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Radial Flows and Angular Momentum Conservation in Galactic Chemical Evolution
Astrophysics of Galaxies · Submitted 31 Jul 2012
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim By this comparison the average rotational velocity of the onfalling material can be constrained to 0.7 < v/V_c < 0.75, or respectively ~ 160 km/s when assuming a constant disc circular velocity of V_c = 220 km/s.
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The abstract, sentence by sentence
We study the effects of radial flows on Galactic chemical evolution. A simple analytic scheme is developed prescribing the coupling of infall from the intergalactic medium and radial flows within the disc based on angular momentum conservation. We show that model parameters are tightly constrained by the observed [Fe/H]-abundance gradient in the Galactic disc. By this comparison the average rotational velocity of the onfalling material can be constrained to 0.7 < v/V_c < 0.75, or respectively ~ 160 km/s when assuming a constant disc circular velocity of V_c = 220 km/s. We test the robustness of this value against the influence of other processes. For a very simple model of inside-out formation this value changes only by \Delta v/V_c ~ 0.1, i.e. ~ 20 km/s, and significantly less on more realistic scenarios, showing that inside-out formation does not alone explain the abundance gradient. Effects of other uncertain parameters, e.g. star formation history and star formation efficiency have very small impact. Other drivers of inflow beyond our explicit modelling are assessed by adding a fixed inflow across the whole disc. The churning amplitude only mildly affects the results mostly by slightly flattening the metallicity gradient in the inner disc. A new process causing radial gas flows due to the ejection of material by stars moving on non-circular orbits is studied and seems to contribute negligibly to the total flows. We further show that gaseous outer discs cannot be the main source feeding the persistent star formation in the inner regions by a direct inflow.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We study the effects of radial flows on Galactic chemical evolution. | contribution 0.81 | 0.90 | 0.03 | unclear 0.69 |
| s1 | A simple analytic scheme is developed prescribing the coupling of infall from the intergalactic medium and radial flows within the disc based on angular momentum conservation. | method 0.86 | 0.94 | 0.07 | asserted 0.99 |
| s2 | We show that model parameters are tightly constrained by the observed [Fe/H]-abundance gradient in the Galactic disc. | result 0.99 | 0.93 | 0.25 | asserted 1.00 |
| s3 | By this comparison the average rotational velocity of the onfalling material can be constrained to 0.7 < v/V_c < 0.75, or respectively ~ 160 km/s when assuming a constant disc circular velocity of V_c = 220 km/s. | result 1.00 | 0.93 | 0.38 | asserted 0.95 |
| s4 | We test the robustness of this value against the influence of other processes. | method 0.66 | 0.91 | 0.03 | asserted 0.54 |
| s5 | For a very simple model of inside-out formation this value changes only by \Delta v/V_c ~ 0.1, i.e. ~ 20 km/s, and significantly less on more realistic scenarios, showing that inside-out formation does not alone explain the abundance gradient. | result 0.76 | 0.94 | 0.18 | asserted 1.00 |
| s6 | Effects of other uncertain parameters, e.g. star formation history and star formation efficiency have very small impact. | result 0.98 | 0.89 | 0.05 | asserted 1.00 |
| s7 | Other drivers of inflow beyond our explicit modelling are assessed by adding a fixed inflow across the whole disc. | method 0.82 | 0.89 | 0.03 | asserted 0.67 |
| s8 | The churning amplitude only mildly affects the results mostly by slightly flattening the metallicity gradient in the inner disc. | result 0.98 | 0.89 | 0.04 | asserted 0.93 |
| s9 | A new process causing radial gas flows due to the ejection of material by stars moving on non-circular orbits is studied and seems to contribute negligibly to the total flows. | result 0.84 | 0.92 | 0.05 | hedged possibility 0.95 |
| s10 | We further show that gaseous outer discs cannot be the main source feeding the persistent star formation in the inner regions by a direct inflow. | result 0.93 | 0.91 | 0.16 | asserted 0.99 |
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The paper
Original abstract
We study the effects of radial flows on Galactic chemical evolution. A simple analytic scheme is developed prescribing the coupling of infall from the intergalactic medium and radial flows within the disc based on angular momentum conservation. We show that model parameters are tightly constrained by the observed [Fe/H]-abundance gradient in the Galactic disc. By this comparison the average rotational velocity of the onfalling material can be constrained to 0.7 < v/V_c < 0.75, or respectively ~ 160 km/s when assuming a constant disc circular velocity of V_c = 220 km/s. We test the robustness of this value against the influence of other processes. For a very simple model of inside-out formation this value changes only by \Delta v/V_c ~ 0.1, i.e. ~ 20 km/s, and significantly less on more realistic scenarios, showing that inside-out formation does not alone explain the abundance gradient. Effects of other uncertain parameters, e.g. star formation history and star formation efficiency have very small impact. Other drivers of inflow beyond our explicit modelling are assessed by adding a fixed inflow across the whole disc. The churning amplitude only mildly affects the results mostly by slightly flattening the metallicity gradient in the inner disc. A new process causing radial gas flows due to the ejection of material by stars moving on non-circular orbits is studied and seems to contribute negligibly to the total flows. We further show that gaseous outer discs cannot be the main source feeding the persistent star formation in the inner regions by a direct inflow.
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How the literature uses it
5 arXiv papers cite this in 13 sentences
Papers citing it · 4 sentences without a confident label
Compares with it 1 paper
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While the radial and temporal shapes hence differ, the magnitude of our recovered mismatch, $≈0.1-0.5$ across the disc, is comparable to the values found by and [ref] .
The impact of hot mode accretion and angular momentum conservation on metallicity gradients of galactic discs · CGM kinematics · 1.00
Cites it as background 3 papers
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While modern abundances have been used to track, e.g., disc evolution, stellar radial migration, or also flows and accretion scenarios of the Galactic disc [ref] , the early, very metal-poor stars found predominantly in the halo have triggered the creation of scenarios with low-number stochasticity and, in extreme cases, the strategy to fit single extremely metal-poor stars with single "progenitors" that polluted their parent cloud (e.g., [ref] ).
Mixing stochasticity relinquishes evidence for magnetorotational hypernovae · Introduction · 0.89
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Radial inflow of the gas within the disk of a galaxy redistributes metals [ref] ; galaxy interactions are especially effective in inducing large-scale inflow and flattening metallicity gradients ( [ref] ; Torrey et al., in preparation).
Thermal-Instability-Driven Turbulent Mixing in Galactic Disks: I. Effective Mixing of Metals · INTRODUCTION · 0.81
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Some GCE models [ref] use the $η_wind = 0$ limit and instead use radial gas flows [ref] to adjust the metallicity gradient in their models.
Towards a measurement of the primordial helium isotope ratio · Galactic Chemical Evolution of $^3$He/$^4$He · 0.86
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