(Abundances), Atmospheric Structure, and the Mass Loss ... · AGB – major mass loss phase for low...

25
(Abundances), Atmospheric Structure, and the Mass Loss Process in Miras Ken Hinkle (NOAO) Thomas Lebzelter (Vienna) Oscar Straniero (INAF)

Transcript of (Abundances), Atmospheric Structure, and the Mass Loss ... · AGB – major mass loss phase for low...

Page 1: (Abundances), Atmospheric Structure, and the Mass Loss ... · AGB – major mass loss phase for low mass stars AGB mass loss rates ~10-6 M! yr-1. White dwarf iniPal mass to final

(Abundances),AtmosphericStructure,andtheMassLossProcessinMiras

KenHinkle(NOAO)ThomasLebzelter(Vienna)

OscarStraniero(INAF)

Page 2: (Abundances), Atmospheric Structure, and the Mass Loss ... · AGB – major mass loss phase for low mass stars AGB mass loss rates ~10-6 M! yr-1. White dwarf iniPal mass to final

AGB–majormasslossphaseforlowmassstars

AGBmasslossrates~10-6M! yr-1.

WhitedwarfiniPalmasstofinalmassrelaPon–

byendofMiraphase

>0.5M! lost

Weidemann2000AA363647

Page 3: (Abundances), Atmospheric Structure, and the Mass Loss ... · AGB – major mass loss phase for low mass stars AGB mass loss rates ~10-6 M! yr-1. White dwarf iniPal mass to final

Whatisthemasslossmechanism?

TextbookmodelofMiraextendedatmosphere

Clearoverallpicturebutmanydetailsremainunkown

Gail&Sedlmayr2014,’PhysicsandChemistyofCircumstellarDustShells,(CambridgeUniv.Press),Chapter16.

Page 4: (Abundances), Atmospheric Structure, and the Mass Loss ... · AGB – major mass loss phase for low mass stars AGB mass loss rates ~10-6 M! yr-1. White dwarf iniPal mass to final

ExpandingCircumstellarShell

Page 5: (Abundances), Atmospheric Structure, and the Mass Loss ... · AGB – major mass loss phase for low mass stars AGB mass loss rates ~10-6 M! yr-1. White dwarf iniPal mass to final

StellarPulsaDon

Page 6: (Abundances), Atmospheric Structure, and the Mass Loss ... · AGB – major mass loss phase for low mass stars AGB mass loss rates ~10-6 M! yr-1. White dwarf iniPal mass to final

Photospheric–CircumstellarconnecDon

Page 7: (Abundances), Atmospheric Structure, and the Mass Loss ... · AGB – major mass loss phase for low mass stars AGB mass loss rates ~10-6 M! yr-1. White dwarf iniPal mass to final

Howdoweexploretheinner-circumstellar/extendedphotosphericregion?

•  Masers–Images,especiallySiO

•  Interferometry–near-IR/radiosizesandimages•  IRSpectroscopy

Page 8: (Abundances), Atmospheric Structure, and the Mass Loss ... · AGB – major mass loss phase for low mass stars AGB mass loss rates ~10-6 M! yr-1. White dwarf iniPal mass to final

LowexcitaDon2-0COlinesandH2OlinesinMirasareasymmetric

Tsujinamedtheregionprobedbytheselinesthe“MOLsphere”(ApJ540L99)

Tsuji’sworklimitedtonon-variablestars

Hinkle1978,ApJ,220,210

Page 9: (Abundances), Atmospheric Structure, and the Mass Loss ... · AGB – major mass loss phase for low mass stars AGB mass loss rates ~10-6 M! yr-1. White dwarf iniPal mass to final

AlongDmeseriesofInfraredobservaDonsoftheS-typeMiraχCygsuggestedaquasi-staDonaryMOLsphere

Filledsymbols=photosphere,opensymbols=MOLsphere

Hinkleetal.1982,ApJ,252,697

Hinkleetal1982

Page 10: (Abundances), Atmospheric Structure, and the Mass Loss ... · AGB – major mass loss phase for low mass stars AGB mass loss rates ~10-6 M! yr-1. White dwarf iniPal mass to final

StellarpulsaDonmodels

StaPonaryMOLsphereisatmanyR*

Nowotny,Höfner,&Aringer2010,AA,514A35

Page 11: (Abundances), Atmospheric Structure, and the Mass Loss ... · AGB – major mass loss phase for low mass stars AGB mass loss rates ~10-6 M! yr-1. White dwarf iniPal mass to final

