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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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Crya

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


Crya

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


Crya

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


Crya

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 loss does not happen smoothly

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)


Crya

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


Crya

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


Crya

Self-consistentmass-loss in SPS modelsRosa A. González-Lópezlira

Mass LossReturnfromStarstoGalaxies, STScI, 30 March 2012

CRyA

A very interactive procedure


Crya

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


Crya

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)


Crya

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


Crya

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


Crya

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


Crya

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


Crya

Self-consistentmass-loss in SPS modelsRosa A. González-Lópezlira

Mass LossReturnfromStarstoGalaxies, STScI, 30 March 2012

CRyA

Data: SAGE

(Srinivasan,

Meixner et al.)


Crya

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


Crya

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


Crya

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


Crya

Self-consistentmass-loss in SPS modelsRosa A. González-Lópezlira

Mass LossReturnfromStarstoGalaxies, STScI, 30 March 2012

CRyA

There is A LOT to do…

Thanks!


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