Radiative and Kinetic Feedback by Low-Mass Primordial Stars

Whalen, Daniel J.; Hueckstaedt, R. M.; McConkie, Thomas

doi:10.1088/0004-637x/712/1/101

Cited by 39 publications

(52 citation statements)

References 67 publications

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“…In the study presented here (originally published in [9,10]), we use idealized simulations that combine multifrequency radiation transport with non-equilibrium chemistry, hydrodynamics, and radiative cooling. Ionization fronts have finite widths, with H 2 -photodissociating radiation and X-rays generally traveling ahead of the ionizing radiation.…”

Section: Local Effects Of Ionizing Radiationmentioning

confidence: 99%

“…This is particularly true in Population III stars, where the surface temperatures are extremely high. In this proceedings we present results from [10], which focuses on Ifronts from Pop III stars with masses of 15-40 M ⊙ . A grid of simulations are performed, varying both the central number density of an idealized 1.35 × 10 5 M ⊙ halo and the distance between the star and the density peak of this halo (and, thus, the intensity of incident radiation at the halo).…”

Section: Local Effects Of Ionizing Radiationmentioning

confidence: 99%

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Local and Global Radiative Feedback from Population III Star Formation

O’Shea¹,

Whalen²,

Yoshida³

2010

AIP Conference Proceedings

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Abstract. We present an overview of recent work that focuses on understanding the radiative feedback processes that are potentially important during Population III star formation. Specifically, we examine the effect of the Lyman-Werner (photodissociating) background on the early stages of primordial star formation, which serves to delay the onset of star formation in a given halo but never suppresses it entirely. We also examine the effect that both photodissociating and ionizing radiation in I-fronts from nearby stellar systems have on the formation of primordial protostellar clouds. Depending on the strength of the incoming radiation field and the central density of the halos, Pop III star formation can be suppressed, unaffected, or even enhanced. Understanding these and other effects is crucial to modeling Population III star formation and to building the earliest generations of galaxies in the Universe.

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Section: Local Effects Of Ionizing Radiationmentioning

confidence: 99%

Section: Local Effects Of Ionizing Radiationmentioning

confidence: 99%

Local and Global Radiative Feedback from Population III Star Formation

O’Shea¹,

Whalen²,

Yoshida³

2010

AIP Conference Proceedings

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“…This can have a relevant effect (radiative feedback; Efstathiou 1992) on the surrounding medium and on the later star formation history (e.g. Ciardi et al 2000a, 2001; Whalen, Abel & Norman 2004; Iliev, Shapiro & Raga 2005; Alvarez, Bromm & Shapiro 2006; Iliev et al 2006, 2009; Mellema et al 2006; Susa & Umemura 2006; Gnedin, Tassis & Kravtsov 2009; Susa, Umemura & Hasegawa 2009; Whalen, Hueckstaedt & McConkie 2010; Paardekooper et al 2011; Petkova & Springel 2011; Wolcott‐Green, Haiman & Bryan 2011). Therefore, appropriate radiative transfer (RT) calculations, coupled with hydrodynamics and chemistry, must be performed in order to consistently explore the repercussions on the destruction or enhancement of molecules, and hence on structure formation in the early Universe.…”

Section: Introductionmentioning

confidence: 99%

Radiative feedback and cosmic molecular gas: numerical method

Petkova¹,

Maio²

2012

Monthly Notices of the Royal Astronomical Society

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We present results from self-consistent 3D numerical simulations of cosmic structure formation with a multi-frequency radiative transfer scheme and non-equilibrium molecular chemistry of 13 primordial species (e-, H, H+, H-, He, He+, He++, H2, H2+, D, D+, HD, HeH+), performed by using the simulation code GADGET. We describe our implementation and show tests for ionized sphere expansion in a static and dynamic density field around a central radiative source, and for cosmological abundance evolution coupled with the cosmic microwave background radiation. As a demonstrative application of radiative feedback on molecular gas, we run also cosmological simulations of early structure formation in a ~1Mpc size box. Our tests agree well with analytical and numerical expectations. Consistently with other works, we find that ionization fronts from central sources can boost H2 fractions in shock-compressed gas. The tight dependence on H2 lead to a corresponding boost of HD fractions, as well. We see a strong lowering of the the typical molecular abundances up to several orders of magnitudes which partially hinders further gas collapse of pristine neutral gas, and clearly suggests the need of re-ionized gas or metal cooling for the formation of the following generation of structures.Comment: 16 pages, 9 figures; title changed; discussion extended; in press on MNRA

