Supernova Nucleosynthesis in Population III 13-50 M☉ Stars and Abundance Patterns of Extremely Metal-poor Stars

By Nozomu Tominaga, H. Umeda, Ken'ichi Nomoto. 2007

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We perform hydrodynamic and nucleosynthesis calculations of core-collapse supernovae (SNe) and hypernovae (HNe) of Population (Pop) III stars. We provide new yields for the main-sequence mass of MMS = 13-50 M☉ and the explosion energy of E = (1–40) × 1051 ergs to apply to chemical evolution studies. Our HN yields based on the mixing-fallback model of explosions reproduce the observed abundance patterns of extremely metal-poor (EMP) stars (-4 < [Fe/H] < -3), while those of very metal-poor (VMP) stars (-3 < [Fe/H] < -2) are reproduced by the normal SN yields integrated over the Salpeter initial mass function. Moreover, the observed trends of abundance ratios [X/Fe] against [Fe/H] with small dispersions for the EMP stars can be reproduced as a sequence resulting from the various combination of MMS and E. This is because we adopt the empirical relation that a larger amount of Fe is ejected by more massive HNe. Our results imply that the observed trends with small dispersions do not necessarily mean the rapid homogeneous mixing in the early Galactic halo at [Fe/H] < -3 but can be reproduced by the "inhomogeneous" chemical evolution model. In addition, we examine how the modifications of the distributions of the electron mole fraction Ye and the density in the presupernova models improve the agreement with observations. In this connection, we discuss possible contributions of nucleosynthesis in the neutrino-driven wind and the accretion disk.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/629ed84696fd1864da357ce91d49efa702ed6fa0

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THE MASS SPECTRUM OF THE FIRST STARS (2014, background): “…stars (Heger & Woosley 2002; Umeda & Nomoto 2002) and the abundance patterns of the metal-poor stars are well reproduced by supernova explosions of first stars as massive as the supernova progenitor stars in the present day (M 100 M ; Tominaga et al. 2007; Tominaga 2009; Heger & Woosley 2010).”
The evolution of isotope ratios in the Milky Way Galaxy (2011, background): “The [(Co, Zn)/Fe] trend can be explained by HNe under the assumption that the observed stars were enriched by only a single supernova (Tominaga et al. 2007).”
The Destruction of Cosmological Minihalos by Primordial Supernovae (2008, methodology): “The Truelove&McKee (1999) free-expansion solution for the supernova blast is completely parameterized by the mass, kinetic energy, and maximum velocity of the ejecta, which are listed in Table 5 (Heger &Woosley 2002; Tominaga et al. 2007).”
NUCLEOSYNTHESIS AND EVOLUTION OF MASSIVE METAL-FREE STARS (2008, background): “Other recent surveys of zero-metallicity massive stars are Woosley & Weaver (1995), Marigo et al. (2001), Heger & Woosley (2002), Chieffi & Limongi (2004), Umeda & Nomoto (2005), Hirschi et al. (2006), and Tominaga et al. (2007).”
THE MOST METAL-POOR STARS. II. CHEMICAL ABUNDANCES OF 190 METAL-POOR STARS INCLUDING 10 NEW STARS WITH [Fe/H] ⩽ −3.5,, (2012, background): “The abundance patterns of these stars can constrain yields from zero metallicity supernovae (e.g., Limongi et al. 2003; Umeda & Nomoto 2005; Meynet et al. 2006; Tominaga et al. 2007; Heger & Woosley 2010; Limongi & Chieffi 2012).”
Nucleosynthesis in Stars and the Chemical Enrichment of Galaxies (2013, background): “In fact, Maeda & Nomoto (2003), Tominaga et al. (2007), and Tominaga (2009) have simulated jet-like explosions and shown that their nucleosynthesis yields can be similar to those found in the mixing and fallback model because the materials around the jet axis are ejected and the materials around…”
NUGRID STELLAR DATA SET. I. STELLAR YIELDS FROM H TO BI FOR STARS WITH METALLICITIES Z = 0.02 and Z = 0.01 (2013, background): “…but the ultimate yield is complex (e.g., Woosley & Weaver 1995; Chieffi et al. 1998; Limongi et al. 2000; Woosley et al. 2002; Nomoto et al. 2006; Tominaga et al. 2007; Thielemann et al. 2011) and specific discussion is needed for different species (see for example Rauscher et al. 2002; Tur et…”
How Much 56Ni Can Be Produced in Core-Collapse Supernovae? Evolution and Explosions of 30-100 M☉ Stars (2007, methodology): “From precise comparisons, M(56Ni) is estimated to be typically 0.1 − 0.4M⊙ (Tominaga et al. 2007b; UN05) and comparable to a typical present day hypernovae such as SN1998bw.”
Near-Field Cosmology with Extremely Metal-Poor Stars (2015, background): “5.3.5 Type II supernovae with relativistic jets (Tominaga et al. 2007) A relativistic jet-induced black-hole-forming explosion of a 40M⊙ supernova leads to infall of inner material that “decreases the [ejected] amount of inner core material (Fe) relative to that of outer material (C)”.”
CARBON-ENHANCED METAL-POOR STAR FREQUENCIES IN THE GALAXY: CORRECTIONS FOR THE EFFECT OF EVOLUTIONARY STATUS ON CARBON ABUNDANCES (2014, background): “Among these are massive, zero/low-metallicity stars, with/without rotation (Meynet et al. 2006, 2010), and mixing and fallback Type II supernovae, often referred to as “faint supernovae” (Umeda & Nomoto 2005; Tominaga et al. 2007).”
HIGH-RESOLUTION SPECTROSCOPY OF EXTREMELY METAL-POOR STARS FROM SDSS/SEGUE. I. ATMOSPHERIC PARAMETERS AND CHEMICAL COMPOSITIONS (2012, background): “…production of the material incorporated into CEMP-no stars is pollution of the interstellar medium by so- called faint supernovae associated with the first generations of stars, which experience extensive mixing and fallback during their explosions (Umeda & Nomoto 2003, 2005; Tominaga et al. 2007).”
CARBON-ENHANCED METAL-POOR STARS IN SDSS/SEGUE. I. CARBON ABUNDANCE ESTIMATION AND FREQUENCY OF CEMP STARS (2013, background): “…mixing episodes (Meynet et al. 2006, 2010); and (3) faint supernovae associated with the first generations of stars, which experience extensive mixing and fallback during their explosions and eject large amounts of C and O (Umeda & Nomoto 2003, 2005; Tominaga et al. 2007; Ito et al. 2009, 2013).”
NUCLEOSYNTHESIS IN ELECTRON CAPTURE SUPERNOVAE OF ASYMPTOTIC GIANT BRANCH STARS (2008, background): “The production of each element in a supernova, in particular of those synthesized in the innermost ejecta, is severely affected by the choice of these parameters (see, e.g., Tominaga et al. 2007; Heger & Woosley 2008).”