Massive Stars: Where the Wild Things Are

Lecture 3 given at the "Look & Listen" Astrophysics School, Playa del Carmen (Mexico), 2014. Topics: Explosive Death of Massive Stars

Transcript

1. Massive Stars: Where the wild things are Matteo Cantiello Kavli Institute for Theoretical Physics (University of California Santa Barbara)
2. M/M . 8 8 . M/M . 10 10 . M/M . 25 140 . M/M . 250 Final Fate of Massive Stars Mexico 2014 Matteo Cantiello Look&Listen WD or Type Ia SN Electron Capture SN Iron Core collapse SN (Type II, Ibc), NS remnant Pair Instability SN Else: BH remnants + GRBs: Rare Channel
3. SN Zoo Mexico 2014 Matteo Cantiello Look&Listen Smith (2010)
4. SN Zoo Mexico 2014 Matteo Cantiello Look&Listen Arcavi et al. 2010 [Adapted from Crowther 2012]
5. Type II-P Supernovae 30 17 20 40 25 • No type II-P progenitor is found for Mini ~> 17 Msun (Smartt et al. 2009) Red Supergiants Problem Matteo Cantiello Skyhouse– 03/30/2012 • Is mass-loss stronger than expected? Mexico 2014 Matteo Cantiello Look & Listen
6. Pulsations in RSGs Fe He H Important property of the structure of the majority of pre- SN stars: they are pulsationally unstable. The excitation is due to the k-mechanism Mexico 2014 Matteo Cantiello Look & Listen Mexico 2014 Matteo Cantiello Look & Listen
7. Pulsations in RSGs Fe He H Pulsation is caused by partial ionization of Hydrogen for T< 5000 K (Li & Gong, 1994; Heger et al. 1997) Important property of the structure of the majority of pre- SN stars: they are pulsationally unstable. The excitation is due to the k-mechanism Mexico 2014 Matteo Cantiello Look & Listen Mexico 2014 Matteo Cantiello Look & Listen
8. Pulsations in RSGs Matteo Cantiello Skyhouse– 03/30/2012 0 5 10 15 20 25 t-t 0 [yr] 1200 1400 1600 1800 R/R -2 -1 0 1 2 Mach # RSG Phase Y c = 0.7 t 0 = 6.851 Myr 25M V ini = 200 km/s Z=0.02 Radius v surf / c s 3.543 3.528 3.513 3.498 3.484 log T 5.25 5.30 5.35 5.40 log L/L Paxton et al. 2013 Mexico 2014 Matteo Cantiello Look & Listen
9. Pulsations in RSGs Matteo Cantiello Skyhouse– 03/30/2012 30 17 20 40 25 Yoon & Cantiello 2010 Mexico 2014 Matteo Cantiello Look & Listen
10. Type II-P Supernovae 30 17 20 40 25 • No type II-P progenitor is found for Mini ~> 17 Msun (Smartt et al. 2009) • Calculations by Dessart et al. (2010) support Mini ~< 20 Msun (But see also Utrobin & Chugai 2009) Pulsations remove most of the H envelope in models with Mini >~19...20 Msun Red Supergiants Problem Matteo Cantiello Skyhouse– 03/30/2012 Mexico 2014 Matteo Cantiello Look & Listen
11. Type IIn supernovae Credit: Nasa/Humphrey If VY CMa were to explode now, it would results in a Type IIn (Smith et al. 2009) Matteo Cantiello Skyhouse– 03/30/2012 Mexico 2014 Matteo Cantiello Look & Listen
12. Type IIn supernovae Credit: Nasa/Humphrey If VY CMa were to explode now, it would results in a Type IIn (Smith et al. 2009) • If eruption-like event occurs ~1000 yrs before core collapse, a moderately luminous Type IIn SN could be observed (like 1988Z) Matteo Cantiello Skyhouse– 03/30/2012 Mexico 2014 Matteo Cantiello Look & Listen
13. Type IIn supernovae Credit: Nasa/Humphrey If VY CMa were to explode now, it would results in a Type IIn (Smith et al. 2009) Matteo Cantiello Skyhouse– 03/30/2012 Mexico 2014 Matteo Cantiello Look & Listen
14. Stellar Eruptions Matteo Cantiello Skyhouse– 03/30/2012 • Eta Carinae is a supermassive (~120 solar mass) star • Underwent extreme brightening called “Great Eruption” in 1837 for 20 years • In 1843 was 2nd brightest extrasolar object as viewed from Earth with apparent magnitude -1 • A Lesser Eruption occurred in 1890 • Highly eccentric binary Mexico 2014 Matteo Cantiello Look & Listen
15. Various lines of evidence suggest that very massive stars experience extreme mass-loss episodes shortly before they explode as a supernova (few years to tens of days). Pre-SN Eruptions Matteo Cantiello Skyhouse– 03/30/2012 E.g. Ofek et al. 2013, Dopita et al. 1984, Chugai et al. 1994, Gal-Yam & Leonard 2009, Ofek et al. 2010, Smith et al. 2010, Foley et al. 2010... Only a couple of theoretical ideas exist that can potentially explain these this peculiar behaviour:  Pulsational pair instability: Woosley at el. 2007  Wave-driven mass loss: Quataert & Shiode 2012, Shiode & Quataert 2013 Ofek et al. 2013 Mexico 2014 Matteo Cantiello Look & Listen