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“…The feedback from star formation on subsequent generations of stars has been considered widely in the literature (e.g. Couchman & Rees 1986; Mac Low & Shull 1986; Dekel & Rees 1987; Ostriker & Gnedin 1996; Haiman, Rees & Loeb 1997a; Omukai & Nishi 1999; Glover & Brand 2001; Machacek, Bryan & Abel 2001; O’Shea et al 2005; Yoshida et al 2007; Wise & Abel 2007; Whalen et al 2008; Mesinger, Bryan & Haiman 2009; Whalen, Hueckstaedt & McConkie 2010; Gnedin 2010).…”

Section: Introductionmentioning

confidence: 99%

The micro-structure of the intergalactic medium - I. The 21 cm signature from dynamical minihaloes

Meiksin¹

2011

Monthly Notices of the Royal Astronomical Society

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A unified description is provided for the 21 cm signatures arising from minihaloes against a bright background radio source and against the cosmic microwave background (CMB), within the context of a dynamical collapsing cosmological spherical halo. The effects of gas cooling via radiative atomic and molecular processes and of star formation on setting the maximum mass of the minihaloes giving rise to a 21 cm signal are included. Models are computed both with and without molecular hydrogen formation, allowing for its possible suppression by an ambient ultraviolet radiation field. The spectral signatures and equivalent width distributions are computed for a Λcold dark matter cosmology. The detectability of minihaloes in absorption against bright background radio sources is discussed in the context of future measurements by a Square Kilometre Array (SKA) and the LOw Frequency ARray (LOFAR). The brightness temperature differential relative to the CMB is also computed. Several generic scenarios are considered. For the cosmological parameter constraints from the Wilkinson Microwave Anisotropy Probe (WMAP), in the absence of any form of galactic feedback, the number of systems per unit redshift in absorption against a bright radio source at 8 < z < 10 is dN/dz≃ 10 for observed equivalent widths exceeding 0.1 kHz. For larger equivalent widths, somewhat fewer systems are predicted at increasing redshifts. The estimated numbers are independent of the presence of star formation in the haloes following molecular hydrogen formation except for rare, high equivalent width systems, which become fewer. LOFAR could plausibly detect a minihalo signal against a 30 mJy source in a 1200 h integration. SKA could detect the signal against a weaker 6 mJy source in as little as 24 h. Adding cosmological constraints from the Atacama Cosmology Telescope (ACT) suppresses the predicted number of all the absorbers by as much as an order of magnitude. In the presence of a background of ambient Ly photons of sufficient intensity to couple the gas spin temperature to the kinetic temperature, as may be produced by the first star‐forming objects, the number of weak absorption systems is substantially boosted, by more than two orders of magnitude, rendering the signal readily detectable. Weak absorption features arising from the cold infalling regions around the minihaloes may appear as mock emission lines relative to the suppressed continuum level. A moderate amount of heating of the intergalactic medium (IGM), however, would greatly reduce the overall number of absorption systems. By contrast, the absorption signal of minihaloes against the CMB is distinguishable from the diffuse IGM signature only for a limited scenario of essentially no feedback and moderate redshifts, z < 19. The strength of the signal is dominated by the more massive minihaloes, and so is sensitive to a cut‐off in the upper minihalo mass range imposed by any star formation and its consequences. Once the first star‐forming systems provide feedback in the form of Ly pho...

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Radiative and Kinetic Feedback by Low-Mass Primordial Stars

Cited by 39 publications

References 67 publications

Local and Global Radiative Feedback from Population III Star Formation

Local and Global Radiative Feedback from Population III Star Formation

Radiative feedback and cosmic molecular gas: numerical method

The micro-structure of the intergalactic medium - I. The 21 cm signature from dynamical minihaloes

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