Supernova Simulation Tool V2.0
Astrophyzix Flagship Physics Instrument
A real-time supernova engine combining shock modelling, nucleosynthesis, spectral synthesis,
and full light‑curve generation. This is not an animation — it is a working astrophysics
instrument built for research‑grade analysis. Adjusting explosion energy, ejecta mass, nickel yield, opacity, or velocity instantly
recomputes the light curve, spectrum, and remnant outcome.
This module is a copyright registered asset of Astrophyzix © 2026
Astrophyzix Supernova Simulator
Core-Collapse / Type Ia / Pair-Instability Module v2.0
Astrophyzix Flagship Series Copyright © 2026
Astrophyzix Flagship Series Copyright © 2026
Sim
Params
Light
Spectra
Nucleo
Remnant
Export
Refs
t = 0.0 s
R = 0 km
v = 0 km/s
R = 0 km
v = 0 km/s
L = 0
T = 0 K
E = 0 foe
T = 0 K
E = 0 foe
Visualization Toggles
Layers
Shock front
RT instab
Nu heat
Convect
Heavy only
Ni-56 chain
r-process
SN TypeII-P
Energy budget--
IntegratorRK4
Adjust progenitor and explosion parameters. SN type is recomputed automatically.
Progenitor
Explosion
Numerics
Compare Templates
Synthetic
SN 1987A
Type Ia
II-P plateau
Type IIb
Type Ic
Governing Equation (Arnett 1982)
Bolometric luminosity from radioactive heating
L(t) = M_Ni * [eps_Ni * exp(-t/tau_Ni)
+ eps_Co * (exp(-t/tau_Co) - exp(-t/tau_Ni)) * f]
Diffusion timescale (Arnett)
t_d = sqrt( 2 * kappa * M_ej / (beta * c * v_ej) )
tau_Ni = 8.8 d, tau_Co = 111.3 d, eps_Ni = 3.9e10 erg/g/s, eps_Co = 6.78e9 erg/g/s.
Plateau model applies recombination at T_rec = 5500 K for II-P.
Line Identification
H (II)
He I (Ib)
Si II (Ia)
O I (Ic)
Ca II
Fe II
Mg II
S II
Approximate SYN++-style continuum + P-Cygni profile model. Velocity broadening
from photospheric expansion v_ph(t). Continuum: blackbody at T_phot(t).
Yield Table
| Element | M [Msun] | Mass frac | Bar |
|---|
Notes
Yields interpolated from tabulated grids: Nomoto W7/WDD2 (Ia), Woosley & Weaver
1995 / Woosley & Heger 2007 (CCSN), Heger & Woosley 2002 (PISN).
The r-process zone marks ejecta with Ye < 0.45 and entropy s > 100 k_B/baryon
(when present); not every CCSN produces strong r-process.
Predicted Compact Remnant
Mass-Mapping Logic
M < 8 Msun: No SN; degenerate WD remnant (CO or ONe).
8 - 25 Msun: Neutron star (M_NS ~ 1.2-2.0 Msun).
25 - 40 Msun (low Z): NS or fallback BH.
25 - 40 Msun (high Z): NS via mass loss.
40 - 140 Msun: Direct-collapse BH likely.
140 - 260 Msun: PISN; complete disruption, no remnant.
> 260 Msun: BH via photo-disintegration.
Magnetar branch active when B > 1e14 G and rapid rotation.
8 - 25 Msun: Neutron star (M_NS ~ 1.2-2.0 Msun).
25 - 40 Msun (low Z): NS or fallback BH.
25 - 40 Msun (high Z): NS via mass loss.
40 - 140 Msun: Direct-collapse BH likely.
140 - 260 Msun: PISN; complete disruption, no remnant.
> 260 Msun: BH via photo-disintegration.
Magnetar branch active when B > 1e14 G and rapid rotation.
Equations
Gravitational mass from baryonic (Lattimer-Yahil)
M_grav = M_bary - 0.075 * M_bary^2 / Msun
Magnetar spindown luminosity
L_mag = (B^2 R^6 Omega^4) / (6 c^3)
Export current simulation data as plain text / CSV. Files are generated client-side
from the running model (no server, no upload).
All values reported in CGS unless stated; mass in Msun.
Key Equations
Sedov-Taylor blast wave
R(t) = xi * (E / rho_0)^(1/5) * t^(2/5), xi ~ 1.15
Chandrasekhar mass
M_Ch = 5.83 * (Y_e)^2 * Msun ~ 1.44 Msun
Free-fall time of iron core
t_ff ~ (G * rho)^(-1/2) ~ 0.1 s for rho ~ 1e10 g/cm3
Total neutrino energy
E_nu_tot ~ 3 * 10^53 erg ~ 0.99 * E_grav
Pair-instability condition
Gamma_1 < 4/3 when k_B T > m_e c^2 (T > 6e9 K)
Energy conservation check
E_kin + E_int + E_rad + E_nu = E_grav (released)
Assumptions
Spherical symmetry for hydrodynamics (deviations rendered as RT/RM perturbations).
Homologous expansion in optically thick phase. One-zone Arnett model for light curve.
LTE blackbody continuum for spectra; line opacities from approximate Sobolev profiles.
Yields interpolated from published 1D explosion grids; mixing parameterized.
Float64 IEEE-754 throughout (JS native double). Optional WebGPU compute path
where supported for the shock advection step.
References
Arnett, W.D. 1982, ApJ 253, 785. Type I SN light curve.
Arnett, W.D. 1996, "Supernovae and Nucleosynthesis", Princeton.
Burrows, A. 2013, RMP 85, 245. Neutrino-driven explosions.
Heger, A. & Woosley, S.E. 2002, ApJ 567, 532. Pair-instability nucleosynthesis.
Janka, H.-T. 2012, ARNPS 62, 407. Core-collapse mechanisms.
Khokhlov, A.M. 1991, A&A 245, 114. Deflagration-to-detonation transition.
Lattimer, J.M. & Yahil, A. 1989, ApJ 340, 426. Neutron star mass.
Nomoto, K., Thielemann, F.-K., Yokoi, K. 1984, ApJ 286, 644. W7 model.
Woosley, S.E. & Weaver, T.A. 1995, ApJS 101, 181. Massive star evolution.
Woosley, S.E. & Heger, A. 2007, Phys.Rep. 442, 269. Massive star deaths.
Bethe, H.A. & Wilson, J.R. 1985, ApJ 295, 14. Delayed neutrino mechanism.
Sedov, L.I. 1959, "Similarity and Dimensional Methods", Academic Press.
Kasen, D. 2010, ApJ 708, 1025. Type Ia spectra modelling.
Numerical Methods
RK4: classical 4th-order; fixed step.
RKF45: embedded 4(5) Runge-Kutta-Fehlberg; adaptive step via local error estimate.
Leapfrog: 2nd-order symplectic; energy-preserving for conservative dynamics.
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