Stellar Rotation I

Lecture given at MESA School 2012

Transcript

1. Matteo Cantiello Kavli Institute for Theoretical Physics (University of California Santa Barbara) Stellar Rotation I
2. Outline § Disclaimer § Observed rotation rates § Rotating stars § Hydrostatic equilibrium § Radiative equilibrium: Von Zeipel Theorem § Modeling rotating stars in 1D: shellular rotation law § Diffusion Approximation § Meridional circulation § Rotational Instabilities § Impact of rotation on stellar evolution § Lifetimes, Luminosities, Surface Abundances... § Final angular momentum content: SNe, GRBs § Spin of compact remnants (WD, NS, BH) UCSB 2012 Matteo Cantiello MESA School
3. Rotating stars: observations
4. Range of rotational velocity NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School Fukuda 1982 “In practice all stars are rotating around their axis” - Maeder & Meynet
5. B Stars in the bright star catalogue NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School Abt et al. 2002
6. Galactic OB Stars NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School Huang & Gies 2006
7. VLT-FLAMES Tarantula Survey (PI: Evans): ~ 900 OB stars observed spectroscopically in 30 Dor (LMC) region. Multi-epoch observations to separate binaries from single stars. (Evans et al. 2010) VLT-Flames Tarantula Survey Image credit: NASA, ESA CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School
8. B Stars in 30 Doradus NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School Dufton et al. Submitted
9. OB Stars in 30 Doradus NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School VTFS, private communication Veq (km/s) B Stars O Stars P
10. VFTS 102, fastest rotating star* NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School Dufton et al. 2011
11. VFTS 102, fastest rotating star* NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School Veq ~ 600 km/s Dufton et al. 2011
12. Effects of Rotation
13. Effects of rotation NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School Rotation
14. Effects of rotation NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School Rotation Hydrostatic equilibrium
15. Effects of rotation NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School Rotation Radiative equilibrium Hydrostatic equilibrium
16. Effects of rotation NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School Rotation Radiative equilibrium Rotational Mixing Hydrostatic equilibrium
17. Effects of rotation NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School Rotation Mass loss Radiative equilibrium Rotational Mixing Hydrostatic equilibrium
18. Hydrostatic Effects
19. The centrifugal term NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School Georgy, Phd Thesis
20. The centrifugal term NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School The centrifugal force reduces the local gravity.The effect depends on the co-latitude, resulting in departures from spherical simmetry. Tassoul (1978) showed that, except for stars close to critical rotation, the deformation is axially symmetric. Even when this is not the case only the outer most layers of the star are affected (very little mass). In the Roche approximation:
21. Departure from spherical structure NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School Georgy, Phd Thesis In the Roche approximation the deformation of the star approaches the value Req/Rp=1.5
22. Interferometry of rotating stars NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School Domiciano Da Souza et al.2003 Achernar (Be star) Star rotating at 96% of critical velocity (311 km/s) VLTI Observations show that: Req/Rp~1.5
23. Barotropic Star NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School If Omega is constant (Solid body rotation) or has cilindric symmetry, the centrifugal acceleration can be derived from a potential (V). The eq. of Hydrostatic Equilibrium then implies that the star is Barotropic
24. Barotropic Star NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School constant on equipotentials g
25. Baroclinic Star NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School For different rotation laws (e.g. Shellular), the centrifugal acceleration can not be derived from a potential (V). In this case Isobars and Equipotentials DO NOT coincide. The star is Baroclinic
26. Baroclinic Star NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School not constant on equipotentials g
27. Baroclinicity leads to instabilities NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School g Isobar Isoentropic A B C Assumption: adiabatic displacement
28. Baroclinicity leads to instabilities NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School g Isobar Isoentropic A B C Stable (higher density) Assumption: adiabatic displacement
29. Baroclinicity leads to instabilities NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School g Isobar Isoentropic A B C Stable (higher density) Unstable (hotter) Assumption: adiabatic displacement
30. Mass-loss
31. NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School Ekstrom et al. 2008 N.B. Effects of radiation not included Critical Velocity
32. NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School Critical Velocity Gamma-Omega Limit
33. Rotationally enhanced Mass-loss NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School Theoretically one expects additional mass-loss as the star approaches critical rotation, as material becomes less and less bound to the stellar surface. Langer, 1998 See Georgy et al. 2011 for a more thorough discussion of rotationally enhanced mass-loss
34. NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School /mesa/star /work Run_star ../data /private MESA Star /public Inlist prole_columns log_columns run_star_extra.f sub other_* extra_jdot §/private/winds.f
35. NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School §/private/winds.f
36. Effects of rotation NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School Rotation Mass loss Hydrostatic equilibrium
37. Effects of rotation NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School Rotation Mass loss Radiative equilibrium Hydrostatic equilibrium
38. Radiative Equilibrium
39. NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School The thermal flux through the surface of a (radiative) rotating star is proportional to the local effective gravity. Since this depends on the co-latitude, one expects a greater radiative flux at the poles than at the equator. The Von Zeipel Theorem Convective Core € ω Von Zeipel (1924)
40. NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School The thermal flux through the surface of a (radiative) rotating star is proportional to the local effective gravity. Since this depends on the co-latitude, one expects a greater radiative flux at the poles than at the equator. The Von Zeipel Theorem Convective Core € ω Von Zeipel (1924)
41. NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School In the case of solid body rotation: Both geff and Teff vary over the surface of a rotating star and influence the emergent spectrum. The equatorial regions are fainter and cooler than the polar ones, which are brighter and hotter (the differences of Teff may reach a factor of 2). This effect is called the gravity darkening.The von Zeipel theorem in a star with shellular rotation shows only minor differences (Maeder, 1999, Maeder & Meynet 2012) The Von Zeipel Theorem Von Zeipel (1924)
42. Interferometry of rotating stars NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School Domiciano Da Souza et al.2005 Altair (A7IV-V Star) VLTI Observations Von Zeipel ‘gravity darkening’ Confirmed
43. Interferometry of rotating stars NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School Domiciano Da Souza et al.2005 Altair (A7IV-V Star) VLTI Observations Von Zeipel ‘gravity darkening’ Confirmed
44. Interferometry of rotating stars NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School Altair (A7IV-V Star): Von Zeipel ‘gravity darkening’ but with a different exponent
45. Interferometry of rotating stars NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School
46. Modeling Rotating Stars
47. The computational Challenge NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors § Stars are rotating balls of hot plasma § They undergo a variety of instabilities § Large range of timescales § It would be ideal to perform fully (magneto) hydrodynamic calculations. But this is currently computationally impossible. § At this time 3D stellar evolution calculations can evolve a few hours of a star life. § How can we model rotation in a 1D, implicit code? UCSB 2012 Matteo Cantiello MESA School
48. According to Zahn (1975), Chaboyer & Zahn (1992), and Zahn (1992), anisotropic turbulence acts much stronger on isobars than in the perpendicular direction. This enforces a shellular rotation law (Meynet & Maeder 1997), and it sweeps out compositional differences on isobars. Therefore it can be assumed that matter on isobars is approximately chemically homogeneous. Together with the shellular rotation, this allows us to retain a one-dimensional approximation. The specific angular momentum, j, of a mass shell is treated as a local variable, and the angular velocity, omega, is computed from the specific moment of inertia, i. (Heger et al. 2000) The Shellular Approximation NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School Rotation and especially differential rotation generates turbulent motions. On the Earth, we have the example of west winds and jet streams. In a radiative zone, the turbulence is stronger (Zahn, 1992) in the horizontal than in the vertical direction, because in the vertical direction the stable thermal gradient opposes a strong force to the fluid motions. In this approach, mass shells correspond to isobars instead of spherical shells.
49. The structure equations of rotating stars NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School For a star in shellular rotation it is possible to modify the eqs of stellar structure to include the effect of the centrifugal force while keeping the form of the equations very close to that of the non- rotating case. Basically all quantities are redefined on isobars. Mass conservation Hydrostatic Eq. Energy transport ... Endal & Sofia 1978
50. NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School /mesa/star /work Run_star ../data /private MESA Star /public Inlist prole_columns log_columns run_star_extra.f sub other_* extra_jdot §/private/hydro_rotation.f
51. NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School §/private/hydro_rotation.f
52. Diffusion Equations NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School Transport of chemical species: Transport of angular momentum:
53. Advection- Diffusion Scheme NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School An alternative approach is to solve an advection-diffusion equation for the transport of angular momentum (e.g. in the GENEVA code or the ROSE code). However, as MESA adopts the diffusion approximation (like e.g. KEPLER and STERN), I will not discuss the advection-diffusion scheme here. Nevertheless I suggest you have a look at the relevant literature (e.g. Mader & Meynet 2000, 2012) A very interesting work comparing the different implementations has been published by Potter et al. 2012. While it has been claimed that the advection-diffusion scheme is mathematically more sound, a key result of Potter’s work is that is not yet possible to prefer one of the two implementations, given the available observational constraints.
