Upload
phamtuyen
View
217
Download
0
Embed Size (px)
Citation preview
Physics of Primordial Star Formation
Naoki YoshidaUniversity of Tokyo
SFDE17 Bootcamp, Quy Nhon, August 6th�
1. The standard cosmological model 2. Growth of density fluctuations
3. Assembly of dark matter halos
So far, we learned
OBSERVATIONS OF HII REGIONS
Weak dependence on metallicity (O abundance) indicating other source(s) than stars.
HELIUM PRODUCTIONIn cosmology text books, we learn (simply
read) that hydrogen and helium were produced by Big Bang during “the first three minutes”, without thinking why it is needed.
It was not so, historically. All the elements other than hydrogen were thought to be formed in stars.
But it quickly turned out it wouldn’t work....
HYDROGEN BURNING IN STARS
The$net$result$of$hydrogen$burning$is$the$fusion$$of$four$H$nuclei$into$one$4He$nucleus.$The$difference$in$binding$energy$is$26.731$MeV,$hence$~$7MeV$per$H.$(Not$all$this$energy$is$emiEed$as$photons$from$the$surface,$though.$Think$about$“Where$does$the$rest$go$?”)$
Galaxies are not He factoryOne can calculate light-to-helium production ratio as follows: Let’s take a galaxy with L ~ 1011 Lsun. Over a cosmological time of 10 Gyrs, it releases a total energy of ~ 7.5x1073 eV.
Its stellar mass would be ~ a few x1011 Msun. Then it contains ~ 2 x 1068 hydrogen nuclei.
This gives a mean energy output of 0.3 MeV per hydrogen nuclei. This is way too small compared with 7MeV per hydrogen burning.
Galaxies (stars) are luminous, but not as much as it should, in order to produce helium to ~ 25% in mass. There must be another He factory.
GALAXIES ARE NOT HELIUM FACTORIES
BBN PREDICTION
Helium abundance relatively insensitive to the baryon density. Lithium abundance is another, highly
interesting mystery.
In the beginning, there was a sea of light elements
and dark matter…
and tiny ripples left over from the Big Bang
1. What Observations Tell Us 2. Formation of Primordial Gas Clouds
3. Thermal Evolution of a Primordial Gas 4. From Big Bang Ripples to a Protostar
Contents
SURVIVING EARLY GENERATION STARS
Wavelength
Fe Fe Ca
Almost no iron!!
Num
ber o
f sta
rs
Iron abundance wrt sun There are stars in MW with very low metal content.
Progress since last century
metallicity
Starforma-onintheearlyuniverse
Cosmological recombination at t = 380Kyrs ↓ Non-linear formation of dark matter clumps ↓ Virialization → chemical reactions take place (hydrogen molecules are formed) ↓ Gas condensation at the center of DM clumps ↓ Runaway collapse of a massive molecular cloud = star-formation
• Collisional ionization, recombination
• Formation of molecules (H2, HD, H3+, H2+, HD+, HeH)
• Photoionization, photo-dissociation
• Radiative cooling collisional excitation, collisional ionization, recombination, Bbremsstrahlung, compton cooling, CMB heating
Primordialgaschemistry e, H, H+, H-, H2, H2
+, He, He+, He++ D, D+, D-, HD, HD+
~ 50-70 reactions
Composition: 76% H, 24% He、10-5 D、little Li
Starsareformed…
in a cold, dense, molecular gas cloud. Gravity alone does not make it. Gravity actually compresses and heats the gas. We need a mechanism to cool a gas cloud. Radiative cooling removes the excess energy (i.e., lowers the gas pressure) and makes it possible for the gas to cool and condense. Radiative cooling operates only if there are coolants. How did all this happen in the early universe ?
Inthepresent-dayuniverse…
Interstellar gas can cool by, e.g., - Metallic ions such as Fe, Si, O - Molecules such as CO, OH - Dust thermal emission
None of these coolants existed in the early universe.
Primordialcoolingfunc-on
HHe+
H2 For the gas in a dark halo to cool, hydrogen molecules must be formed in some way.
Galaxies
Photo-a?achmentH2forma-on
H2Forma-on:Gasphasereac-ons
Slowreac-ons,relyingonresidualelectronsasacatalyst. Becomeeffec-veatT>1000K(M~105Msun)Molecularfrac-onreaches~0.001
Photo-a?achmentH2forma-on
H2Forma-on:Gasphasereac-ons
Slowreac-ons,relyingonresidualelectronsasacatalyst. Becomeeffec-veatT>1000K(M~105Msun)Molecularfrac-onreaches~0.001
Formation on dust grains
H2Forma-on:Present-day
This reaction is much faster than the gas-phase reactions.
Almost all the hydrogen atoms are converted to molecules at relatively low densities
if there are a sufficient amount of dust grains.
