Resolving the Formation of Protogalaxies. III. Feedback from the First Stars

By John H. Wise, Tom Abel. 2007

216 citations recorded by the source corpus.

The first stars form in dark matter halos of masses ~106 M☉ as suggested by an increasing number of numerical simulations. Radiation feedback from these stars expels most of the gas from the shallow potential well of their surrounding dark matter halos. We use cosmological adaptive mesh refinement simulations that include self-consistent Population III star formation and feedback to examine the properties of assembling early dwarf galaxies. Accurate radiative transport is modeled with adaptive ray tracing. We include supernova explosions and follow the metal enrichment of the intergalactic medium. The calculations focus on the formation of several dwarf galaxies and their progenitors. In these halos, baryon fractions in 108 M☉ halos decrease by a factor of 2 with stellar feedback and by a factor of 3 with supernova explosions. We find that radiation feedback and supernova explosions increase gaseous spin parameters up to a factor of 4 and vary with time. Stellar feedback, supernova explosions, and H2 cooling create a complex, multiphase interstellar medium whose densities and temperatures can span up to 6 orders of magnitude at a given radius. The pair-instability supernovae of Population III stars alone enrich the halos with virial temperatures of 104 K to approximately 10−3 of solar metallicity. We find that 40% of the heavy elements resides in the intergalactic medium (IGM) at the end of our calculations. The highest metallicity gas exists in supernova remnants and very dilute regions of the IGM.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/2ec69a636377167d5f79fc848a8285e7ae289688

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Citations in the corpus

Photodissociation of H2 in protogalaxies: modelling self‐shielding in three‐dimensional simulations (2011, methodology): “…studies have typically either adopted the optically–thin dissociation rate throughout (Machacek et al. 2001, 2003; Mesinger et al. 2006, 2009; Wise & Abel 2007, 2008a,b; Greif et al. 2010), relied upon estimating NH2 from local properties of the gas (Bromm & Loeb 2003; Johnson et al. 2008;…”
The birth of a galaxy – II. The role of radiation pressure (2012, methodology): “The blastwave is modelled by injecting the explosion energy and ejecta mass into a sphere of 10 pc, smoothed at its surface to improve numerical stability (Wise & Abel 2008).”
The First Stars: Mass Growth Under Protostellar Feedback (2011, background): “…provided the early metal enrichment of the intergalactic medium (IGM; Madau et al. 2001; Mori et al. 2002; Bromm et al. 2003; Wada & Venkatesan 2003; Norman et al. 2004; Tornatore et al. 2007; Greif et al. 2007, 2010; Wise & Abel 2008; Maio et al. 2011; recently reviewed in Karlsson et al. 2011).”
ramses-rt: radiation hydrodynamics in the cosmological context (2013, background): “…affect the state of the surrounding gas via ionization and heating and may even prevent it from falling in or condensing into external gravitational potentials, especially small ones (e.g. Wise & Abel 2008; Ocvirk & Aubert 2011), which can then in turn significantly alter the ionization history.”
Self-regulated star formation in galaxies via momentum input from massive stars (2011, result): “…an ionizing background matching that at z = 0.3 This is similar to the approach in a number of other simulations (see e.g. Robertson & Kravtsov 2008; Wise & Abel 2008; Ceverino & Klypin 2009) and gives identical results to the tabulated (T) presented in Sánchez-Salcedo, Vázquez-Semadeni & Gazol…”
Near-Field Cosmology with Extremely Metal-Poor Stars (2015, background): “As structure formation and Population III stellar evolution proceeded, of order 10 such minihalos merged to form so-called “atomic cooling halos” (Wise & Abel 2008, Greif et al. 2008) with dark matter masses of ∼ 108 M⊙ at redshifts of z ∼ 10−15.”
Ubiquitous seeding of supermassive black holes by direct collapse (2012, background): “However, in massive pristine haloes (Tvir >∼ 10 4 K) we form 10 stars following a Salpeter IMF, with mass cut offs at 10 and 100M⊙ (e.g. Greif et al. c© 0000 RAS, MNRAS000, 1–19 2008; Johnson et al. 2008; Wise & Abel 2008).”
GALAXY PROPERTIES AND UV ESCAPE FRACTIONS DURING THE EPOCH OF REIONIZATION: RESULTS FROM THE RENAISSANCE SIMULATIONS (2016, background): “…halo (Kitayama et al. 2004; Whalen et al. 2004, 2008; Kitayama & Yoshida 2005; Abel et al. 2007), leaving behind a gas-poor halo that only recovers by cosmological accretion after tens of megayears (Wise & Abel 2008b; Greif et al. 2010; Wise et al. 2012b; Muratov et al. 2013; Jeon et al. 2014).”
Galaxy formation theory (2010, background): “Feedback processes are clearly of crucial importance here—for example, Wise and Abel (2008b) show that feedback during the formation of protogalaxies at early times can effectively boost the angular momentum content of such systems by factors of three o five.”
FORMATION RATES OF POPULATION III STARS AND CHEMICAL ENRICHMENT OF HALOS DURING THE REIONIZATION ERA (2009, background): “…is a crucial issue that can be properly addressed only once cosmological simulations of Population III star formation will be able to go past the formation of the first protostellar core and follow multiple episodes of star formation (see Wise & Abel 2008 for promising progress in this direction).”
The First Billion Years project: the impact of stellar radiation on the co-evolution of Populations II and III (2012, background): “…these processes, with many results gleaned from cosmological simulations of early SNe feedback and metal enrichment (e.g. Tornatore et al. 2007; Wise & Abel 2008; Wiersma et al. 2009a; Greif et al. 2010; Maio et al. 2011; Wise et al. 2012) and of the build-up of the global background (e.g.…”
IONIZING PHOTON ESCAPE FRACTIONS FROM HIGH-REDSHIFT DWARF GALAXIES (2008, methodology): “Closer inspection of collapsing halos in radiation hydrodynamics simulations also shows high-redshift, low-mass halos can collapse and is indeed regulated by the filtering mass. Prior to reionization, Gnedin (2000) showed that the filtering mass smoothly increases from ∼106 M⊙ before any star format”
THE BIRTH OF A GALAXY: PRIMORDIAL METAL ENRICHMENT AND STELLAR POPULATIONS (2010, methodology): “The blastwave is modeled by injecting the explosion energy and ejecta mass into a sphere of 10 pc, smoothed at its surface to improve numerical stability (Wise & Abel 2008).”