54. Effects of rotation NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School Rotation Mass loss Radiative equilibrium Hydrostatic equilibrium
55. Effects of rotation NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School Rotation Mass loss Radiative equilibrium Rotational Mixing Hydrostatic equilibrium
56. Rotational Instabilities
57. Differential rotation is expected to arise in stars because of hydrostatic structural evolution, mass loss and meridional circulation. As a consequence, stars are subject to a number of local hydrodynamic instabilities. These instabilities arise and cause diffusion of angular momentum (and chemicals) while they try to bring the star back to solid body rotation, its lowest energy state. The unstable interiors of rotating stars NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School
58. Rotational Instabilities § Rotational “instabilities” mix rotating stars § Different timescales: secular/dynamical instabilities § MESA § (Eddington - Sweet circulation) (ES) § Dynamical and Secular Shear (DSI, SSI) § Goldreich-Schubert-Fricke (GSF) § Solberg - Høiland (SH) § (Tayler - Spruit) (TS) § See /mesa/star/private/rotation_mix_info.f NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School
59. Eddington - Sweet (D_ES) NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School
60. Thermal imbalance drives circulations NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School
61. Thermal imbalance drives circulations NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School
62. Thermal imbalance drives circulations NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors Convective Core Meridional circulation UCSB 2012 Matteo Cantiello MESA School
63. Meridional Circulation NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School Maeder & Meynet 2002 20 Msun Vini = 300 km/s
64. Meridional Circulation NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School Maeder & Meynet 2002 20 Msun Vini = 300 km/s τES ∝τKH ωK ω ⎛ ⎝ ⎜ ⎞ ⎠ ⎟ 2
65. Eddington - Sweet (D_ES) § Is a meridional circulation mixing the stellar interior § In massive stars is one of the most efficient processes § Mixing process on t KH € ω NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors Convective Core Meridional circulation UCSB 2012 Matteo Cantiello MESA School A diffusion coefficient D_ES enters the diffusion equations
66. Eddington - Sweet (D_ES) § Is a meridional circulation mixing the stellar interior § In massive stars is one of the most efficient processes § Mixing process on t KH τES ∝τKH ωK ω ⎛ ⎝ ⎜ ⎞ ⎠ ⎟ 2 € ω NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors Convective Core Meridional circulation UCSB 2012 Matteo Cantiello MESA School A diffusion coefficient D_ES enters the diffusion equations
67. Dynamical Shear (D_DSI) NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School
68. Dynamical Shear (D_DSI) NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School Jake Simon (JILA)
69. Dynamical Shear (D_DSI) NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School § Works very well on horizontal surfaces (isobars) and justifies (together with the baroclinic instabilities) the Shellular approximation § In the vertical direction it is strongly inhibited by density gradients. Can only work for large degree of differential rotation § Mixing process on t Dynamical § Results in D_DSI, entering the diffusion equations = ...
70. NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School /mesa/star /work Run_star ../data /private MESA Star /public Inlist prole_columns log_columns run_star_extra.f sub other_* extra_jdot §/private/rotation_mix_info.f
71. NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School §/private/rotation_mix_info.f
72. Dynamical Shear (D_DSI) NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School
73. NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School § In the presence of a stabilizing thermal gradient, an eddy might have to wait for heat to diffuse out before an overturn is energetically favorable § Mixing process on t KH § Results in D_SSI, entering the diffusion equations Secular Shear (D_SSI) Thermal Timescale
74. Solberg - Høiland (D_SH) NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School r Rayleigh Criterion for stability € ω
75. Solberg - Høiland (D_SH) NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School r Including the effects of stratification etc. Solberg - Høiland Criterion for stability € ω
76. Solberg - Høiland (D_SH) NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School Heger et al. 2000 § For no rotation (or constant j) we recover Ledoux § Can reduce size of convective regions (as j tends to increase outside, one has an extra restoring force) § Results in D_SH, entering the diffusion equations
77. Goldreich-Schubert-Fricke (D_GSF) NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School § Baroclinic instability § Two criteria: one is the secular analog of the SH, the other is an analog of the Taylor-Proudman theorem. § The second criteria is generally in contradiction with the shellular law. GSF would try to enforce uniform rotation. D_GSF entering the diffusion equations € ω
78. Spruit-Tayler (D_ST) NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School § Dynamo in a radiative layer § Magnetic energy is generated from differential rotation § Initially a seed magnetic field is stretched by the differential rotation, amplifying the toroidal component of the field § An instability in the toroidal component of the field (Tayler instability) is used to close the dynamo loop Spruit 2002 Convec
79. Tayler Instability NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School Spruit 1999 This is used to generate a poloidal component from the toroidal component of the field
80. Magnetic fields § Spruit-Tayler Dynamo (Spruit 2002) § Core - Envelope coupling 1. Differential rotation winds up toroidal component of B 2. Magnetic torques tend to restore rigid rotation Convective Core If the envelope slows down angular momentum is also removed from the core NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School
