On the Typical Timescale for the Chemical Enrichment from Type Ia Supernovae in Galaxies

By F. Matteucci, S. Recchi. 2001

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We calculate the Type Ia supernova (SN) rate for different star formation histories in galaxies by adopting the most popular and recent progenitor models. We show that the timescale for the maximum in the SN Ia rate, which corresponds also to time of the maximum enrichment, is not unique but is a strong function of the adopted stellar lifetimes, initial mass function, and star formation rate. This timescale varies from ~ 40-50 Myr for an instantaneous starburst to ~0.3 Gyr for a typical elliptical galaxy to ~ 4.0-5.0 Gyr for a disk of a spiral galaxy like the Milky Way. We also show that the typical timescale of 1 Gyr, often quoted as the typical timescale for the SNe Ia, is just the time at which, in the solar neighborhood, the Fe production from SNe Ia starts to become important and not the time at which SNe Ia start to explode. As a consequence of this, a change in slope in the [O/Fe] ratio is expected in correspondence of this timescale. We conclude that the suggested lack of SNe Ia at low metallicities produces results at variance with the observed [O/Fe] versus [Fe/H] relation in the solar region. We also compute the SN Ia rates for different galaxies as a function of redshift and predict an extended maximum between redshift z ~ 3.6 and z ~ 1.6 for elliptical galaxies, and two maxima, one at z ~ 3 and the other at z ~ 1, for spiral galaxies, under the assumption that galaxies start forming stars at zf ~ 5 and ΩM = 0.3, ΩΛ = 0.7.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/7e47951af1409ce4771b431b19facaac85fa411a

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THE SEGUE STELLAR PARAMETER PIPELINE. V. ESTIMATION OF ALPHA-ELEMENT ABUNDANCE RATIOS FROM LOW-RESOLUTION SDSS/SEGUE STELLAR SPECTRA (2010, background): “Substantially, more Fe is generated by Type Ia supernovae (SNe Ia), whose progenitor lifetimes are much longer (on the order of 0.1 Gyr to a few Gyr; Matteucci & Recchi 2001).”
The rates of type Ia supernovae - I. Analytical formulations (2005, background): “Quantitatively, the actual constraint on the formation timescales also varies with the duration of the star formation episode in the system (Matteucci & Recchi 2001).”
The Milky Way’s stellar disk (2013, background): “Therefore, until type Ia supernovae, with typical delay times of 2Gyr (e.g., Matteucci & Recchi 2001; Dahlen et al. 2008; Maoz et al. 2011), start occurring, the early disk’s ISM, and stars formed out of it, has [α/Fe] that is higher than it is today.”
Black Hole Masses and Enrichment of z ~ 6 SDSS Quasars (2007, methodology): “Assuming an enrichment time of 0.3 Gyr appropriate for an elliptical galaxy (Matteucci & Recchi 2001), the onset of star formation would have been at z & 8.”
From star clusters to dwarf galaxies: the properties of dynamically hot stellar systems (2008, background): “Matteucci & Recchi (2001) and Greggio (2005) suggest median time scales between some ten Myr and a few Gyr for the evolution of white dwarfs into SN I, depending on the initial conditions for the population.”
Two populations of progenitors for type ia supernovae (2005, methodology): “Different explosion models (Greggio & Renzini 1983; Yungelson & Livio 2000; Matteucci & Recchi 2001; Belczynski et al. 2005; Greggio 2005) predict different delay times between the formation of the progenitor system and the SN explosion.”
Formation and dynamical evolution of multiple stellar generations in globular clusters (2008, background): “This time is not unambiguously determined, and its value for a SF of short duration is estimated in the range 40 < tpk < 300 Myr (Matteucci & Recchi 2001; Mannucci et al. 2006).”
Formation of isolated dwarf galaxies with feedback (2009, methodology): “On the other hand, we are satisfied that allowing the lifetime to be a ‘free parameter’ of the model, the best fit to the observations is obtained with a minimum lifetime of around 100 Myrs, compatible with the value suggested by Matteucci & Recchi (2001).”
STELLAR ABUNDANCES IN THE SOLAR NEIGHBORHOOD: THE HYPATIA CATALOG (2014, background): “…[Fe/H] increases, so does the general timeline of chemical evolution – where we expect to see contributions from core-collapse supernovae for low values of [Fe/H] and the effects – 14 – from SN Ia at higher values (Wheeler et al. 1989; Matteucci & Recchi 2001; Gibson et al. 2003; Chiappini 2011).”
Galactic Chemical Evolution: Carbon through Zinc (2006, background): “The shortest lifetime of SNe Ia depends on the SN Ia model: ∼ 0.1 Gyr for the double-degenerate (Tutukov & Yungelson 1994), ∼ 0.3 Gyr for Matteucci & Recchi (2001)’s model, and ∼ 0.5 Gyr for our single-degenerate model (K98). ii) Some anomalous stars (e.g., Nissen & Schuster 1997) have [O/Fe] ∼ 0…”
Iron Emission in the z = 6.4 Quasar SDSS J114816.64+525150.3 (2003, background): “…so we re-created their template spectrum using information given in their publ shed article. initial mass function, and may be much shorter than the canonical 1 Gyr for an intense starburst in the core of a rapidly forming elliptical galaxy (Friaça & Terlevich 1998; Matteucci & Recchi 2001).”
Gemini Near-Infrared Spectroscopy of Luminous z ∼ 6 Quasars: Chemical Abundances, Black Hole Masses, and Mg II Absorption (2007, background): “It has been shown that the timescale of Fe enrichment from SNe Ia strongly depends on star formation histories of host galaxies and can be much shorter in high-redshift quasar environments (e.g., Friaca & Terlevich 1998; Matteucci & Recchi 2001).”
Formation Histories of Dwarf Galaxies in the Local Group (2004, background): “The time scale depends on the star formation history and could be as short as 50Myr for a bursting mode of star formation (Matteucci & Recchi 2001).”
Chemical enrichment of galaxy clusters from hydrodynamical simulations (2007, methodology): “This functional form of f (μ) has been derived from statistical studies of the stellar population in the solar neighbourhood (Tutukov & Iungelson 1980; Matteucci & Recchi 2001).”
Oxygen, carbon and nitrogen evolution in galaxies (2002, background): “The main change in slope occurs at [Fe/H]≃ −0.6 dex and corresponds to the time at which the type Ia SN rate in the disk reaches a maximum, roughly 1 Gyr after the gap (see also Matteucci and Recchi 2001).”
Production of dust by massive stars at high redshift (2011, methodology): “From explosion models (e.g., Greggio and Renzini, 1983; Matteucci and Recchi, 2001; Greggio, 2005) differentdelay times are predicted.”
Europium production: neutron star mergers versus core-collapse supernovae (2013, methodology): “The adopted progenitor model for SNeIa is the single-degenerate model as suggested by Greggio & Renzini (1983) and later reproposed by Matteucci & Recchi (2001).”