Chemo-Dynamical evolution of dwarf spheroidal galaxies

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1 11 th Russbach School on Nuclear Astrophysics Chemo-Dynamical evolution of dwarf spheroidal galaxies Yutaka Hirai! (The University of Tokyo, NAOJ)! Jun Hidaka (NAOJ), Takayuki R. Saitoh (Titech),! Michiko Fujii(NAOJ), Shota Shibagaki (UTokyo), Grant J. Mathews (U. Notre Dome),! and Toshitaka Kajino (NAOJ, UTokyo)

2 Dwarf Galaxies Leo II dwarf galaxy Milky Way Dwarf Galaxies 1/17 Tolstoy et al NAOJ

3 Galaxy Formation Dwarf Galaxies might be building blocks of the Milky Way We can observe each star in nearby dwarf galaxies to estimate star formation histories and metallcity. Dwarf galaxies are useful tool to study galaxy 2/17 formation and evolution

4 Observation Star Formation Histories of dwarf galaxies Each dwarf galaxies might experience Starkenburg et al different evolution. Star formation histories affect the chemical 3/17 abundance pattern of galaxies

5 Elemental Abundance Pattern of dwarf galaxies Dwarf Milky Galaxies Way [Mg/Fe] Type II Supernovae Type Ia Supernovae Type II Supernovae Type Ia Supernovae Old Tolstoy et al Lower [Mg/Fe] Time Solar Abundance New -2 [Fe/H] -1 0 Systematically different chemical abundance 4/17 pattern from Milky Way

6 Present dwarf galaxies and building blocks of the Milky Way are different? Nearby dsphs We need detailed simulation of dwarf galaxy evolution 5/17

7 Physical Processes inside a galaxy Cooling Gas We need to simulate dynamical and chemical evolution of galaxies at the same time! O, Mg! Fe Fe Chemical and Dynamical Evolution! = Chemodynamical White evolution dwarf binaries Massive Stars Type II Supernovae Type Ia Supernova 6/17

8 Our Ultimate Goal to reveal the chemo-dynamical evolution of dwarf galaxies in order to construct a comprehensive picture of the formation and evolution of the Milky Way in terms of the origin and evolution of atomic elements! 7/17

9 Today s goal to construct a chemo-dynamical evolution code! to find important physics on star formation histories Next Goal to implement supernova nucleosynthesis yields which we are calculating in our Tokyo Group into the present chemo-dynamical code! to study the chemical evolution and dynamical evolution of dwarf spheroidal galaxies simultaneously as building blocks of understanding the Milky Way 8/17

10 Importance of star formation for chemical enrichment inside a galaxy Cooling Star Formation Gas O, Mg! Fe Fe Massive Stars Type II Supernova Chemical Enrichment White dwarf binaries Type Ia Supernova 9/17

11 Chemo-Dynamical Evolution Code Dark Matter (Gravity, Tree method) Star (Feedback) Gas (Hydrodynamics, SPH method, ASURA (Saitoh & Makino, 2013)) 10/17

12 Star Formation Law and Supernova Feedback Radiative Cooling Gas Particles Low Temperature! Collapsing (T < K) Star Formation Fe High Density! (ρ > 0.1 cm -3 ) Supernova Mg E = η erg η: Feedback Energy Efficiency 11/17

13 Past Studies (Revaz & Jablonka 2012) Star Formation History Chemical Abundance Pattern Successfully reproduce star formation histories and chemical abundance patterns But they reduce the energy of the supernova 12/17 explosion (10 49 erg)

14 Initial Condition Density Profile: pseudo-isothermal profile Radial Density Profile Density Distribution 13/17 Total Number of Particles: 2 16 Mass of One Gas Particle: 10 3 M

15 Star Formation Histories Simulation Observation Relative SFR Total mass of the model galaxy: M Bursty early phase star formation due to the initial collapse of the model galaxy Time (Gyr) Relative SFR Sculptor dwarf galaxy Time (Gyr) Sculptor dwarf galaxy seems to evolve isolated 14/17

16 Importance of supernova feedback Relative SFR Weak Feedback (10 49 erg) Normal Feedback (10 51 erg) Total mass of the model galaxy: M Supernova feedback strongly affects the star formation rate! Strong feedback blew away the gas inside the galaxy! Time (Gyr) Chemical abundance pattern may be affected by supernova feedback For near future We need to check more massive galaxy and effects of 15/17 merger with feedback

17 Next Prospects 3 Constraining the sites of r- process elements Origin of r-process elements: [Eu/Fe] Type II supernovae? Neutron Star Mergers? [Fe/H] SAGA databese (Suda et al. 2008) The answer might be in chemodynamical simulation of dwarf galaxies! 16/17

18 Summary Dwarf spheroidal galaxies is useful tool to study galaxy formation and evolution.! We constructed chemical and dynamical evolution code.! Supernova feedback is an important process to derive star formation histories.! We will include chemical feedback such as r-process elements to deeply study evolution of dwarf galaxies and origin of elements 17/17

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