leiden 2007

Binary star progenitors of long GRBsM. Cantiello, S.-C. Yoon, N. Langer, and M. Livio A&A 465, L29-L33 (2007): 

Matteo Cantiello Astronomical Institute Utrecht Binary star progenitors of long GRBs M. Cantiello, S.-C. Yoon, N. Langer, and M. Livio A&A 465, L29-L33 (2007)

Outline of the talk:: 

Outline of the talk: Ingredients for long GRBs: Collapsar Scenario Chemically Homogeneous Evolution The binary channel for long GRBs Runaway GRBs and observations Conclusions

Recipe to make a long GRB: 

Recipe to make a long GRB Collapsar Scenario (Woosley, 1993) Massive core (enough to produce a BH) Compact size Rapidly rotating core (enough to produce an accretion disk around the BH)

The “angular momentum” issue: 

The “angular momentum” issue Stellar evolution models including rotation and magnetic fields: It’s hard to fulfill all the requirements of the collapsar scenario It is possible to remove the envelope (WR winds) but too much angular momentum is lost during the RSG and WR phases (magnetic torques) A possible solution: Chemically Homogeneous evolution (Yoon & Langer 2005 - Heger & Woosley 2006)

Chemically Homogeneous Evolution: 

Chemically Homogeneous Evolution If rotationally induced chemical mixing during the main sequence occurs faster than the built-up of chemical gradients due to nuclear fusion the star evolves chemically homogeneous (Maeder, 1987) The star evolves blueward and becomes directly a Wolf Rayet (no Red Super Giant phase). This is because the envelope and the core are mixed by the meridional circulation -> no Hydrogen envelope Because the star is not experiencing the RSG phase it retains an higher angular momentum in the core (Yoon & Langer, 2005) R~1 Rsun R~1000 Rsun WR RSG The only evolutionary sequences of collapsing, single, massive stars that satisfy the Collapsar scenario are the ones that evolve Chemically Homogeneous (fast rotating massive stars)

The binary model: 

The binary model We used a 1D hydrodynamic binary evolution code to evolve massive binary systems (rotation and magnetic fields included) 16+15 Msun P= 5 days SMC metallicity (Z=0.004)

Results: 

Results Zero Age Main Sequence Begin of Mass transfer End of Mass transfer Primary dies as a SN Thereafter the accreted companion is a fast rotating, runaway WR star. It evolves chemically homogeneous and at the end of the evolution fulfills the requirements of the collpsar model.

Rotational Velocities: 

Rotational Velocities This model explains how a massive star can obtain the high rotational velocity needed to evolve quasi-chemically homogeneous and fulfills the Collapsar scenario for Long GRBs Unlike the single star model, the star doesn’t need to be born with an high rotational velocity The donor star dies as a SN type Ib/c 7Myrs before the collapse of the accreting companion The system is likely to be broke up by the SN kick (80%) The accreting companion (GRB progenitor) becomes a Runaway WR star Runaway GRBs

NGC 346: a cluster of young stars in the SMC: 

NGC 346: a cluster of young stars in the SMC Credit: Mokiem et al. 2007 Rotational Velocity vs Surface Helium Rotational Velocity vs Radial Velocity Low number statistics... But interesting!

Observational Consequences: 

Observational Consequences Position of GRB in the sky: Hammer et. al 2006 Afterglow properties: Van Marle et al. 2006 Constant Density

Conclusions: 

Conclusions Fast rotating massive stars can evolve chemically homogeneous (due to rotational mixing) and becomes long GRB It is possible to spin up a star in a massive binary system The accreted star fulfills the collapsar model for long GRB The progenitor is likely to be a runaway WR and travel several hundred pc before collapse Observational consequences for the Runaway GRBs Position in the sky Afterglow characterized by a constant density medium

Thank you: 

Thank you

Meridional Circulation: 

Meridional Circulation (Vega, a Fast rotating star - J.Aufdenberg) For Massive stars the most important contribution to rotational mixing is due to the Meridional (Eddington-Sweet) circulation It’s due to the fact that the pole of a rotating star is hotter than the equator (Von Zeipel Theorem) Mixing acts on the thermal timescale (Kelvin Helmoltz)

Binary vs Single star: 

Binary vs Single star Comparison between the internal structure of a long GRB progenitor produced by mass accretion in a binary system (top) and a long GRB progenitor produced by a single, rapidly rotating star (bottom). After mass accretion the two models are almost identical

1D Approximation: 

1D Approximation Anisotropic turbulence acts much stronger on isobars, which coincide with equipotential surfaces, than in the perpendicular direction. This enforces “Shellular” rotation rather than cylindrical and sweeps out compositional differences on equipotential surfaces. Therefore it can be assumed that the matter on equipotential surfaces is chemically homogeneous. This assumption it’s actually the assumption that baroclinic instabilities (which act on a dynamical timescale) are very efficient on mixing horizontally the star (A.Heger, PhD Thesis)

Chemically Homogeneous Evolution: 

Chemically Homogeneous Evolution

Final angular momentum: 

Final angular momentum