1,266 research outputs found
Solubility isotope effects in aqueous solutions of methane
The isotope effect on the Henry's law coefficients of methane in
aqueous solution (H/D and C-12/C-13 substitution) are interpreted using
the statistical mechanical theory of condensed phase isotope effects.
The missing spectroscopic data needed for the implementation of the
theory were obtained either experimentally (infrared measurements), by
computer simulation (molecular dynamics technique), or estimated using
the Wilson's GF matrix method. The order of magnitude and sign of both
solute isotope effects can be predicted by the theory. Even a crude
estimation based on data from previous vapor pressure isotope effect
studies of pure methane at low temperature can explain the inverse
effect found for the solubility of deuterated methane in water. (C)
2002 American Institute of Physics
A Comprehensive Comparative Test of Seven Widely-Used Spectral Synthesis Models Against Multi-Band Photometry of Young Massive Star Clusters
We test the predictions of spectral synthesis models based on seven different
massive-star prescriptions against Legacy ExtraGalactic UV Survey (LEGUS)
observations of eight young massive clusters in two local galaxies, NGC 1566
and NGC 5253, chosen because predictions of all seven models are available at
the published galactic metallicities. The high angular resolution, extensive
cluster inventory and full near-ultraviolet to near-infrared photometric
coverage make the LEGUS dataset excellent for this study. We account for both
stellar and nebular emission in the models and try two different prescriptions
for attenuation by dust. From Bayesian fits of model libraries to the
observations, we find remarkably low dispersion in the median E(B-V) (~0.03
mag), stellar masses (~10^4 M_\odot) and ages (~1 Myr) derived for individual
clusters using different models, although maximum discrepancies in these
quantities can reach 0.09 mag and factors of 2.8 and 2.5, respectively. This is
for ranges in median properties of 0.05-0.54 mag, 1.8-10x10^4 M_\odot and
1.6-40 Myr spanned by the clusters in our sample. In terms of best fit, the
observations are slightly better reproduced by models with interacting binaries
and least well reproduced by models with single rotating stars. Our study
provides a first quantitative estimate of the accuracies and uncertainties of
the most recent spectral synthesis models of young stellar populations,
demonstrates the good progress of models in fitting high-quality observations,
and highlights the needs for a larger cluster sample and more extensive tests
of the model parameter space.Comment: Accepted for publication in MNRAS (14 Jan. 2016). 30 pages, 16
figures, 9 table
The VLT-FLAMES Tarantula Survey XXI. Stellar spin rates of O-type spectroscopic binaries
The initial distribution of spin rates of massive stars is a fingerprint of
their elusive formation process. It also sets a key initial condition for
stellar evolution and is thus an important ingredient in stellar population
synthesis. So far, most studies have focused on single stars. Most O stars are
however found in multiple systems. By establishing the spin-rate distribution
of a sizeable sample of O-type spectroscopic binaries and by comparing the
distributions of binary sub-populations with one another as well as with that
of presumed single stars in the same region, we aim to constrain the initial
spin distribution of O stars in binaries, and to identify signatures of the
physical mechanisms that affect the evolution of the massive stars spin rates.
