5,534 research outputs found
Effects of moderate abundance changes on the atmospheric structure and colours of Mira variables (Research Note)
Aims. We study the effects of moderate deviations from solar abundances upon
the atmospheric structure and colours of typical Mira variables. Methods. We
present two model series of dynamical opacity-sampling models of Mira variables
which have (1) 1 solar metallicity 3 and (2) "mild" S-type C/O abundance ratio
([C/O]=0.9) with typical Zr enhancement (solar +1.0). These series are compared
to a previously studied solar-abundance series which has similar fundamental
parameters (mass, luminosity, period, radius) that are close to those of o Cet.
Results. Both series show noticeable effects of abundance upon stratifications
and infrared colours but cycle-to-cycle differences mask these effects at most
pulsation phases, with the exception of a narrow-water-filter colour near
minimum phase.Comment: 4 pages, 3 figures, accepted for A&
Oscillatory convective modes in red giants: a possible explanation of the long secondary periods
We discuss properties of oscillatory convective modes in low-mass red giants,
and compare them with observed properties of the long secondary periods (LSPs)
of semi-regular red giant variables. Oscillatory convective modes are very
nonadiabatic g modes and they are present in luminous stars, such as red
giants with \log L/{\rm L}_\odot \ga 3. Finite amplitudes for these modes are
confined to the outermost nonadiabatic layers, where the radiative energy flux
is more important than the convective energy flux. The periods of oscillatory
convection modes increase with luminosity, and the growth times are comparable
to the oscillation periods. The LSPs of red giants in the Large Magellanic
Cloud (LMC) are observed to lie on a distinct period-luminosity sequence called
sequence D. This sequence D period-luminosity relation is roughly consistent
with the predictions for dipole oscillatory convective modes in AGB models if
we adopt a mixing length of 1.2 pressure scale height ().
However, the effective temperature of the red-giant sequence of the LMC is
consistent to models with , which predict periods too short by a
factor of two.Comment: 7 pages, 6 figures, accepted for publication in MNRA
Ultra-Low Amplitude Cepheids in the Large Magellanic Cloud
The MACHO variables of LMC Field 77 that lie in the vicinity of the Cepheid
instability strip are reexamined. Among the 144 variables that we identify as
Cepheids we find 14 that have Fourier amplitudes <0.05 mag in the MACHO red
band, of which 7 have an amplitude <0.006 mag : we dub the latter group of
stars ultra-low amplitude (ULA) Cepheids. The variability of these objects is
verified by a comparison of the MACHO red with the MACHO blue lightcurves and
with those of the corresponding OGLE LMC stars. The occurrence of ULA Cepheids
is in agreement with theory. We have also discovered 2 low amplitude variables
whose periods are about a factor of 5--6 smaller than those of F Cepheids of
equal apparent magnitude. We suggest that these objects are Cepheids undergoing
pulsations in a surface mode and that they belong to a novel class of Strange
Cepheids (or Surface Mode Cepheids) whose existence was predicted by Buchler et
al. (1997).Comment: 4 pages, 5 figures, slightly revised, to appear in ApJ Letter
The Mira-based distance to the Galactic centre
Mira variables are useful distance indicators, due to their high luminosities
and well-defined period-luminosity relation. We select 1863 Miras from SAAO and
MACHO observations to examine their use as distance estimators in the Milky
Way. We measure a distance to the Galactic centre of kpc,
which is in good agreement with other literature values. The uncertainty has
two components of 0.2 kpc each: the first is from our analysis and
predominantly due to interstellar extinction, the second is due to zero-point
uncertainties extrinsic to our investigation, such as the distance to the Large
Magellanic Cloud (LMC). In an attempt to improve existing period-luminosity
calibrations, we use theoretical models of Miras to determine the dependence of
the period-luminosity relation on age, metallicity, and helium abundance, under
the assumption that Miras trace the bulk stellar population. We find that at a
fixed period of , changes in the predicted magnitudes can
be approximated by , and these coefficients are
nearly independent of period. The expected overestimate in the Galactic centre
distance from using an LMC-calibrated relation is 0.3 kpc. This
prediction is not validated by our analysis; a few possible reasons are
discussed. We separately show that while the predicted color-color diagrams of
solar-neighbourhood Miras work well in the near-infrared, though there are
