dc.creator | Gomez Maqueo Chew, Yilen | |
dc.date.accessioned | 2020-08-22T20:35:55Z | |
dc.date.available | 2010-08-05 | |
dc.date.issued | 2010-08-05 | |
dc.identifier.uri | https://etd.library.vanderbilt.edu/etd-07262010-141255 | |
dc.identifier.uri | http://hdl.handle.net/1803/13613 | |
dc.description.abstract | This thesis presents the analysis of two double-lined, detached, eclipsing binary systems
associated with the young Orion Nebula Cluster, 2MASS J05352184–0546085
and Parenago 1802. We present a multi-band, multi-epoch analysis including both
radial velocity and light curves to determine the eclipsing binaries' properties. The
components of both systems have ages of ~ 1 Myrs and are found to be in the pre-main
sequence (PMS) phase. They provide valuable observational constraints for the early
stages of theoretical evolutionary models. The goal of this thesis is to precisely determine
the physical properties of the components of two low-mass eclipsing binaries
and to characterize their orbits.
Parenago 1802 is the lowest mass twin system known among PMS binaries. The
eclipsing components have equal masses (~ 0.4 Msun) to within ~ 3 %. The components'
radii are large as expected for PMS stars, but they differ by ~ 7 %. Their
effective temperatures differ by ~ 9 %. We measure the photometric rotation period
of the components from the periodic variability, and find that the components are
not yet synchronized to their orbital motion. The small, but significant eccentricity
(e = 0.0166 ± 0.003) of the orbit makes this system one of the shortest period
(~ 4.674 d) PMS, close binaries known to be non-circular.
The eclipsing binary 2MASS J05352184–0546085 is the only known system composed
of two substellar objects with masses below the hydrogen burning limit (M1 =
0.0572 ± 0.0033 and M2 = 0.0366 ± 0.0022 Msun). The components' radii are larger
than those of older brown dwarfs of similar masses. The more massive brown dwarf
is found to be rotating over four times faster and appears to be cooler than its companion.
We find that surface spots, probably due to enhanced activity, may explain
the observed apparent temperature reversal if they cover a large area (~ 65%) of the
more massive component in a symmetric configuration.
In both cases, the theoretical models are able to reproduce some but not all of
the systems' observed properties. These young, eclipsing systems thus underline the
successful predictions in the low-mass regime of the current evolutionary models but
also their limitations. | |
dc.format.mimetype | application/pdf | |
dc.subject | astronomy | |
dc.subject | star | |
dc.subject | eclipsing binary | |
dc.subject | pre-main sequence | |
dc.subject | brown dwarf | |
dc.title | On the Analysis of Two Low-Mass, Eclipsing Binary Systems in the Young Orion Nebula Cluster | |
dc.type | dissertation | |
dc.contributor.committeeMember | Andrej Prsa | |
dc.contributor.committeeMember | David A. Weintraub | |
dc.contributor.committeeMember | David J. Ernst | |
dc.contributor.committeeMember | Robert A. Knop | |
dc.contributor.committeeMember | Robert C. O'Dell | |
dc.type.material | text | |
thesis.degree.name | PHD | |
thesis.degree.level | dissertation | |
thesis.degree.discipline | Physics | |
thesis.degree.grantor | Vanderbilt University | |
local.embargo.terms | 2010-08-05 | |
local.embargo.lift | 2010-08-05 | |
dc.contributor.committeeChair | Keivan G. Stassun | |