the chemical composition of the sunbrogiato/physun/grevesse.pdf · the chemical composition of the...
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![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](https://reader030.vdocuments.fr/reader030/viewer/2022041020/5ecf0de640546506d6278a9c/html5/thumbnails/1.jpg)
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
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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
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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)
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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)
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3D solar atmosphere models3D solar atmosphere modelsIngredients:
• Radiative-hydrodynamical• Time-dependent• 3-dimensional• Simplified radiative transfer• LTE
Essentially parameter freeEssentially parameter free
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3D successes !
• Topology and convective motions• …
For the first time, line profilesFor the first time, line profilesare perfectly reproduced
• But computing time !
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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)
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Averaged line profilesAveraged line profiles
1D vs Sun
3D vs Sun
No micro- and macroturbulence needed in 3D!
Shift!
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Line asymmetriesLine asymmetriesThe asymmetries and shifts of spectral
lines are very well reproduced
Observations3D model3D model
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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
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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)!!!
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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
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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)
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SummarySummary
• 3D : Granulation and line profiles• NLTE• All indicators agree• No dependence on I or E exc
C,N,O
Other elements
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ImplicationsImplications
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ImplicationsImplicationsSignificantly lower solar metallicity Z
– Z=0.0194 (Anders & Grevesse 1989)– Z=0.0122 (Asplund et al. 2005)
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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
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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
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Turck-Chièze et al. (2004)
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Significantly lower solar metallicity Z=0.0122
Makes Sun normal compared with surroundings
FIP
ImplicationsImplications
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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
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Significantly lower solar metallicity Z=0.0122
Makes Sun normal compared with surroundings
FIP
ImplicationsImplications
Solar NEON ! High or Low? LOW!!!
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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!
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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 !
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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
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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
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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…)
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13C, 18O, (17O) from IR CO
Sun ≡≡≡≡ Earth
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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, …)
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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
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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)
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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
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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
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C
O
cz
Opacity inside the Sun
NeFe
N
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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
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�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*
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*«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
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HH��������T TT T☺☺☺☺☺☺☺☺PICS PICS ��������
Solar O��������Solar O��������(4 recent papers …)
Solar Neon?
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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)
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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
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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))
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• 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
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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
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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
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[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!!!)
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[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
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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
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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
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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
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