offsets from the model predictions in the optical and mid-infrared.Comment: Accepted for publication in The Astrophysical Journal. 16 pages, 8
figures, 6 table
Semiregular variables with periods lying between the period-luminosity sequences C', C, and D
We analyze the distribution of semiregular variables and Mira stars in the period-luminosity plane. Our sample consists of 6169 oxygen-rich long-period variables in the Large Magellanic Cloud included in the OGLE-III Catalog of Variable Stars. There are many stars with periods that lie between the well-known sequences C and C′. Most of these stars are multi-periodic and the period ratios suggest that these stars oscillate in the same mode as the sequence C stars. Models suggest that this mode is the fundamental radial pulsation mode. The stars with primary periods between sequences C and C′ preferentially lie on an additional sequence (named F), and a large fraction of these stars also have long secondary periods (LSPs) that lie between sequences C and D. There are also a small number of stars with primary periods lying between sequences C and D. The origin of this long-period variability is unknown, as is the cause of sequence D variability. In addition, the origin of sequence F is unknown but we speculate that sequence F variability may be excited by the same phenomenon that causes the LSPs
A new interpretation of the period-luminosity sequences of long-period variables
Period-luminosity (PL) sequences of long period variables (LPVs) are commonly
interpreted as different pulsation modes, but there is disagreement on the
modal assignment. Here, we re-examine the observed PL sequences in the Large
Magellanic Cloud, including the sequence of long secondary periods (LSPs), and
their associated pulsation modes. Firstly, we theoretically model the sequences
using linear, radial, non-adiabatic pulsation models and a population synthesis
model of the LMC red giants. Then, we use a semi-empirical approach to assign
modes to the pulsation sequences by exploiting observed multi-mode pulsators.
As a result of the combined approaches, we consistently find that sequences B
and C both correspond to first overtone pulsation, although there
are some fundamental mode pulsators at low luminosities on both sequences. The
masses of these fundamental mode pulsators are larger at a given luminosity
than the mass of the first overtone pulsators. These two sequences B and
C are separated by a small period interval in which large amplitude
pulsation in a long secondary period (sequence D variability) occurs, meaning
that the first overtone pulsation is not seen as the primary mode of pulsation.
Observationally, this leads to the splitting of the first overtone pulsation
sequence into the two observed sequences B and C. Our two
independent examinations also show that sequences A, A and C
correspond to third overtone, second overtone and fundamental mode pulsation,
respectively.Comment: 10 pages, 7 figures, accepted for publication in Ap
Modulations in Multi-Periodic Blue Variables in the LMC
As shown by Mennickent, et al(2003), a subset of the blue variable stars in
the Large Magellanic Cloud exhibit brightness variability of small amplitude in
the period range 2.4 to 16 days as well as larger amplitude variability with
periods of 140 to 600 days, with a remarkably tight relation between the long
and the short periods. Our re-examination of these objects has led to the
discovery of additional variability. The Fourier spectra of 11 of their 30
objects have 3 or 4 peaks above the noise level and a linear relation of the
form f_a = 2(f_b - f_L) among three of the frequencies. An explanation of this
relation requires an interplay between the binary motion and that of a third
object. The two frequency relations together with the Fourier amplitude ratios
pose a challenging modeling problem.Comment: 4 pages, 3 figures, Astrophysical Journal (in press
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Measured Water Temperature Characteristics in a Pipeline Distribution System
YesThis paper describes the design, development, deployment and performance assessment of a
prototype system for monitoring the 'health' of a water distribution network based on the
temperature distribution and time-dependent variations in temperature across the network. It
has been found that the water temperature can reveal unusual events in a water distribution
network, indicated by dynamic variations in spatial temperature differential. Based on this
indication it is shown how patterns of changes in the water temperature can be analysed using
AQUIS pipeline distribution software and used in conjunction with hydraulic (e.g. flow and
pressure) sensors to indicate the state of ¿health¿ of the network during operation
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