Pre-supernova mass-loss predictions for massive stars Jorick Vink (Keele University)

Outline Introduction Mass loss predictions OB & WR - f(Z) Mass loss predictions OB & LBV - f(T) Radio SNe with variable CSM Summary

Evolution of a Massive Star

Radiation-driven wind by Lines Lucy & Solomon (1970) Castor, Abbott & Klein (1975) = CAK Wind STAR Fe dM/dt = f (Z, L, M, Teff)

Radiation-driven wind by Lines Abbott & Lucy (1985) dM/dt = f (Z, L, M, Teff)

OB Mass loss parameter study

Wind momenta for Galactic O stars Models Vink, de Koter & Lamers (2000)

Vink et al. (2001) Mokiem et al. (2007) Wind momenta at low Z Data (Mokiem) Models (Vink) Vink et al. (2001) Mokiem et al. (2007)

Which element drives WR winds? - Fe  WR mass loss depends on Z host - C  it does NOT depend on Z host

Z-dependence of WR winds WN WC Vink & de Koter (2005, A&A 442, 587)

This is a gif file Lamers et al. (1995), Crowther et al. (2006) Vink et al. (1999): Fe IV III

Stars should pass the bistable limit During evolution from O  B LBVs on timescales of years

LBVs in the HRD Smith, Vink & de Koter (2004)

The mass loss of LBVs Stahl et al. (2001) Vink & de Koter (2002) Models Data Stahl et al. (2001) Vink & de Koter (2002)

Stars should pass the bistable limit During evolution from O  B LBVs on timescales of years Implications for circumstellar medium (CSM) Mass-loss rate up ~ 2 wind velocity down ~ 2 CSM density variations ~ 4

Radio Supernovae S=Flux SN Ic 1990B Weiler et al. (2000) Time

SN-CSM interaction  radio Weiler et al. (2002)

Mass Loss Results from Radio SNe OB star? WR?

CSM: a constant mass-loss rate Wind Density Radius

CSM: a varying LBV mass-loss rate Wind Density Radius

The Radio SN 2001ig Ryder et al. (2004)

The Radio SN 2001ig Ryder et al. (2004)  t = 150 days

Predicted period AGB star  w = 10 km/s  Period = 50 years Ryder et al. (2004) AGB star  w = 10 km/s  Period = 50 years

Predicted period AGB star  w = 10 km/s  Period = 50 years Ryder et al. (2004) AGB star  w = 10 km/s  Period = 50 years LBV  w = 100 km/s  Period = 5 years ! Kotak & Vink (2006)

WR Binary Pinwheel nebulae? Tuthill et al. (1999) But……

2003bg: the twin of 2001ig 2003bg , 2001ig Soderberg et al. (2006)

Progenitors AGB star Binary WR system WR star LBV b

Progenitors AGB star Binary WR system WR star LBV Kotak & Vink (2006)

Speculation on Radio SNe that show sinusoidal variations H-rich H-poor OB/RSG  LBV  WR SN II  ?  Ibc

Summary Monte Carlo mass loss predictions successful:  OB & WR stars as a function of Z  The bistability jump between O and B  LBV mass loss variability Radio SNe with (quasi)-sinusoidal modulations may have LBV progenitors

The bi-stability Jump HOT Fe IV low dM/dt high V(inf) Low density COOL Fe III dM/dt = 5 dM/dt HOT V(inf) = ½ vinf HOT High density = 10 HOT