81. Stockholm 2009 Matteo Cantiello Long GRB Progenitors Debate on the ST Dynamo Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School § The ST dynamo is still under review § While the Tayler instability is sound, the loop proposed by Spruit has been criticized § Simulations of Zahn et al. 2007 could not find a dynamo action § On the other hand simulations of Braithwaite et al. 2006 showed the Spruit-Tayler dynamo § The jury is still out, but it looks like a j-transport mechanism similar to the ST has to work in stars to reproduce some observations (e.g. asteroseismology and spin rates of compact remnants. g-waves could also play a role)
82. § Spin of compact remnants (Heger et al. 2005, Suijs et al. 2008) § Core-envelope coupling leads to spin-down of the core Convective Core Stockholm 2009 Matteo Cantiello Long GRB Progenitors Magnetic fields Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School
83. Stockholm 2009 Matteo Cantiello Long GRB Progenitors Need for an extra j-transport mechanism Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School Langer 2012
84. Evolutionary effects
85. Impact of rotation § Change in luminosity (size of the core, mean molecular weight) § Lifetimes (size of the core) § Surface abundances (Li, B, N, He...) § Mass-loss § WR/O ratio, Red to Blue SG, SN type § Final angular momentum § SN type § GRB NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School
86. Calibrating Rotational Mixing
87. Calibration § Nitrogen (CN, CNO equilibrium) § The compositional barrier § The hope of Asteroseismology NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School
88. The Hunter Diagram
89. Chemical homogeneous evolution
90. Final fate of massive stars
91. Rotation and Fossil Fields
92. Chemically Homogeneous Evolution I NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School Langer (2012)
93. The Hunter Diagram NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School Brott et al. 2011
94. The Hunter Diagram II NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School Brott et al. 2011
95. Chemically Homogeneous Evolution I Time RSG WR Slow rotator Fast rotator NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School
96. Chemically Homogeneous Evolution I Time RSG WR Slow rotator Fast rotator NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School
97. Chemically Homogeneous Evolution II R~1000 Rsun RSG R~1 Rsun WR Fast rotator Slow rotator NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School
98. Chemically Homogeneous Evolution II R~1000 Rsun RSG R~1 Rsun WR Fast rotator Slow rotator CCSN NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School
99. Chemically Homogeneous Evolution II GRB R~1000 Rsun RSG R~1 Rsun WR Fast rotator Slow rotator CCSN NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School
100. Chemically Homogeneous Evolution II GRB § Fast rotating massive stars can evolve chemically homogeneous § If mass loss is not too high (Low Z) -> Long GRB R~1000 Rsun RSG R~1 Rsun WR Fast rotator Slow rotator CCSN NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School
101. Gamma Ray Bursts NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School
102. Gamma Ray Bursts NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors The most luminous electromagnetic transients in the universe UCSB 2012 Matteo Cantiello MESA School
103. GRB 090429B Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors Cucchiara et al. 2011 z ~ 9.4 (tUniverse ~ 520 Myrs) CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School
104. GRB 090429B Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors Cucchiara et al. 2011 z ~ 9.4 (tUniverse ~ 520 Myrs) CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School
105. Two classes of GRBs NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors § 70% Long (t > 2s) § Associated with the death of massive stars § 30% Short (t < 2s) § Merger of compact objects? (e.g. Berger 2011) Image credit: Price & Rosswog UCSB 2012 Matteo Cantiello MESA School
106. Long GRBs Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School
107. Long GRBs Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors § SN (Type Ic, BL) - GRB connection (e.g Stanek et al. 2003, Modjaz et al. 2006, see also Soderberg et al. 2010) § Found in regions of massive star formation (Bloom et al. 1999, Fruchter et al. 2006) § Most (all?) long GRBs produced by the death of massive stars (Woosley & Bloom 2006) CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School
108. Long GRBs Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors § SN (Type Ic, BL) - GRB connection (e.g Stanek et al. 2003, Modjaz et al. 2006, see also Soderberg et al. 2010) § Found in regions of massive star formation (Bloom et al. 1999, Fruchter et al. 2006) § Most (all?) long GRBs produced by the death of massive stars (Woosley & Bloom 2006) Which massive stars explode as Long Gamma-Ray Bursts? CfA 2012 Matteo Cantiello Long GRB Progenitors UCSB 2012 Matteo Cantiello MESA School
109. Central Engines
110. Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors Central Engines 101 Collapsar Woosley 1993 CfA 2012 Matteo Cantiello Long GRB Progenitors
111. Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors Central Engines 101 Collapsar Woosley 1993 Eacc ~ 0.01..1Msunc2~1052..54ergs CfA 2012 Matteo Cantiello Long GRB Progenitors
112. Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors Central Engines 101 Millisecond Magnetar Usov 1992 CfA 2012 Matteo Cantiello Long GRB Progenitors
113. Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors Central Engines 101 Erot ~ 3 1052 (P/ms)-2 (R/10km)2 ergs Millisecond Magnetar Usov 1992 CfA 2012 Matteo Cantiello Long GRB Progenitors
114. Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors Central Engines 101 (Spitkovski 2006) Erot ~ 3 1052 (P/ms)-2 (R/10km)2 ergs Millisecond Magnetar Usov 1992 CfA 2012 Matteo Cantiello Long GRB Progenitors
115. • Collapsar Scenario (e.g. Paczinski, Woosley, Macfadyen...) • Magnetar Scenario (e.g. Usov, Thompson, Duncan, Wheeler, Metzger, Bucciantini...) § Massive core (BH - NS) § Rapidly rotating core (accretion disk/magnetar) § Compact size R * /c ≈ τengine Recipe to make a long GRB NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors
116. Stellar Evolution