16. (Pulsational) Pair Instability SNe Matteo Cantiello Skyhouse– 03/30/2012 NASA/CXC/M ! e+ + e Mexico 2014 Matteo Cantiello Look & Listen
17. Pop III Stars: Final Fate Matteo Cantiello Skyhouse– 03/30/2012 NASA/CXC/M Yoon et al. 2012 Mexico 2014 Matteo Cantiello Look & Listen
18. Wave Driven Mass-Loss Matteo Cantiello Skyhouse– 03/30/2012 NASA/CXC/M Quatart & Shiode 2012 Mexico 2014 Matteo Cantiello Look & Listen 25 MSun
19. Wave Driven Mass-Loss Matteo Cantiello Skyhouse– 03/30/2012 NASA/CXC/M Quatart & Shiode 2012 Mexico 2014 Matteo Cantiello Look & Listen
20. Very Massive Stars
21. Very Massive Stars Mexico 2014 Matteo Cantiello Look&Listen
22. Very Massive Stars Mexico 2014 Matteo Cantiello Look&Listen Crowther et al. (2010) MIni ~300 MSun MIni~240 MSun
23. Gamma Ray Bursts
24. Gamma Ray Bursts NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors IPMU 2012 Matteo Cantiello Long GRB Progenitors Mexico 2014 Matteo Cantiello Look&Listen
25. Gamma Ray Bursts NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors The most luminous electromagnetic transients in the universe IPMU 2012 Matteo Cantiello Long GRB Progenitors Mexico 2014 Matteo Cantiello Look&Listen
26. 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 IPMU 2012 Matteo Cantiello Long GRB Progenitors Mexico 2014 Matteo Cantiello Look&Listen
27. 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) IPMU 2012 Matteo Cantiello Long GRB Progenitors Mexico 2014 Matteo Cantiello Look&Listen
28. 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) IPMU 2012 Matteo Cantiello Long GRB Progenitors Mexico 2014 Matteo Cantiello Look&Listen
29. Two classes of GRBs NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors 70% Long (t > 2s) Associated with the death of massive stars (e.g. Nomoto et al. 2011) 30% Short (t < 2s) Merger of compact objects? (e.g. Berger 2011) Image credit: Price & Rosswog IPMU 2012 Matteo Cantiello Long GRB Progenitors Mexico 2014 Matteo Cantiello Look&Listen
30. Long GRBs Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors IPMU 2012 Matteo Cantiello Long GRB Progenitors Mexico 2014 Matteo Cantiello Look&Listen
31. 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, Nomoto 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) IPMU 2012 Matteo Cantiello Long GRB Progenitors Mexico 2014 Matteo Cantiello Look&Listen
32. 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, Nomoto 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? IPMU 2012 Matteo Cantiello Long GRB Progenitors Mexico 2014 Matteo Cantiello Look&Listen
33. • 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 IPMU 2012 Matteo Cantiello Long GRB Progenitors Mexico 2014 Matteo Cantiello Look&Listen
34. Stockholm 2009 Matteo Cantiello Long GRB Progenitors Sedgwick 2011 Matteo Cantiello Long GRB Progenitors Central Engines 101 Collapsar Woosley 1993 IPMU 2012 Matteo Cantiello Long GRB Progenitors Mexico 2014 Matteo Cantiello Look&Listen
35. 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 IPMU 2012 Matteo Cantiello Long GRB Progenitors Mexico 2014 Matteo Cantiello Look&Listen
36. 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 IPMU 2012 Matteo Cantiello Long GRB Progenitors Mexico 2014 Matteo Cantiello Look&Listen
37. 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 IPMU 2012 Matteo Cantiello Long GRB Progenitors Mexico 2014 Matteo Cantiello Look&Listen
38. 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 IPMU 2012 Matteo Cantiello Long GRB Progenitors Mexico 2014 Matteo Cantiello Look&Listen
39. 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 IPMU 2012 Matteo Cantiello Long GRB Progenitors Mexico 2014 Matteo Cantiello Look&Listen
40. 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 IPMU 2012 Matteo Cantiello Long GRB Progenitors Mexico 2014 Matteo Cantiello Look&Listen
41. 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 IPMU 2012 Matteo Cantiello Long GRB Progenitors Mexico 2014 Matteo Cantiello Look&Listen
42. 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 IPMU 2012 Matteo Cantiello Long GRB Progenitors Mexico 2014 Matteo Cantiello Look&Listen
43. 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 IPMU 2012 Matteo Cantiello Long GRB Progenitors Mexico 2014 Matteo Cantiello Look&Listen
