The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the...

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Nicolas Grevesse Centre Spatial de Liège and Institut d‘Astrophysique et de Géophysique, Université de Liège, Belgium The chemical composition The chemical composition of the Sun of the Sun Géophysique, Université de Liège, Belgium Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany Jacques Sauval Observatoire Royal de Belgique, Bruxelles, Belgium

Transcript of The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the...

Page 1: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

Nicolas GrevesseCentre Spatial de Liège and Institut d‘Astrophysiqu e et de

Géophysique, Université de Liège, Belgium

The chemical composition The chemical composition of the Sunof the Sun

Géophysique, Université de Liège, Belgium

Martin AsplundMax-Planck-Institut für Astrophysik (MPA)

Garching, Germany

Jacques SauvalObservatoire Royal de Belgique, Bruxelles, Belgium

Page 2: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

Former Solar Abundance TablesFormer Solar Abundance Tables

� Anders and Grevesse 1989

� Grevesse and Noels 1993

Grevesse and Sauval 1998� Grevesse and Sauval 1998

Changes from 1980 to 2000 : mostly Atomic Data

Page 3: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany
Page 4: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

Line formation in solar granulationLine formation in solar granulation[Fe,Si,C,N,O,Na[Fe,Si,C,N,O,Na--Ca,(FeCa,(Fe--Group),…]Group),…]

* 1D models 3D model

* LTE NLTE

* All indicators (atoms + molecules)* Best lines +atomic & molecular data

Abundances

Solar abundances:Martin Asplund (MPA-Garching)Carlos Allende Prieto (MSSL-UK)Nicolas Grevesse (Liège)David Lambert (Austin)Jacques Sauval (Brussels)Patrick Scott (Stockholm)

3D stellar modelling:Mats Carlsson (Oslo) Remo Collet (Uppsala)Åke Nordlund (Copenhagen)Bob Stein (Michigan State)Regner Trampedach (ANU)

Page 5: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

New Results

M. Asplund, N. Grevesse, A.J. Sauval, in Cosmic abundancesas records of stellar evolution and nucleosynthesis, Eds T.G.BarnesIII & F.N. Bash, ASP Conf. Ser. 336, 2005, p.25-38(65th birthday D.L. Lambert)

N. Grevesse, M. Asplund, A.J. Sauval, in Elements stratification in stars, 40 years of atomic diffusion, Eds G. Alecian, O. Richard

N. Grevesse, M. Asplund, A.J. Sauval, in Elements stratification in stars, 40 years of atomic diffusion, Eds G. Alecian, O. Richard& S. Vauclair, EAS Pub. Ser. 17, 2005, p.21-32(65th birthday G. Michaud)

N. Grevesse, M. Asplund, A.J. Sauval, in Space Science Reviews, 130, 105-114, 2007(80th birthday J. Geiss)

Page 6: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

3D solar atmosphere models3D solar atmosphere modelsIngredients:

• Radiative-hydrodynamical• Time-dependent• 3-dimensional• Simplified radiative transfer• LTE

Essentially parameter freeEssentially parameter free

Page 7: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

3D successes !

• Topology and convective motions• …

For the first time, line profilesFor the first time, line profilesare perfectly reproduced

• But computing time !

Page 8: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

Observations : All line profiles show …

• Widths much larger than thermal widths

MICROTURBULENCEMICROTURBULENCE

• λλλλcenter blueshifted (2 mA ���� 100 m/s at 600 nm)

• Asymmetries (C shapes : ~ 300 m/s i.e. 6 mA)

Page 9: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

Averaged line profilesAveraged line profiles

1D vs Sun

3D vs Sun

No micro- and macroturbulence needed in 3D!

Shift!

