The evolution of the Milky Way from its earliest phases: Constraints on stellar nucleosynthesis

By P. François, F. Matteucci, R. Cayrel, M. Spite, F. Spite, Cristina Chiappini Observatoire de ParisMeudon, Daut, Trieste, -INAF. 2004

183 citations recorded by the source corpus.

We computed the evolution of the abundances of O, Mg, Si, Ca, K, Ti, Sc, Ni, Mn, Co, Fe and Zn in the Milky Way. We made use of the most widely adopted nucleosynthesis calculations and compared the model results with observational data with the aim of imposing constraints upon stellar yields. To best fit the data in the solar neighborhood, when adopting the Woosley & Weaver (1995, ApJS, 101, 181) yields for massive stars and the Iwamoto et al. (1999, ApJS, 125, 439) ones for type Ia SNe, it is required that: i) the Mg yields should be increased in stars with masses from 11 to 20 Mand decreased in masses larger than 20 M� . The Mg yield should be also increased in SNe Ia. ii) The Si yields should be slightly increased in stars above 40 M� , whereas those of Ti should be increased between 11 and 20 Mand above 30 M� . iii) The Cr and Mn yields should be increased in stars with masses in the range 11-20 M� ; iv) the Co yields in SNe Ia should be larger and smaller in stars in the range 11-20 M� ; v) the Ni yield from type Ia SNe should be decreased; vi) the Zn yield from type Ia SNe should be increased. vii) The yields of O (metallicity dependent SN models), Ca, Fe, Ni, and Zn (the solar abundance case) in massive stars from Woosley & Weaver (1995) are the best to fit the abundance patterns of these elements since they do not need any changes. We also adopted the yields by Nomoto et al. (1997, Nucl. Phys. A, 621, 467) and Limongi & Chieffi (2003, ApJ, 592, 404) for massive stars and discuss the corrections required in these yields in order to fit the observations. Finally, the small spread in the (el/Fe) ratios in the metallicity range from (Fe/H) = − 4.0 up to−3.0 dex (Cayrel et al. 2004, A&A, 416, 1117) is a clear sign that the halo of the Milky Way was well mixed even in the earliest phases of its evolution.

