Constraining the shape of convective core overshooting using slowly pulsating B-type stars
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1 Constraining the shape of convective core overshooting using slowly pulsating B-type stars May Gade Pedersen Supervisor and promoter Prof. Dr. Conny Aerts Co-supervisor Dr. Péter I. Pápics Collaborator: Dr. Tamara Rogers Stellar Hydro Days IV Victoria, Canada 30 May, 2017
2 The chemical factories of the Universe Credit: LucasVB/Wikimedia OB-type stars Production of heavy elements Fed back to environment Influences e.g. Credit: NASA Formation of stars and planetary systems Evolution of galaxies and the Universe
3 The chemical factories of the Universe Common feature Convective core Fully mixed More fuel High sensitivity to near core mixing processes! Credit: Adapted from
4 The chemical factories of the Universe Internal mixing processes Convective core overshooting Rotation Major problem! Poorly known and constrained! High uncertainty in stellar structure and evolution models! Credit: Adapted from
5 Asteroseismology using g-modes O B A FG K M B3-B8 High-order g-modes P = days Luminosity Slowly Pulsating B-type (SPB) stars Why gravity-modes? Probe near-core regions Sensitive to changes in dp series (same ℓ, m) Δ μ Temperature Figure courtesy Péter I. Pápics
6 Asteroseismology using g-modes Slowly Pulsating B-type (SPB) stars B3-B8 High-order g-modes P = days SPB star Why gravity-modes? Probe near-core regions Sensitive to changes in dp series (same ℓ, m) Δ μ Pápics et al. 2016
7 Asteroseismology using g-modes
8 Asteroseismology using g-modes
9 Asteroseismology using g-modes
10 Asteroseismology using g-modes
11 Asteroseismology using g-modes
12 Asteroseismology using g-modes
13 Asteroseismology using g-modes
14 Asteroseismology using g-modes
15 Asteroseismology using g-modes Δ Mixing changes μ!
16 Theoretical period spacing series Stellar model for specific input physics Step overshoot Exp. overshoot Theoretical pulsation mode properties Ext. Exp. overshoot
17 Effect on stellar evolution
18 Effect on stellar evolution
19 Effect on stellar evolution
20 Step overshoot Diffusive mixing in overshooting region given as For dr αovhp,cc: r0: Convection Overshooting MESA: f0 D0
21 Exponential overshoot Diffusive mixing in overshooting region cc r0: Convection Overshooting MESA: f0 D0
22 Extended exponential overshoot Diffusive mixing in overshooting region For dr dr2: cc For dr > dr2: cc r0: Convection Overshooting MESA: f0 D0 D2 dr2
23 Varying f0 (i.e. D0) f0 D0
24 Varying f0 (i.e. D0) Step overshoot Exponential overshoot
25 Varying f0 (i.e. D0) Step overshoot Exponential overshoot
26 Varying f0 (i.e. D0) Step overshoot Exponential overshoot Xc = 0.50
27 Varying αov and f Strength
28 Varying αov and f Step overshoot Exponential overshoot
29 Varying αov and f Step overshoot Exponential overshoot
30 Varying αov and f Step overshoot Exponential overshoot
31 Varying Dext Extra mixing
32 Varying Dext Step overshoot Exponential overshoot
33 Varying Dext Step overshoot Exponential overshoot
34 Varying Dext Step overshoot Exponential overshoot
35 Varying f2 Extension Switch
36 Varying f2
37 Varying f2
38 Varying f2 Extended Exponential Overshoot Exponential overshoot w. Dext
39 Implementation of results from 2D hydrodynamical simulations of particle mixing
40 Implementation of results from 2D hydrodynamical simulations Set by f0 Set by fov Set as Dext Profile provided by Dr. Tamara Rogers
41 Implementation of results from 2D hydrodynamical simulations
42 Implementation of results from 2D hydrodynamical simulations
43 Implementation of results from 2D hydrodynamical simulations
44 Implementation of results from 2D hydrodynamical simulations
45 Conclusions Choice of core overshooting influences the evolution of stars Choice of f0 is important! Seismic modelling of period spacing series Constraints on strength and shape of core overshooting
46 Future work New SPB's Moravveji et al. 2015, 2016 Pápics et al. 2016
47 Thank you for your attention!
48 Varying f2 Extension Switch
49 Varying f2 Xc = 0.65
50 Varying f2 Xc = 0.35
51 Varying f2 Xc = 0.05
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