35 research outputs found
Updated High-Temperature Opacities for the Dartmouth Stellar Evolution Program and their Effect on the Jao Gap Location
The Jao Gap, a 17 percent decrease in stellar density at
identified in both Gaia DR2 and EDR3 data, presents a new method to probe the
interior structure of stars near the fully convective transition mass. The Gap
is believed to originate from convective kissing instability wherein asymmetric
production of He causes the core convective zone of a star to
periodically expand and contract and consequently the stars' luminosity to
vary. Modeling of the Gap has revealed a sensitivity in its magnitude to a
population's metallicity primarily through opacity. Thus far, models of the Jao
Gap have relied on OPAL high-temperature radiative opacities. Here we present
updated synthetic population models tracing the Gap location modeled with the
Dartmouth stellar evolution code using the OPLIB high-temperature radiative
opacities. Use of these updated opacities changes the predicted location of the
Jao Gap by mag as compared to models which use the OPAL opacities.
This difference is likely too small to be detectable in empirical data.Comment: 15 pages, 13 figures; Accepted for publication in The Astrophysical
Journa
The impact of pollution on stellar evolution models
An approach is introduced for incorporating the concept of stellar pollution
into stellar evolution models. The approach involves enhancing the metal
content of the surface layers of stellar models. In addition, the surface
layers of stars in the mass range of 0.5-2.0 Solar masses are mixed to an
artificial depth motivated by observations of lithium abundance. The behavior
of polluted stellar evolution models is explored assuming the pollution occurs
after the star has left the fully convective pre main sequence phase. Stellar
models polluted with a few Earth masses of iron are significantly hotter than
stars of the same mass with an equivalent bulk metallicity. Polluted stellar
evolution models can successfully reproduce the metal-rich, parent star tau
Bootis and suggest a slightly lower mass than standard evolution models.
Finally, the possibility that stars in the Hyades open cluster have accreted an
average of 0.5 Earth masses of iron is explored. The results indicate that it
is not possible to rule out stellar pollution on this scale from the scatter of
Hyades stars on a color-magnitude diagram. The small amount of scatter in the
observational data set does rule out pollution on the order of 1.5 Earth masses
of iron. Pollution effects at the low level of 0.5 Earth masses of iron do not
produce substantial changes in a star's evolution.Comment: 14 pages, 3 figures, AASTeX, to appear in the 10/10/03 issue of Ap
From Canonical to Enhanced Extra Mixing in Low-Mass Red Giants: Tidally Locked Binaries
Stellar models which incorporate simple diffusion or shear induced mixing are
used to describe canonical extra mixing in low mass red giants of low and solar
metallicity. These models are able to simultaneously explain the observed Li
and CN abundance changes along upper red giant branch (RGB) in field
low-metallicity stars and match photometry, rotation and carbon isotopic ratios
for stars in the old open cluster M67. The shear mixing model requires that
main sequence (MS) progenitors of upper RGB stars possessed rapidly rotating
radiative cores and that specific angular momentum was conserved in each of
their mass shells during their evolution. We surmise that solar-type stars will
not experience canonical extra mixing on the RGB because their more efficient
MS spin-down resulted in solid-body rotation, as revealed by helioseismological
data for the Sun. Thus, RGB stars in the old, high metallicity cluster NGC 6791
should show no evidence for mixing in their carbon isotopic ratios.
We develop the idea that canonical extra mixing in a giant component of a
binary system may be switched to its enhanced mode with much faster and
somewhat deeper mixing as a result of the giant's tidal spin-up. This scenario
can explain photometric and composition peculiarities of RS CVn binaries. The
tidally enforced enhanced extra mixing might contribute to the star-to-star
abundance variations of O, Na and Al in globular clusters. This idea may be
tested with observations of carbon isotopic ratios and CN abundances in RS CVn
binaries.Comment: 47 pages, 19 figures, accepted for publication in Ap
UBVI CCD Photometry of the Old Open Cluster Berkeley 17
Photometric UBVI CCD photometry is presented for NGC 188 and Berkeley 17.
Color-magnitude diagrams (CMDs) are constructed and reach well past the
main-sequence turn-off for both clusters. Cluster ages are determined by means
of isochrone fitting to the cluster CMDs. These fits are constrained to agree
with spectroscopic metallicity and reddening estimates. Cluster ages are
determined to be 7.0+/-0.5 Gyr for NGC 188, and 10.0+/- 1.0 Gyr for Berkeley
17, where the errors refer to uncertainties in the relative age determinations.
