4,377 research outputs found
Modeling Convective Core Overshoot and Diffusion in Procyon Constrained by Asteroseismic Data
We compare evolved stellar models, which match Procyons mass and position in
the HR diagram, to current ground-based asteroseismic observations. Diffusion
of helium and metals along with two conventional core overshoot descriptions
and the Kuhfuss nonlocal theory of convection are considered. We establish that
one of the two published asteroseismic data reductions for Procyon, which
mainly differ in their identification of even versus odd l-values, is a
significantly more probable and self-consistent match to our models than the
other. The most probable models according to our Bayesian analysis have evolved
to just short of turnoff, still retaining a hydrogen convective core. Our most
probable models include Y and Z diffusion and have conventional core overshoot
between 0.9 and 1.5 pressure scale heights, which increases the outer radius of
the convective core by between 22% to 28%, respectively. We discuss the
significance of this comparatively higher than expected core overshoot amount
in terms of internal mixing during evolution. The parameters of our most
probable models are similar regardless of whether adiabatic or nonadiabatic
model p-mode frequencies are compared to the observations, although, the
Bayesian probabilities are greater when the nonadiabatic model frequencies are
used. All the most probable models (with or without core overshoot, adiabatic
or nonadiabatic model frequencies, diffusion or no diffusion, including priors
for the observed HRD location and mass or not) have masses that are within one
sigma of the observed mass 1.497+/-0.037 Msun
The Pulsation Properties of Procyon A
A grid of stellar evolution models for Procyon A has been calculated. These
models include the best physics available to us (including the latest opacities
and equation of state) and are based on the revised astrometric mass of Girard
et al (1996). Models were calculated with helium diffusion and with the
combined effects of helium and heavy element diffusion. Oscillation frequencies
for l=0,1,2 and 3 p-modes and the characteristic period spacing for the g-modes
were calculated for these models. We find that g-modes are sensitive to model
parameters which effect the structure of the core, such as convective core
overshoot, the heavy element abundance and the evolutionary state (main
sequence or shell hydrogen burning) of Procyon A. The p-modes are relatively
insensitive to the details of the physics used to model Procyon A, and only
depend on the evolutionary state of Procyon A. Hence, observations of p-mode
frequencies on Procyon A will serve as a robust test of stellar evolution
models.Comment: 4 pages, to appear in ApJ
On the detection of Lorentzian profiles in a power spectrum: A Bayesian approach using ignorance priors
Aims. Deriving accurate frequencies, amplitudes, and mode lifetimes from
stochastically driven pulsation is challenging, more so, if one demands that
realistic error estimates be given for all model fitting parameters. As has
been shown by other authors, the traditional method of fitting Lorentzian
profiles to the power spectrum of time-resolved photometric or spectroscopic
data via the Maximum Likelihood Estimation (MLE) procedure delivers good
approximations for these quantities. We, however, show that a conservative
Bayesian approach allows one to treat the detection of modes with minimal
assumptions (i.e., about the existence and identity of the modes).
Methods. We derive a conservative Bayesian treatment for the probability of
Lorentzian profiles being present in a power spectrum and describe an efficient
implementation that evaluates the probability density distribution of
parameters by using a Markov-Chain Monte Carlo (MCMC) technique.
Results. Potentially superior to "best-fit" procedure like MLE, which only
provides formal uncertainties, our method samples and approximates the actual
probability distributions for all parameters involved. Moreover, it avoids
shortcomings that make the MLE treatment susceptible to the built-in
assumptions of a model that is fitted to the data. This is especially relevant
when analyzing solar-type pulsation in stars other than the Sun where the
observations are of lower quality and can be over-interpreted. As an example,
we apply our technique to CoRoT observations of the solar-type pulsator HD
49933.Comment: 12 pages, 11 figures, accepted for publication in Astronomy and
Astrophysic
The nature of p-modes and granulation in HD 49933 observed by CoRoT
Context: Recent observations of HD49933 by the space-photometric mission
CoRoT provide photometric evidence of solar type oscillations in a star other
than our Sun. The first published reduction, analysis, and interpretation of
the CoRoT data yielded a spectrum of p-modes with l = 0, 1, and 2. Aims: We
present our own analysis of the CoRoT data in an attempt to compare the
detected pulsation modes with eigenfrequencies of models that are consistent
with the observed luminosity and surface temperature. Methods: We used the
Gruberbauer et al. frequency set derived based on a more conservative Bayesian
analysis with ignorance priors and fit models from a dense grid of model
spectra. We also introduce a Bayesian approach to searching and quantifying the
best model fits to the observed oscillation spectra. Results: We identify 26
frequencies as radial and dipolar modes. Our best fitting model has solar
composition and coincides within the error box with the spectroscopically
determined position of HD49933 in the H-R diagram. We also show that
lower-than-solar Z models have a lower probability of matching the observations
than the solar metallicity models. To quantify the effect of the deficiencies
in modeling the stellar surface layers in our analysis, we compare adiabatic
and nonadiabatic model fits and find that the latter reproduces the observed
frequencies better.Comment: accepted to be published in A&A, 9 pages, 5 figure
Thermodynamics of viscous dark energy in an RSII braneworld
We show that for an RSII braneworld filled with interacting viscous dark
energy and dark matter, one can always rewrite the Friedmann equation in the
form of the first law of thermodynamics, , at apparent horizon.