Subfields: Astronomy and Astrophysics

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Citations in the corpus

The s-Process in Massive Stars at Low Metallicity: The Effect of Primary 14N from Fast Rotating Stars (2008, unknown): “In the initial composition, α−enhancements for the light isotopes are included according to Mishenina et al. (2000) for the oxygen and to Goswami & Prantzos (2000) and François et al. (2004) for the other elements.”
Reconstructing the star formation history of the Milky Way disc(s) from chemical abundances (2014, methodology): “Secondly, because of the numerous uncertainties in the input physics of any GCE model (see, for example, François et al. 2004; Romano et al. 2005, 2010; Matteucci et al. 2009), we will explore how changing the choices made when designing the basic model used in sections 4 and 5 (summarized in…”
Supernova Nucleosynthesis in Population III 13-50 M☉ Stars and Abundance Patterns of Extremely Metal-poor Stars (2007, background): “CA04 and François et al. (2004) suggested the following interpretation of the observed small dispersions; the elements have been already mixed homogeneously in the halo, even below ½Fe/H < 3, and the trends are due to the difference of the lifetime of progenitors with different masses.”
First stars VIII. Enrichment of the neutron-capture elements in the early Galaxy (2007, unknown): “In homogeneous chemical evolution models (François et al. 2004), instantaneous mixing is assumed and more variation in the yield can be allowed, because it is integrated over the different stellar masses as the galaxy evolves.”
The evolution of the Galactic metallicity gradient from high-resolution spectroscopy of open clusters (2008, result): “This correction is in agreement with the empirical stellar yields adopted by François et al. (2004).”
Evolution of interstellar dust and stardust in the solar neighbourhood (2007, background): “5 where these abundances are deﬁnitely too low, a familiar problem (e.g. Goswami & Prantzos 2000; Francois et al. 2004).”
Chemodynamical evolution of the Milky Way disk II: Variations with Galactic radius and height above the disk plane (2014, methodology): “The exact amount of this effect (i.e., the absolute values of [Mg/Fe] at a different [Fe/H]) is strongly dependent on the adopted stellar yields of Mg, Fe and the SNIa rates (here we adopt the same stellar yields as in François et al. 2004).”
Chemical evolution with rotating massive star yields - I. The solar neighbourhood and the s-process elements (2018, result): “…that similar results are obtained with the yields of Woosley & Weaver (1995) (see e.g Timmes et al. 1995; Goswami & Prantzos MNRAS 000, 1–31 (2017) 2000; François et al. 2004), while those of Nomoto et al. (2013) reproduce correctly the behavior of Mg as an α element (see also Romano et al. 2010).”
Quantifying the uncertainties of chemical evolution studies II. Stellar yields (2010, methodology): “While detailed nucleosynthesis calculations still have to establi h whether the modifications proposed by François et al. (2004) have a physical ground, HNe can provide an alternate solution: Kobayashi et al. (2006) have obtained a nice fit to the [Mg/Fe] versus [Fe/H] relation traced by solar…”
HIGH-RESOLUTION SPECTROSCOPY OF EXTREMELY METAL-POOR STARS FROM SDSS/SEGUE. I. ATMOSPHERIC PARAMETERS AND CHEMICAL COMPOSITIONS (2012, result): “This indicates that there is no large scatter in the abundance ratios of these elements even at very low metallicity, as suggested by previous studies (François et al. 2004; Arnone et al. 2005; Andrievsky et al. 2010).”
The Apache Point Observatory Galactic Evolution Experiment (APOGEE) (2007, unknown): “• Ca, Ti: Two more elements with strong ties to SN II yields, but which may also have some fraction produced in SN Ia (e.g., François et al. 2004; Nomoto et al. 2013).”
Galaxy formation theory (2010, background): “…evolution are well established within the monolithic collapse scenario (Matteucci and Greggio 1986; Matteucci and Gibson 1995; Timmes et al. 1995; François et al. 2004; Pipino and Matteucci 2004, 2006; Romano et al. 2005), but have only received limited study within the physically motivated…”
Very low-metallicity massive stars: - Pre-SN evolution models and primary nitrogen production (2006, methodology): “These provide new constraints for the stellar evolution models (see Chiappini et al. 2005; François et al. 2004; Prantzos 2005).”
s‐Process in low‐metallicity stars – I. Theoretical predictions (2010, background): “…other α elements (20Ne, 24Mg, 28Si, 32S, 36Ar, 40Ca, 48Ti), we adopt a linear relation [α/Fe] = −0.3 [Fe/H] at disc metallicities (−1 ≤ [Fe/H] ≤ 0), and an average constant [α/Fe] = 0.3 dex for [Fe/H] ≤ −1, following the trend observed in unevolved stars (Cayrel et al. 2004; François et al. 2004).”
Chemical enrichment of galaxy clusters from hydrodynamical simulations (2007, unknown): “A different approach has been followed by François et al. (2004), who inferred stellar yields by requiring that their model of chemical evolution reproduces the observed enrichment pattern of the Milky Way.”
Chemical enrichment in cosmological, smoothed particle hydrodynamics simulations (2009, background): “In fact, some authors (e.g. François et al. 2004) use observations and chemi al evolution models to derive stellar yields for a number of elements, and the results show marked differences from yields derivedfrom nucleosynthetic calculations.”
Stellar Abundance and Galactic Chemical Evolution through LAMOST Spectroscopic Survey (2006, background): “Simple chemical evolution models assume gas infall as the main ingredients (e.g. Chiappini et al. 1997, 2001; Goswami & Prantzos 2000; Hou et al. 2000; Francois et al. 2004).”
A strong case for fast stellar rotation at very low metallicities (2006, result): “The chemical evolution model presented here (without outflows) also agrees well with several other abundance ratios (François et al. 2004).”
Chemical evolution with radial mixing (2008, background): “The nucleosynthetic yields of individual metals are in many cases still subject to significant uncertainties (e.g. Thomas, Greggio & Bender 1998); in fact, models of the chemical evolution of the solar neighbourhood have been used to constrain these yields (Francois et al. 2004).”