The Nucleosynthesis of 26Al and 60Fe in Solar Metallicity Stars Extending in Mass from 11 to 120 M☉: The Hydrostatic and Explosive Contributions

By M. Limongi, A. Chieffi. 2006

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We present the 26Al and 60Fe yields produced by a generation of solar metallicity stars ranging in mass between 11 and 120 M☉. We discuss the production sites of these γ-ray emitters and quantify the relative contributions of the various components. We provide the contributions of the wind, the C convective shell, and the explosive Ne/C burning to the total 26Al yield together with the contributions of the He convective shell, the C convective shell, and the explosive Ne/C burning to the 60Fe yield. We conclude that, at variance with current beliefs, 26Al is mainly produced by the explosive C/Ne burning over most of the mass interval analyzed here, while 60Fe is mainly produced by the C convective shell and the He convective shell. By means of these yields we try to reproduce two quite strong observational constraints related to the abundances of these nuclei in the interstellar medium, i.e., the number of γ1.8 photons per Lyman continuum photon, RGxL, and the 60Fe/26Al γ-ray line flux ratio. RGxL is found to be roughly constant along the Galactic plane (and of the order of 1.25 × 10-11), while the 60Fe/26Al ratio has been recently measured by both RHESSI (0.17 ± 0.05) and SPI (INTEGRAL) (0.11 ± 0.03). We can quite successfully fit simultaneously both ratios for a quite large range of exponents of the power-law initial mass function. We also address the fit to γ2 Velorum, and we find that a quite large range of initial masses, at least from 40 to 60 M☉, do eject an amount of 26Al (through the wind) compatible with the current upper limit quoted for this W-R star: such a result removes a long-standing discrepancy between the models and the observational data.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/b3368e2c0f770630ff2081e5ebcaf6a7bdf8e41c

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Citations in the corpus

Abundance, distribution, and origin of 60Fe in the solar protoplanetary disk (2012, background): “In massive stars, 26 Al is produced by proton capture on 25 Mg, which occurs in more external regions than the site where 60 Fe is made (Limongi and Chieffi, 2006).”
PRE-SUPERNOVA EVOLUTION OF ROTATING SOLAR METALLICITY STARS IN THE MASS RANGE 13–120 M☉ AND THEIR EXPLOSIVE YIELDS (2012, methodology): “In the first case the He convective shell turns out to be hotter then in the second one (Limongi & Chieffi 2006); such a different behavior will have profound and interesting implications on the production of some specific isotopes (see below).”
COMPACT REMNANT MASS FUNCTION: DEPENDENCE ON THE EXPLOSION MECHANISM AND METALLICITY (2011, methodology): “For example, the Limongi & Chieffi (2006) solar metallicity models are very similar to the Woosley et al. (2002) models at 1/3 solar metallicity.”
NUGRID STELLAR DATA SET. I. STELLAR YIELDS FROM H TO BI FOR STARS WITH METALLICITIES Z = 0.02 and Z = 0.01 (2013, result): “Beyond the mass cut, our stellar structure is in very good agreement with pre-collapse stellar models (Limongi & Chieffi 2006; Woosley et al. 2002; Young & Fryer 2007).”
Nucleosynthesis and remnants in massive stars of solar metallicity (2007, background): “With Z = 0.04 and Vrot = 300 km s−1, Palacios et al. (2005) get a whopping 2.2 × 10−3 M .3 Limongi and Chieffi (2006) have also recently (after our present study was completed) examined the sensitivity of 60Fe and 26Al production to the prescription for mass loss and the slope of the IMF.”
THE LANDSCAPE OF THE NEUTRINO MECHANISM OF CORE-COLLAPSE SUPERNOVAE: NEUTRON STAR AND BLACK HOLE MASS FUNCTIONS, EXPLOSION ENERGIES, AND NICKEL YIELDS (2014, methodology): “…uWHW02 10−4Z⊙ 11.0 – 60 246 HShen Woosley et al. (2002) sWHW02 Z⊙ 10.8 – 40 100 LS180, LS220, LS375, HShen Limongi & Chieffi (2006) LC06A Z⊙ 11 – 120 15 HShen Limongi & Chieffi (2006) LC06B Z⊙ 40 – 120 4 HShen zWHW02 104 106 108 1010 D en si ty [g c m -3 ] Z =…”
STELLAR ABUNDANCES IN THE SOLAR NEIGHBORHOOD: THE HYPATIA CATALOG (2014, background): “Aluminum, whose only stable isotope is 27Al, is mainly synthesized in hydrostatic carbon and neon burning (Arnett & Thielemann 1985; Thielemann & Arnett 1985; Woosley & Weaver 1995; Limongi & Chieffi 2006).”
CORE-COLLAPSE SUPERNOVAE FROM 9 TO 120 SOLAR MASSES BASED ON NEUTRINO-POWERED EXPLOSIONS (2015, background): “Limongi & Chieffi (2006a) have discussed other uncertainties that might bring the models and observations into better agreement, including a modified IMF, mass loss, modified cross sections, and overshoot mixing.”
TRACING CHEMICAL EVOLUTION OVER THE EXTENT OF THE MILKY WAY'S DISK WITH APOGEE RED CLUMP STARS (2014, methodology): “We adopt the yields of Chieffi & Limongi (2004) and Limongi & Chieffi (2006) for SNII, the W70 model of Iwamoto et al. (1999) for SNIa, and Karakas (2010) for AGB stars.”
THE COMPACTNESS OF PRESUPERNOVA STELLAR CORES (2013, background): “5 as a function of main sequence mass for a variety of surveys due to Woosley et al. (2002), Woosley & Heger (2007) and Limongi & Chieffi (2006), and a subset of that data is shown in Fig.”
TYPE Ib/c SUPERNOVAE IN BINARY SYSTEMS. I. EVOLUTION AND PROPERTIES OF THE PROGENITOR STARS (2010, methodology): “According to recent stellar models adopting the most up-to-date stellar winds mass loss rates (Meynet & Maeder 2003, 2005; Eldridge & Vink 2006; Limongi & Chieffi 2006; Georgy et al. 2009), the final masses (Mf) of helium stars produced by mass-losing single stars appear to be too massive to…”
SPI observations of the diffuse ^60Fe emission in the Galaxy (2007, methodology): “…our SPI result (also see Table 2), with upper limits shown at 2σ for all reported values, and comparison with the recent theoretical estimates (the upper hatched region from Prantzos 2004; the horizontal line taken from Timmes et al. 1995; the lower hatched region, see Limongi & Chieffi 2006).”
BLACK HOLE FORMATION IN FAILING CORE-COLLAPSE SUPERNOVAE (2010, methodology): “Limongi & Chieffi (2006)3 performed such a study, adopting two different mass-loss rates for the W-R stage of solar-metallicity stars withM & 40M⊙.”
The 511 keV emission from positron annihilation in the Galaxy (2010, background): “Limongi and Chieffi (2006) find that in their Z =Z⊙ models explosive nucleosynthesis is always dominant; however, models with rotation and at Z >Z⊙ (appropriate for the inner Galaxy) may modify this conclusion somewhat.”
Nucleosynthesis in Stars and the Chemical Enrichment of Galaxies (2013, methodology): “…and 25 M and ( from left to right) Z = 0 and 0.02, respectively, including comparisons among various models: (blue lines) Rauscher et al. (2002) and Heger & Woosley (2010); ( green lines) Limongi & Chieffi (2006, 2012); and (red lines) Kobayashi et al. (2006) and Tominaga, Umeda & Nomoto (2007).”