3yearvelocityDmeseriesfortheMiraRCas

MovingMOLspherePeriod≠pulsaPonperiod

OpPcalperiod=430days,

solidsymbol=photosphere

opensymbol=MOLsphere

Page 12: (Abundances), Atmospheric Structure, and the Mass Loss ... · AGB – major mass loss phase for low mass stars AGB mass loss rates ~10-6 M! yr-1. White dwarf iniPal mass to final

RadiuschangesduetopulsaDon

HighexcitaPonlines–periodicvelocitychanges,1R*

LowexcitaPonlines–aperiodic,>2R*

Nowotny,Höfner,&Aringer2010,AA,514A35

Page 13: (Abundances), Atmospheric Structure, and the Mass Loss ... · AGB – major mass loss phase for low mass stars AGB mass loss rates ~10-6 M! yr-1. White dwarf iniPal mass to final

LowexcitaDonlineprofilechangewithDme

Linesusuallyblendedbutoccasionallyseparated—allowsmeasurementofMOLspherelines

Page 14: (Abundances), Atmospheric Structure, and the Mass Loss ... · AGB – major mass loss phase for low mass stars AGB mass loss rates ~10-6 M! yr-1. White dwarf iniPal mass to final

CurveofGrowthAnalysis

-15 -14 -13 -12-5

-4.8

-4.6

-4.4

-4.2

-4

R Cas 84 Jun 12EmpiricaldeterminaPonoftemperature

+=planeparallelmodel

Page 15: (Abundances), Atmospheric Structure, and the Mass Loss ... · AGB – major mass loss phase for low mass stars AGB mass loss rates ~10-6 M! yr-1. White dwarf iniPal mass to final

1000Kgas=2–3R*

Models–GastemperatureanddustcondensaDonvsradius

"COobservedwouldbeatabout2R*

"DustcondensaPonatabout3R*

(Nowotnyetal.2010,Reid&Menten1997,ApJ,476327)

Interferometry-radiusofthecoolmolecularlayer"2.2R*

FLOUR/IOTA2.2μmobservaPons

(Perrinetal.2004AA426279)

Page 16: (Abundances), Atmospheric Structure, and the Mass Loss ... · AGB – major mass loss phase for low mass stars AGB mass loss rates ~10-6 M! yr-1. White dwarf iniPal mass to final

Massoftheshell

•  Curveofgrowthwellfitbyplane-parallelmodel–suggeststhinlayer

•  Assuming:–  Rshell=2Rmira– Rmira=400R!

– Sphericalsymmetry– Solarabundances

•  Mshell=3x10-5M!

Page 17: (Abundances), Atmospheric Structure, and the Mass Loss ... · AGB – major mass loss phase for low mass stars AGB mass loss rates ~10-6 M! yr-1. White dwarf iniPal mass to final

Modelsprovidedensity

Nowotnyetal.(2010)

Assumingρ=10-13gcm-2at2R*,logNL(CO)=21.3resultsinashell>1000R!thick.

ThethinnershellsuggestedbytheobservaDonsrequiresdensity10–100xlower.

Page 18: (Abundances), Atmospheric Structure, and the Mass Loss ... · AGB – major mass loss phase for low mass stars AGB mass loss rates ~10-6 M! yr-1. White dwarf iniPal mass to final

H2Olinespresent

SimilarvelocitychangestoCObutnotidenPcal

Probesvelocitystructure

1000K–gasconsistslargelyofCOandH2O--abundances

Page 19: (Abundances), Atmospheric Structure, and the Mass Loss ... · AGB – major mass loss phase for low mass stars AGB mass loss rates ~10-6 M! yr-1. White dwarf iniPal mass to final

MiraMOLsphere

•  Temperature~1000-1400K•  Density~10-15g/cm3

•  Modelssuggestradius2-4R*,atmosphereextendedbystellarpulsaPon

•  DustcondensaPonzone•  Interferometrysuggestsradius2R*•  MOLspheremass~10-5M•  Timevariable–episodicmassloss

Page 20: (Abundances), Atmospheric Structure, and the Mass Loss ... · AGB – major mass loss phase for low mass stars AGB mass loss rates ~10-6 M! yr-1. White dwarf iniPal mass to final

RichphotosphericspectrumintheIR

Isotopiclines:12CO13CO

C16OC17O

C18O

Page 21: (Abundances), Atmospheric Structure, and the Mass Loss ... · AGB – major mass loss phase for low mass stars AGB mass loss rates ~10-6 M! yr-1. White dwarf iniPal mass to final

