The effect of different type Ia supernova progenitors on Galactic chemical evolution

Matteuccí, F.; Spitoni, E.; Recchi, Simone; Valiante, Rosa

doi:10.1051/0004-6361/200911869

Cited by 130 publications

(142 citation statements)

References 57 publications

(90 reference statements)

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“…4 Matteucci et al (2006Matteucci et al ( , 2009; Yates et al (2013); all these studies agree that the average number of prompt Type Ia SNe can vary from ∼ 15 per cent to a maximum of ∼ 30 per cent with respect to the integrated number of Type Ia SNe, hence a percentage which should be lower than the 50 per cent assumed by Mannucci et al (2006), although these authors concluded that for their data also a percentage of 30 per cent could be acceptable. Finally, the models with the double degenerate scenario (dashed-dotted red curves) predict a steeper declining trend of the [α/Fe] ratios than the single degenerate scenario as first Type Ia SNe explode.…”

Section: Exploring the Effect Of Different Dtds For Type Ia Snementioning

confidence: 82%

A simple and general method for solving detailed chemical evolution with delayed production of iron and other chemical elements

Vincenzo

Matteuccí²,

Spitoni³

2016

Mon. Not. R. Astron. Soc.

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We present a theoretical method for solving the chemical evolution of galaxies, by assuming an instantaneous recycling approximation for chemical elements restored by massive stars and the Delay Time Distribution formalism for the delayed chemical enrichment by Type Ia Supernovae. The galaxy gas mass assembly history, together with the assumed stellar yields and initial mass function, represent the starting point of this method. We derive a simple and general equation which closely relates the Laplace transforms of the galaxy gas accretion history and star formation history, which can be used to simplify the problem of retrieving these quantities in the galaxy evolution models assuming a linear Schmidt-Kennicutt law. We find that -once the galaxy star formation history has been reconstructed from our assumptions -the differential equation for the evolution of the chemical element X can be suitably solved with classical methods. We apply our model to reproduce the [O/Fe] and [Si/Fe] vs. [Fe/H] chemical abundance patterns as observed at the solar neighborhood, by assuming a decaying exponential infall rate of gas and different delay time distributions for Type Ia Supernovae; we also explore the effect of assuming a nonlinear Schmidt-Kennicutt law, with the index of the power law being k = 1.4. Although approximate, we conclude that our model with the single degenerate scenario for Type Ia Supernovae provides the best agreement with the observed set of data. Our method can be used by other complementary galaxy stellar population synthesis models to predict also the chemical evolution of galaxies.

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Section: Exploring the Effect Of Different Dtds For Type Ia Snementioning

confidence: 82%

A simple and general method for solving detailed chemical evolution with delayed production of iron and other chemical elements

Vincenzo

Matteuccí²,

Spitoni³

2016

Mon. Not. R. Astron. Soc.

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“…In the so-called single degenerate scenario, a C-O white dwarf (WD) in a close binary system explodes due to gas accretion from a companion in a binary system. Another proposed scenario for Type Ia SNe is the so-called double degenerate case, where two WDs merge, thus triggering the explosion (see Matteucci et al 2009 and references therein). Matteucci et al (2009) Greggio & Renzini (1983) and Matteucci & Greggio (1986) and is expressed as (see more details in Matteucci 2001)…”

