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/LSun

http://www.public.iastate.edu/~lwillson/UppsalaTalkOne.pdf,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

dNRuido

Señal * dN

Noise

Signal *

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 t

t + input SED + radiative transfer output SED

Analytic approach

Pioneered by Bressan et al. 1998, Lançon & Mouhcine 2002; 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

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

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

t10 £ 0.15: 80% AMC, 20% SiC0.15 < t10 £ 0.8: 90% AMC, 10% SiC

t10 > 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

Xseed : mass fraction of seed element in circumstellar shell (take solar and scale by Z)Aseed : seed element atomic weightAdust : 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 pressureand absorption, and dust cross section per gas particle sgas

After Marigo et al. 2008 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

fSiC follows YC = XC/AC

YC,1 = XO/AO – 2XSi/ASi

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)

ci: mass abundance of dust speciesa: dust size = 0.1mmdust,i: grain massQext(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

t: Radiative transfer with 1-D code DUSTY (Ivezic, Nenkova & Elitzur 1999 )

C star, Z=0.008, M=4.2e-6Msun yr-1, t=1.1 O-rich star, Z=0.008, M=4.9e-6Msunyr-1, t=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

dNRuido

Señal * dN

Noise

Signal *

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

dNRuido

Señal * dN

Noise

Signal *

Radiative transfer

Dust mixtures

e.g., Fuel ConsumptionTheorem (Renzini & Buzzoni 1986)

DM DL DR DT, P, C/O,vexp

SEDs

tAGB n*,Mc

…

. 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!