THE NUCLEOSYNTHETIC IMPRINT OF 15-40 M{sub sun} PRIMORDIAL SUPERNOVAE ON METAL-POOR STARS

Journal Article · Wed Jan 20 00:00:00 EST 2010 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/709/1/11· OSTI ID:21392365

Joggerst, C C; Woosley, S E ^[1]; Almgren, A; Bell, J ^[2]; Heger, Alexander ^[3]; Whalen, Daniel ^[4]

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1. Department of Astronomy and Astrophysics, University of California at Santa Cruz, Santa Cruz, CA 95060 (United States)
2. Computational Research Division, Lawrence Berkeley National Lab, Berkeley, CA 94720 (United States)
3. School of Physics and Astronomy, University of Minnesota, Twin Cities, Minneapolis, MN 55455 (United States)
4. Theoretical Astrophysics (T-2), Los Alamos National Laboratory, Los Alamos, NM 87545 (United States)

The inclusion of rotationally induced mixing in stellar evolution can alter the structure and composition of pre-supernova stars. We survey the effects of progenitor rotation on nucleosynthetic yields in Population III and II supernovae (SNe) using the new adaptive mesh refinement code CASTRO. We examine piston-driven spherical explosions in 15, 25, and 40 M{sub sun} stars at Z = 0 and 10{sup -4} Z{sub sun} with three explosion energies and two rotation rates. Rotation in the Z = 0 models resulted in primary nitrogen production and a stronger hydrogen burning shell which led all models to die as red supergiants (in contrast to the blue supergiant progenitors made without rotation). On the other hand, the Z = 10{sup -4} Z{sub sun} models that included rotation ended their lives as compact blue stars. Because of their extended structure, the hydrodynamics favors more mixing and less fallback in the metal-free stars than the Z = 10{sup -4} models. As expected, higher energy explosions produce more enrichment and less fallback than do lower energy explosions, and at constant explosion energy, less massive stars produce more enrichment and leave behind smaller remnants than do more massive stars. We compare our nucleosynthetic yields to the chemical abundances in the three most iron-poor stars yet found and reproduce the abundance pattern of one, HE 0557-4840, with a zero metallicity, 15 M{sub sun}, 2.4 x 10{sup 51} erg SN. A Salpeter IMF-averaged integration of our yields for Z = 0 models with explosion energies of 2.4 x 10{sup 51} erg or less is in good agreement with the abundances observed in larger samples of extremely metal-poor (EMP) stars, provided 15 M{sub sun} stars are included. Since the abundance patterns of EMP stars likely arise from a representative sample of progenitors, our yields suggest that 15-40 M{sub sun} core-collapse SNe with moderate explosion energies contributed the bulk of the metals to the early universe.

• OSTI ID: 21392365
• Journal Information: Astrophysical Journal, Vol. 709, Issue 1; Other Information: DOI: 10.1088/0004-637X/709/1/11; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
ABUNDANCE
COSMOLOGY
ELECTROMAGNETIC PULSES
EXPLOSIONS
HYDRODYNAMICS
HYDROGEN BURNING
IRON
NUCLEAR REACTIONS
NUCLEOSYNTHESIS
PISTONS
ROTATION
STAR EVOLUTION
SUPERNOVAE
UNIVERSE
BINARY STARS
ELECTROMAGNETIC RADIATION
ELEMENTS
ERUPTIVE VARIABLE STARS
EVOLUTION
FLUID MECHANICS
MACHINE PARTS
MECHANICS
METALS
MOTION
PULSES
RADIATIONS
STAR BURNING
STARS
SYNTHESIS
TRANSITION ELEMENTS
VARIABLE STARS