Structure and Evolution of Massive Stars (and of the less massive ones also...) Ana Palacios, LUPM / Université de Montpellier
The Hertzsprung Russell diagram New reduction fo Hipparcos Catalog
The evolutionary path of stars Stars move from red to blue to red again The fate of low and intermediate mass stars and their evolutionary path are relatively well known and constrained. The evolutionary path and fate of massive stars is very uncertain Iben 1991
The evolution of massive stars Mass loss driven evolution Maeder et al., 2008, IAUS 250 normal evolution 60 M Groh et al. 2014
Standard structural evolution of a massive star Heger & Woosley
Standard structural evolution of a massive star Onion-skin structure of the core of an evolved massive star Kippenhahn & Weigert book new edition
Expected fate from standard stellar evolution models SNIIP, other SNII, SNIb/Ic Eldridge et al. 2013
Expected surface abundance variations in massive stars O: No variation expected BSG to RSG : 4 He H 14 N 12 C and 14 O C and 22 14 N 12 16 WC: WN : Ne and 16 O Mg 25 Meynet & Maeder, 2003, A&A 404, 975 N 12 22 C and Ne 16 O
Standard structural evolution of an intermediate mass star (1) Evolution up to the e-agb Kippenhahn & Weigert book new edition
Expected surface abundance variations in IM stars 4 He 12C 13C 14N 3 He 7Li After the 2nd DUP, 4He and N appear 14 enhanced at the surface of the star 1.14 x 108
Expected surface abundance variations in IM stars H-burning (HBS+HBB) 14 N,13C,15N,23Na,25,26Mg, 26,27Al He-burning (HeBS+pulse) 12 C,16O,18O,19F,20Ne,22Ne,25,26Mg figure by M. Forestini
Standard structural evolution of an intermediate mass star (2) AGB and post-agb evolution Kippenhahn & Weigert book new edition
Expected fate of stars from standard stellar evolution models After Siess 2006
The drivers of evolution Nucleosynthesis through exothermic nuclear reactions Mass loss for massive or evolved stars See Talk by F. Martins
The drivers of evolution Nucleosynthesis through exothermic nuclear reactions Mass loss for massive or evolved stars See Talk by F. Martins What processes actually matter in shaping the structure and evolution of stars?
The drivers of evolution Nucleosynthesis through exothermic nuclear reactions Mass loss for massive or evolved stars See Talk by F. Martins What processes actually matter in shaping the structure and evolution of stars? Any process that will affect the internal chemical stratification and the surface opacities
The drivers of evolution Nucleosynthesis through exothermic nuclear reactions Mass loss for massive or evolved stars See Talk by F. Martins What processes actually matter in shaping the structure and evolution of stars? Any process that will affect the internal chemical stratification and the surface opacities It is the case of dynamical processes
The drivers of evolution Nucleosynthesis through exothermic nuclear reactions Mass loss for massive or evolved stars See Talk by F. Martins What processes actually matter in shaping the structure and evolution of stars? Any process that will affect the internal chemical stratification and the surface opacities It is the case of dynamical processes Rotation
The drivers of evolution Nucleosynthesis through exothermic nuclear reactions Mass loss for massive or evolved stars See Talk by F. Martins What processes actually matter in shaping the structure and evolution of stars? Any process that will affect the internal chemical stratification and the surface opacities It is the case of dynamical processes Rotation Waves
The drivers of evolution Nucleosynthesis through exothermic nuclear reactions Mass loss for massive or evolved stars See Talk by F. Martins What processes actually matter in shaping the structure and evolution of stars? Any process that will affect the internal chemical stratification and the surface opacities It is the case of dynamical processes Rotation Waves Magnetic fields
The drivers of evolution Nucleosynthesis through exothermic nuclear reactions Mass loss for massive or evolved stars See Talk by F. Martins What processes actually matter in shaping the structure and evolution of stars? Any process that will affect the internal chemical stratification and the surface opacities It is the case of dynamical processes Rotation Waves Magnetic fields Turbulent instabilities
Successes and caveats of present-day models of low and intermediate-mass stars Modern models including rotation and other non-standard transport processes have improved the comparison with observations in terms of surface abundances Charbonnel & Lagarde 2010.
