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V/144 MIR spectroscopy of low-mass binary stars and brown dwarfs (Mace, 2014)
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Beginning of ReadMe :V/144 Near-IR spectroscopy of low-mass binaries and brown dwarfs (Mace, 2014)
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Investigating low-mass binary stars and brown dwarfs with near-infrared
spectroscopy
Mace G.N.
<Thesis, University of California, Los Angeles (2014)>
=2014yCat.5144....0M
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ADC_Keywords: Stars, dwarfs ; Stars, double and multiple ;
Infrared sources ; Photometry, infrared
Abstract:
The mass of a star at formation determines its subsequent evolution
and demise. Low-mass stars are the most common products of star
formation and their long main-sequence lifetimes cause them to
accumulate over time. Star formation also produces many
substellar-mass objects known as brown dwarfs, which emerge from their
natal molecular clouds and continually cool as they age, pervading the
Milky Way. Low-mass stars and brown dwarfs exhibit a wide range of
physical characteristics and their abundance make them ideal subjects
for testing formation and evolution models. I have examined a pair of
pre-main sequence spectroscopic binaries and used radial velocity
variations to determine orbital solutions and mass ratios.
Additionally, I have employed synthetic spectra to estimate their
effective temperatures and place them on theoretical
Hertzsprung-Russell diagrams. From this analysis I discuss the
formation and evolution of young binary systems and place bounds on
absolute masses and radii. I have also studied the late-type T dwarfs
revealed by the Wide-field Infrared Survey Explorer (WISE). This
includes the exemplar T8 subdwarf Wolf 1130C, which has the lowest
inferred metallicity in the literature and spectroscopic traits
consistent with old age. Comparison to synthetic spectra implies that
the dispersion in near-infrared colors of late-type T dwarfs is a
result of age and/or thin sul de clouds. With the updated census of
the L, T, and Y dwarfs we can now study specific brown dwarf
subpopulations. Finally, I present a number of future studies that
would develop our understanding of the physical qualities of T dwarf
color outliers and disentangle the tracers of age and atmospheric
properties.
The thesis is available at:
http://www.astro.ucla.edu/~gmace/thesis.html