The effects of different Type Ia SN yields on Milky Way chemical evolution

Marco Palla

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The effects of different Type Ia SN yields on Milky Way chemical evolution

Marco Palla

Astrophysics of Galaxies · Submitted 29 Jan 2021

abstract compiled · 2026-09-23 · no language-model review

The authors' main claim The comparison of chemical evolution model results with observations suggests that a combination of near-Chandrasekar and sub-Chandrasekar yields is necessary to reproduce the data of V, Cr, Mn and Ni, with different fractions depending on the adopted massive stars stellar yields.

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What the abstract itself states, as probabilities: claims first 0.02 · states limitation 0.44 · human participants 0.01 · controlled comparison 0.20 · randomized assignment 0.01 · states quantitative result 0.07 · compares with prior results 0.87 · mentions code or data availability 0.02.

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We study the effect of different Type Ia SN nucleosynthesis prescriptions on the Milky Way chemical evolution. To this aim, we run detailed one-infall and two-infall chemical evolution models, adopting a large compilation of yield sets corresponding to different white dwarf progenitors (near-Chandrasekar and sub-Chandrasekar) taken from the literature. We adopt a fixed delay time distribution function for Type Ia SNe , in order to avoid degeneracies in the analysis of the different nucleosynthesis channels. We also combine yields for different Type Ia SN progenitors in order to test the contribution to chemical evolution of different Type Ia SN channels. The results of the models are compared with recent LTE and NLTE observational data. We find that "classical" W7 and WDD2 models produce Fe masses and [$\alpha$/Fe] abundance patterns similar to more recent and physical near-Chandrasekar and sub- Chandrasekar models. For Fe-peak elements, we find that the results strongly depend either on the white dwarf explosion mechanism (deflagration-to-detonation, pure deflagration, double detonation) or on the initial white dwarf conditions (central density, explosion pattern). The comparison of chemical evolution model results with observations suggests that a combination of near-Chandrasekar and sub-Chandrasekar yields is necessary to reproduce the data of V, Cr, Mn and Ni, with different fractions depending on the adopted massive stars stellar yields. This comparison also suggests that NLTE and singly ionised abundances should be definitely preferred when dealing with most of Fe-peak elements at low metallicity.

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#	sentence	role	the authors' own work	states the main conclusion	strength
s0	We study the effect of different Type Ia SN nucleosynthesis prescriptions on the Milky Way chemical evolution.	contribution 0.97	0.89	0.02	asserted 0.61
s1	To this aim, we run detailed one-infall and two-infall chemical evolution models, adopting a large compilation of yield sets corresponding to different white dwarf progenitors (near-Chandrasekar and sub-Chandrasekar) taken from the literature.	method 0.99	0.92	0.02	asserted 0.87
s2	We adopt a fixed delay time distribution function for Type Ia SNe , in order to avoid degeneracies in the analysis of the different nucleosynthesis channels.	method 0.99	0.87	0.02	asserted 0.98
s3	We also combine yields for different Type Ia SN progenitors in order to test the contribution to chemical evolution of different Type Ia SN channels.	method 0.89	0.91	0.03	asserted 0.90
s4	The results of the models are compared with recent LTE and NLTE observational data.	method 0.95	0.67	0.02	asserted 0.95
s5	We find that "classical" W7 and WDD2 models produce Fe masses and [$\alpha$/Fe] abundance patterns similar to more recent and physical near-Chandrasekar and sub- Chandrasekar models.	result 1.00	0.93	0.20	asserted 1.00
s6	For Fe-peak elements, we find that the results strongly depend either on the white dwarf explosion mechanism (deflagration-to-detonation, pure deflagration, double detonation) or on the initial white dwarf conditions (central density, explosion pattern).	result 0.99	0.95	0.12	asserted 1.00
s7	The comparison of chemical evolution model results with observations suggests that a combination of near-Chandrasekar and sub-Chandrasekar yields is necessary to reproduce the data of V, Cr, Mn and Ni, with different fractions depending on the adopted massive stars stellar yields.	result 0.74	0.89	0.53	hedged possibility 1.00
s8	This comparison also suggests that NLTE and singly ionised abundances should be definitely preferred when dealing with most of Fe-peak elements at low metallicity.	interpretation 0.80	0.74	0.14	hedged possibility 0.79

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The paper

Original abstract

We study the effect of different Type Ia SN nucleosynthesis prescriptions on the Milky Way chemical evolution. To this aim, we run detailed one-infall and two-infall chemical evolution models, adopting a large compilation of yield sets corresponding to different white dwarf progenitors (near-Chandrasekar and sub-Chandrasekar) taken from the literature. We adopt a fixed delay time distribution function for Type Ia SNe , in order to avoid degeneracies in the analysis of the different nucleosynthesis channels. We also combine yields for different Type Ia SN progenitors in order to test the contribution to chemical evolution of different Type Ia SN channels. The results of the models are compared with recent LTE and NLTE observational data. We find that "classical" W7 and WDD2 models produce Fe masses and [$\alpha$/Fe] abundance patterns similar to more recent and physical near-Chandrasekar and sub- Chandrasekar models. For Fe-peak elements, we find that the results strongly depend either on the white dwarf explosion mechanism (deflagration-to-detonation, pure deflagration, double detonation) or on the initial white dwarf conditions (central density, explosion pattern). The comparison of chemical evolution model results with observations suggests that a combination of near-Chandrasekar and sub-Chandrasekar yields is necessary to reproduce the data of V, Cr, Mn and Ni, with different fractions depending on the adopted massive stars stellar yields. This comparison also suggests that NLTE and singly ionised abundances should be definitely preferred when dealing with most of Fe-peak elements at low metallicity.

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6 arXiv papers cite this in 11 sentences

Each citing sentence is taken from the citing paper's LaTeX source and typed by Pith's classifier. A label appears at probability 0.8 or more (0.95 for support), a contest at 0.7 or more; the quoted words are the citing authors'. How each label was checked · JSON

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Compares with it 1 paper

This is in contrast with the case of binary-stripped stars, which produce Cr in amounts comparable to Fe, in better agreement with most commonly adopted yield prescriptions in the literature (see also [ref] ).

The effects of yields from binary massive stars as functions of metallicity · Chromium · 0.83

Cites it as background 2 papers

These three elements are synthesised by means of different processes and stellar sources / timescales: Mg is mainly produced by hydrostatic burning in massive stars [ref] , Si is made during explosive burning in massive stars with non-negligible contribution from Type Ia ( [ref] and references therein), and Ni is primarily produced by Type Ia SNe ( [ref] and references therein).

The chemical DNA of the Magellanic Clouds VI. Origin and evolution of neutron-capture elements in the SMC · $α$ and Fe-peak elements abundance patterns · 0.84
For a more in depth exploration of the impact of different type Ia SN yields on MW chemical evolution see the recent work by [ref] .

The challenge of simultaneously matching the observed diversity of chemical abundance patterns in cosmological hydrodynamical simulations · Metallicity distribution · 0.91

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Cites as background 1 paper

Nonetheless, the physics governing SNe Ia is still largely debated (see [ref] for a review).

Type Ia Supernova Sub-classes and Progenitor Origin · Introduction · 0.97

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