Successes and caveats of present-day models of low and intermediate-mass stars Modern models including rotation and other non-standard transport processes have improved the comparison with observations in terms of surface abundances Palacios et al. 2003 Vini = 110 km/s Charbonnel & Lagarde 2010. Vini = 110 km/s
Successes and caveats of present-day models of low and intermediate-mass stars Modern models including rotation and other non-standard transport processes have improved the comparison with observations in terms of surface abundances Palacios et al. 2003 Michaud et al. 2008 Vini = 110 km/s Charbonnel & Lagarde 2010. Vini = 110 km/s
Successes and caveats of present-day models of low and intermediate-mass stars Modern models including rotation and other non-standard transport processes give hints for improvement on the side of angular momentum evolution vzams = 50 km/s Ω/2π (μhz) vzams = 20 km/s Garcia et al., 2011 Internal solar rotation profile inversion using 4608 days of MDI and GOLF data. Eggenberger et al., 2005 Charbonnel & Talon, 2005
Successes and caveats of present-day models of low and intermediate-mass stars Asteroseismology with Kepler has revolutionized our view of red giant stars X RGB stars Δ Clump stars 2nd Clump stars Mosser et al. 2012, A&A 548, A10 27
Successes and caveats of present-day models of low and intermediate-mass stars SubGiant and Red Giant Branches / Clump Inversion of the rotation gradient in subgiant branch stars from the Kepler fields The direction of the arrows indicates increasing age Deheuvels et al. 2014 28
Successes and caveats of present-day models of low and intermediate-mass stars Modern models including rotation and other non-standard transport processes give hints for improvement on the side of angular momentum evolution Cantiello et al. 2014
Uncertainties due to constitutive physics Impact of physical inputs within one code STAREVOL MESA Martins & Palacios 2013
Uncertainties due to constitutive physics Differences between publicly available grids Martins & Palacios 2013
Uncertainties due to constitutive physics Jones et al. (2015)
Uncertainties due to nuclear physics Large uncertainties on the nuclear reaction rates associated to He and C burning impact on stellar yields Helium burning Carbon burning Bennet et al. 2012 West et al. 2013 West et al. 2013
Uncertainties due to nuclear physics Large uncertainties on the nuclear reaction rates associated to He and C burning impact on stratification of white dwarfs S. Charpinet
Uncertainties due to nuclear physics Large uncertainties on the nuclear reaction rates associated to He and C burning impact on stratification of white dwarfs S. Charpinet Asteroseismology can help here
Uncertainties due to nuclear physics Large uncertainties on the nuclear reaction rates associated to He and C burning impact on stellar yields Pignatari et al. 2013 West et al. 2013
The dynamical drivers of evolution Rotation modification of the stellar structure (centrifugal forces, non-sphericity, gravity darkening) modification of the mass loss transport of angular momentum and chemicals (macroscopic movements and hydrodynamical instabilities) Magnetic Fields modification of the stellar structure (Lorentz torque, magnetic energy, ohmic diffusion) transport of angular momentum and chemicals (MHD instabilities) Internal Gravity Waves transport of angular momentum (and chemicals) Thermohaline mixing transport of chemicals
Impact of rotation on structure and evolution Modification of evolutionary paths and fate of massive stars Georgy et al. 2012
Impact of rotation on structure and evolution Modification of evolutionary paths and fate of massive stars Groh et al. 2013
Impact of rotation on the nucleosynthesis Georgy et al. 2012
Impact of rotation on structure and evolution Meynet et al. 2013 The choice of prescriptions impacts the evolutionary tracks advection nuclear microscopic processes diffusion Turbulence + merid. circ.
Impact of rotation on structure and evolution Chieffi & Limongi 2013
Impact of magnetic fields on structure and evolution Small percentage of massive stars with detected surface large-scale magnetic fields MiMes collaboration
Impact of magnetic fields on structure and evolution Magnetic fields introduced by means of instabilities - Taylor-Spruit instability - MRI Suijs et al. 2008
Impact of magnetic fields on structure and evolution Wheeler et al. 2015
Impact of magnetic fields on structure and evolution Wheeler et al. 2015
Impact of magnetic fields on structure and evolution Magnetic fields introduced by means of the exerted torque through winds Propose to spin down the core of massive stars Georgy et al. 2012
Summary Stellar structure and evolution : zero order known for evoltuion not driven by mass loss Disparity between the massive stars and less massive ones concerning evolutionary path and fate Large uncertainties from the point of view of models Clear impact of rotation and angular momentum transport processes on structure and evolution Necessity to improve the description / understanding of the dynamical processes