.260 0.146 0.095 - spec ssep  0.270 0.069 0.096 - spec ssep 
M7f 0.035 0.114 0.065 - spec
ssep 		 0.054 0.048 0.069 - spec ssep  
OV1 OV2
Xc xcc mcc dmcc data Xc xcc mcc dmcc data
M2a 0.425 0.088 0.104 - spec ssep  0.509 0.125 0.222 - spec ssep 
M2b 0.390 0.085 0.101 - spec ssep  0.488 0.122 0.220 - spec ssep 
M2c 0.266 0.077 0.100 - spec ssep  0.406 0.111 0.216 - spec ssep 
M2d 0.126 0.066 0.066 - spec ssep  0.327 0.095 0.109 - spec ssep 
M3b 0.544 0.098 0.117 - spec ssep  0.587 0.132 0.248 - spec ssep 
M3c 0.421 0.088 0.116 - spec ssep  0.504 0.120 0.230 - spec ssep 
M3d 0.324 0.081 0.115 - spec ssep  0.440 0.111 0.222 - spec ssep 
M3e 0.000 0.000 0.000 0 spec ssep  0.185 0.082 0.197 - spec ssep 
M5c 0.592 0.108 0.154 - spec ssep  0.616 0.137 0.264 - spec ssep 
M5d 0.510 0.100 0.151 - spec ssep  0.530 0.108 0.183 - spec ssep 
M5e 0.237 0.074 0.137 - spec ssep  0.367 0.097 0.235 - spec ssep 
M7d 0.572 0.116 0.180 - spec ssep  0.592 0.140 0.278 - spec ssep 
M7e 0.352 0.088 0.165 - spec ssep  0.417 0.107 0.249 - spec ssep 
M7f 0.207 0.082 0.158 - spec ssep  0.316 0.089 0.238 - spec ssep 

For each model two kinds of small separations were calculated:
One may compare small separations for models with various mixing recipes on the figures below. For each pair (M, D) two panels are presented, d_01 (left) and d_02 (right). The small separations for four evolutionary scenarios are gathered on both panels.
Small separations for 1.2M models(ps)
Small separations for 1.2M models.(ps)
Small separations for 1.3M models.(ps)
Small separations for 1.3M models.(ps)
Small separations for 1.5M models.(ps)
Small separations for 1.7M models.(ps)

HELAS Workshop Vienna, September 2006