SurfaceisotopicraDosalteredbydredge-ups

2ndand3rddredge-upsdependonmass

ϭƐƚĚƵƉ

Z'�������ĞdžƚƌĂͲŵŝdžŝŶŐ

ϮŶĚĚƵƉ

ϯƌĚ���ĚƵƉ

,��

ϭϮ�ͬϭϯ�

ϭϲKͬϭϳK

ϭϲKͬϭϴK

1stdredge-uponRGB.CNOcyclematerialmixedtosurfaceresultsinlargechangesinisotopicraPos.2nddredge-uptakesplaceforstarsofmass>4M☉duringtheearlyAGB.

3rddredge-upduringlateAGB.ProductsofHeburningmixedtosurface.

• Moremixingforstarsundergoingstrongthermalpulses.

• Lowmassstarsdonotexperiencestrongthermalpulses.

• ThermalpulsesarealsoweakerinthemostmassiveAGBstars

• HotBosomburningoccursformassiveAGBstars

Stranieroetal.2006NuclearPhysicsA,777,311

Page 22: (Abundances), Atmospheric Structure, and the Mass Loss ... · AGB – major mass loss phase for low mass stars AGB mass loss rates ~10-6 M! yr-1. White dwarf iniPal mass to final

12C/13Cand16O/17OdependoniniDalmass

ModelpredicPonsforsolarcomposiPonareintoppanel

Measuredparametersareinbosompanel.NotesymbolsfordifferentclassesofAGBstars.

Mstarswithlarge16O/17Ohavenotexperienced3rddredge-upandhavemassesbelow1.5M!.

ThesamplewaslimitedtobrightMirasmostlypickedrandomlyfromthefieldsoisdominatedbyoxygenrich(M-type)Miras.

Page 23: (Abundances), Atmospheric Structure, and the Mass Loss ... · AGB – major mass loss phase for low mass stars AGB mass loss rates ~10-6 M! yr-1. White dwarf iniPal mass to final

Presolarsiliconcarbidedustgrain-AGBstarmaterialinthelab

• Grainsareisolatedfrommatrixmaterialofmeteorites.• Near-alloxygenrichgrainsoriginateinAGBstarwinds.• Abundancescanbederivedfromthegrains.• TimeCapsule

Image:GailandSedlmayer,PhysicsandChemistryofCircumstellarDustShells2013

Page 24: (Abundances), Atmospheric Structure, and the Mass Loss ... · AGB – major mass loss phase for low mass stars AGB mass loss rates ~10-6 M! yr-1. White dwarf iniPal mass to final

Miraandgrainisotopicabundances

1E-5 1E-4 1E-3 0.011E-4

1E-3

0.01

17O/16O

18O/16O

Filledcircles=Miras

Opensquares=grains

Shivtorightresultsfromincreasing17Oand18OabundancesduetogalacPcchemicalevoluPon(GCE)overthelast4Gyr.

AGBstarabundancesarepredictedtopopulatethecentraldenseregion.

ThelargespreadintheMiravaluesinthe18O/16OaxisresultsfromdifficulPesinmeasuringthe18OandinanincreasingspreadofiniPal18OabundancesduetoGCE.

Page 25: (Abundances), Atmospheric Structure, and the Mass Loss ... · AGB – major mass loss phase for low mass stars AGB mass loss rates ~10-6 M! yr-1. White dwarf iniPal mass to final

Atmospheres, pulsation, and mass-loss of AGB stars and supergiants

Atmospheres, pulsation, and mass-loss of AGB stars and supergiants

Isoconversionalanalysisforthe prediction of mass-loss ...930440/FULLTEXT01.pdf · Isoconversionalanalysisforthe prediction of mass-loss rates during pyrolysis of biomass Lina Norberg

Isoconversionalanalysisforthe prediction of mass-loss ...930440/FULLTEXT01.pdf · Isoconversionalanalysisforthe prediction of mass-loss rates during pyrolysis of biomass Lina Norberg

Mass Loss from Red Giant Branch (and AGB) Stars in Globular Clusters Andrea Dupree Harvard-Smithsonian Center for Astrophysics AGB Workshop: 20 May 2010.

Mass Loss from Red Giant Branch (and AGB) Stars in Globular Clusters Andrea Dupree Harvard-Smithsonian Center for Astrophysics AGB Workshop: 20 May 2010.

