CRyA Mass Loss Return from Stars to Galaxies, STScI, 30 March 2012 Self-consistent mass-loss in stellar population synthesis models Rosa A. González-Lópezlira CRyA, UNAM/AIfA, Bonn dust Gonzalez-Lopezlira et al. 2010, MNRAS, 403, 1213

CRyA Self-consistent mass-loss in SPS models Rosa A. González-Lópezlira Mass Loss Return from Stars to Galaxies, STScI, 30 March 2012 Gustavo Bruzual CIDA, Mérida, Venezuela Stéphane Charlot IAP, Paris, France Laurent Loinard CRyA, UNAM, Morelia, Mexico Javier Ballesteros-P. CRyA, UNAM, Morelia, Mexico Collaborators

CRyA Self-consistent mass-loss in SPS models Rosa A. González-Lópezlira Mass Loss Return from Stars to Galaxies, STScI, 30 March 2012 Stellar mass-loss Drives chemical enrichment and evolution of galaxies Replenishes molecular gas destroyed by energetic photons Shapes the AGB and PN luminosity functions Determines WD mass spectrum and cooling times SNe Ia progenitor mass and frequency SNe II, Ib, Ic rate

CRyA Self-consistent mass-loss in SPS models Rosa A. González-Lópezlira Mass Loss Return from Stars to Galaxies, STScI, 30 March 2012 TP-AGB stars in intermediate age populations  Thermal pulses  Convective dredge-up  Envelope ejection  Obscured  Only recently resolution in mid-IR  M = f(L, M, Z)?. } etc. L/L Su n from Boothroyd, Sackmann & Kramer 1993

CRyA Self-consistent mass-loss in SPS models Rosa A. González-Lópezlira Mass Loss Return from Stars to Galaxies, STScI, 30 March 2012 Bowen & Willson (1991), in Willson (2000) Mass-loss does not happen smoothly (Reimers 1975)

CRyA Self-consistent mass-loss in SPS models Rosa A. González-Lópezlira Mass Loss Return from Stars to Galaxies, STScI, 30 March 2012  Required to include M and dusty envelopes in contribution from TP-AGB for all evolutionary stages and all Z Challenges for SSP models Need an analytic approach: no empirical dusty spectra for all Z and phases Hard constraints only for Galactic and Magellanic Z, (recently, also for low metallicities; Girardi et al. 2010, ANGST).

CRyA Self-consistent mass-loss in SPS models Rosa A. González-Lópezlira Mass Loss Return from Stars to Galaxies, STScI, 30 March 2012  M,L,T(star type, age, Z)  M + dust mixture     + input SED + radiative transfer  output SED Analytic approach Pioneered by Bressan et al. 1998, Lançon & Mouhcine 2002; Piovan et al

CRyA Self-consistent mass-loss in SPS models Rosa A. González-Lópezlira Mass Loss Return from Stars to Galaxies, STScI, 30 March 2012 A very interactive procedure

CRyA Self-consistent mass-loss in SPS models Rosa A. González-Lópezlira Mass Loss Return from Stars to Galaxies, STScI, 30 March 2012 O-rich stars Carbon stars    3: 90% warm AMS, 5% ens, 5% forst 3    15: 90% cold AMS, 5% enst, 5% forst    15: 80% cold AMS, 10% ens, 10% forst    0.15: 80% AMC, 20% SiC    0.8: 90% AMC, 10% SiC     0.8: 100% AMC Mixtures: Suh (1999,2000,2002) C. Kemper’s talk

CRyA Self-consistent mass-loss in SPS models Rosa A. González-Lópezlira Mass Loss Return from Stars to Galaxies, STScI, 30 March 2012 Carbon stars (C/O ≥ 0.97) O-rich stars (C/O < 0.97) Following Piovan et al. 2003

CRyA Self-consistent mass-loss in SPS models Rosa A. González-Lópezlira Mass Loss Return from Stars to Galaxies, STScI, 30 March 2012 X seed : mass fraction of seed element in circumstellar shell (take solar and scale by Z) A seed : seed element atomic weight A dust : dust species molecular weight f dust,i : fraction of seed element condensed into grains of each dust species A and B depend on: dust condensation T, dust efficiency coefficients for radiation pressure and absorption, and dust cross section per gas particle  gas After Marigo et al and Ferrarotti & Gail 2006

CRyA Self-consistent mass-loss in SPS models Rosa A. González-Lópezlira Mass Loss Return from Stars to Galaxies, STScI, 30 March 2012 Carbon stars O-rich stars f SiC follows Y C = X C /A C Y C,1 = X O /A O – 2X Si /A Si

CRyA Self-consistent mass-loss in SPS models Rosa A. González-Lópezlira Mass Loss Return from Stars to Galaxies, STScI, 30 March 2012 Piovan et al. (2003)  i : mass abundance of dust species a: dust size = 0.1  m dust,i : grain mass Q ext (i): extinction coefficients of species

CRyA Self-consistent mass-loss in SPS models Rosa A. González-Lópezlira Mass Loss Return from Stars to Galaxies, STScI, 30 March 2012  : Radiative transfer with 1-D code DUSTY (Ivezic, Nenkova & Elitzur 1999 ) C star, Z=0.008, M=4.2e-6M sun yr -1,  =1.1O-rich star, Z=0.008, M=4.9e-6M sun yr -1,  =0.21 Input SED: Aringer Input SED: Lançon..

CRyA Self-consistent mass-loss in SPS models Rosa A. González-Lópezlira Mass Loss Return from Stars to Galaxies, STScI, 30 March 2012 Data: SAGE (Srinivasan, Meixner et al.)

CRyA Self-consistent mass-loss in SPS models Rosa A. González-Lópezlira Mass Loss Return from Stars to Galaxies, STScI, 30 March 2012 Marigo & Girardi 2007, based on Bowen & Willson 1991 What if you want to tweak you mass loss? E. Villaver’s talk

CRyA Self-consistent mass-loss in SPS models Rosa A. González-Lópezlira Mass Loss Return from Stars to Galaxies, STScI, 30 March 2012 Radiative transfer Dust mixtures e.g., Fuel Consumption Theorem (Renzini & Buzzoni 1986)  M   L   R   T, P, C/O,v exp SEDs t AGB n *,M c …. e.g., Marigo & Girardi 2007

CRyA Self-consistent mass-loss in SPS models Rosa A. González-Lópezlira Mass Loss Return from Stars to Galaxies, STScI, 30 March 2012 Data: SAGE-LMC Calibration/exploration: SBF in the mid-IR

CRyA Self-consistent mass-loss in SPS models Rosa A. González-Lópezlira Mass Loss Return from Stars to Galaxies, STScI, 30 March 2012 There is A LOT to do… Thanks!