Type Ib/Ic supernovae: effect of nickel mixing on the early-time color
  evolution and implications for the progenitors

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Abstract

We investigate the effect of mixing of radioactive nickel (\(^{56}\)Ni) on the early-time color evolution of Type Ib and Ic supernovae (SNe Ib/Ic) using multi-group radiation hydrodynamics simulations. We consider both helium-rich and helium-poor progenitors. Mixing of \(^{56}\)Ni is parameterized using a Gaussian distribution function. We find that the early-time color evolution with a weak \(^{56}\)Ni mixing is characterized by three different phases: initial rapid reddening, blueward evolution due to the delayed effect of \(^{56}\)Ni heating, and redward evolution thereafter until the transition to the nebular phase. With a strong \(^{56}\)Ni mixing, the second phase disappears. We compare our models with the early-time color evolution of several SNe Ib/Ic (SN1999ex, SN 2008D, SN 2009jf, iPTF13bvn, SN 1994I, SN 2007gr, SN 2013ge, and 2017ein) and find signatures of relatively weak and strong \(^{56}\)Ni mixing for SNe Ib and SNe Ic, respectively. This suggests that SNe Ib progenitors are distinct from SN Ic progenitors in terms of helium content and that \(^{56}\)Ni mixing is generally stronger in the carbon-oxygen core and weaker in the helium-rich envelope. We conclude that the early-time color evolution is a powerful probe of \(^{56}\)Ni mixing in SNe Ib/Ic.

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H. Tartara, M. Spence, A. Filippenko … (1996)

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Modules for Experiments in Stellar Astrophysics (MESA)

Lars Bildsten, Frank Timmes, Falk Herwig … (2010)

Stellar physics and evolution calculations enable a broad range of research in astrophysics. Modules for Experiments in Stellar Astrophysics (MESA) is a suite of open source libraries for a wide range of applications in computational stellar astrophysics. A newly designed 1-D stellar evolution module, MESA star, combines many of the numerical and physics modules for simulations of a wide range of stellar evolution scenarios ranging from very-low mass to massive stars, including advanced evolutionary phases. MESA star solves the fully coupled structure and composition equations simultaneously. It uses adaptive mesh refinement and sophisticated timestep controls, and supports shared memory parallelism based on OpenMP. Independently usable modules provide equation of state, opacity, nuclear reaction rates, and atmosphere boundary conditions. Each module is constructed as a separate Fortran 95 library with its own public interface. Examples include comparisons to other codes and show evolutionary tracks of very low mass stars, brown dwarfs, and gas giant planets; the complete evolution of a 1 Msun star from the pre-main sequence to a cooling white dwarf; the Solar sound speed profile; the evolution of intermediate mass stars through the thermal pulses on the He-shell burning AGB phase; the interior structure of slowly pulsating B Stars and Beta Cepheids; evolutionary tracks of massive stars from the pre-main sequence to the onset of core collapse; stars undergoing Roche lobe overflow; and accretion onto a neutron star. Instructions for downloading and installing MESA can be found on the project web site (http://mesa.sourceforge.net/).