Chemical Evolution and the Mass Function of Stellar Mass Black Holes
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1 .. and Neutron Stars Chemical Evolution and the Mass Function of Stellar Mass Black Holes Benoit Côté Postdoctoral Fellow Collaborators C. Fryer, K. Belczynski, B. O Shea, C. Ritter, F. Herwig, M. Pignatari, B. Wehmeyer 2017 Sagan Exoplanet Summer Workshop Microlensing in the Era of WFIRST NASA Exoplanet Science Institute, Caltech August 8th 2017
2 Life Cycle of Stars
3 Definition of Metals
4 Definition of Metals
5 Definition of Metals METALS
6 Sources of Chemical Enrichments Core-collapse supernovae Crab nebula
7 Sources of Chemical Enrichments Core-collapse supernovae Crab nebula Type Ia supernovae Cassiopeia A
8 Sources of Chemical Enrichments Core-collapse supernovae Crab nebula Type Ia supernovae Stellar winds from low-mass stars Cassiopeia A Cat eye nebula
9 Sources of Chemical Enrichments Neutron star merger Core-collapse supernovae svs.gsfc.nasa.gov Crab nebula Type Ia supernovae Stellar winds from low-mass stars Cassiopeia A Cat eye nebula
10 Sources of Chemical Enrichments svs.gsfc.nasa.gov WR 124 Crab nebula Cassiopeia A Cat eye nebula
11 Galaxy Evolution and Gas Circulation Galactic inflows Keres et al. (2005)
12 Galaxy Evolution and Gas Circulation Galactic inflows Galactic outflows Keres et al. (2005) M82 (Hubble, Chandra, Spitzer)
13
14 Galactic Chemical Evolution Milky Way STELLAB
15 Galactic Chemical Evolution Tolstoy et al. (2009)
16 Connecting the Smallest and the Largest Scales Côté, Ritter, O Shea, et al. (2016) see also Côté, Ritter, Herwig, et al. (2017)
17 Connecting the Smallest and the Largest Scales Côté, Ritter, O Shea, et al. (2016) see also Côté, Ritter, Herwig, et al. (2017) Comes with the difficult challenge of dealing with uncertainties at all scales.
18 Connecting the Smallest and the Largest Scales Côté, Ritter, O Shea, et al. (2016) see also Côté, Ritter, Herwig, et al. (2017) Great opportunity to make progress in multiple fields of research simultaneously and build a coherent picture of how stars and galaxies evolve in the universe What about neutron stars and black holes?.. but comes with the difficult challenge of dealing with uncertainties at all scales.
19 Production of Oxygen in Massive Stars Milky Way OMEGA and Kobayashi et al. (2006) massive star yields
20 Production of Oxygen in Massive Stars Milky Way galaxy All massive stars between 8 and 40 Msun OMEGA and Kobayashi et al. (2006) massive star yields
21 Oxygen, Massive Stars, and Black Holes Smartt (2015) Supernova progenitor Initial mass [Msun]
22 Oxygen, Massive Stars, and Black Holes Smartt (2015) Supernova progenitor Black hole formation Initial mass [Msun]
23 Oxygen, Massive Stars, and Black Holes Milky Way galaxy All massive stars between 8 and 40 Msun OMEGA and Kobayashi et al. (2006) massive star yields
24 Oxygen, Massive Stars, and Black Holes Milky Way galaxy All massive stars between 8 and 40 Msun explode Only massive stars between 8 and 20 Msun OMEGA and Kobayashi et al. (2006) massive star yields
25 Oxygen, Massive Stars, and Black Holes Milky Way galaxy All massive stars between 8 and 40 Msun explode Only massive stars between 8 and 20 Msun explode Where does Oxygen come OMEGA and Kobayashi et al. (2006) massive star yields
26 Massive Star and Supernova Models log mass fraction Heger & Woosley (2010) see also Heger, Fryer, Woosley, et al. (2003) Enclosing mass [Msun]
27 Massive Star and Supernova Models Fe Si O He H log mass fraction Heger & Woosley (2010) see also Heger, Fryer, Woosley, et al. (2003) Enclosing mass [Msun]
28 Massive Star and Supernova Models Fe Si O He H log mass fraction Heger & Woosley (2010) see also Heger, Fryer, Woosley, et al. (2003) Enclosing mass [Msun]
