The First Supernova Explosions: Energetics, Feedback, and Chemical Enrichment

By Thomas Greif, Jarrett L. Johnson, V. Bromm, Ralf Klessen. 2007

136 citations recorded by the source corpus.

We perform three-dimensional smoothed particle hydrodynamics simulations in a realistic cosmological setting to investigate the expansion, feedback, and chemical enrichment properties of a 200 M☉ pair-instability supernova in the high-redshift universe. We find that the SN remnant propagates for a Hubble time at z ≃ 20 to a final mass-weighted mean shock radius of 2.5 kpc (proper), roughly half the size of the H II region, and in this process sweeps up a total gas mass of 2.5 × 105 M☉. The morphology of the shock becomes highly anisotropic once it leaves the host halo and encounters filaments and neighboring minihalos, while the bulk of the shock propagates into the voids of the intergalactic medium. The SN entirely disrupts the host halo and terminates further star formation for at least 200 Myr, while in our specific case it exerts positive mechanical feedback on neighboring minihalos by shock-compressing their cores. In contrast, we do not observe secondary star formation in the dense shell via gravitational fragmentation, due to the previous photoheating by the progenitor star. We find that cooling by metal lines is unimportant for the entire evolution of the SN remnant, while the metal-enriched, interior bubble expands adiabatically into the cavities created by the shock, and ultimately into the voids with a maximum extent similar to the final mass-weighted mean shock radius. Finally, we conclude that dark matter halos of at least Mvir ≳ 108 M☉ must be assembled to recollect all components of the swept-up gas.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/0dc741535c6e65bb0be78f32c56587ca19afb7fa

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Citations in the corpus

Fluctuations in the high-redshift Lyman–Werner background: close halo pairs as the origin of supermassive black holes (2008, background): “Metal enrichment by the nearby star forming galaxy (that is responsible for the large local LW flux), is not necessarily a problem, since the expelled metals most efficiently mix in the outer edge of the collapsing halo, while leaving the inner core pristine (Greif et al. 2007; Cen & Riquelme 2008).”
Resolving the Formation of Protogalaxies. III. Feedback from the First Stars (2007, background): “Thus gas structures in the host halo are totally disrupted and expelled, effectively enriching the surrounding intergalactic medium (IGM) with the SN ejecta (Bromm & Loeb 2003; Kitayama & Yoshida 2005; Greif et al. 2007).”
Building up the Population III initial mass function from cosmological initial conditions (2016, background): “…same massive Pop III stars also left behind the first metal-enriched SN remnants (e.g. 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 et al. 2012; Maio et al. 2011; recently reviewed in Karlsson et al. 2013).”
Near-Field Cosmology with Extremely Metal-Poor Stars (2015, unknown): “At the other extreme of the energy scale, the authors reported that high-energy PISNe would have sufficient energy to remove all gas from the minihalo (see also Greif et al. 2007).”
The first galaxies : assembly, cooling and the onset of turbulence (2008, background): “On the other hand, if mergers are absent or incoming haloes are not sufficiently massive, accretion could be suppressed for & 100 Myr (Johnson & Bromm 2007).”
THE MASS SPECTRUM OF THE FIRST STARS (2014, background): “(A color version of this figure is available in the online journal.) induce second generation star formation by the compression of nearby density peaks or the fragmentation of the shocked gas (Greif et al. 2007; Sakuma & Susa 2009; Chiaki et al. 2013; Dhanoa et al. 2014).”
FORMATION RATES OF POPULATION III STARS AND CHEMICAL ENRICHMENT OF HALOS DURING THE REIONIZATION ERA (2009, background): “More typical explosions may instead enrich significantly less gas (≈ 106 M ) although at a correspondingly higher metallicity (see Bromm et al. 2003; Kitayama & Yoshida 2005; Greif et al. 2007; Whalen et al. 2008).”
Population III Star Formation in a ΛCDM Universe. II. Effects of a Photodissociating Background (2007, background): “This allows us to ignore complex radiative, chemical and dynamical effects that would vastly complicate our calculations (O’Shea et al. 2005a; Johnson et al. 2006; Yoshida et al. 2007; Greif et al. 2007; Abel et al. 2007; Ahn & Shapiro 2007).”
The first stars: formation of binaries and small multiple systems (2009, unknown): “…E-mail: minerva@astro.as.utexas.edu supernovae (SNe) they spread heavy elements through the IGM, thereby providing the initial cosmic metal enrichment (e.g. Madau et al. 2001; Mori et al. 2002; Bromm et al. 2003; Wada & Venkatesan 2003; Norman et al. 2004; Greif et al. 2007; Tornatore et al. 2007).”
THE SPECTRAL EVOLUTION OF THE FIRST GALAXIES. I. JAMES WEBB SPACE TELESCOPE DETECTION LIMITS AND COLOR CRITERIA FOR POPULATION III GALAXIES (2011, background): “…the ejecta from the first pop III supernovae may take ∼ 108 yr to cool sufficiently to be used in the subsequent formation of pop II and pop I stars (Greif et al. 2007), the time it takes before metal emission lines start to emerge from the surrounding nebula may be much shorter, perhaps no more…”
The Destruction of Cosmological Minihalos by Primordial Supernovae (2008, methodology): “Numerical simulations excluding these phenomenon indicate that metals do not significantlymix with the IGM until gas falls back into the dark matter potential after about a Hubble time (Greif et al. 2007).”
The First Billion Years project: the impact of stellar radiation on the co-evolution of Populations II and III (2012, background): “…a large fraction (e.g. Heger et al. 2003) of Pop III stars explode as supernovae (SNe) and eject the first heavy elements into the c© 2012 RAS intergalactic medium (e.g. Ferrara et al. 2000; Bromm et al. 2003; Kitayama & Yoshida 2005; Greif et al. 2007; Vasiliev et al. 2008; Whalen et al. 2008).”
The birth of a galaxy – II. The role of radiation pressure (2012, methodology): “Because we resolve the blastwave relatively well with several cells across at its initialization, the thermal energy is converted into kinetic energy and agrees with the SedovTaylor solution (e.g. Greif et al. 2007).”
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).”
THE BIRTH OF A GALAXY: PRIMORDIAL METAL ENRICHMENT AND STELLAR POPULATIONS (2010, methodology): “Because we resolve the blastwave relatively well with several cells across at its initialization, the thermal energy is converted into kinetic energy and agrees with the Sedov-Taylor solution (e.g. Greif et al. 2007).”