Radio and Far Infrared Observations of AGB Mass Loss

Radio and Far Infrared Observations of AGB Mass Loss

Full Stokes (IQUV) spectropolarimetry of AGB and post AGB ...

Full Stokes (IQUV) spectropolarimetry of AGB and post AGB ...

Lecture 8 Semiconvection, Mass Loss, and Rotation

Lecture 8 Semiconvection, Mass Loss, and Rotation

Mass Loss from Galactic Bulge AGB stars€¦ · Solar neigh. Schulteis et al. 2003 . Mass Loss rate from IR Schulteis et al. 2003 . SMA project: • Use SMA to spatially filter the

Mass Loss from Galactic Bulge AGB stars€¦ · Solar neigh. Schulteis et al. 2003 . Mass Loss rate from IR Schulteis et al. 2003 . SMA project: • Use SMA to spatially filter the

WOOD THERMODEGRADATION: EXPERIMENTAL ANALYSIS AND … · 2005). The resulting anhydrous mass loss (ML) is representative for physical and chemical wood transformations. Mass loss

WOOD THERMODEGRADATION: EXPERIMENTAL ANALYSIS AND … · 2005). The resulting anhydrous mass loss (ML) is representative for physical and chemical wood transformations. Mass loss

MESS - Mass loss of Evolved StarS Initial Resultshomepage.oma.be/marting/ESAC_Dec09_MESS.pdf · MESS - Mass loss of Evolved StarS Initial Results Martin Groenewegen marting@oma.be

MESS - Mass loss of Evolved StarS Initial Resultshomepage.oma.be/marting/ESAC_Dec09_MESS.pdf · MESS - Mass loss of Evolved StarS Initial Results Martin Groenewegen [email protected]

SAGE AGB & post-AGB

SAGE AGB & post-AGB

ECO Oxygen Technologies › wp-content › uploads › TRA-To...250 150 100 AGB-lnfluent AGB- Beganntng of Box Tank AGB- ank AGB-1st Cascade AGB-2nd Cascade PC-lnfluent Channel Location

ECO Oxygen Technologies › wp-content › uploads › TRA-To...250 150 100 AGB-lnfluent AGB- Beganntng of Box Tank AGB- ank AGB-1st Cascade AGB-2nd Cascade PC-lnfluent Channel Location

Puntuación de condición muscular - WSAVA...Norma muscle mass Mode muscle loss Mild muscle loss muscle loss 2014 Normal muscle mass Moderate muscle loss Mild muscle loss muscle loss

Puntuación de condición muscular - WSAVA...Norma muscle mass Mode muscle loss Mild muscle loss muscle loss 2014 Normal muscle mass Moderate muscle loss Mild muscle loss muscle loss

Feeding Assistant Training Session #2€¦ · skin, dry skin, hair loss 4. Weight loss 5. Muscle mass loss 6. Fat mass loss 7. Fluid accumulation/edema. Signs of Dehydration 1. Dry

Feeding Assistant Training Session #2€¦ · skin, dry skin, hair loss 4. Weight loss 5. Muscle mass loss 6. Fat mass loss 7. Fluid accumulation/edema. Signs of Dehydration 1. Dry

©L. A. Willson 5/2004 Mass Loss at the Tip of the AGB L. A. Willson Iowa State University.

©L. A. Willson 5/2004 Mass Loss at the Tip of the AGB L. A. Willson Iowa State University.

THE FIRST GALAXY FORMATION MODEL WITH THE TP-AGB: BASIC REVISION OF THE MASS-LUMINOSITY RELATION

THE FIRST GALAXY FORMATION MODEL WITH THE TP-AGB: BASIC REVISION OF THE MASS-LUMINOSITY RELATION

Light and heavy elements nucleosynthesis in low mass AGB Stars

Light and heavy elements nucleosynthesis in low mass AGB Stars

Mass Loss in Evolutionary Models of Low and Intermediate Mass Stars

Mass Loss in Evolutionary Models of Low and Intermediate Mass Stars

Angular Momentum and Mass Loss for Hot Stars

Angular Momentum and Mass Loss for Hot Stars

THE AGB NEWSLETTER - Keele Universitydwarves, bipolar planetary nebulae, water fountains, silicates, mass loss, elemental abundances, atomic data, radiative transfer, stellar interiors

THE AGB NEWSLETTER - Keele Universitydwarves, bipolar planetary nebulae, water fountains, silicates, mass loss, elemental abundances, atomic data, radiative transfer, stellar interiors

Measuring stellar mass loss in di erent environments

Measuring stellar mass loss in di erent environments