Grids of Stellar Evolution Models
Presupernova Structure of Rotating Stars

Data from Heger, Langer, & Woosley (2000)

Hydro / EOS data explanation

column data unit
grid cell number ---
cell outer total mass mass coordinate at the cell top interface g
cell outer radius radius coordinate at the cell top interface cm
cell outer velocity velocity of the cell top interface cm s-1
cell density average density of the cell g cm-3
cell temperature average temperature of the cell K
cell pressure average pressure of the cell dyn cm-2
cell specific energy average specific energy of the cell erg g-1
cell specific entropy average specific entropy of cell kB baryon-1
cell angular velocity average angular velocity of the cell rad s-1
cell A_bar average mean mass number of nuclei in the cell 1
cell Y_e average electrons per baryon in the cell 1
stability hydrodynamic stability of outer cell boundary ---

Network data explanation

APPROX: approximative 19 isotope network
QSE: Quasi Statitstical Equilibrium
isotopes treated in three NSE subgroups which are connected by "bottleneck" reactions
137 isotope network for weak rates
NSE: Nuclear Statistical Equilibrium
137 isotope network for weak rates

column network unit
APPROX QSE / NSE
neutrons neutrons neutrons (mass fraction)
H1 1H protons (mass fraction)
He3 3He --- (mass fraction)
He4 4He 1 < A < 6 (mass fraction)
C12 12C --- (mass fraction)
N14 14N --- (mass fraction)
O16 16O 16O (unburned yet) (mass fraction)
Ne20 20Ne --- (mass fraction)
Mg24 24Mg 22 < A < 29, excluding 28Si (mass fraction)
Si28 28Si 28Si (mass fraction)
S32 32S 28 < A < 36 (mass fraction)
Ar36 36Ar 35 < A < 40 (mass fraction)
Ca40 40Ca 39 < A < 44 (mass fraction)
Ti44 44Ti 43 < A < 48 (mass fraction)
Cr48 48Cr 47 < A < 52 (mass fraction)
Fe52 52Fe --- (mass fraction)
Fe54 54Fe (+56Fe) A approximately 2*Z+2, Iron Peak (mass fraction)
Ni56 56Ni A < 2*Z+2, Iron Peak (mass fraction)
Fe56 --- 56Fe only (mass fraction)
'Fe' --- A > 2*Z + 3, Iron Peak, excluding 56Fe (mass fraction)


The Data

Stars of solar initial metallicity, strong molecular weight barriers
In Heger, Langer, & Woosley (2000) these are the models of the "B" series, i.e., E15B etc.

mass
(solar masses)
ZAMS equatorial rotation velocity
0 km/s 100 km/s 200 km/s 300 km/s
15.0 169 kByte 172 kByte 173 kByte 180 kByte
20.0 188 kByte 194 kByte 195 kByte 191 kByte


Stars of solar initial metallicity, weak mean molecular weight barriers
In Heger, Langer, & Woosley (2000) these are the models of the series without "B", i.e., E15 etc.

mass
(solar masses)
ZAMS equatorial rotation velocity
200 km/s
10.0 181 kByte
12.0 197 kByte
15.0 203 kByte
20.0 196 kByte
25.0 130 kByte

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Acknowledgements: This work has been supported by Prime Contract No. W-7405-ENG-48 between The Regents of the University of California and the United States Department of Energy, by the Deutsche Forschungsgemeinschaft through grants La 587/15 and La 587/16, by the National Science Foundation (AST 97-31569) and by the Alexander von Humboldt Foundation. AH was, in part, supported by a "Doktorandenstipendium aus Mitteln des 2. Hochschulprograms".

Alexander Heger
Thursday, 26-Aug-2004 03:51:55 AEST