Page 10: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

Line asymmetriesLine asymmetriesThe asymmetries and shifts of spectral

lines are very well reproduced

Observations3D model3D model

Page 11: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

Balance 1DBalance 1D--3D3DVarious ways to test modelsQ : Does the model reproduce …

Test 1D 3D

• Ic=F(λλλλ) ~Yes ~• Ic=F(λλλλ) ~Yes ~• C/L var. ~Yes ~• Granulation No Yes• Widths of lines Yes Yes• Shifts of lines No Yes• Asymmetries No Yes• ≠≠≠≠ indicators No Yes• Dependence I,EEx No Yes• High freq oscillations No Yes

Page 12: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

Oxygen diagnosticsOxygen diagnosticsDiscordant results in 1D: log O~8.6-8.9Excellent agreement in 3D: log O=8.66+/-0.05O isotopic abundances: 16O/18O=480+/-30

LinesHolweger-

Müller3D Difference

[O I] 8.76+/-0.02 8.68+/-0.01 -0.08 [O I] 8.76+/-0.02 8.68+/-0.01 -0.08

O I 8.64+/-0.08 8.64+/-0.02 0.00

OH, dv=0 8.82+/-0.01 8.65+/-0.02 -0.17

OH, dv=1 8.87+/-0.03 8.61+/-0.03 -0.26

OH, dv=2 8.80+/-0.06 8.57+/-0.06 -0.23

*If LTE (O I): log O=8.82+/-0.10 (Δ=-0.18 dex)!!!

Page 13: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

Carbon diagnosticsCarbon diagnosticsDiscordant results in 1D: log C~8.4-8.7Excellent agreement in 3D: log O=8.39+/-0.05C isotopic abundances: 12C/13C=87+/-4

LinesHolweger-

Müller3D Difference

[C I] 8.45 8.39 -0.06[C I] 8.45 8.39 -0.06

C I 8.39+/-0.03 8.36+/-0.03 -0.03

CH, dv=1 8.53+/-0.04 8.38+/-0.04 -0.15

CH, A-X 8.59+/-0.04 8.45+/-0.03 -0.14

C2, Swan 8.53+/-0.03 8.44+/-0.03 -0.09

CO, dv=1 8.60+/-0.01 8.40+/-0.01 -0.20

CO, dv=2 8.69+/-0.02 8.37+/-0.01 -0.32

Page 14: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

Element 1D 3D 3D-1D

Na I 6.27±±±±0.04 6.17±±±±0.04 -0.10

Mg I 7.64±±±±0.23 7.57±±±±0.23 -0.07

Mg II 7.56±±±±0.08 7.53±±±±0.08 -0.03

Al I 6.45±±±±0.06 6.37±±±±0.06 -0.08

Si I 7.55±±±±0.04 7.51±±±±0.04 -0.04

Si II 7.46 7.45 -0.01

Na – Ca and Fe

Si II 7.46 7.45 -0.01

P I 5.37±±±±0.04 5.36±±±±0.04 -0.01

S I 7.17±±±±0.05 7.14±±±±0.05 -0.03

K I 5.20±±±±0.07 5.08±±±±0.07 -0.12

Ca I 6.43±±±±0.04 6.30±±±±0.04 -0.13

Ca II 6.34±±±±0.08 6.32±±±±0.08 -0.02

Fe I 7.50±±±±0.05 7.44±±±±0.05 -0.06

Fe II 7.47±±±±0.10 7.45±±±±0.10 -0.02

Heavier elements : See older tables (but -0.03 dex for Kr and Xe)

Page 15: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

SummarySummary

• 3D : Granulation and line profiles• NLTE• All indicators agree• No dependence on I or E exc

C,N,O

Other elements

Page 16: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

ImplicationsImplications

Page 17: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

ImplicationsImplicationsSignificantly lower solar metallicity Z

– Z=0.0194 (Anders & Grevesse 1989)– Z=0.0122 (Asplund et al. 2005)

Page 18: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

New solar metallicityNew solar metallicityElement Abundance Contribution

to Z (%)

