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J/MNRAS/408/827      Simulations of supernova explosions        (Dessart+, 2010)
Determining the main-sequence mass of type II supernova progenitors.
    Dessart L., Livne E., Waldman R.
   <Mon. Not. R. Astron. Soc., 408, 827-840 (2010)>
   =2010MNRAS.408..827D
ADC_Keywords: Supernovae ; Models, atmosphere

Keywords: hydrodynamics - radiative transfer - stars: atmospheres -
          stars: supernovae: general

Abstract:
    We present radiation-hydrodynamic simulations of core-collapse
    supernova (SN) explosions, artificially generated by driving a 
    piston at the base of the envelope of a rotating or non-rotating
    red-supergiant progenitor star. We search for trends in ejecta
    kinematics in the resulting Type II-Plateau (II-P) SN, exploring
    dependencies with explosion energy and pre-SN stellar-evolution model.

File Summary:

       FileName      Lrecl  Records   Explanations

ReadMe            80        .   This file
table1.dat        65        9   Summary of the properties for a representative
                              sample of pre-SN models employed in this study
simul.dat        103      229   Summary of properties (tables 2-7 of the paper)


Byte-by-byte Description of file: table1.dat

   Bytes Format Units   Label     Explanations

   1-  3  A3    ---     Model     Pre-SN model designation (1)
   5-  8  F4.1  Msun    Mi        Initial mass (i.e. the main-sequence mass)
  10- 14  F5.2  Msun    Mf        Final mass (i.e. the mass at core collapse)
  16- 19  F4.2  Msun    Mcore     Lagrangian mass delimiting outer edge of the core
  21- 24  F4.2  Msun    MeO       Lagrangian mass delimiting outer edge of the
                                oxygen (O) shell
  26- 29  F4.2  Msun    MeHe      Lagrangian mass delimiting outer edge of the
                                helium (He) shell
  31- 35  F5.2  Msun    MiH       Lagrangian mass delimiting inner edge of the
                                hydrogen (H) shell
  37- 40  F4.2  Msun    MHenv     Mass of the hydrogen-rich envelope
  42- 46  F5.2  10+8km  DR        Size of the hydrogen-rich envelope (in 1013cm)
  48- 53  F6.3  10+8km  R*        surface radius (in 1013cm)
  55- 59  F5.3  10+44J  Egrav     Gravitational energy of the progenitor
                                envelope outside of Mcore (in 1051erg)
  61- 65  F5.3  10+44J  Ebind     Binding energy of the progenitor envelope
                                outside of Mcore (in 1051erg)

Note (1): pre-SN models are:
  * Non-rotating ('s' series): Woosley, Heger and Weaver, 2002, 
    Rev. Modern Phys. 74, 1015 (WHW02)
  * rotating ('E' series): Heger, Langer & Woosley, 2000ApJ...528..368H (HLW00)


Byte-by-byte Description of file: simul.dat

   Bytes Format Units   Label     Explanations

       1  I1    ---     Case      [2/7] Model cases (1)
   3- 15  A13   ---     Sim       Simulation Name
  17- 20  F4.1  Msun    Mi        Initial mass
  22- 24  F3.1  10+44W  Ekin      asymptotic ejecta kinetic energy
  26- 29  F4.2  Msun    Mp        Piston mass cut
  31- 35  I5    km/s    Vp        Piston speed
  37- 41  F5.2  Msun    Mf        Final mass
  43- 46  F4.2  Msun    Mrem      Mass of the remnant (2)
  48- 52  F5.2  Msun    Mej       Mass of the ejecta
  54- 57  I4    km/s    Vinner    Mean velocity of the inner 0.1M☉
                                   of the ejecta
  59- 62  I4    km/s    VeO       Velocity at the outer edge of the oxygen shell
  64- 67  I4    km/s    ViH       Velocity at the inner edge of the hydrogen
                                   shell
  69- 73  I5    km/s    Vp15d     Photospheric velocity at 15d after shock
                                   breakout
  75- 78  I4    km/s    Vp50d     Photospheric velocity at 50d after shock
                                   breakout
  80- 83  F4.2  10+44W  Eej       Effective asymptotic ejecta kinetic energy
                                   (in 1051erg)
  85- 86  I2    %       f(H)      Fraction endowed by the hydrogen-rich part
                                   of the ejecta
  88- 93  F6.4  Msun    MO        Ejected oxygen mass
  95- 97  F3.1  d       tSBO      Delay time between the piston trigger and
                                   shock breakout
  99-103  F5.1  d       dtP       Plateau duration (3)

Note (1): Cases as follows:
   2 = for a representative set of V1D simulations based on the non
       -rotating pre-SN models of Woosley, Heger and Weaver, 2002, 
       Rev. Modern Phys. 74, 1015
   3 = for non-rotating pre-SN models of Woosley, Heger and Weaver, 2002,
       Rev. Modern Phys. 74, 1015; main-sequence mass in range 11-15M☉
   4 = for non-rotating pre-SN models of Woosley, Heger and Weaver, 2002,
       Rev. Modern Phys. 74, 1015; main-sequence mass in range 16-20M☉
   5 = for non-rotating pre-SN models of Woosley, Heger and Weaver, 2002,
       Rev. Modern Phys. 74, 1015; main-sequence mass in range 21-25M☉
   6 = for non-rotating pre-SN models of Woosley, Heger and Weaver, 2002,
       Rev. Modern Phys. 74, 1015; main-sequence mass in range 26-30M☉
   7 = for our V1D simulations based on the rotating pre-SN models
       E10, E12, E15 and E20 of Heger et al., 2000ApJ...528..368H
Note (2): i.e. the material that fails to escape and accumulates in the
     neutron star or black hole.
Note (3): defined as the time it takes the luminosity to decrease after the
     plateau peak by a factor of 10; note that no 56Ni is injected in the
     ejecta, so that this plateau duration is a lower limit.


History:
    From electronic version of the journal
(End)                                      Patricia Vannier [CDS]    03-May-2011