# Revisiting the Radial Metallicity Gradient-Age Relation in the Milky Way's Thin and Thick Disks

## TL;DR

This study investigates the metallicity gradient-age relation in the Milky Way's thin and thick disks, revealing a flattening in the thin disk and a positive gradient in the thick disk, informing models of Galactic evolution.

## Contribution

It provides new observational evidence of the distinct metallicity gradient behaviors in the MW's disks using spectroscopic and asteroseismic data.

## Key findings

- Flattening of the thin disk's metallicity gradient with age
- Confirmation of a positive metallicity gradient in the thick disk
- Possible explanations include radial migration and early enrichment processes

## Abstract

Galactic disks typically exhibit a negative radial metallicity gradient, indicating faster enrichment in the inner regions. Recent studies report that this gradient becomes flatter with increasing stellar age in the Milky Way's (MW) thin disk, while the thick disk exhibits a mildly positive gradient across all ages. In this work, we revisit the metallicity gradient-age relation (MGAR) in both the thin and thick disks of the MW, using spectroscopic data from LAMOST DR8 and stellar ages calibrated with asteroseismology. Our results show a steadily flattening MGAR in the thin disk and confirm a positive gradient $\sim0.013\,\mathrm{dex\,kpc^{-1}}$ in the thick disk. The flattening in the thin disk may be caused by large-scale radial migration induced by transient spiral arms, or by a time-dependent steepening of the interstellar medium (ISM) metallicity gradient as suggested by recent FIRE2 simulations. The positive gradient in the thick disk may reflect early enrichment of the outer regions by strong feedback or starburst-driven outflows in a turbulent, gas-rich proto-disk. These findings suggest distinct chemodynamical evolution paths for the MW's thin and thick disks and provide valuable constraints for future models of Galactic chemical evolution.