Cooling of Pre-Galactic Gas Clouds by Hydrogen Molecule

Matsuda, Takuya; Sato, H.; Takeda, Hiroyuki

doi:10.1143/ptp.42.219

Cited by 105 publications

(82 citation statements)

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“…Although the literature on this subject extends all the way back to the sixties (Saslaw & Zipoy 1967, Peebles & Dicke 1968, Hirasawa 1969, Matsuda et al 1969, Hutchins 1976, Silk 1983, Palla et al 1983, Lepp & Shull 1984, Couchman 1985, Couchman & Rees 1986, Lahav 1986), this review focuses on the progress made over the past decade in the modern context of CDM cosmologies.…”

Section: Fig 2-artist's Illustration Of One Of the Current Designs mentioning

confidence: 99%

In the beginning: the first sources of light and the reionization of the universe

2001

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The formation of the first stars and quasars marks the transformation of the universe from its smooth initial state to its clumpy current state. In popular cosmological models, the first sources of light began to form at a redshift z = 30 and reionized most of the hydrogen in the universe by z = 7. Current observations are at the threshold of probing the hydrogen reionization epoch. The study of high-redshift sources is likely to attract major attention in observational and theoretical cosmology over the next decade.

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Section: Fig 2-artist's Illustration Of One Of the Current Designs mentioning

confidence: 99%

In the beginning: the first sources of light and the reionization of the universe

2001

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“…(23)(24)(25)(26)(27)(28), are strictly equivalent to the standard MLA equations presented in the previous section, as was derived in Paper I [Eq. (31) was not derived in that paper and we give a proof in Appendix A 2].…”

Section: General Descriptionmentioning

confidence: 99%

“…Corrections at the percent level are still important, and several works have been devoted to the problem [5,8,25,[28][29][30][31][32][33][34][35]. The most important effect is continuum opacity in the He I 2 1 P o − 1 1 S line due to photoionization of neutral hydrogen, which requires a detailed line + continuum radiative transfer analysis [30,31,34].…”

Section: Introductionmentioning

confidence: 99%

HyRec: A fast and highly accurate primordial hydrogen and helium recombination code

2011

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We present a state-of-the-art primordial recombination code, HyRec, including all the physical effects that have been shown to significantly affect recombination. The computation of helium recombination includes simple analytic treatments of hydrogen continuum opacity in the He I 2 1 P o − 1 1 S line, the He I] 2 3 P o − 1 1 S line, and treats feedback between these lines within the on-the-spot approximation. Hydrogen recombination is computed using the effective multilevel atom method, virtually accounting for an infinite number of excited states. We account for two-photon transitions from 2s and higher levels as well as frequency diffusion in Lyman-α with a full radiative transfer calculation. We present a new method to evolve the radiation field simultaneously with the level populations and the free electron fraction. These computations are sped up by taking advantage of the particular sparseness pattern of the equations describing the radiative transfer. The computation time for a full recombination history is ∼ 2 seconds. This makes our code well suited for inclusion in Monte Carlo Markov chains for cosmological parameter estimation from upcoming high-precision cosmic microwave background anisotropy measurements.

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“…Therefore, one of the fundamental questions on the star formation in primeval galaxies is, '' What kind of stars (i.e., Population III stars) were made in such extremely metaldeficient gas clouds? '' (Matsuda, Sato, & Takeda 1969;Yoneyama 1972;Yoshii & Saio 1986, hereafter YS86;Silk 1977a;Tegmark et al 1997;Nakamura & Umemura 1999, 2002Bromm, Coppi, & Larson 1999;Bromm et al 2001;Bromm, Coppi, & Larson 2002;.…”

Section: Introductionmentioning

confidence: 99%

Effects of a Burst of Formation of First‐Generation Stars on the Evolution of Galaxies

Shioya

Taniguchi

Murayama

et al. 2002

ApJ

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First-generation (Population III) stars in the universe play an important role in the early enrichment of heavy elements in galaxies and intergalactic medium and thus affect the history of galaxies. The physical and chemical properties of primordial gas clouds are significantly different from those of present-day gas clouds observed in the nearby universe because the primordial gas clouds do not contain any heavy elements, which are important coolants in gas. Previous theoretical considerations have suggested that typical masses of the first-generation stars are between several solar masses and %10 M , although it has been argued that the formation of very massive stars (e.g., >100 M ) is also likely. If stars with several solar masses are the most popular ones at the epoch of galaxy formation, most stars will evolve to hot (e.g., e10 5 K), luminous ($10 4 L ) stars with gaseous and dusty envelopes prior to going on to die as white dwarf stars. Although the duration of this phase is short (e.g., $10 5 yr), such evolved stars could contribute both to the ionization of gas in galaxies and to the production of a lot of dust grains if the formation of intermediate-mass stars is highly enhanced. We compare gaseous emission-line properties of such nebulae with some interesting highredshift galaxies such as IRAS F10214+4724 and powerful radio galaxies.

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Cooling of Pre-Galactic Gas Clouds by Hydrogen Molecule

Cited by 105 publications

References 0 publications

In the beginning: the first sources of light and the reionization of the universe

In the beginning: the first sources of light and the reionization of the universe

HyRec: A fast and highly accurate primordial hydrogen and helium recombination code

Effects of a Burst of Formation of First‐Generation Stars on the Evolution of Galaxies

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