Robert Izzard Université Libre de Bruxelles
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1 Binary Star Populations: Keys to Understanding Stellar Astrophysics Robert Izzard Université Libre de Bruxelles with Onno Pols, Evert Glebbeek and Richard Stancliffe
2 A Short Journey... Your Night Sky: Why Binaries? My Biased View of (Binary) Stellar Evolution Chemically Peculiar Stars: CEMPs Did Asymptotic Giant stars make the CEMPs? Population study Pin down Key Physics Time for a demo?
3 Night Sky Declination (Latitude) Yale Bright Star Catalogue, Stars Brighter than 5th Mag Right Ascension (Longitude)
4 Night Sky Binaries Declination (Latitude) Yale Bright Star Catalogue, Stars Brighter than 5th Mag Right Ascension (Longitude)
5 Night Sky Binaries Declination (Latitude) Yale Bright Star Catalogue, Stars Brighter than 5th Mag Algol Capella Castor Regulus Procyon Rigel Sirius Mizar Arcturus Antares Right Ascension (Longitude)
6 Night Sky in Brussels! Declination (Latitude) Yale Bright Star Catalogue, Stars Brighter than 5th Mag Algol Capella Castor Regulus Procyon Rigel Sirius Mizar Arcturus Antares Right Ascension (Longitude)
7 Useful numbers Stars brighter than 5th magnitude in Yale catalogue 1618 star systems 793 binary systems Binary Fraction = = 49% 51 single stars : 98 stars in binaries Most stars are in binaries!
8 Why Binaries? (1) Accurate stellar masses, radii, luminosities Gamma-ray bursts: long and short, oldest known events! (redshift 8) Type Ia supernovae: Standard candles (?) Tell us Universe is expanding? Galactic Evolution: SN Ia, novae Stellar mergers X-ray binaries Chemically peculiar stars (my favourites!): probe early Galactic evolution Vital to understanding galaxies, stellar clusters, star formation, cosmology...
9 Why Binaries? (1) Accurate stellar masses, radii, luminosities Gamma-ray bursts: long and short, oldest known events! (redshift 8) Type Ia supernovae: Standard candles (?) Tell us Universe is expanding? Galactic Evolution: SN Ia, novae Stellar mergers X-ray binaries Chemically peculiar stars (my favourites!): probe early Galactic evolution Vital to understanding galaxies, stellar clusters, star formation, cosmology...
10 Why Binaries? (1) Accurate stellar masses, radii, luminosities Gamma-ray bursts: long and short, oldest known events! (redshift 8) Type Ia supernovae: Standard candles (?) Tell us Universe is expanding? Galactic Evolution: SN Ia, novae Stellar mergers X-ray binaries Chemically peculiar stars (my favourites!): probe early Galactic evolution Vital to understanding galaxies, stellar clusters, star formation, cosmology...
11 Why Binaries? (1) Accurate stellar masses, radii, luminosities Gamma-ray bursts: long and short, oldest known events! (redshift 8) Type Ia supernovae: Standard candles (?) Tell us Universe is expanding? Galactic Evolution: SN Ia, novae Stellar mergers X-ray binaries Chemically peculiar stars (my favourites!): probe early Galactic evolution Vital to understanding galaxies, stellar clusters, star formation, cosmology...
12 Why Binaries? (1) Accurate stellar masses, radii, luminosities Gamma-ray bursts: long and short, oldest known events! (redshift 8) Type Ia supernovae: Standard candles (?) Tell us Universe is expanding? Galactic Evolution: SN Ia, novae Stellar mergers X-ray binaries Chemically peculiar stars (my favourites!): probe early Galactic evolution Vital to understanding galaxies, stellar clusters, star formation, cosmology...
13 Why Binaries? (1) Accurate stellar masses, radii, luminosities Gamma-ray bursts: long and short, oldest known events! (redshift 8) Type Ia supernovae: Standard candles (?) Tell us Universe is expanding? Galactic Evolution: SN Ia, novae Stellar mergers X-ray binaries Chemically peculiar stars (my favourites!): probe early Galactic evolution Vital to understanding galaxies, stellar clusters, star formation, cosmology...
14 Why Binaries? (1) Accurate stellar masses, radii, luminosities Gamma-ray bursts: long and short, oldest known events! (redshift 8) Type Ia supernovae: Standard candles (?) Tell us Universe is expanding? Galactic Evolution: SN Ia, novae Stellar mergers X-ray binaries Chemically peculiar stars (my favourites!): probe early Galactic evolution Vital to understanding galaxies, stellar clusters, star formation, cosmology...
15 Why Binaries? (2) International Astronomical Union Symposium: Binary Stars as Critical Tools and Tests in Contemporary Astrophysics To understand galaxies we need to understand stars, but since most are members of binary and multiple star systems, we need to study and understand binary stars. I would add: Sometimes binary stars are the only way to understand single stars...
