Asymptotic Giant Branch stars
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1 Asymptotic Giant Branch stars Falk Herwig Los Alamos National Laboratory Theoretical Astrophysics Group LA Neutron Science Center Falk Herwig, May 8, 2006, 1
2 Introduction: AGB evolution NGC 6826 (Balick etal) IRC , Speckle image, Menchikov etal 2002 Herwig 2005, ARAA. JINA NSF site visit: AGB stars Falk Herwig, May 8, 2006, 2
3 JINA focus AGB stars: Why do we care? AGB stars account for ~75% of the stellar material re-ejeted into the ISM Large fraction (~40%) of C, primary producer of N Half of all trans-iron elements are made by the s-process in AGB stars At very low metallicity in the early Universe: large primary production of many light n-heavy species (like 23 Na, 24/25 Mg) AGB (including s-process) yields for near-field cosmology applications (e.g. Venn etal. 204, Fenner etal. 2006) to study cosmological formation history of our galaxy and it s dwarf spheroidal satellites Test bed for physics of mixing and nucleosynthesis: plenty observables of intrinsic nuclear production Supernova progenitors: WD for SNIa, super AGB for ONe core-collapse JINA NSF site visit: AGB stars Falk Herwig, May 8, 2006, 3
4 AGB star research at JINA Astro physics simulation: 1D stellar evolution 2D and 3D stellar hyrodynamics Nuclear network calculations Nuclear physics: Nuclear physics experiments Charged particle: e.g. 22 Ne n-capture X-section: Sm-Eu-Gd Weak interactions Nuclear theory and rate evaluation Astrophysics Observables: Stellar spectroscopy, surveys Pre-solar grains JINA NSF site visit: AGB stars Falk Herwig, May 8, 2006, 4
5 A JINA Observation - Astrophysics Project: The AGB signature in C-rich extremely metal-poor (binary) stars [Fe/H] Models: -2.3 Herwig 2004, ApJS Sivarani etal 2006, ApJ submitted. JINA NSF site visit: AGB stars Falk Herwig, May 8, 2006, 5
6 A JINA Astrophysics - Nuclear Theory/Evaluation project: Dredge-up mixing in AGB stars and nuclear reaction rates Total C yield as a function of nuclear reaction rate = what one 2M star of 0.5 Z ejects into the ISM. Herwig etal 2006, PRC Herwig & Austin 2004, ApJ. JINA NSF site visit: AGB stars Falk Herwig, May 8, 2006, 6
7 JINA Computational Astrophysics - Nuclear Experiment project: s-process, Hydrodynamics and Mixing of He-shell Flash Convection 2D, 1200x400, Herwig etal 2006, ApJ. On this slide is a convection movie Showing the entropy fluctuations in the life presentation. JINA NSF site visit: AGB stars Falk Herwig, May 8, 2006, 7
8 JINA Computational Astrophysics - Nuclear Experiment project: s-process, Hydrodynamics and Mixing of He-shell Flash Convection Determine convective overshoot mixing for stellar interior nuclear burning zones Validate through astrophysical abundance observables: through bare pre-wd cores (Werner & Herwig 2006, PASP review) Sm-Eu-Gd s-process project Blue solid: diffusion coefficient reflecting hydrodynamic mixing, black: vertical and horizontal rms-velocities, light blue: entropy (scaled), the plateau indicates the convectively unstable region (Freytag & Herwig, 2006, in prep). JINA NSF site visit: AGB stars Falk Herwig, May 8, 2006, 8
9 JINA Computational Astrophysics - Nuclear Experiment project: s-process in hydrodynamic convection simulations Eularian trajectories: Temperature evolutions: High-temperature s-process nucleosynthesis in the He-shell flash convection zone along trajectories from hydrdoynamics simulation, involves: Updated s-process network with T- dependent weak interactions and n- capture cross sections (JINA student Pignatari) New n-cross sections for unstable species (Reifarth@LANSCE, former JINA student Courture, now LANL post-doc) This is a movie in the life presentation. JINA NSF site visit: AGB stars Falk Herwig, May 8, 2006, 9