These ages are compared to the ages of relatively metal-rich inner halo/thick
disk globular clusters and other old open clusters. Berkeley 17 and NGC 6791
are the oldest open clusters with an age of 10 Gyr. They are 2 Gyr younger than
the thick disk globular clusters. These results confirm the status of Berkeley
17 as one of the oldest known open cluster in the Milky Way, and its age
provides a lower limit to the age of the Galactic disk.Comment: to appear in AJ; 28 pages, 9 figure
The RR Lyrae variables and Horizontal Branch of NGC6656 (M22)
The first calibrated broadband UBVI time-series photometry is presented for
the RR Lyrae variable stars in NGC6656 (M22), with observations spanning a
range of twenty-two years. We have also redetermined the variability types and
periods for the RR Lyrae stars identified previously by photographic
observations, revising the number of fundamental-mode RR Lyrae variables (RR0)
to 10 and the number of first-overtone variables (RR1) to 16. The mean periods
of the RR0 and RR1 variables are _{RR0}=0.66 \pm 0.02 d and _{RR1}=0.33
\pm 0.01 d, respectively, supporting an Oosterhoff II classification for the
cluster. The number ratio of RR1- to all RR-type variables is N_1/N_{RR}=0.61,
also consistent with an Oosterhoff II designation. Both the RR Lyrae stars'
minimum light colors and the blue edge of the RR Lyrae instability strip
suggest E(B-V)=0.36 \pm 0.02 mag toward M22. Regarding the HB morphology of
M22, we find (B-R)/(B+V+R)=+0.97 \pm 0.1 and at least one "gap" located in an
unusual part of the blue HB, in the middle of the so-called hot HB stars.Comment: accepted to A
STELLAR POPULATION MODELS AND INDIVIDUAL ELEMENT ABUNDANCES. II. STELLAR SPECTRA AND INTEGRATED LIGHT MODELS
ABSTRACT The first paper in this series explored the effects of altering the chemical mixture of the stellar population on an element-by-element basis on stellar evolutionary tracks and isochrones to the end of the red giant branch. This paper extends the discussion by incorporating the fully consistent synthetic stellar spectra with those isochrone models in predicting integrated colors, Lick indices, and synthetic spectra. Older populations display element ratio effects in their spectra at higher amplitude than younger populations. In addition, spectral effects in the photospheres of stars tend to dominate over effects from isochrone temperatures and lifetimes, but, further, the isochrone-based effects that are present tend to fall along the age-metallicity degeneracy vector, while the direct stellar spectral effects usually show considerable orthogonality
The ACS Survey of Galactic Globular Clusters. I. Overview and Clusters Without Previous HST Photometry
We present the first results of a large ACS Survey of Galactic globular
clusters. This Hubble Space Telescope (HST) Treasury project is designed to
obtain photometry with S/N > ~10 for main sequence stars with masses > ~0.2Msun
in a sample of globulars using the Advanced Camera for Surveys (ACS) Wide Field
Channel. Here we focus on clusters without previous HST imaging data. These
include NGC 5466, 6779, 5053, 6144, Palomar 2, E 3, Lynga 7, Palomar 1, and NGC
6366. Our CMDs extend reliably from the horizontal branch to as much as seven
magnitudes fainter than the main sequence turnoff and represent the deepest
CMDs published to-date for these clusters. Using fiducial sequences for three
standard clusters (M92, NGC 6752, and 47 Tuc) with well-known metallicities and
distances, we perform main sequence fitting on the target clusters in order to
obtain estimates of their distances and reddenings. These comparisons along
with fitting the cluster main sequences to theoretical isochrones yield ages
for the target clusters. We find that the majority of the clusters have ages
that are consistent with the standard clusters at their metallicities. The
exceptions are E 3 which appears ~2 Gyr younger than 47 Tuc, and Pal 1, which
could be as much as 8 Gyr younger than 47 Tuc.Comment: 22 pages, 29 figures, accepted for publication in The Astronomical
Journal, April 2007. High resolution version available at
http://www.astro.ufl.edu/~ata/GC_Treasury/Web_Page/publications.htm