We use ground-based optical spectroscopy obtained in the framework of the
VLT-FLAMES Tarantula Survey (VFTS) to establish the projected equatorial
rotational velocities (\vrot) for components of 114 spectroscopic binaries in
30 Doradus. The \vrot\ values are derived from the full-width at half-maximum
(FWHM) of a set of spectral lines, using a FWHM vs. \vrot\ calibration that we
derive based on previous line analysis methods applied to single O-type stars
in the VFTS sample. The overall \vrot\ distribution of the primary stars
resembles that of single O-type stars in the VFTS, featuring a low-velocity
peak (at \vrot < 200 kms) and a shoulder at intermediate velocities (200 <
\vrot < 300 kms). The distributions of binaries and single stars however
differ in two ways. First, the main peak at \vrot \sim100 kms is broader and
slightly shifted toward higher spin rates in the binary distribution compared
to that of the presumed-single stars. Second, the \vrot distribution of
primaries lacks a significant population of stars spinning faster than 300 kms
while such a population is clearly present in the single star sample.Comment: 16 pages, 16 figures, paper accepted in Astronomy & Astrophysic
Searching for compact objects in the single-lined spectroscopic binaries of the young Galactic cluster NGC 6231
Recent evolutionary computations predict that a few percent of massive OB
stars in binary systems should have a dormant BH companion. Despite several
reported X-ray quiet OB+BH systems over the last couple of years, finding them
with certainty remains challenging. These have great importance as they can be
gravitational wave (GW) source progenitors, and are landmark systems in
constraining supernova kick physics. This work aims to characterise the hidden
companions to the single-lined spectroscopic binaries (SB1s) in the B star
population of the young open Galactic cluster NGC 6231 to find candidate
systems for harbouring compact object companions. With the orbital solutions
for each SB1 previously constrained, we applied Fourier spectral disentangling
to multi-epoch optical VLT/FLAMES spectra of each target to extract a potential
signature of a faint companion, and to identify newly disentangled double-lined
spectroscopic binaries (SB2s). For targets where the disentangling does not
reveal any signature of a stellar companion, we performed atmospheric and
evolutionary modelling on the primary to obtain constraints on the unseen
companion. Seven newly classified SB2 systems with mass ratios down to near 0.1
were identified. From the remaining targets, for which no faint companion could
be extracted from the spectra, four are found to have companion masses in the
predicted mass ranges of neutron stars (NSes) and BHes. Two of these have
companion masses between 1 and 3.5 , making them potential hosts of
NSes (or lower mass main sequence stars). The other two are between 2.5 to 8
and 1.6 and 26 , respectively, and so are identified as
candidates for harbouring BH companions. However, unambiguous identification of
these systems as X-ray quiet compact object harbouring binaries requires follow
up observations.Comment: Submitted to A&
Poly-MTO, {(CH_3)_{0.92} Re O_3}_\infty, a Conducting Two-Dimensional Organometallic Oxide
Polymeric methyltrioxorhenium, {(CH_{3})_{0.92}ReO_{3}}_{\infty} (poly-MTO),
is the first member of a new class of organometallic hybrids which adopts the
structural pattern and physical properties of classical perovskites in two
dimensions (2D). We demonstrate how the electronic structure of poly-MTO can be
tailored by intercalation of organic donor molecules, such as
tetrathiafulvalene (TTF) or bis-(ethylendithio)-tetrathiafulvalene (BEDT-TTF),
and by the inorganic acceptor SbF. Integration of donor molecules leads to
a more insulating behavior of poly-MTO, whereas SbF insertion does not
cause any significant change in the resistivity. The resistivity data of pure
poly-MTO is remarkably well described by a two-dimensional electron system.
Below 38 K an unusual resistivity behavior, similar to that found in doped
cuprates, is observed: The resistivity initially increases approximately as
ln) before it changes into a dependence below 2 K.
As an explanation we suggest a crossover from purely two-dimensional
charge-carrier diffusion within the \{ReO\} planes at high
temperatures to three-dimensional diffusion at low temperatures in a
disorder-enhanced electron-electron interaction scenario (Altshuler-Aronov
correction). Furthermore, a linear positive magnetoresistance was found in the
insulating regime, which is caused by spatial localization of itinerant
electrons at some of the Re atoms, which formally adopt a electronic
configuration. X-ray diffraction, IR- and ESR-studies, temperature dependent
magnetization and specific heat measurements in various magnetic fields suggest
that the electronic structure of poly-MTO can safely be approximated by a
purely 2D conductor.Comment: 15 pages, 16 figures, 2 table
Rotational properties of the O-type star population in the Tarantula region
The 30 Doradus (30\,Dor) region in the Large Magellanic Cloud (also known as
the Tarantula Nebula) is the nearest massive starburst region, containing the
richest sample of massive stars in the Local Group. It is the best possible
laboratory to investigate aspects of the formation and evolution of massive
stars. Here, we focus on rotation which is a key parameter in the evolution of
these objects. We establish the projected rotational velocity, ,
distribution of an unprecedented sample of 216 radial velocity constant
() O-type stars in 30\,Dor observed in
the framework of the VLT-FLAMES Tarantula Survey (VFTS). The distribution of
shows a two-component structure: a peak around 80 and a high-velocity tail extending up to 600 .
