PhD Recruitment, February 12, API/GRAPPA Massive Stars Mass Loss Mathieu Renzo Advisors: S. N. Shore, C. D. Ott 1 / 12
Mass Loss - Why is it important ... ... for the environment of the stars? • Chemical and dynamical evolution of Galaxies • Effects on star formation • Giant bubbles ... for the stellar structure? • Evolutionary timescale • Final fate (BH, NS or WD?) • Light curve (LC) and explosion spectrum • Appearence: CSM and wind features (WR) • Role in the solution of the RSG problem? 2 / 12
Mass Loss - Possible Driving Mechanisms Metal Line Driving ⇐ Winds Dynamical Instabilities ⇐ LBVs, Episodic Mass Loss, Super-Eddington Winds Binary interactions ⇐ Roche Lobe Overflows Figure: η Car, false colors. (RLO) 3 / 12
Mass Loss in Stellar Evolution Codes ( ) Parametric models with large uncertainties (clumpiness, non-wind mass loss) encapsulated in efficiency factor: ˙ M ( L , T eff , Z , R , M , ... ) ← η ˙ M ( L , T eff , Z , R , M , ... ) Figure: From Smith 2014, ARA&A, 52, 487S 4 / 12
Mass Loss - Different ˙ M prescriptions with Grid of Z ⊙ stellar models (Renzo et al. , in preparation) : • Initial mass: M ZAMS = { 15, 20, 25, 30 } M ⊙ ; • Efficiency: 1 1 η = { 1, 10 } ; 3 , • Different combinations of wind mass loss rates for “hot”, “cool” and WR stars: Kudritzki et al. ’89; Vink et al. ’00, ’01; Van Loon et al. ’05; Nieuwenhuijzen et al. ’90; De Jager et al. ’88; Nugis & Lamers ’00; Hamann et al. ’98. 5 / 12
Mass Loss - Preliminary Results with Example: M ZAMS = 15 M ⊙ , Z ⊙ evolutionary tracks 5.2 5.2 Kudritzki et al. , de Jager et al. Vink et al. , de Jager et al. 5.1 5.1 5.0 5.0 4.9 4.9 4.8 4.8 log ( L / L ⊙ ) log ( L / L ⊙ ) 4.7 4.7 4.6 4.6 4.5 4.5 η = 1.0 η = 1.0 4.4 4.4 η = 0.33 η = 0.33 4.3 4.3 η = 0.1 η = 0.1 4.2 4.2 4.6 4.4 4.2 4.0 3.8 3.6 3.4 4.6 4.4 4.2 4.0 3.8 3.6 3.4 log ( T eff / [ K ]) log ( T eff / [ K ]) ⇒ Early (“hot”) wind influences subsequent evolution 6 / 12
Experiment with Episodic Mass Loss (e.g. RLO) • ∆ M wind ≪ ∆ M episodic (?) • Could explain H-poor progenitors of SNIIb/Ib/Ic and/or CSM for SNIIn • Dynamics ⇒ not ready 5.4 stripped 4 M ⊙ unstripped 5.3 stripped 1 M ⊙ stripped 5 M ⊙ 5.2 stripped 2 M ⊙ stripped 6 M ⊙ 5.1 stripped 3 M ⊙ stripped 7 M ⊙ 5.0 log 10 ( L / L ⊙ ) 4.9 4.8 4.7 4.6 4.5 4.4 M ZAMS = 15 M ⊙ , Z ⊙ 4.3 Stripping 4.2 4.5 4.4 4.3 4.2 4.1 4.0 3.9 3.8 3.7 3.6 3.5 log 10 ( T eff / [ K ])
Experiment with Episodic Mass Loss (e.g. RLO) • ∆ M wind ≪ ∆ M episodic (?) • Could explain H-poor progenitors of SNIIb/Ib/Ic and/or CSM for SNIIn Always Global • Dynamics ⇒ not ready Hydrostatic 5.4 Equilibrium stripped 4 M ⊙ unstripped 5.3 stripped 1 M ⊙ stripped 5 M ⊙ 5.2 stripped 2 M ⊙ stripped 6 M ⊙ 5.1 stripped 3 M ⊙ stripped 7 M ⊙ 5.0 log 10 ( L / L ⊙ ) 4.9 4.8 4.7 4.6 ⇒ LC (SNEC) 4.5 4.4 M ZAMS = 15 M ⊙ , Z ⊙ (Morozova et al. , 4.3 Stripping 4.2 in preparation) 4.5 4.4 4.3 4.2 4.1 4.0 3.9 3.8 3.7 3.6 3.5 log 10 ( T eff / [ K ]) 7 / 12