117. Stellar progenitors of GRBs § Observationally GRB/SN ~ 1/1000 § Collapsar need compact progenitor with massive, fast rotating core § Canonical evolution of single stars including rotation and B fields can not do it CfA 2012 Matteo Cantiello Long GRB Progenitors
118. Stellar progenitors of GRBs § Observationally GRB/SN ~ 1/1000 § Collapsar need compact progenitor with massive, fast rotating core § Canonical evolution of single stars including rotation and B fields can not do it Core Envelope CfA 2012 Matteo Cantiello Long GRB Progenitors
119. Stellar progenitors of GRBs § Observationally GRB/SN ~ 1/1000 § Collapsar need compact progenitor with massive, fast rotating core § Canonical evolution of single stars including rotation and B fields can not do it CfA 2012 Matteo Cantiello Long GRB Progenitors
120. Stellar progenitors of GRBs § Observationally GRB/SN ~ 1/1000 § Collapsar need compact progenitor with massive, fast rotating core § Canonical evolution of single stars including rotation and B fields can not do it A possible solution: Chemically Homogeneous evolution (Yoon & Langer 2005 - Heger & Woosley 2006) CfA 2012 Matteo Cantiello Long GRB Progenitors
121. Key-ingredient: fast rotation € τ Mix τMS <1 The star can not build a compositional gradient and evolves quasi chemically homogeneous How to avoid the core-envelope structure? Rotational “instabilities” can efficiently mix a massive star If Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors
122. Any candidates for this evolutionary scenario?
123. VLT-FLAMES Tarantula Survey (PI: Evans): ~ 900 OB stars observed spectroscopically in 30 Dor (LMC) region. Multi-epoch observations to separate binaries from single stars. (Evans et al. 2010) VLT-Flames Tarantula Survey Image credit: NASA, ESA CfA 2012 Matteo Cantiello Long GRB Progenitors
124. VLT-FLAMES Tarantula Survey (PI: Evans): ~ 900 OB stars observed spectroscopically in 30 Dor (LMC) region. Multi-epoch observations to separate binaries from single stars. § Nitrogen surface abundances § Rotational velocities § Binary fraction § A statistically significant sample of the most massive stars (see e.g. Crowther et al. 2010) (Evans et al. 2010) 30 Doradus (HST) VLT-Flames Tarantula Survey LCOGT 2012 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors
125. VLT-Flames Tarantula Survey: A Chemically Homogeneous Star NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Bestenlehner et al. 2011 Sedgwick 2011 Matteo Cantiello Long GRB Progenitors VFTS 682 H-rich WR Star (WN5h) ~30 pc away from R136 in the LMC (Tarantula Nebula) Teff~53kK log(L/Lsun)~6.5 Can be explained with a chemically homogeneous Mini~[120-210] Msun star Requires initial rotation Veq>200 km/s See Martins et al. 2009 for other 2 CH candidates LCOGT 2012 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors
126. § Chemically homogeneous evolution needs high rotational velocity Rotational velocity NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors LCOGT 2012 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors
127. § Chemically homogeneous evolution needs high rotational velocity Stars born with high rotational velocity Single star progenitors (Yoon at al. 2006) Rotational velocity NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors LCOGT 2012 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors
128. Single star progenitors (Yoon, Langer & Norman, 2006) § Long GRBs prefer low metallicity (i.e. weaker winds) Z ~ 1/5 ZSun (SMC) § This metallicity threshold is sensitive to mass-loss efficiency ≤ NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors LCOGT 2012 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors
129. § Chemically homogeneous evolution needs high rotational velocity Stars born with high rotational velocity Single star progenitors (Yoon at al. 2006) Rotational velocity NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors LCOGT 2012 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors
130. § Chemically homogeneous evolution needs high rotational velocity Stars born with high rotational velocity Single star progenitors (Yoon at al. 2006) Rotational velocity Stars spun-up in binary systems Binary star progenitors (Cantiello et al. 2007) NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors LCOGT 2012 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors
131. § Chemically homogeneous evolution needs high rotational velocity Stars born with high rotational velocity Single star progenitors (Yoon at al. 2006) Rotational velocity Stars spun-up in binary systems Binary star progenitors (Cantiello et al. 2007) NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Other binary progenitor models of long GRB (e.g.: Tidal spin up, Binary Mergers, Explosive Common-Envelope Ejection) Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors LCOGT 2012 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors
132. A huge fraction of Massive stars is in binaries! NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Courtesy: H. Sana Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors LCOGT 2012 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors
133. Binary star progenitors § We want to spin-up a star and induce chemically homogeneous evolution Mass (angular momentum) accretion NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors LCOGT 2012 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors
134. Binary star progenitors § We want to spin-up a star and induce chemically homogeneous evolution Mass (angular momentum) accretion NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors § A merger is also a possible way to obtain a single, fast rotating massive star (e.g. Fryer et al., Podsiadlowski et al.) Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors LCOGT 2012 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors
135. SN Spin up by accretion Rotational Mixing!! M * ~ 13M Sun M co ~ 10M Sun J co ~ 2x1016cm2/s NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors 15M Sun 16M Sun Case B mass transfer 21M Sun SN Vrun ~ 30 km/s Runaway Wolf-Rayet LGRB Credit: A. Feild (STScI) Veq ~ 700 km/s LCOGT 2012 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors
136. Any candidates for this binary evolutionary scenario?
137. VLT-Flames Tarantula Survey LCOGT 2012 Matteo Cantiello Long GRB Progenitors Image credit: NASA, ESA CfA 2012 Matteo Cantiello Long GRB Progenitors
138. VLT-Flames Tarantula Survey LCOGT 2012 Matteo Cantiello Long GRB Progenitors Image credit: NASA, ESA CfA 2012 Matteo Cantiello Long GRB Progenitors
139. Dufton et al. 2011
140. Veq ~ 600 km/s Dufton et al. 2011
141. Veq ~ 600 km/s It’s a Runaway Dufton et al. 2011
142. Veq ~ 600 km/s It’s a Runaway Lies close to a young Pulsar Dufton et al. 2011
143. Lies close to a Pulsar and a SNR LCOGT 2012 Matteo Cantiello Long GRB Progenitors Image credit: NASA, ESA d~12 pc CfA 2012 Matteo Cantiello Long GRB Progenitors Dufton et al. 2011
144. Pulsar - VFTS102 Connection LCOGT 2012 Matteo Cantiello Long GRB Progenitors Image credit: NASA, ESA § Diffuse X-ray emission consistent with bow- shock if pulsar is moving at ~1000 km/s Wang & Gotthelf (1998) § Adopting estimated age of pulsar (5000-24000 yrs Marshall et al. 1998, Chu et al. 1992 ), velocity for being casually connected to VFTS102 is 500-2500 km/s § An attractive scenario, but needs to be confirmed (HST proper motion study PI: Lennon) § Other scenarios are possible (e.g dynamical ejection) CfA 2012 Matteo Cantiello Long GRB Progenitors
145. GRB Observations
146. Prediction: Metallicity Threshold (Yoon, Langer & Norman, 2006) § Long GRBs prefer low metallicity (i.e. weaker winds) Z ~ 1/5 ZSun (SMC) § This metallicity threshold is sensitive to mass-loss efficiency ≤ NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors LCOGT 2012 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors
147. Observations: Metallicity Threshold? NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors (Modjaz et al.2007) Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors LCOGT 2012 Matteo Cantiello Long GRB Progenitors Diagnostic: KD02 CfA 2012 Matteo Cantiello Long GRB Progenitors
148. Observations: Metallicity Threshold? NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors (Modjaz et al.2007) Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Z ~ 0.2 - 0.6 ZSun Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors LCOGT 2012 Matteo Cantiello Long GRB Progenitors Diagnostic: KD02 CfA 2012 Matteo Cantiello Long GRB Progenitors
149. Observations: LGRBs prefer low Metallicity? NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors (Levesque et al.2010) Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors LCOGT 2012 Matteo Cantiello Long GRB Progenitors Diagnostic: KK04 CfA 2012 Matteo Cantiello Long GRB Progenitors Tremonti et al. 2004 M-Z relation
150. Observations: LGRBs prefer low Metallicity? NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors (Levesque et al.2010) Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors LCOGT 2012 Matteo Cantiello Long GRB Progenitors Diagnostic: KK04 Kocevski et al. 2009 CfA 2012 Matteo Cantiello Long GRB Progenitors Tremonti et al. 2004 M-Z relation
151. Observations: LGRBs prefer low Metallicity? NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors (Levesque et al.2010) Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors LCOGT 2012 Matteo Cantiello Long GRB Progenitors Diagnostic: KK04 Kocevski et al. 2009 CfA 2012 Matteo Cantiello Long GRB Progenitors Tremonti et al. 2004 M-Z relation
152. Or maybe even something else... NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors LCOGT 2012 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors § The low metallicity observed in long GRB host galaxies is just a consequence of the observed correlation between SSFR and Z (Mannucci et al. 2011)
153. Conclusions § Long GRBs? Fast rotating massive stars that evolve chemically homogeneous § Two classes of progenitors: single and binary stars § In massive binaries it is possible to spin up a star and form a rapidly rotating collapsing core § This scenario is likely to produce a runaway WR which travels several hundred pc before collapse § Both single and binary progenitors prefer low Z § The origin of observed low-metallicity trend for GRB host galaxies is currently debated § VLT-Flames Tarantula Survey: chemically homogeneous star and most rapidly-rotating O-star NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors LCOGT 2012 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors
155. !
