CaltechAUTHORS
  A Caltech Library Service

Neutron Star Mergers are the Dominant Source of the r-process in the Early Evolution of Dwarf Galaxies

Duggan, Gina E. and Kirby, Evan N. and Andrievsky, Serge M. and Korotin, Sergey A. (2018) Neutron Star Mergers are the Dominant Source of the r-process in the Early Evolution of Dwarf Galaxies. Astrophysical Journal, 869 (1). Art. No. 50. ISSN 1538-4357. http://resolver.caltech.edu/CaltechAUTHORS:20181211-140648144

[img] PDF - Published Version
See Usage Policy.

2314Kb
[img] PDF - Accepted Version
See Usage Policy.

1842Kb

Use this Persistent URL to link to this item: http://resolver.caltech.edu/CaltechAUTHORS:20181211-140648144

Abstract

There are many candidate sites of the r-process: core-collapse supernovae (CCSNe; including rare magnetorotational core-collapse supernovae), neutron star mergers (NSMs), and neutron star/black hole mergers. The chemical enrichment of galaxies—specifically dwarf galaxies—helps distinguish between these sources based on the continual build-up of r-process elements. This technique can distinguish between the r-process candidate sites by the clearest observational difference—how quickly these events occur after the stars are created. The existence of several nearby dwarf galaxies allows us to measure robust chemical abundances for galaxies with different star formation histories. Dwarf galaxies are especially useful because simple chemical evolution models can be used to determine the sources of r-process material. We have measured the r-process element barium with Keck/DEIMOS medium-resolution spectroscopy. We present the largest sample of barium abundances (almost 250 stars) in dwarf galaxies ever assembled. We measure [Ba/Fe] as a function of [Fe/H] in this sample and compare with existing [α/Fe] measurements. We have found that a large contribution of barium needs to occur at more delayed timescales than CCSNe in order to explain our observed abundances, namely the significantly more positive trend of the r-process component of [Ba/Fe] versus [Fe/H] seen for [Fe/H] ≾ -1.6 when compared to the [Mg/Fe] versus [Fe/H] trend. We conclude that NSMs are the most likely source of r-process enrichment in dwarf galaxies at early times.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-4357/aaeb8eDOIArticle
https://arxiv.org/abs/1809.04597arXivDiscussion Paper
ORCID:
AuthorORCID
Duggan, Gina E.0000-0002-9256-6735
Kirby, Evan N.0000-0001-6196-5162
Additional Information:© 2018. The American Astronomical Society. Received 2018 July 16; revised 2018 October 17; accepted 2018 October 20; published 2018 December 11. This material is based upon work supported by the National Science Foundation Graduate Research Fellowship under grant No. DGE-1745301 and the National Science Foundation under grant No. AST-1614081. Facility: Keck:II (DEIMOS). - Software: MOOG (Sneden 1973), spec2d pipeline (Cooper et al. 2012; Newman et al. 2013), scipy (Jones et al. 2001).
Funders:
Funding AgencyGrant Number
NSF Graduate Research FellowshipDGE-1745301
NSFAST-1614081
Subject Keywords:galaxies: abundances; galaxies: dwarf; galaxies: evolution; Local Group; nuclear reactions, nucleosynthesis, abundances; stars: abundances
Record Number:CaltechAUTHORS:20181211-140648144
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20181211-140648144
Official Citation:Gina E. Duggan et al 2018 ApJ 869 50
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:91692
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:11 Dec 2018 22:18
Last Modified:11 Dec 2018 22:18

Repository Staff Only: item control page