O 8.66 43.7

C 8.39 17.6

Fe 7.45 9.4

Ne 7.84 8.3

Si 7.51 5.4

C+N+O ~ 2/3 Z

Si 7.51 5.4

N 7.80 5.3

Mg 7.55 5.2

S 7.14 2.6

X=0.7393 Y=0.2485 Z=0.0122 Z/X=0.0165

Anders, Grevesse 1989 Z=0.019 Z/X=0.027Grevesse, Noels 1993 Z=0.017 Z/X=0.024Grevesse, Sauval 1998

Page 19: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

Significantly lower solar metallicity Z=0.0122

Makes Sun normal compared with surroundings– Young O,B stars in solar neighborhood– Local interstellar medium/Orion nebula

ImplicationsImplications

Page 20: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

Turck-Chièze et al. (2004)

Page 21: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

Significantly lower solar metallicity Z=0.0122

Makes Sun normal compared with surroundings

FIP

ImplicationsImplications

Page 22: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

FIPFIP

Ar Ne

SWslow SWrapid SEP

Old Abund. 2.7 1.8 3.25

New Abund. 2.0 1.4 2.4

Quiet Cor.

1.25-1.66

0.8-1.1

Page 23: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

Significantly lower solar metallicity Z=0.0122

Makes Sun normal compared with surroundings

FIP

ImplicationsImplications

Solar NEON ! High or Low? LOW!!!

Page 24: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

Significantly lower solar metallicity Z=0.0122

Makes Sun normal compared with surrounding

FIP

ImplicationsImplications

Solar NEON ! High or Low?

Alters cosmic yardstick [X/H], [X/Fe]… WARNING!

Page 25: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

Significantly lower solar metallicity Z=0.0122

Makes Sun normal compared with surroundings

Solar NEON ! High or Low?

ImplicationsImplications

FIP

Alters cosmic yardstick [X/H], [X/Fe], …

Agreement with meteorites !

Page 26: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

Photospheric vs meteoriticPhotospheric vs meteoritic

Very good agreement with C1 carbonaceous chondrites in general

Volatiles

Exceptions: Cl, Ga, Rb, Ag, In, W, Au

Mean difference otherwise: -0.01+/-0.06 dex

Note: change in meteoritic scale by -0.04 dex due to 3D analysis of Si

Solar depletion

Page 27: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

Significantly lower solar metallicity Z=0.0122

Makes Sun normal compared with surroundings

Solar NEON ! High or Low?

ImplicationsImplications

FIP

Alters cosmic yardstick [X/H], [X/Fe], …

Agreement with meteorites !

Diffusion ���� Protosolar abundances ∆∆∆∆ (Proto-Now) = 0.05 dex Z Proto =0.0132 (Z/X)Proto =0.0185

Page 28: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

Significantly lower solar metallicity Z=0.0122Makes Sun normal compared with surroundingsSolar NEON ! High or Low?

FIPAlters cosmic yardstick [X/H], [X/Fe], …Agreement with meteorites !

ImplicationsImplications

Agreement with meteorites !Protosolar abundances ���� Diffusion !

Isotopes(exercise of futility-B.Gutafsson- 65th…)

Page 29: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

13C, 18O, (17O) from IR CO

Sun ≡≡≡≡ Earth

Page 30: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

Significantly lower solar metallicity Z=0.0122Makes Sun normal compared with surroundingsSolar NEON ! High or Low?

FIPAlters cosmic yardstick [X/H], [X/Fe], …Agreement with meteorites !

ImplicationsImplications

Agreement with meteorites !Protosolar abundances ���� Diffusion !Isotopes

(Large) impacts in stellar structure and evolution

… (Giant planets, TTauri, Herbig Ae/Be, Gas/Dust rati o in dense clouds,Beat Cepheids, …)

Page 31: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

Significantly lower solar metallicity Z=0.0122Makes Sun normal compared with surroundingsSolar NEON ! High or Low?

FIPAlters cosmic yardstick [X/H], [X/Fe], …Agreement with meteorites !

