Supermassive black hole formation by the cold accretion shocks in the first galaxies

K. Inayoshi; K. Omukai

doi:10.1063/1.4754373

Supermassive black hole formation by the cold accretion shocks in the first galaxies

K. Inayoshi, K. Omukai

Research output: Chapter in Book/Report/Conference proceeding › Conference contribution

1 Citation (Scopus)

Abstract

We propose a new scenario for supermassive star (SMS; ≳10 ⁵M_⊙) formation in shocked regions of colliding cold accretion flows near the centers of first galaxies. When the post-shock density is high enough for collisionally exciting H₂ rovibrational levels (≳10⁴cm^-3), enhanced H₂ collisional dissociation suppresses the gas to cool below 8000 K. In this case, the layer fragments into massive clouds (≳10⁵M_⊙), which collapse isothermally (∼ 8000 K) by the Lyα cooling without subsequent fragmentation. As an outcome, SMSs are expected to form and evolve eventually to seeds of supermassive black holes. By calculating thermal evolution of the shocked gas, we delimit the range of post-shock conditions for the SMS formation. We also find that metal enrichment does not affect the SMS forming condition for ≲10^-3Z_⊙ if metals are in the gas phase.

Original language	English
Title of host publication	First Stars IV - From Hayashi to the Future -
Pages	309-312
Number of pages	4
DOIs	https://doi.org/10.1063/1.4754373
Publication status	Published - 2012 Dec 1
Externally published	Yes
Event	1st Stars IV: From Hayashi to the Future - Kyoto, Japan Duration: 2012 May 21 → 2012 May 25

Publication series

Name	AIP Conference Proceedings
Volume	1480
ISSN (Print)	0094-243X
ISSN (Electronic)	1551-7616

Other

Other	1st Stars IV: From Hayashi to the Future
Country	Japan
City	Kyoto
Period	12/5/21 → 12/5/25

Keywords

Pop III stars
first galaxies
supermassive black holes

ASJC Scopus subject areas

Physics and Astronomy(all)

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10.1063/1.4754373

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title = "Supermassive black hole formation by the cold accretion shocks in the first galaxies",

abstract = "We propose a new scenario for supermassive star (SMS; ≳10 5M⊙) formation in shocked regions of colliding cold accretion flows near the centers of first galaxies. When the post-shock density is high enough for collisionally exciting H2 rovibrational levels (≳104cm-3), enhanced H2 collisional dissociation suppresses the gas to cool below 8000 K. In this case, the layer fragments into massive clouds (≳105M⊙), which collapse isothermally (∼ 8000 K) by the Lyα cooling without subsequent fragmentation. As an outcome, SMSs are expected to form and evolve eventually to seeds of supermassive black holes. By calculating thermal evolution of the shocked gas, we delimit the range of post-shock conditions for the SMS formation. We also find that metal enrichment does not affect the SMS forming condition for ≲10-3Z⊙ if metals are in the gas phase.",

keywords = "Pop III stars, first galaxies, supermassive black holes",

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T1 - Supermassive black hole formation by the cold accretion shocks in the first galaxies

AU - Inayoshi, K.

AU - Omukai, K.

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N2 - We propose a new scenario for supermassive star (SMS; ≳10 5M⊙) formation in shocked regions of colliding cold accretion flows near the centers of first galaxies. When the post-shock density is high enough for collisionally exciting H2 rovibrational levels (≳104cm-3), enhanced H2 collisional dissociation suppresses the gas to cool below 8000 K. In this case, the layer fragments into massive clouds (≳105M⊙), which collapse isothermally (∼ 8000 K) by the Lyα cooling without subsequent fragmentation. As an outcome, SMSs are expected to form and evolve eventually to seeds of supermassive black holes. By calculating thermal evolution of the shocked gas, we delimit the range of post-shock conditions for the SMS formation. We also find that metal enrichment does not affect the SMS forming condition for ≲10-3Z⊙ if metals are in the gas phase.

AB - We propose a new scenario for supermassive star (SMS; ≳10 5M⊙) formation in shocked regions of colliding cold accretion flows near the centers of first galaxies. When the post-shock density is high enough for collisionally exciting H2 rovibrational levels (≳104cm-3), enhanced H2 collisional dissociation suppresses the gas to cool below 8000 K. In this case, the layer fragments into massive clouds (≳105M⊙), which collapse isothermally (∼ 8000 K) by the Lyα cooling without subsequent fragmentation. As an outcome, SMSs are expected to form and evolve eventually to seeds of supermassive black holes. By calculating thermal evolution of the shocked gas, we delimit the range of post-shock conditions for the SMS formation. We also find that metal enrichment does not affect the SMS forming condition for ≲10-3Z⊙ if metals are in the gas phase.

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KW - first galaxies

KW - supermassive black holes

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