29 Massive Star and Supernova Models Fe Si O He H log mass fraction Heger & Woosley (2010) see also Heger, Fryer, Woosley, et al. (2003) Enclosing mass [Msun]
30 Massive Star and Supernova Models Fe Si O He H log mass fraction Black Hole Heger & Woosley (2010) see also Heger, Fryer, Woosley, et al. (2003) Enclosing mass [Msun]
31 Massive Star and Supernova Models Fe Si O He H log mass fraction Neutron Star Heger & Woosley (2010) see also Heger, Fryer, Woosley, et al. (2003) Enclosing mass [Msun]
32 Massive Star and Supernova Models Fe Si O He H log mass fraction Neutron Star Heger & Woosley (2010) see also Heger, Fryer, Woosley, et al. (2003) Enclosing mass [Msun]
33 Massive Star and Supernova Models Fe Si O He H log mass fraction Neutron Star? Heger & Woosley (2010) see also Heger, Fryer, Woosley, et al. (2003) Enclosing mass [Msun]
34 Massive Star and Supernova Models Fe Si O He H This changes our vision of how O and Fe are produced log mass fraction Neutron Star? Heger & Woosley (2010) see also Heger, Fryer, Woosley, et al. (2003) Enclosing mass [Msun]
35 Massive Star and Supernova Models Fe Si O He H This changes our vision of how O and Fe are produced log mass fraction Neutron Star To test this theory, we need to know the relation between the initial mass and the final (remnant) mass of massive stars.? Heger & Woosley (2010) see also Heger, Fryer, Woosley, et al. (2003) Enclosing mass [Msun]
36 Neutron Star and Black Hole Mass Function Belczynski, Wiktorowicz, Fryer, et al. (2012) Observation of binary systems
37 Neutron Star and Black Hole Mass Function Belczynski, Wiktorowicz, Fryer, et al. (2012) Observation of binary systems
38 Neutron Star and Black Hole Mass Function Belczynski, Wiktorowicz, Fryer, et al. (2012) Observation of binary systems
39 Neutron Star and Black Hole Mass Function Belczynski, Wiktorowicz, Fryer, et al. (2012) Observation of binary systems Prescription used by the NuGrid collaboration (Pignatari et al. 2016; C. Ritter et al. in prep.)
40 Neutron Star and Black Hole Mass Function Belczynski, Wiktorowicz, Fryer, et al. (2012) Observation of binary systems ~ 80 neutron stars ~ 20 black holes Prescription used by the NuGrid collaboration (Pignatari et al. 2016; C. Ritter et al. in prep.)
41 Neutron Star and Black Hole Mass with Microlensing J. C. Yee & C. B. Henderson (Themes document)
42 Neutron Star and Black Hole Mass with Microlensing Barry, Kruk, Anderson, et al. (2014)
43 Neutron Star and Black Hole Mass with Microlensing Barry, Kruk, Anderson, et al. (2014)
44 WFIRST and Galactic Chemical Evolution Côté, Ritter, O Shea et al. (2016) see also Côté, Ritter, Herwig, et al. (2017)
45 WFIRST and Galactic Chemical Evolution Côté, Ritter, O Shea et al. (2016) see also Côté, Ritter, Herwig, et al. (2017) Neutron star and black hole mass distributions
46 WFIRST and Galactic Chemical Evolution Côté, Ritter, O Shea et al. (2016) Neutron star and black hole mass distributions Uncertainties in the remnant mass make stellar models very uncertain (Fe yields).
47 Enrichment Timing and Evolution of [Fe/H] Origin of r-process elements neutron star mergers? Using Europium (Eu) as a tracer Fe Time Fe Eu Image built from Tauris, Kramer, Freire et al. (2017)
48 Enrichment Timing and Evolution of [Fe/H] Origin of r-process elements neutron star mergers? Using Europium (Eu) as a tracer Matteucci, Romano, Arcones, et al. (2014) Fe 3 simulations with 3 different delay times [Eu/Fe] Time Fe [Fe/H] Fe Fe Eu Eu Image built from Tauris, Kramer, Freire et al. (2017)
![Enrichment Timing and Evolution of [Fe/H] How about slowing](/docs-images/76/73342210/images/49-2.jpg "down the evolution of [Fe/H]?")