H + H on dust → H2 + dust
H2rota-onaltransi-on A hydrogen atom hits a H2 molecule in the ground-level (J=0). The H2 molecule got excited to J=2. After a while, it emits a photon spontaneously, to be back in the J=0.
H2coolingrate A hydrogen atom hits a H2 molecule in the ground-level (J=0). The H2 molecule got excited to J=2. After a while, it emits a photon spontaneously, to be back in the J=0.
H2cooling:Abriefhistory Late 60’s ) Pregalactic clouds, molecular hydrogen
Matsuda-Sato-Takeda, Yoneyama, Saslaw & Zipoy
Peebles & Dicke (globular cluster)
Early 80’s ) Primordial star formation, fragmentation
Palla-Stahler-Salpeter, Yoshii, Silk, Couchman & Rees (DM)
2000’s) Cosmological simulations, pre-collapse
Omukai-Nishi, Bromm+, Abel+, NY, Greif
2010’s) Protostellar evolution, final masses
Hosokawa, Hirano, …
PrimordialgascloudBromm, Coppi, Larson 2002
Physical properties of H2 molecules connected to thermal evolution. ΔE (J=2 → 0) ~ 512 K sets the minimum temperature. Non-LTE cooling to LTE cooling “loitering”.
Molecularfrac-onWhat you get must be more than what you need
what you need
what you get = asymptotic fraction
Hydrogen recombination
Formation of H2
Radiative cooling
Left-over electroms
H, H-
Electron depletion
H, e-
t_cool ~ t_hubble
+
Tegmark et al. (1997)
Temperature
CosmologicalFirstObjects
Computer simulation by Yoshida et al. (2003)
Web-like structure in the early universe. Halo mass ~ 1,000,000 Msun Gas clouds are ~ 1000 Msun. Strongly clustered.
Matter distribution
Tage = 300 million years
Resultfroma3Dcosmo.simula-on
Halos that host gas clouds are populated above the critical line, as predicted.
THERMAL EVOLUTION OF A PRIMORDIAL GAS
adiabatic contraction
H2 formation line cooling (non-LTE)
loitering (~LTE)
3-body reaction
Heat release
opaque to molecular
line
collision induced emission T [K]
104
103
102
opaque to continuum
adiabatic, high-P
dissociation
number density
Cooling rate from NLTE (~ density2) to LTE (~ density) Jeans mass ~ T1.5/n0.5
~ 500 Msun
0.3Mpc
5pc
0.01pc A new born proto-star with T* ~ 20,000K
r ~ 10 Rsun!
Self-gravitating cloud
Fully-molecular core
THERMAL EVOLUTION OF A PRE-STELLAR GAS
adiabatic contraction
H2 formation line cooling (non-LTE)
loitering (~LTE)
3-body reaction
Heat release
opaque to molecular
line
collision induced emission T [K]
104
103
102 number density
opaque to continuum
adiabatic, high-P
The Physics
dissociation
Ahydrogenmoleculecan
Rotate, and vibrate Emit and absorb photons Be formed, and destroyed Collide with other atoms
Radiative cooling (gas temperature↓)
Chemical cooling and heating (T ↓↑)
Interact with photons, cooling and heating
Quantum energy levels
At high densities, H2 molecules are formed by
H2 formation by 3-body reactions
• The reaction rate ∝ density3. • The core becomes almost fully molecular• Significant heat release (4.48eV per molecule)
Rot-vibra-onaltransi-onsinLTEPar-clenumberdensity~1010/cc,
temperature~1000K
Thelevelpopula-on(energydistribu-on)
isLTEforJ=0-20,v=0-2
H2isahomo-nuclearmolecule;nodipoletransi-on
→quadropoletransi-on(ΔJ=2)
Radia-veTransfer1:molecularlines
Example)H2J=6→4transi-onatT~1000K
For τ >0.1, the cloud core becomes optically thick to H2 lines、and then line cooling is inefficient (τ4,6 ~1 for Lcore~0.0001pc)
1010-14
Netmolecularcoolingrate
CIE cooling
Omukai98 1D full RT
optic
ally
thic
k /
thin
3D calculation
8 10 12 14 16 log (n)
NY, Omukai, Hernquist, Abel (2006)
Λthick = Σ βescape nk,l A k,l hν
Structure of a disk: with/without radiative transfer
3D effect important in post-collapse simulations
3D transferco
olin
g ef
ficie
ncy
line continuum
Hirano & NY, 2013, ApJisotropic
density
CollisionInducedEmission
Duringcollisions,acollisionpairactsasa‘super-molecule’,genera-nganinducedelectricdipole.
hν
continuum emission
1014-17
Op-callythinCIEcoolingrate
η (ν) = σ nH2 exp(-hν/kT) 2hν3 c2
H2-H2 (Borysow et al. 2001) H2-He (Jorgensen et al 2000) @ n ~ 1013 - 1017
Equilibriumchemistry:theSahaequa-ons
A set of coupled equations including the energy equation are solved self-consistently:
H-H2
H-H+
>1016