In addition, the generalized second law of thermodynamics can fulfilled in a
region enclosed by the apparent horizon on the brane for both constant and time
variable 5-dynamical Newton's constant . These results hold regardless of
the specific form of the dark energy. Our study further support that in an
accelerating universe with spatial curvature, the apparent horizon is a
physical boundary from the thermodynamical point of view.Comment: 11 page
The power of low-resolution spectroscopy: On the spectral classification of planet candidates in the ground-based CoRoT follow-up
Planetary transits detected by the CoRoT mission can be mimicked by a
low-mass star in orbit around a giant star. Spectral classification helps to
identify the giant stars and also early-type stars which are often excluded
from further follow-up.
We study the potential and the limitations of low-resolution spectroscopy to
improve the photometric spectral types of CoRoT candidates. In particular, we
want to study the influence of the signal-to-noise ratio (SNR) of the target
spectrum in a quantitative way. We built an own template library and
investigate whether a template library from the literature is able to reproduce
the classifications. Including previous photometric estimates, we show how the
additional spectroscopic information improves the constraints on spectral type.
Low-resolution spectroscopy (1000) of 42 CoRoT targets covering a
wide range in SNR (1-437) and of 149 templates was obtained in 2012-2013 with
the Nasmyth spectrograph at the Tautenburg 2m telescope. Spectral types have
been derived automatically by comparing with the observed template spectra. The
classification has been repeated with the external CFLIB library.
The spectral class obtained with the external library agrees within a few
sub-classes when the target spectrum has a SNR of about 100 at least. While the
photometric spectral type can deviate by an entire spectral class, the
photometric luminosity classification is as close as a spectroscopic
classification with the external library. A low SNR of the target spectrum
limits the attainable accuracy of classification more strongly than the use of
external templates or photometry. Furthermore we found that low-resolution
reconnaissance spectroscopy ensures that good planet candidates are kept that
would otherwise be discarded based on photometric spectral type alone.Comment: accepted for publication in Astronomische Nachrichten; 12 pages, 4
figures, 7 table
Toward a New Kind of Asteroseismic Grid Fitting
Recent developments in instrumentation (e.g., in particular the Kepler and
CoRoT satellites) provide a new opportunity to improve the models of stellar
pulsations. Surface layers, rotation, and magnetic fields imprint erratic
frequency shifts, trends, and other non-random behavior in the frequency
spectra. As our observational uncertainties become smaller, these are
increasingly important and difficult to deal with using standard fitting
techniques. To improve the models, new ways to compare their predictions with
observations need to be conceived. In this paper we present a completely
probabilistic (Bayesian) approach to asteroseismic model fitting. It allows for
varying degrees of prior mode identification, corrections for the discrete
nature of the grid, and most importantly implements a treatment of systematic
errors, such as the "surface effects." It removes the need to apply semi-
empirical corrections to the observations prior to fitting them to the models
and results in a consistent set of probabilities with which the model physics
can be probed and compared. As an example, we show a detailed asteroseismic
analysis of the Sun. We find a most probable solar age, including a 35 +- 5
million year pre-main sequence phase, of 4.591 billion years, and initial
element mass fractions of X_0 = 0.72, Y_0 = 0.264, Z_0 = 0.016, consistent with
recent asteroseismic and non-asteroseismic studies.Comment: 15 pages, 5 figures, accepted for publication in The Astrophysical
Journal; v2 contains minor changes made in the proofs (updated references &
corrected typos
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