49 Enrichment Timing and Evolution of [Fe/H] How about slowing down the evolution of [Fe/H]? Lower star formation efficiency
50 Enrichment Timing and Evolution of [Fe/H] How about slowing down the evolution of [Fe/H]? H Fe Lower star formation efficiency H Fe H Fe
51 Enrichment Timing and Evolution of [Fe/H] How about slowing down the evolution of [Fe/H]? H Fe Ishimaru, Wanajo & Prantzos (2015) Lower star formation efficiency H Fe Lower star formation efficiency Bigger gas reservoirs reduce [Fe/H] H Fe
52 Enrichment Timing and Evolution of [Fe/H] Ishimaru, Wanajo & Prantzos (2015)
53 Enrichment Timing and Evolution of [Fe/H] Ishimaru, Wanajo & Prantzos (2015)
54 Enrichment Timing and Evolution of [Fe/H] Ishimaru, Wanajo & Prantzos (2015)
55 Enrichment Timing and Evolution of [Fe/H] Galactic inflows Ishimaru, Wanajo & Prantzos (2015) H H H Keres et al. (2005) Galactic outflows Fe Fe Fe Fe M82 (Hubble, Chandra, Spitzer)
56 Physics Behind the [Eu/Fe]-[Fe/H] Plot Côté, Belczynski, Fryer, et al. (2017)
57 Physics Behind the [Eu/Fe]-[Fe/H] Plot Côté, Belczynski, Fryer, et al. (2017) Gas concentration (H)
58 Physics Behind the [Eu/Fe]-[Fe/H] Plot Côté, Belczynski, Fryer, et al. (2017) Gas concentration (H) Gas circulation [Fe/H]
59 Physics Behind the [Eu/Fe]-[Fe/H] Plot Côté, Belczynski, Fryer, et al. (2017) Gas concentration (H) Gas circulation [Fe/H] Stellar models (Fe)
60 Physics Behind the [Eu/Fe]-[Fe/H] Plot Côté, Belczynski, Fryer, et al. (2017) Gas concentration (H) Gas circulation [Fe/H] K. Belczynski s models Stellar models (Fe) Merger rates of compact binary objects (Eu)
61 Physics Behind the [Eu/Fe]-[Fe/H] Plot Côté, Belczynski, Fryer, et al. (2017) Gas concentration (H) Gas circulation [Fe/H] K. Belczynski s models Stellar models (Fe) Relation between initial and remnant mass (neutron stars and black holes) Merger rates of compact binary objects (Eu)
62 Breaking the Degeneracy We need multiple constraints to break the degeneracy. Côté, O Shea, Ritter, et al. (2017) Inflow rate [Fe/H] Outflow rate
63 Breaking the Degeneracy Côté, O Shea, Ritter, et al. (2017) We need multiple constraints to break the degeneracy. J. C. Yee & C. B. Henderson (Themes document) Inflow rate Outflow rate
64 Breaking the Degeneracy We need multiple constraints to break the degeneracy. We need to break the degeneracy at all scales. Côté, Ritter, O Shea et al. (2016) see also Côté, Ritter, Herwig, et al. (2017)
65 Breaking the Degeneracy We need multiple constraints to break the degeneracy. We need to break the degeneracy at all scales. Neutron star and black hole mass distributions Côté, Ritter, O Shea et al. (2016) see also Côté, Ritter, Herwig, et al. (2017)
66 Conclusions Understanding the evolution of stars and galaxies using chemical elements is a degenerate process, and the stellar models are the foundation.
67 Conclusions Understanding the evolution of stars and galaxies using chemical elements is a degenerate process, and the stellar models are the foundation. WFIRST and microlensing can constrain the mass function of neutron stars and black holes.
68 Conclusions Understanding the evolution of stars and galaxies using chemical elements is a degenerate process, and the stellar models are the foundation. WFIRST and microlensing can constrain the mass function of neutron stars and black holes. The field of chemical evolution allows to create a more coherent picture of how stars and galaxies evolve and interact. Any additional constraint help in getting closer to this big picture.
69 Open-Source Chemical Evolution Pipeline Côté, Ritter, Herwig, et al. (2017) SYGMA - Stellar Yields for Galactic Modeling Applications (C. Ritter et al. 2017, in prep.) OMEGA - One-zone Model for the Evolution of GAlaxies (Côté, O Shea, Ritter, et al. 2017) GAMMA - Galaxy Assembly with Merger-trees for Modeling Abundances (Côté et al. in prep.) STELLAB - STELLar ABundances, observational data plotting tool Open-source codes
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