ImplicationsImplications

Agreement with meteorites !Protosolar abundances ���� Diffusion !Isotopes

Changes stellar structure and evolution

… (Giant planets, TTauri, Herbig Ae/Be, Gas/Dust rati o in dense clouds, …)

But Problems Standard Models - Helioseismology

Page 32: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

Rcz/R =0.713±0.001

Helioseismology

Rcz/R����=0.713±0.001

Y = 0.248±0.005

Sound speed – Precision 10-4

(He depends on EOS)

Page 33: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

The Paradise ...Rcz/R����

=0.713±0.001

Ys = 0.248±0.005

YYss=0.246=0.246RRczcz/R=0.714/R=0.714

A. Miglio, J. Montalban, A. Noels

Page 34: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

Troubles in Paradise ...

YY =0.243=0.243

Rcz/R����=0.713±0.001

Ys = 0.248±0.005

with new abundances

YYss=0.246=0.246RRczcz/R=0.714/R=0.714

YYss=0.243=0.243RRczcz/R=0.727/R=0.727

YYss=0.246=0.246RRczcz/R=0.714/R=0.714

A. Miglio, J. Montalban, A. Noels

Page 35: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

C

O

cz

Opacity inside the Sun

NeFe

N

Page 36: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

Solutions?Solutions?

Erroneous solar CNO abundances?− Hopefully not (see O here after)

Missing opacity?− Apparently not

J. Bahcall, A. Antia, S. Basu, M. Pinsonneault, J. Guzik, S. Turck-Chièze,S. Vauclair, A. Miglio, J. Montalban, A. Noels, …

− Apparently notUnderestimated element diffusion?

− UnlikelyInternal gravity waves?

− PossiblyUnderestimated solar Ne abundance?

− NO

Page 37: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

�The terrible tragedy of Science is the murder ofbeautiful theories by ugly facts. (W. Fowler?)

*The most interesting topics are the ones where Theory and Observations disagree.

*Thanks to these challenges Progress ismade in both fields*

Page 38: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

*«The*«The mattermatter raisedraised byby AsplundAsplund etet alal..((20042004)) thereforethereforechallengeschallenges eithereither thethe opacityopacity calculations,calculations, thethe nuclearnuclearreactionreaction rates,rates, oror thethe basicbasic physicsphysics ofof stellarstellar evolution,evolution,NOTNOT HELIOSEISMOLOGY,HELIOSEISMOLOGY, asas somesome spectatorsspectators havehave

surmisedsurmised..

FromFrom seismologicalseismological structurestructure inversions,inversions, wewe knowknow thatthatthethe solarsolar modelsmodels areare notnot accurateaccurate bybythethe solarsolar modelsmodels areare notnot accurateaccurate bybyhelioseismologicalhelioseismological standardsstandards.. ThereforeTherefore thethe propertiesproperties(i(i..ee.. forfor exampleexample thethe chemicalchemical composition)composition) inferredinferredfromfrom thesethese calibrationscalibrations couldcould bebe moremore contaminatedcontaminated bybysystematicsystematic errorserrors thanthan byby errorserrors inin thethe observedobservedfrequencies»frequencies»

GG.. HoudekHoudek andand DD..OO.. GoughGough 200720076565thth birthdaybirthday DD.. GoughGough

Page 39: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

HH��������T TT T☺☺☺☺☺☺☺☺PICS PICS ��������

Solar O��������Solar O��������(4 recent papers …)

Solar Neon?

Page 40: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

Solar Ne abundanceSolar Ne abundance

We used Ne/O=0.15 (SEP, SW, Corona at ≠ T)

ANe = 7.84

0.24 dex (1.74x) smaller than older values

Such ‘low’ Ne/O solar values have been confirmed by

• Young (2005) Quiet Sun (EUV, CDS, Soho)

• Schmelz et al. (2005) Active regions (X rays)

Page 41: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

Solar Ne abundanceSolar Ne abundanceNew studies of solar neighborhood suggested that solar Ne is underestimated

B stars

Cunha et al. (2006):Drake & Testa (2005):

New solar

Orion

log O

Ne/

O

X-ray luminosity(see also Liefke and Schmitt (2006))

*The <solar model problem> solved by the abundance of Neon in nearby stars

Page 42: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

Drake & Testa (2005):

Solar Ne abundanceSolar Ne abundanceVery recent studies of solar neighborhood show

that solar Ne is NOT underestimated !