Section: Appendix B: the Chemical Evolution Model Adopted In This Workmentioning

confidence: 99%

Chemodynamical evolution of the Milky Way disk

Minchev

Chiappini

Martig

2013

A&A

442

574

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In the first paper of this series, we present a new approach for studying the chemo-dynamical evolution in disk galaxies, which consists of fusing disk chemical evolution models with compatible numerical simulations of galactic disks. This method avoids known star formation and chemical enrichment problems encountered in simulations. Here we focus on the Milky Way, by using a detailed thindisk chemical evolution model (matching local observables, which are weakly affected by radial migration) and a simulation in the cosmological context, with dynamical properties close to those of our Galaxy. We examine in detail the interplay between in situ chemical enrichment and radial migration and their impact on key observables in the solar neighborhood, e.g., the age-metallicityvelocity relation, the metallicity distribution, and gradients in the radial and vertical directions. We show that, due to radial migration from mergers at high redshift and the central bar at later times, a sizable fraction of old metal-poor high-[α/Fe] stars can reach the solar vicinity. This naturally accounts for a number of recent observations related to both the thin and thick disks, despite the fact that we use thin-disk chemistry only. Although significant radial mixing is present, the slope in the age-metallicity relation is only weakly affected, with a scatter compatible with recent observational work. While we find a smooth density distribution in the [O/Fe]-[Fe/H] plane, we can recover the observed discontinuity by selecting particles according to kinematic criteria used in high-resolution samples to define the thin and thick disks. We outline a new method for estimating the birth place of the Sun and predict that the most likely radius lies in the range 4.4 < r < 7.7 kpc (for a current location at r = 8 kpc). A new, unifying model for the Milky Way thick disk is offered, where both mergers and radial migration play a role at different stages of the disk evolution. We show that in the absence of early-on massive mergers the vertical velocity dispersion of the oldest stars is underestimated by a factor of ∼2 compared with observations. We can, therefore, argue that the Milky Way thick disk is unlikely to have been formed through a quiescent disk evolution. An observational test involving both chemical and kinematic information must be devised to ascertain this possibility.

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“…Kobayashi et al 1998;Greggio 2005;Matteucci et al 2009). We chose the following form, given in Kawata & Gibson (2003):…”

Section: Making Chemical Evolution Tracks (Part A)mentioning

confidence: 99%

Reconstructing the star formation history of the Milky Way disc(s) from chemical abundances

Snaith

Haywood

Matteo

et al. 2015

A&A

170

262

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We develop a chemical evolution model to study the star formation history of the Milky Way. Our model assumes that the Milky Way has formed from a closed-box-like system in the inner regions, while the outer parts of the disc have experienced some accretion. Unlike the usual procedure, we do not fix the star formation prescription (e.g. Kennicutt law) to reproduce the chemical abundance trends. Instead, we fit the abundance trends with age to recover the star formation history of the Galaxy. Our method enables us to recover the star formation history of the Milky Way in the first Gyrs with unprecedented accuracy in the inner (R < 7−8 kpc) and outer (R > 9−10 kpc) discs, as sampled in the solar vicinity. We show that half the stellar mass formed during the thick-disc phase in the inner galaxy during the first 4−5 Gyr. This phase was followed by a significant dip in star formation activity (at 8−9 Gyr) and a period of roughly constant lower-level star formation for the remaining 8 Gyr. The thick-disc phase has produced as many metals in 4 Gyr as the thin-disc phase in the remaining 8 Gyr. Our results suggest that a closed-box model is able to fit all the available constraints in the inner disc. A closed-box system is qualitatively equivalent to a regime where the accretion rate maintains a high gas fraction in the inner disc at high redshift. In these conditions the SFR is mainly governed by the high turbulence of the interstellar medium. By z ∼ 1 it is possible that most of the accretion takes place in the outer disc, while the star formation activity in the inner disc is mostly sustained by the gas that is not consumed during the thick-disc phase and the continuous ejecta from earlier generations of stars. The outer disc follows a star formation history very similar to that of the inner disc, although initiated at z ∼ 2, about 2 Gyr before the onset of the thin-disc formation in the inner disc.

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The effect of different type Ia supernova progenitors on Galactic chemical evolution

Cited by 130 publications

References 57 publications

A simple and general method for solving detailed chemical evolution with delayed production of iron and other chemical elements

A simple and general method for solving detailed chemical evolution with delayed production of iron and other chemical elements

Chemodynamical evolution of the Milky Way disk

Reconstructing the star formation history of the Milky Way disc(s) from chemical abundances

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