16 Why are binaries so different? 1. Single star evolution 2. Binary star evolution A biased view of the evolution of low/intermediate mass stars
17 Single Star Evolution Time/Gyr
18 Single Star Evolution Time/Gyr
19 Single Star Evolution Time/Gyr
20 Single Star Evolution Time/Gyr
21 Single Star Evolution Time/Gyr
22 Binary Star Evolution Time/Gyr
23 Binary Star Evolution Time/Gyr
24 Binary Star Evolution Time/Gyr
25 Binary Star Evolution Time/Gyr
26 What happens next? Two cases: Close binary: Roche-lobe overflow Distant binary: Wind accretion
27 Close binary: Roche-lobe Overflow Roche Lobe overflow
28 Common Envelope (Fast)
29 No chemical peculiarities White Dwarf + Chemically Normal Star
30 Distant Binary: Wind Accretion
31 Wind Accretion: Giant Wind
32 Wind Accretion: Gravitational Focusing
33 Wind Accretion: Accretion
34 Wind Accretion 6: Primary Death White Dwarf + Chemically Peculiar Star
35 Do we see chemically peculiar stars? YES! A family of them: Ba stars CH stars Carbon enhanced metal-poor stars
36 Carbon-Enhanced Metal-Poor Stars CEMPs Metal-poor Galactic halo: oldest stars [Fe/H] 2 Binary fraction consistent with all binaries About 1000 CEMPs known Statistically significant number! about 20% of all metal-poor stars! Not evolved enough to make their own carbon Must come from a companion star! Fashionable... but well-observed because of this [A/B] = log(a/a ) log(b/b )
37 Carbon-Enhanced Metal-Poor Stars CEMPs Metal-poor Galactic halo: oldest stars [Fe/H] 2 Binary fraction consistent with all binaries About 1000 CEMPs known Statistically significant number! about 20% of all metal-poor stars! Not evolved enough to make their own carbon Must come from a companion star! Fashionable... but well-observed because of this [A/B] = log(a/a ) log(b/b )
38 Carbon-Enhanced Metal-Poor Stars CEMPs Metal-poor Galactic halo: oldest stars [Fe/H] 2 Binary fraction consistent with all binaries About 1000 CEMPs known Statistically significant number! about 20% of all metal-poor stars! Not evolved enough to make their own carbon Must come from a companion star! Fashionable... but well-observed because of this [A/B] = log(a/a ) log(b/b )
39 CEMP: Carbon-Enhanced Metal Poor Carbon [C/Fe] / 1000 / Metallicity [Fe/H] 1000 stars from the SAGA database (Suda 2008) Normal Stars [C/Fe]=0
40 CEMP: Carbon-Enhanced Metal Poor Carbon [C/Fe] CEMP / 1000 / 100 EMP Metallicity [Fe/H] EMP=Extremely Metal Poor
41 CEMP: Carbon-Enhanced Metal Poor Carbon [C/Fe] / 1000 / 100 CEMP 20% EMP 80% Metallicity [Fe/H] EMP=Extremely Metal Poor
42 CEMP: Carbon-Enhanced Metal Poor Carbon [C/Fe] / 1000 / 100 CEMP 20% Binaries EMP 80% Metallicity [Fe/H] EMP=Extremely Metal Poor
43 CEMP: Carbon-Enhanced Metal Poor About 1000 CEMPs known Binary fraction consistent with all binaries Metal-poor Galactic halo: oldest stars 20% of all metal-poor stars but... Where did the carbon come from?
44 Candidate Primary Star Primary is Asymptotic Red Giant star? Make carbon and other elements in Ba CH CEMPs IDEAL!
45 Primary Evolution were it a single star Carbon Abundance (mass fraction) e-05 Mass Loss Single Star Time / Myr
46 Hypothesis CEMPs are made by Accretion of Carbon-rich Material from Wind of Asymptotic Giant stars?
47 How to test the idea? Binary Star Model Population Synthesis Compare to Observations: Quantitative Statistical Analysis Can the model explain 20% CEMP/EMP or other observed properties of CEMPs? There are technical and physics issues...
48 Technical issue: Single Stars 10 h 100 = 1, 000 h 6 weeks
49 Technical issue: Binary Stars 10 h = 10, 000, 000 h 1, 000 YEARS
50 Use a Rapid Code 0.1 s = 28 h
51 Rapid Stellar Evolution Code Replace many coupled differential equations with 1. fitting formulae 2. tabulated data based on detailed (single-star) models: R, L, Mcore etc.
52 Rapid Stellar Evolution Code Replace many coupled differential equations with 1. fitting formulae 2. tabulated data based on detailed (single-star) models: R, L, Mcore etc.