10 Final Remarks JINA promotes connecting to and leveraging related projects elsewhere: Aspects of the stellar burn and mix hydrodynamics work are done as part of ASC code V&V. Through adding some resources JINA enables dual use for nuclear astrophysics program. JINA provides a platform to coordinate complementary capabilities: larger and more integrated problems can be attacked, e.g. coordinate n-cross section measurements and modeling at LANL, with charged particle measurements, stellar observations and pre-solar grain laboratory analysis at ND/MSU/Argonne (the Sm-Eu-Gd project ). JINA NSF site visit: AGB stars Falk Herwig, May 8, 2006, 10
11 BACKUP SLIDES: Falk Herwig, May 8, 2006, 11
12 He-shell flashes in AGB stars (with non-standard burning and mixing at extremely low metallicity) Adopted from Herwig, 2005, ARAA, 43. JINA NSF site visit: AGB stars Falk Herwig, May 8, 2006, 12
13 Nuclear Astrophysics: The s process branchings Competition of β-decay and neutron capture depends on n-density and/or temperature, which in turn depends on stellar model and mixing properties. JINA NSF site visit: AGB stars Falk Herwig, May 8, 2006, 13
14 A specific example: branchpoint 154 Eu Gd a Eu a a a Sm a 152 Branching ratio: f= λ β / (λ β + λ n ) β-decay rate: λ β = (ln 2) / t 1/2 n-capture rate: λ n = σ n v T N n f( 154 Eu) ~ 154 Gd/ 152 Gd JINA NSF site visit: AGB stars Falk Herwig, May 8, 2006, 14
15 Sm-Eu-Gd: a collaborative multi-physics, multi-institutional project Astrophysics modeling: Provide theory and simulation to link from nuclear experiment to astrophysical observables -> improve predictive power of models (LANL/T-6). Pre-solar grains: First individual grain isotopic measurements for multiple elements - Sm-Eu-Gd - with new experimental technology (CHARISMA) at Argonne National Lab, collaboration request letter received. Nuclear Physics Experiments with DANCE: (n,γ) measurements of radioactive samples with 4π BaF 2 array, that can not be performed anywhere else First complete experimental data coverage for an entire branching region LANL/LANSCE, T-16 Observations: Systematic campaign Eu hyperfine line splitting to determine Eu isotopic ratios in extremely metal poor stars, sample will be obtained in part from SEGUE/SDSS-II candidates (JINA/MSU). JINA NSF site visit: AGB stars Falk Herwig, May 8, 2006, 15» N u c l e a r A s t r o p h y s i c s w i t h N e u t r o n F a c i l i t i e s a n d L A N L a n d R I A «
16 Abundance evolution through a He-shell flash M ZAMS = 5M, Z = 10-4 Herwig, 2004a,b, ApJ(S) JINA NSF site visit: AGB stars Falk Herwig, May 8, 2006, 16
17 Structure of AGB stars JINA NSF site visit: AGB stars Falk Herwig, May 8, 2006, 17
18 Initial mass and evolution fate JINA NSF site visit: AGB stars Falk Herwig, May 8, 2006, 18
19 Hydrodynamics of He-shell flash convection Collaborators: Bernd Freytag, Robert Hueckstaedt, Frank Timmes 2D and 3D hydrodynamics simulations of a short duration (~20ksec) of He-shell flash convection at a time just before the peak of He-flash Explicit, Eulerian, compressible grid code RAGE Initial conditions: piecewise polytropic stratification with gravity that closely resembles the actual conditions in a specific 2M, Z=0.01 thermal pulse model JINA NSF site visit: AGB stars Falk Herwig, May 8, 2006, 19
20 Convergence vertical v horizontal v Driving x 30 x1 JINA NSF site visit: AGB stars Falk Herwig, May 8, 2006, 20
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