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Mass Loss Return from Stars to Galaxies , STScI , 30 March 2012. CRyA. dust. Self-consistent mass-loss . in stellar population synthesis models. Rosa A. González - Lópezlira. CRyA, UNAM/AIfA, Bonn. Gonzalez- Lopezlira et al. 2010, MNRAS, 403, 1213.
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Mass LossReturnfromStarstoGalaxies, STScI, 30 March 2012 CRyA dust Self-consistent mass-loss in stellar population synthesis models Rosa A. González-Lópezlira CRyA, UNAM/AIfA, Bonn Gonzalez-Lopezlira et al. 2010, MNRAS, 403, 1213
Self-consistentmass-loss in SPS modelsRosa A. González-Lópezlira Mass LossReturnfromStarstoGalaxies, STScI, 30 March 2012 CRyA Collaborators Gustavo Bruzual CIDA, Mérida, Venezuela StéphaneCharlot IAP, Paris, France Laurent LoinardCRyA, UNAM, Morelia, Mexico Javier Ballesteros-P. CRyA, UNAM, Morelia, Mexico
Self-consistentmass-loss in SPS modelsRosa A. González-Lópezlira Mass LossReturnfromStarstoGalaxies, STScI, 30 March 2012 CRyA Stellar mass-loss • Driveschemicalenrichmentandevolutionofgalaxies • Replenishes molecular gas destroyed by energeticphotons • Shapesthe AGB and PN luminosityfunctions • Determines WD massspectrumandcooling times • SNe Ia progenitor mass and frequency • SNe II, Ib, Ic rate
Self-consistentmass-loss in SPS modelsRosa A. González-Lópezlira Mass LossReturnfromStarstoGalaxies, STScI, 30 March 2012 CRyA 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/LSun . http://www.public.iastate.edu/~lwillson/UppsalaTalkOne.pdf, fromBoothroyd, Sackmann & Kramer 1993
Mass-lossdoesnothappensmoothly Self-consistentmass-loss in SPS modelsRosa A. González-Lópezlira Mass LossReturnfromStarstoGalaxies, STScI, 30 March 2012 CRyA (Reimers 1975) Bowen & Willson (1991), in Willson (2000)
Self-consistentmass-loss in SPS modelsRosa A. González-Lópezlira Mass LossReturnfromStarstoGalaxies, STScI, 30 March 2012 CRyA Challenges for SSP models . • Required to include M and dusty envelopes in contribution • from TP-AGB for all evolutionary stages and all Z Hard constraints only for Galactic and MagellanicZ, (recently, also for low metallicities; Girardi et al. 2010, ANGST) Needananalyticapproach: no empiricaldustyspectraforallZandphases
Self-consistentmass-loss in SPS modelsRosa A. González-Lópezlira Mass LossReturnfromStarstoGalaxies, STScI, 30 March 2012 CRyA Analyticapproach Pioneered by Bressan et al. 1998, Lançon & Mouhcine 2002; Piovan et al. 2003 . • M,L,T(startype, age, Z)M + dust mixture t • t + input SED + radiative transfer output SED
Self-consistentmass-loss in SPS modelsRosa A. González-Lópezlira Mass LossReturnfromStarstoGalaxies, STScI, 30 March 2012 CRyA A very interactive procedure
Self-consistentmass-loss in SPS modelsRosa A. González-Lópezlira Mass LossReturnfromStarstoGalaxies, STScI, 30 March 2012 CRyA Carbonstars Mixtures: Suh (1999,2000,2002) t10 £ 0.15: 80% AMC, 20% SiC 0.15 < t10 £ 0.8: 90% AMC, 10% SiC t10 > 0.8: 100% AMC C. Kemper’s talk O-richstars t10 £ 3: 90% warm AMS, 5% ens, 5% forst 3 < t10 £ 15: 90% cold AMS, 5% enst, 5% forst t10> 15: 80% cold AMS, 10% ens, 10% forst
Self-consistentmass-loss in SPS modelsRosa A. González-Lópezlira Mass LossReturnfromStarstoGalaxies, STScI, 30 March 2012 CRyA FollowingPiovan et al. 2003 Carbonstars (C/O ≥ 0.97) O-richstars (C/O < 0.97)
Self-consistentmass-loss in SPS modelsRosa A. González-Lópezlira Mass LossReturnfromStarstoGalaxies, STScI, 30 March 2012 CRyA AandBdependon: dust condensationT, dustefficiency coefficientsforradiationpressure andabsorption, anddust cross sectionper gas particlesgas AfterMarigo et al. 2008 and Ferrarotti & Gail 2006 Xseed : massfractionofseedelement in circumstellarshell (take solar andscale by Z) Aseed : seedelementatomicweight Adust : dustspecies molecular weight fdust,i: fractionofseedelementcondensedintograins ofeachdustspecies
Self-consistentmass-loss in SPS modelsRosa A. González-Lópezlira Mass LossReturnfromStarstoGalaxies, STScI, 30 March 2012 CRyA Carbonstars O-richstars YC = XC/AC fSiCfollows YC,1 = XO/AO– 2XSi/ASi
Self-consistentmass-loss in SPS modelsRosa A. González-Lópezlira Mass LossReturnfromStarstoGalaxies, STScI, 30 March 2012 CRyA Piovan et al. (2003) ci: massabundanceofdustspecies a: dustsize = 0.1m mdust,i: grainmass Qext(i): extinctioncoefficientsofspecies
Self-consistentmass-loss in SPS modelsRosa A. González-Lópezlira Mass LossReturnfromStarstoGalaxies, STScI, 30 March 2012 CRyA t: Radiative transfer with 1-D code DUSTY (Ivezic, Nenkova & Elitzur 1999 ) . . C star, Z=0.008, M=4.2e-6Msunyr-1, t=1.1 O-richstar, Z=0.008, M=4.9e-6Msunyr-1, t=0.21 Input SED: Lançon Input SED: Aringer
Self-consistentmass-loss in SPS modelsRosa A. González-Lópezlira Mass LossReturnfromStarstoGalaxies, STScI, 30 March 2012 CRyA Data: SAGE (Srinivasan, Meixner et al.)
Self-consistentmass-loss in SPS modelsRosa A. González-Lópezlira Mass LossReturnfromStarstoGalaxies, STScI, 30 March 2012 CRyA Whatifyouwanttotweakyoumassloss? E. Villaver’stalk Marigo & Girardi 2007, based on Bowen & Willson 1991
Self-consistentmass-loss in SPS modelsRosa A. González-Lópezlira Mass LossReturnfromStarstoGalaxies, STScI, 30 March 2012 CRyA e.g., Marigo & Girardi 2007 . DM DL DR DT, P, C/O,vexp Dust mixtures … SEDs Radiativetransfer e.g., Fuel Consumption Theorem (Renzini & Buzzoni 1986) tAGBn*,Mc
Self-consistentmass-loss in SPS modelsRosa A. González-Lópezlira Mass LossReturnfromStarstoGalaxies, STScI, 30 March 2012 CRyA Calibration/exploration: SBF in themid-IR Data: SAGE-LMC
Self-consistentmass-loss in SPS modelsRosa A. González-Lópezlira Mass LossReturnfromStarstoGalaxies, STScI, 30 March 2012 CRyA There is A LOT to do… Thanks!