53 My Code: binary_c/nucsyn Rapid single-star model Binary-star evolution algorithm Coupled nucleosynthesis Accurate but 10, 000, 000 faster izzard/binary_c/ Try it yourself: Google for binary_c frontend
54 What I do with my code Make many populations, each 10 6 stars Vary uncertain physics parameters Default physics: [Fe/H] = 2.3 (solar scaled) Accretion efficiency = 1 Efficient thermohaline mixing Primary carbon as detailed models (Karakas 2007) Tag CEMP, EMP stars, count them Compare to observations to find true physics
55 My Main Physics Knobs 1. Accretion efficiency (onto secondary) 2. Mixing efficiency (in secondary) 3. Composition of accreted material (in primary)
56 Physics 1: Accretion onto secondary
57 Physics 1: How much Accretion? (onto secondary) idealised Bondi-Hoyle accretion: Default efficiency 1 shock wave accretion line
58 Physics 1: How much Accretion? (onto secondary) Simulated accretion (val del Borro 2009)
59 Physics 2: How much Mixing? (In secondary)
60 Physics 2: How much Mixing? (In secondary) Thermohaline mixing: Default model with mixing Courtesy of Matteo Cantiello and Evert Glebbeek
61 Physics 3: What Composition is Accreted?
62 Physics 3: What Composition is Accreted? Karakas (2007)
63 Run the simulations...
64 Results What choice of physics gets us 20% CEMPs? Izzard, Glebbeek, Stancliffe and Pols (2009 A&A in press)
65 CEMP/EMP ratio (observed 20 ± 10%) Model Set CEMP/EMP ratio (%)
66 CEMP/EMP ratio (observed 20 ± 10%) Model Set "Default" physics CEMP/EMP ratio (%)
67 CEMP/EMP ratio (observed 20 ± 10%) Model Set Extra Wind Accretion (x3) CEMP/EMP ratio (%)
68 CEMP/EMP ratio (observed 20 ± 10%) Model Set Extra Carbon CEMP/EMP ratio (%)
69 CEMP/EMP ratio (observed 20 ± 10%) Model Set No Thermohaline Mixing CEMP/EMP ratio (%)
70 CEMP/EMP ratio (observed 20 ± 10%) Model Set Carbon at Lower Mass CEMP/EMP ratio (%)
71 CEMP/EMP ratio (observed 20 ± 10%) Model Set Extra Carbon and At Lower Mass CEMP/EMP ratio (%)
72 CEMP/EMP ratio (observed 20 ± 10%) Model Set Extra Carbon Carbon at Lower Mass No Thermohaline Mixing CEMP/EMP ratio (%)
73 Key Results 1. Need MORE CARBON from primary star Found in very low metallicity stellar models [Fe/H] 3 My results suggest source still active at [Fe/H] 2 2. Need carbon in LOW MASS primary stars Canonical Models M 1.2M have carbon My results suggest carbon in M 0.8M IMPORTANT because as many stars in M as 1.2-8M! NEW models agree! (Cristallo, Campbell) 3. MIXING in secondary is not efficient Thermohaline mechanism inefficient? Or something prevents it? Gravitational settling?
74 Key Results 1. Need MORE CARBON from primary star Found in very low metallicity stellar models [Fe/H] 3 My results suggest source still active at [Fe/H] 2 2. Need carbon in LOW MASS primary stars Canonical Models M 1.2M have carbon My results suggest carbon in M 0.8M IMPORTANT because as many stars in M as 1.2-8M! NEW models agree! (Cristallo, Campbell) 3. MIXING in secondary is not efficient Thermohaline mechanism inefficient? Or something prevents it? Gravitational settling?
75 Key Results 1. Need MORE CARBON from primary star Found in very low metallicity stellar models [Fe/H] 3 My results suggest source still active at [Fe/H] 2 2. Need carbon in LOW MASS primary stars Canonical Models M 1.2M have carbon My results suggest carbon in M 0.8M IMPORTANT because as many stars in M as 1.2-8M! NEW models agree! (Cristallo, Campbell) 3. MIXING in secondary is not efficient Thermohaline mechanism inefficient? Or something prevents it? Gravitational settling?
76 Key Results Asymptotic Giant-accretion scenario works... just about! Need some knobs at full for CEMP/EMP 15% Other uncertain physics (wind accretion, common envelope efficiency etc) has little effect Compatible with lowest observed CEMP/EMP ratio (10%) and high binary fraction Initial mass function different at low metallicity? But then we have a NEMP issue... Many other CEMP characteristics to explore
77 Conclusions By looking at binary CEMPs, we can learn about the evolution of stars: when the Galaxy had just formed at low metallicity In these stars: Donor makes carbon down to low mass: 0.8M Gainer does not mix much Challenges for stellar astrophysics!
78 Future Plans Massive stars with chemistry, spin and binary populations With Norbert Langer, Selma de Mink, Sung Chul Yoon, Matteo Cantiello, ESO/VLT FLAMES collaboration.
79 The end
80
81 1. Which stars make CEMPs? M1
82 1. Which stars make CEMPs? M2
83 1. Which stars make CEMPs? separation
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