Commit a6d176df authored by Izzard, Robert Dr (Physics)'s avatar Izzard, Robert Dr (Physics)
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add MNRAS paper

parent 5b759a0c
#LyX 2.3 created this file. For more info see http://www.lyx.org/
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title[A paper for MNRAS]{A paper for Monthly Notices of the Royal Astronomical
Society}
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% in the main text
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author[A.Smith~et~al.]
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{Adam B.~Smith,$^{1}$,
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Jessica Jones,$^{1,2}$,
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Bruce Chan,$^{2}$
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$^{1}$Edinburgh Observatory Cafe, Calton Hill, Edinburgh, EH7 5AA, Scotland.
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$^{2}$Marvel Observatory, New York, United States of America.
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$^{3}$Instiute of Martial Astronomy, Hong Kong.
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\begin_layout Date
Received ...; Accepted...
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\begin_layout Abstract
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Stars: binaries: general – Stars: abundances – Galaxy: disc – Galaxy: abundances
– Galaxy: stellar content
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Introduction
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The stellar evolution of low-mass, those lighter than about
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, single stars is reasonably well understood.
Stars form in radiating, collapsing clouds of mostly hydrogen and helium.
Compression heats the centre of the clouds until nuclear burning begins
in their cores and stars are born.
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\begin_layout Section
Stellar modelling
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We employ two stellar evolution codes to model Galactic thick-disc stars.
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Our observational sample
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We extract a sample of thick-disc stars from APOKASC.
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Results
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Your exciting results go here.
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Our simulated stellar populations match the range of abundances and masses
observed in the APO red-giant sample, but a number of uncertainties – in
the models, observations and interpretation – remain.
Alternative evolutionary pathways, such as triple stars and stellar migration,
are possible.
We discuss these below and suggest avenues for future research that may
help resolve the associated problems.
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Conclusions
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We explore the properties of the binary-star population of low-mass stars
in the thick disc which are more massive than they should be given their
age.
Our models naturally contain a population of red giant stars, from
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of all giants, more massive than the maximum
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that is possible in single-star evolution.
These stars are more likely to be single, merged objects than binary stars,
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Acknowledgements
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We thank the referee for their suggestions which have improved the clarity
of the manuscript.
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Some appendix material
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