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Properties of the outer regions of spiral disks: abundances, colors and ages

Published online by Cambridge University Press:  21 March 2017

Mercedes Mollá ,
Angeles I. Díaz ,
Brad K. Gibson ,
Oscar Cavichia  and
Ángel-R. López-Sánchez
Mercedes Mollá
Affiliation:
Departamento de Investigación Básica, CIEMAT, 28040, Madrid. Spain email: [email protected]
Angeles I. Díaz
Affiliation:
Universidad Autónoma de Madrid, 28049, Madrid, Spain Astro-UAM, Unidad Asociada CSIC, Universidad Autónoma de Madrid, 28049, Madrid, Spain
Brad K. Gibson
Affiliation:
E.A. Milne Centre for Astrophysics, Dept. of Physics & Mathematics, University of Hull, Hull, HU6 7RX, United Kingdom
Oscar Cavichia
Affiliation:
Instituto de Física e Química, Universidade Federal de Itajubá, Av. BPS, 1303, 37500-903, Itajubá-MG, Brazil
Ángel-R. López-Sánchez
Affiliation:
Australian Astronomical Observatory, PO Box 915, North Ryde, NSW 1670, Australia Department of Physics and Astronomy, Macquarie University, NSW 2109, Australia
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Abstract

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We summarize the results obtained from our suite of chemical evolution models for spiral disks, computed for different total masses and star formation efficiencies. Once the gas, stars and star formation radial distributions are reproduced, we analyze the Oxygen abundances radial profiles for gas and stars, in addition to stellar averaged ages and global metallicity. We examine scenarios for the potential origin of the apparent flattening of abundance gradients in the outskirts of disk galaxies, in particular the role of molecular gas formation prescriptions.

Keywords

Galaxy: abundancesGalaxy: evolutiongalaxies: abundancesISM: abundances
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S321: Formation and Evolution of Galaxy Outskirts , March 2016 , pp. 102 - 104
Copyright
Copyright © International Astronomical Union 2017 

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