Robrade, Schmitt & Favata (2008)

Ne/

O

X-ray luminosity

(see also Liefke and Schmitt (2006))

Page 43: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

• Landi et al. 2007 High Ne from solar flares … but possible IFIP (Ne: 21.6, O: 13.6eV)

• Bochsler 2007 Ne and O from solar wind by comparing • Bochsler 2007 Ne and O from solar wind by comparing to He

He very variable in SW. Depending on the adopted He, Ne and O can be high or low

Page 44: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

ISM and OB stars: O and NeISM and OB stars: O and NeGood agreement with low solar O abundance

OB stars

Cunha et al. (2006), Esteban et al. (2004)

Asplund et al.Old solarOrion

Neon? Morel

Page 45: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

O I: 3D semiO I: 3D semi--empirical modelempirical modelSocas-Navarro & Norton 2007: Observations of Fe I lines to map T(x,y,z) over surf ace

⇒⇒⇒⇒ 3D semi-empirical model

O I 777nm non-LTE calculations without H collisions :log O ≈ 8.63 ± 0.08 dex

Page 46: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

[O I]: 630nm in Sunspots[O I]: 630nm in Sunspots

Centeno & Socas-Navarro 2008: Ratio atomic O/Ni in small sunspot log O = 8.86 ± 0.07

BUT

•Correction for wrong gf - 0.06 dex•Corr. for Ni abundance - 0.06 dex•Corr. for CO - 0.08 d ex

• log O = 8.66 (very uncertain!!!)

Page 47: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

[O I]: another 3D model[O I]: another 3D modelAyres 2008: New wavelength calibration of solar atlas and one snapshot of a different 3D model (CO5BOLD)

log O = 8.81 ± 0.02log O = 8.81 ± 0.02If Ni I blend treated as free parameter

Ni contribution much too low

If Ni correct, log O = 8.74but less good fit

Page 48: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

O I+[O I]: another 3D analysis(1)O I+[O I]: another 3D analysis(1)Caffau,Ludwig,Steffen,Ayres,Bonifacio,Cayrel,Freyta g,Plez 2008O I lines with CO5BOLD: log O = 8.77 ± 0.05- Choice of H collisions: ∆∆∆∆log O ≈ +0.02 dex- Equivalent widths: ∆∆∆∆log O ≈ +0.09 dex!

777.1nm777.1nm

777.4nm

777.5nm

Page 49: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

O I+[O I]: another 3D analysis(2)O I+[O I]: another 3D analysis(2)

777.1nm

New equivalent widths New abundances

8.70 (Caffau) 8.69 (us)

777.1nm

777.4nm

777.5nmNew

New

New

Page 50: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany

Oxygen: status reportOxygen: status report

LinesHolweger-

MuellerAsplund et al. (2004)

Real Sun?

[O I] 8.76+/-0.02 8.68+/-0.01 ~8.7

No clear consensus what the real solar O abundance isPersonal guess: log O ≈ 8.70-8.72?

O I 8.64+/-0.08 8.64+/-0.02 ~8.7

OH, dv=0 8.82+/-0.01 8.65+/-0.02

~8.7?OH, dv=1 8.87+/-0.03 8.61+/-0.03

OH, dv=2 8.80+/-0.06 8.57+/-0.06

Stay tuned for a complete re-analysis of ALL elements with NEW 3D solar model

Page 51: The chemical composition of the Sunbrogiato/physun/Grevesse.pdf · The chemical composition of the Sun Martin Asplund Max-Planck-Institut für Astrophysik (MPA) Garching, Germany