44. 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 IPMU 2012 Matteo Cantiello Long GRB Progenitors Mexico 2014 Matteo Cantiello Look&Listen
45. Final Angular Momentum Content 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 IPMU 2012 Matteo Cantiello Long GRB Progenitors 15 16 17 18 19 log j [cm2/s] ZAMS TAMS He Depletion C Depletion Si Depletion j LSO (J) j LSO Kerr j LSO Schwarzschild 16M J ini = 3.2d52 Z=0.0002 0 5 10 15 enclosed mass/M O • 0.0 0.5 1.0 1.5 2.0 Log t ff [s] Free-fall time Calculated with MESA Mexico 2014 Matteo Cantiello Look&Listen
46. GRB Observations
47. 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 IPMU 2012 Matteo Cantiello Long GRB Progenitors Mexico 2014 Matteo Cantiello Look&Listen
48. 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 IPMU 2012 Matteo Cantiello Long GRB Progenitors Mexico 2014 Matteo Cantiello Look&Listen
49. 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 IPMU 2012 Matteo Cantiello Long GRB Progenitors Mexico 2014 Matteo Cantiello Look&Listen
50. 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 IPMU 2012 Matteo Cantiello Long GRB Progenitors Mexico 2014 Matteo Cantiello Look&Listen
51. 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 IPMU 2012 Matteo Cantiello Long GRB Progenitors Mexico 2014 Matteo Cantiello Look&Listen
52. 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 IPMU 2012 Matteo Cantiello Long GRB Progenitors Mexico 2014 Matteo Cantiello Look&Listen
53. 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 IPMU 2012 Matteo Cantiello Long GRB Progenitors Mexico 2014 Matteo Cantiello Look&Listen
54. 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 IPMU 2012 Matteo Cantiello Long GRB Progenitors Mexico 2014 Matteo Cantiello Look&Listen
55. 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 IPMU 2012 Matteo Cantiello Long GRB Progenitors Mexico 2014 Matteo Cantiello Look&Listen
56. SN Spin up by accretion Rotational Mixing!! M* ~ 13MSun Mco ~ 10MSun Jco ~ 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 15MSun 16MSun Case B mass transfer 21MSun 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 IPMU 2012 Matteo Cantiello Long GRB Progenitors Mexico 2014 Matteo Cantiello Look&Listen
57. Massive Binaries
58. NS & GRBs 2009 (ﺓةﻱيﺭرﺩدﻥنﻙكﺱسﺇإﻝلﺍا - Alexandria) Matteo Cantiello Long GRB Progenitors Fireworks 2009 (Bonn) Matteo Cantiello Long GRB Progenitors Sana et al. 2012 (Science) 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 IPMU 2012 Matteo Cantiello Long GRB Progenitors “71% of all stars born as O-type interact with a companion, over half of which do so before leaving the main sequence” Incidence of binarity Mexico 2014 Matteo Cantiello Look&Listen
59. 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 IPMU 2012 Matteo Cantiello Long GRB Progenitors Mass Transfer Mexico 2014 Matteo Cantiello Look&Listen
60. 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 Mexico 2014 Matteo Cantiello Look&Listen Binary interactions are common de Mink et al. 2014
61. Binary interactions 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 Mexico 2014 Matteo Cantiello Look&Listen de Mink et al. 2013
62. OB stars rotate rapidly Matteo Cantiello Pulsations and Magnetic Fields in Massive Stars IAU GA SpS13 – Beijing 2012 P ( VEq sin i ) P ( VEq ) 334 B Stars Dufton et al. 2013 Matteo Cantiello Pulsations, Turbulence and Magnetic Fields in Massive Stars NORDITA – Stockholm 2013 Mexico 2014 Matteo Cantiello Look&Listen
63. Some (Recent) developments: Mexico 2014 Matteo Cantiello Look&Listen Massive stars are known to rotate quite rapidly 10% of massive stars have strong magnetic fields Pre SN eruptions and peculiar SN types identified Most massive stars (70%) are in binary systems Very massive stars seem to exist in the local universe. Long GRBs prefer (but are not exclusively formed) in low metallicity environments
64. Some Outstanding Questions Mexico 2014 Matteo Cantiello Look&Listen Internal mixing of chemicals and angular momentum not fully understood Origin of stellar magnetic fields. Main sequence and compact remnants What is causing Pre SN eruptions and peculiar SN types Physics of stellar mergers and binary interactions. Do PISN occur in the local universe? ...