156. CfA 2012 Matteo Cantiello Long GRB Progenitors mesa.sourceforge.net Open Source, State-of-the-art Stellar evolution
157. Open Source, State-of-the-art Stellar evolution CfA 2012 Matteo Cantiello Long GRB Progenitors
158. CfA 2012 Matteo Cantiello Long GRB Progenitors
159. NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors Thanks! LCOGT 2012 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors
160. NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors Thanks! We don’t believe you LCOGT 2012 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors
161. NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors Thanks! We don’t believe you I have to pee... LCOGT 2012 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors
162. NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors Thanks! We don’t believe you I have to pee... LCOGT 2012 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors
163. Predicted GRB/SN(z) NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Yoon et al. 2006 This relies on the assumed distribution of initial rotational velocities! Sedgwick 2011 Matteo Cantiello Long GRB Progenitors The CfA 2012 Matteo Cantiello Long GRB Progenitors
164. Perceived GRB and SN Distribution as function of z NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Yoon et al. 2006 + cosmic Z evolution model of Langer and Normann 2006 Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors
165. Perceived GRB and SN Distribution as function of z NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Yoon et al. 2006 + cosmic Z evolution model of Langer and Normann 2006 Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors
166. Perceived GRB and SN Distribution as function of z NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors
167. Runaway nature of (some) Long GRB progenitors? Jakobsson et al. 2012
168. Hammer et al. 06: deep spectroscopic observations of nearest GRBs host galaxies revealed the presence of WR and O stars in compact clusters. Surprisingly high spatial resolution imaging shows that GRB/SNe exploded few hundred parsecs away from these regions. Observational Consequence § Position of GRB in the sky NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors See also Han et al. 2010 LCOGT 2012 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors
169. Hammer et al. 06: deep spectroscopic observations of nearest GRBs host galaxies revealed the presence of WR and O stars in compact clusters. Surprisingly high spatial resolution imaging shows that GRB/SNe exploded few hundred parsecs away from these regions. Observational Consequence § Position of GRB in the sky Hammer et. al 2006, NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors See also Han et al. 2010 LCOGT 2012 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors
170. LGRBs prefer low Metallicity NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors (Levesque et al.2010) Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors
171. LGRBs prefer low Metallicity NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors (Levesque et al.2010) Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors
172. Pop III GRB Progenitors NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors Yoon et al. 2012 CfA 2012 Matteo Cantiello Long GRB Progenitors
173. § Chemically homogeneous evolution needs high rotational velocity Stars born with high rotational velocity Single star progenitors (Yoon at al. 2006) Rotational velocity NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Distribution of Vsini/Vk for the young SMC cluster NGC 346 Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors
174. Predicted GRB/SN(Z) NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Yoon et al. 2006 This relies on the assumed distribution of initial rotational velocities! Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors
175. § Spin of compact remnants (Heger et al. 2005, Suijs et al. 2008) § Core-envelope coupling leads to spin-down of the core Convective Core Stockholm 2009 Matteo Cantiello Long GRB Progenitors Magnetic fields Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors
176. Evolution of Internal Structure - Homogeneous Model NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Yoon & Langer 2005 Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors
177. SWIFT GRBs Stockholm 2009 Matteo Cantiello Long GRB Progenitors Credit: Edo Berger (Harvard-Smithsonian CfA) Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors
178. NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Martins et al. 2009 Sedgwick 2011 Matteo Cantiello Long GRB Progenitors SMC: WR1 another chemically homogeneous star? According to Hunter et al. (2008), about 10% of the SMC stars have V sin i higher than 300 km/s CfA 2012 Matteo Cantiello Long GRB Progenitors
179. NGC 346: a cluster of young stars in the SMC Credit: Mokiem et al. 2007 Rotational Velocity vs Radial Velocity NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors
180. NGC 346: a cluster of young stars in the SMC Credit: Mokiem et al. 2007 Rotational Velocity vs Radial Velocity NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors
181. NGC 346: a cluster of young stars in the SMC Credit: Mokiem et al. 2007 Rotational Velocity vs Radial Velocity NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors
182. NGC 346: a cluster of young stars in the SMC Credit: Mokiem et al. 2007 Rotational Velocity vs Radial Velocity Is it possible that binary interaction is the cause of the existence of fast rotators? NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors
183. Evolution of Internal Structure NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Cantiello et al. 2007 Sedgwick 2011 Matteo Cantiello Long GRB Progenitors Binary Progenitor Single Progenitor CfA 2012 Matteo Cantiello Long GRB Progenitors
184. GRB 090429B Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors Cucchiara et al. 2011 z ~ 9.4 (tUniverse ~ 520 Myrs) CfA 2012 Matteo Cantiello Long GRB Progenitors
185. GRB 090429B Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors Cucchiara et al. 2011 z ~ 9.4 (tUniverse ~ 520 Myrs) CfA 2012 Matteo Cantiello Long GRB Progenitors
186. SN Spin up by accretion 16M Sun 15M Sun LGRB Runaway Wolf-Rayet Rotational Mixing!! 4M Sun 21M Sun M * ~ 13M Sun M co ~ 10M Sun J co ~ 2x1016cm2/s Case B mass transfer V ~ 30 km/s NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors
188. 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 NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors
189. 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 NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors
190. 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! NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors CfA 2012 Matteo Cantiello Long GRB Progenitors
196. Specific Angular momentum - Homogeneous Model NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Yoon & Langer 2005 Sedgwick 2011 Matteo Cantiello Long GRB Progenitors LCOGT 2012 Matteo Cantiello Long GRB Progenitors
197. GRB 090423 Text Credit: Gemini Observatory/NSF/AURA. Fox, Cucchiara & Berger Sedgwick 2011 Matteo Cantiello Long GRB Progenitors LCOGT 2012 Matteo Cantiello Long GRB Progenitors
198. GRB 090423 Text Credit: Gemini Observatory/NSF/AURA. Fox, Cucchiara & Berger Sedgwick 2011 Matteo Cantiello Long GRB Progenitors LCOGT 2012 Matteo Cantiello Long GRB Progenitors
199. GRB 090423 Text z = 8.2 tUniverse ~ 630 Myrs Credit: Gemini Observatory/NSF/AURA. Fox, Cucchiara & Berger Sedgwick 2011 Matteo Cantiello Long GRB Progenitors LCOGT 2012 Matteo Cantiello Long GRB Progenitors
200. Stockholm 2009 Matteo Cantiello Long GRB Progenitors Tanvir et al. 2009 Sedgwick 2011 Matteo Cantiello Long GRB Progenitors LCOGT 2012 Matteo Cantiello Long GRB Progenitors
201. ... most are close binaries! NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Courtesy: H. Sana Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors LCOGT 2012 Matteo Cantiello Long GRB Progenitors
202. ... most are close binaries! NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Courtesy: H. Sana Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors LCOGT 2012 Matteo Cantiello Long GRB Progenitors
203. ... most are close binaries! NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Courtesy: H. Sana Leicester 2009 Matteo Cantiello Long GRB Progenitors Binary interactions can not be neglected!!! Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors LCOGT 2012 Matteo Cantiello Long GRB Progenitors
204. Results § 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 single star models, 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 becomes a Runaway WR star and travels few hundred pc before producing a Long GRB Runaway GRBs NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors LCOGT 2012 Matteo Cantiello Long GRB Progenitors
205. ( Zen and The art of ) Evolving stars toward Long GRBs NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors LCOGT 2012 Matteo Cantiello Long GRB Progenitors
206. Conclusions § Long GRBs? Fast rotating massive stars that evolve chemically homogeneous § Two classes of progenitors: single and binary stars § In massive binaries it is possible to spin up a star and form a collapsar § This scenario is likely to produce a runaway WR which travels several hundred pc before collapse § Both single and binary progenitors prefer low Z NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors LCOGT 2012 Matteo Cantiello Long GRB Progenitors
207. Observational Consequences II § Afterglow properties NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors LCOGT 2012 Matteo Cantiello Long GRB Progenitors
208. Observational Consequences II Constant Density Van Marle et al. 2006 § Afterglow properties NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors LCOGT 2012 Matteo Cantiello Long GRB Progenitors
209. Stellar Evolution NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Leicester 2009 Matteo Cantiello Long GRB Progenitors § Hard to fulfill the collapsar scenario § Need compact size (removal of the stellar envelope) and high specific angular momentum in the core § This is expected, since #(GRB/SNe) ~ 1/1000 Core Envelope Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors LCOGT 2012 Matteo Cantiello Long GRB Progenitors
210. More than 50% of Massive stars are in binaries! NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Courtesy: H. Sana Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors LCOGT 2012 Matteo Cantiello Long GRB Progenitors
211. Observational Consequence § Position of GRB in the sky NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors HST Image for: GRB980425, GRB020903 and GRB030329 Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors LCOGT 2012 Matteo Cantiello Long GRB Progenitors
212. Observational Consequence § Position of GRB in the sky Hammer et. al NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors HST Image for: GRB980425, GRB020903 and GRB030329 Leicester 2009 Matteo Cantiello Long GRB Progenitors Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors LCOGT 2012 Matteo Cantiello Long GRB Progenitors