Deciphering Ancient Terrsa 20 Apr 2010 Low-metallicity star formation and Pop III-II transition Kazu Omukai (Kyoto U.) Collaborators: Naoki Yoshida (IPMU, Tokyo) Takashi Hosokawa (JPL & NAOJ)

CONTENTS Prestellar collapse of low-metallicity clouds thermal evolution and fragmentation properties Protostellar evolution by accretion: Upper limit on the stellar mass by stellar feedback

Pop III-II transition First stars (Pop III stars ) theoretically predicted to be very massive (>100M sun ) Stars in the solar neighborhood (Pop I) typically low-mass (0.1-1M sun ) Low-mass Pop II stars exist in the halo. transition of characteristic stellar mass in the early universe from very massive to low-mass ( Pop III-II transition ) This transition is probably caused by accumulation of a certain amount of metals and dusts in ISM ( critical metallicity )

thermal evolution and fragmentation mass M frag ~ M minimum (Bromm et al. 1999) dense core (fragment) ~1000M sun Yoshida, KO, Hernquist 2008 fragmentation M Jeans ~1000M sun Metal-free case

γ< １ vigorous fragmentation, γ ＞１ fragmentation suppressed The Jeans mass at γ~1 (T minimum) gives the fragmentation scale. M frag =M  Fragmentation and thermal evolution  (isothermal)  Li et al Effective ratio of specific heat := dlog p/dlog 

Thermal Evolution of clouds with different Z 1 1) Cooling by dust thermal emission: [M/H] > ) H 2 formation on dust : [M/H] > ) Cooling by fine-str. lines (C and O): [M/H] > -3 1D hydro (spherical) dust/metal ratio same as local ISM [M/H] := log 10 (Z/Z sun ) line-induced dust-induced Low-mass fragments are formed only in the dust-induced mode.

The critical metallicity How much metallicity (dust) is needed for the low-mass star formation ?

Dust-induced fragmentation [M/H]=-5.5 (Z=3x10 -6 Z sun ) Z>~10 -6 Z sun  long filament forms during dust-cooling phase  fragmentation into low- mass (0.1-1M sun ) objects Z cr ~ Z sun Tsuribe & K.O. (2006; 2008) Using T evolution given by 1-zone model 2 nd gen. stars have low-mass components

3D simulation with self-consisitent thermal evolution Simulation set-up A NFW sphere (static potential ） 5 x 10 6 M sun ＠ z=10; T vir ~ 2000 K 1 million gas particles Mass resolution at the center ~ M sun dust-to-gas ratio scaled by metallicity Z Yoshida & KO in prep.

T dust number density (cm -3 ) T gas Temperature (K) Results: [M/H]=-5

For [M/H]=-5, Rapid cooling by dust at high density (n~10 14 cm -3 ) leads to fragmentation. Fragment mass ~ 0.1 Msun 5AU Dust-induced fragmentation

Protostellar Evolution in the Accretion Phase Cloud Core (mass set by fragmentation) Protostar (initially very small M sun) Shu et al Accreting Envelope

Envelope structure at protostar formation at >AU scale ---- higher Temperature and density for lower-Z

Mass accretion rate Lower metallicity  Higher density  Higher accretion rate Mass accetion rate dM * /dt~10c s 3 /G

Protostars in Accretion Phase Protostar hydrostatic Eq.s for Stellar Structure ＋ [radiative shock condition] ENVELOPE Stationary Accretion radiative precursor(< R ph ) stationary hydro outer envelope (>R ph ) free fall (Stahler et al. 1986) Method

For lower metallicities (= higher accretion rate): Protostars have larger radii Protostars are more massive at the onset of H burning. No stationary solution during KH contraction for [M/H]<-5 adiabatic phase t acc < t KH KH contraction ZAMS Swelling t acc ~t KH Four Evolutionary Phases: 1. Adiabatic phase 2. Swelling 3. KH contraction 4. Zero-Age Main Sequence (ZAMS) Accretion time t acc =M * /(dM * /dt) KH timescale t KH =(GM * 2 /R * )/L * Z sun Growth of protostars by accretion

Upper Limit on the stellar mass Low metallicity gas Higher accretion rate Lower opacity  Weaker feedback, Higher upper mass limit Hosokawa & KO 2009 Limit by Radiation force > 0.01Z sun ; M sun Limit by HII region expansion Z sun ; a few 100M sun No stationary accretion <10 -4 Z sun ; 100M sun Case for mass accetion rate dM * /dt~10c s 3 /G by one-zone model

SUMMARY (1) Line cooling affects the thermal evolution only at low densities where the Jeans mass is still high (>10-100M sun ). Dust cooling causes a sudden temperature drop at high density where M Jeans ~0.1M sun, which induces low-mass fragmentation. The critical metallicity for dust-induced fragmentation is [Z/H] cr ~-5 Prestellar evolution of low-Z gas and its fragmentation properties.

SUMMARY (2) In low metallicity gas, high temperature in star forming cores results in high accretion rate. Lower Z protostars become more massive before the arrival to the MS owing to higher accretion. The upper limit on the stellar mass is M sun set by radiation pressure feedback for >0.01Z sun, while it is a few 100M sun set by expansion of HII regions <0.01Z sun. evolution of low-Z protostars and the upper limit on the mass by stellar feedback