this is for holding javascript data
Meredith L. Rawls edited section_Physical_parameters_of_the__.tex
almost 8 years ago
Commit id: 44977333e54403737e149eb002ad0c26dfc944fd
deletions | additions
diff --git a/section_Physical_parameters_of_the__.tex b/section_Physical_parameters_of_the__.tex
index 08b2327..a288811 100644
--- a/section_Physical_parameters_of_the__.tex
+++ b/section_Physical_parameters_of_the__.tex
...
\section{Physical parameters of the RG/EBs}
\label{review}
\subsection{Binary modeling}
\citet{gau16} and \citet{raw16} used JKTEBOP \citep{sou09} and the Eclipsing Light Curve (ELC) program \citep{oro00} to simultaneously fit a combination of light curves and radial velocity observations for a total of 17 RG/EBs observed by \emph{Kepler}. \citet{fra13} did the same for KIC 8410637, which brings the total to 18. For the 14
SB2 systems
that have a with radial velocity
curve curves for both stars, this gives a full dynamic solution: orbital period $P_{orb}$, zeropoint, orbital inclination $i$, eccentricity and argument of periastron
parameterized (parameterized as $e \sin \omega$ and $e \cos
\omega$, \omega$), component masses, component radii, and the effective temperature ratio. For the
remaining four
SB1 systems that have a radial velocity curve for one star only,
this allows the determination of we can determine relative radii
only and no component masses. Of the 18 total systems, 14 have red giants that exhibit solar-like oscillations, which were analyzed in \citet{gau14,gau16} to derive global asteroseismic parameters.
Also mention/review:
\begin{itemize}
\item Stellar atmosphere In this work, we adopt the masses and radii from \citet{fra13,gau16,raw16} from binary modeling
\item Inaccuracy of for the 14 double-lined systems. We further adopt the masses and radii from \citet{gau16} for the four single-lined systems which were derived by combining the asteroseismic scaling relations
\item Measures of photometric variability (percentages) with the mass function and inclination from
\emph{Kepler} \citep{gau14}
\item Any caveats/updates/revisions eclipse modeling. The single-lined binaries' masses and radii have larger systematic uncertainties than their double-lined counterparts because the asteroseismic scaling relations are known to
past results
\end{itemize} overestimate mass by about 15\% on average for evolved stars \citep{gau16}.
%\subsection{KIC 8702921}
%\label{8702921ELC}
%An oscillating red giant To ensure consistent results between JKTEBOP and
faint M-type main sequence star comprise this RG/EB with ELC, we model a
short 19-d orbital period. This system defies the trend in \citet{gau14}, which suggests short-period RG/EBs are more likely to have weak or absent solar-like oscillations due to tidal effects. However, KIC 8702921 boasts the lowest-mass companion star representative subset of
known RG/EBs, which likely explains this discrepancy. It is also the only system RG/EBs using ELC with differential evolution Monte Carlo Markov Chain optimizers \citep[DE-MCMC,][]{ter06}. We find a full dynamic solution for
which we are unable to extract the radial velocity curve of the faint companion. PUT MASS AND RADIUS INFORMATION seven systems with 16 free parameters: LIST HERE.
%\subsection{KIC 9291629}
%\label{9291629ELC}
%This system has a similar orbital period to KIC 8702921, 21 days, but One of the
giant star does not show oscillations. The companion star subset is a
F-type main sequence star, single-lined binary, and
we fit the
system shows less out-of-eclipse variability than KIC 8702921. PUT MASS AND RADIUS INFORMATION HERE.
%\subsection{KIC 3955867}
%\label{3955867ELC}
%This system has a relatively short 34-d orbital period and is composed same 16 free parameters but note that the mass ratio, component masses, scale of
a non-oscillating red giant the system, and
an F-type main sequence star. PUT MASS AND RADIUS INFORMATION HERE.
%\subsection{KIC 4569590}
%\label{4569590ELC}
%KIC 4569590 component radii are unconstrained. Each ELC optimization run is
similar continued long enough to
KIC 3955867. It is composed of a non-oscillating red giant compute more than 400,000 models and
an F-type main sequence star with achieve a
41-d orbital period. PUT MASS AND RADIUS INFORMATION HERE.
%\subsection{KIC 10001167}
%\label{10001167ELC}
%An oscillating red giant robust global solution. In all cases, the stellar masses and
F-type main sequence star comprise this binary radii agree within ONE OR TWO?? sigma with
a relatively long orbital period, 120 days. PUT MASS AND RADIUS INFORMATION HERE.
%\subsection{KIC 9246715}
%\label{9246715ELC}
%This double red giant eclipsing binary has a 171-d orbital period. It was fully characterized in \citet{raw16}, which found $M_1 = 2.171\substack{+0.006\\-0.008} \ M_{\odot}$, $R_1 = 8.37\substack{+0.03\\-0.07} \ R_{\odot}$; $M_2 = 2.149\substack{+0.006\\-0.008} \ M_{\odot}$, $R_2 = 8.30\substack{+0.04\\-0.03} \ R_{\odot}$. The two stars are very nearly twins on those from \citet{gau16}. We present all the
secondary red clump, yet only one shows clear oscillations (almost certainly the slightly less massive star). See \citet{raw16} for a full discussion of how this system's properties were measured masses and
the marginal detection of a second set of oscillations.
%\subsection{KIC 9970396}
%\label{9970396ELC}
%KIC 9970396 has a long 235-d orbital period radii in Table \ref{table:mrcompare} and
is composed show the consistency of
an oscillating red giant and an F-type main sequence companion star. PUT MASS AND RADIUS INFORMATION HERE. the two binary modeling techniques in Figure \ref{fig:mrcompare}.
% put table and figure here