Around 75% of the sample has 0 200
with the other 25% distributed in the high-velocity tail. The presence of the
low-velocity peak is consistent with that found in other studies of late-O and
early-B stars. The high-velocity tail is compatible with expectations from
binary interaction synthesis models and may be predominantly populated by
post-binary interaction, spun-up, objects and mergers. This may have important
implications for the nature of progenitors of long-duration gamma ray bursts.Comment: 4 pages, 1 figure. Conference proceedings article: Massive stars:
from alpha to Omega, 10-14 June 2013, Rhodes, Greec
Mid-to-Late M Dwarfs Lack Jupiter Analogs
Cold Jovian planets play an important role in sculpting the dynamical
environment in which inner terrestrial planets form. The core accretion model
predicts that giant planets cannot form around low-mass M dwarfs, although this
idea has been challenged by recent planet discoveries. Here, we investigate the
occurrence rate of giant planets around low-mass (0.1-0.3M) M dwarfs.
We monitor a volume-complete, inactive sample of 200 such stars located within
15 parsecs, collecting four high-resolution spectra of each M dwarf over six
years and performing intensive follow-up monitoring of two candidate
radial-velocity variables. We use TRES on the 1.5 m telescope at the Fred
Lawrence Whipple Observatory and CHIRON on the Cerro Tololo Inter-American
Observatory 1.5 m telescope for our primary campaign, and MAROON-X on Gemini
North for high-precision follow-up. We place a 95%-confidence upper limit of
1.5% (68%-confidence limit of 0.57%) on the occurrence of sin1M giant planets out to the water snow line and provide additional
constraints on the giant planet population as a function of sin
and period. Beyond the snow line ( K K), we place
95%-confidence upper limits of 1.5%, 1.7%, and 4.4% (68%-confidence limits of
0.58%, 0.66%, and 1.7%) for 3MsinM,
0.8MsinM, and 0.3MsinM giant planets; i.e., Jupiter analogs are rare around
low-mass M dwarfs. In contrast, surveys of Sun-like stars have found that their
giant planets are most common at these Jupiter-like instellations.Comment: Accepted for publication in AJ; 19 pages, 5 figures, 2 table
Quantum key distribution and 1 Gbit/s data encryption over a single fibre
We perform quantum key distribution (QKD) in the presence of 4 classical
channels in a C-band dense wavelength division multiplexing (DWDM)
configuration using a commercial QKD system. The classical channels are used
for key distillation and 1 Gbps encrypted communication, rendering the entire
system independent from any other communication channel than a single dedicated
fibre. We successfully distil secret keys over fibre spans of up to 50 km. The
separation between quantum channel and nearest classical channel is only 200
GHz, while the classical channels are all separated by 100 GHz. In addition to
that we discuss possible improvements and alternative configurations, for
instance whether it is advantageous to choose the quantum channel at 1310 nm or
to opt for a pure C-band configuration.Comment: 9 pages, 7 figure
Rotational velocities of single and binary O-type stars in the Tarantula Nebula
Rotation is a key parameter in the evolution of massive stars, affecting
their evolution, chemical yields, ionizing photon budget, and final fate. We
determined the projected rotational velocity, , of 330 O-type
objects, i.e. 210 spectroscopic single stars and 110 primaries in
binary systems, in the Tarantula nebula or 30 Doradus (30\,Dor) region. The
observations were taken using VLT/FLAMES and constitute the largest homogeneous
dataset of multi-epoch spectroscopy of O-type stars currently available. The
most distinctive feature of the distributions of the
presumed-single stars and primaries in 30 Dor is a low-velocity peak at around
100\,. Stellar winds are not expected to have spun-down the
bulk of the stars significantly since their arrival on the main sequence and
therefore the peak in the single star sample is likely to represent the outcome
of the formation process. Whereas the spin distribution of presumed-single
stars shows a well developed tail of stars rotating more rapidly than
300\,, the sample of primaries does not feature such a
high-velocity tail. The tail of the presumed-single star distribution is
attributed for the most part -- and could potentially be completely due -- to
spun-up binary products that appear as single stars or that have merged. This
would be consistent with the lack of such post-interaction products in the
binary sample, that is expected to be dominated by pre-interaction systems. The
peak in this distribution is broader and is shifted toward somewhat higher spin
rates compared to the distribution of presumed-single stars. Systems displaying
large radial velocity variations, typical for short period systems, appear
mostly responsible for these differences.Comment: 6 pages, 3 figures, Proceedings IAU Symposium No. 307, 2014, 'New
windows on massive stars: asteroseismology, interferometry, and
spectropolarimetry
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