Light Curve from the Stripped Models with SNEC 44 M0 M3 M6 M1 M4 M7 M2 M5 M8 Dashed: log 10 L [10 x erg/s] 43 E ej = 10 51 ergs , 42 Plain: E ej = 2 × 10 51 ergs 41 0 50 100 150 Time since breakout (days) Figure: From Morozova et al. , in preparation 8 / 12
Mass Loss - Conclusions Improvement needed for the dynamical instabilities • Mass loss is important both for the stellar structures and their environment; • Several mass loss mechanisms, many neglected in stellar evolution codes; • Large theoretical and observational uncertainties on the mass loss rate ˙ M ; • Effects of these uncertainties unexplored in a systematic way. Thank you for your attention. 9 / 12
Challenges: near-to-super-Eddington envelopes dP gas � L Edd � = dP rad − 1 , dr dr L rad ● ● ● ● ● ● ● ● ● ● ● ● ● ● 2.5 Z=0.02 − 9 . 9 ● ● ● 70 M ⊙ , T e ff = 5000 K ● ● ● ● a) ● ● ● ● ● log ( ρ ) ● ● Z=0.01 ● ● ● ● ● ● ● ● ● ● ● ● ● ● − 10 . 0 ● ● ● ● ● ● ● ● Z=0.004 ● ● ● ● ● ● ● ● ● ● ● 2.0 ● ● ● ● ● ● ● ● ● ● ● ● Z=0.001 − 10 . 1 ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● κ [cm 2 g − 1 ] ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● Z=0.0001 ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● 1.5 ● ● ● ● ● ● ● � b) ● ● ● ● ● ● ● ● ● ● ● ● gas ● ● ● ● 2 . 38 ● ● ● ● ● ● ● ● ● ● ● P ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● � ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● log ● ● ● ● ● ● ● ● ● 1.0 ● ● ● ● OPAL: X = 0.7, log ( ρ / T 63 ) = − 5 2 . 31 ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● 3 . 3 ● ● ● ● ● ● ● ● ● ● ● ● ● ● 0.5 ● ● ● ● c) ● ● ● ● log ( P ) ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● 3 . 0 ● ● ● 5.0 5.5 6.0 6.5 7.0 ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● log 10 ( T / [ K ]) ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● 2 . 7 ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● 80 ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● A k B ) ● ● d) ● ● M ZAMS � 20 M ⊙ ⇒ insufficient F MLT ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● conv ● ● ● ● ● ● ● ● ● S / ( N ● ● ● ● ● 60 ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● MLT++: ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● 1000 1100 1200 1300 ∇ T − ∇ ad → α ∇ f ∇ ( ∇ T − ∇ ad ) r / R ⊙ Figure: From Paxton et al. α ∇ ≡ α ∇ ( β , Γ Edd ) , f ∇ ≪ 1 2013, ApJS, 208, 5p 10 / 12
Episodic Mass Loss: Choice of Stripping Moment 5.2 unstripped 5.1 M = 15 M ⊙ , Z = Z ⊙ 5.0 Convective Envelope Maximum Extension 4.9 log 10 ( L / L ⊙ ) 4.8 4.7 4.6 Middle SGB 4.5 4.4 R = 375 R ⊙ ≡ max ( R ) 4.3 2 4.2 4.5 4.4 4.3 4.2 4.1 4.0 3.9 3.8 3.7 3.6 3.5 3.4 log 10 ( T eff / [ K ]) 11 / 12
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