We have analysed the ISO-SWS spectrum of Jupiter in the 12-16 micron range, where several hydrocarbons exhibit rovibrational bands. Using temperature information from the methane and hydrogen ...emissions, we derive the mixing ratios (q) of acetylene and ethane at two independent pressure levels. For acetylene, we find \(q=(8.9^{+1.1}_{-0.6})\times10^{-7}\) at 0.3 mbar and \(q=(1.1^{+0.2}_{-0.1})\times10^{-7}\) at 4 mbar, giving a slope \(-d\ln q / d\ln P=0.8\pm0.1\), while for ethane \(q=(1.0\pm0.2)\times10^{-5}\) at 1 mbar and \(q=(2.6^{+0.5}_{-0.6})\times10^{-6}\) at 10 mbar, giving \(-d\ln q / d\ln P=0.6\pm0.2\). The ethane slope is consistent with the predictions of Gladstone et al. (1996), but that predicted for acetylene is larger than we observe. This disagreement is best explained by an overestimation of the acetylene production rate compared to that of ethane in the Gladstone et al. (1996) model. At 15.8 micron, methylacetylene is detected for the first time at low jovian latitudes, and a stratospheric column density of \((1.5\pm0.4)\times10^{15}\) molecule.cm-2 is inferred. We also derive an upper limit for the diacetylene column density of \(7\times10^{13}\) molecule.cm-2.
Extrasolar satellites are generally too small to be detected by nominal searches. By analogy to the most active body in the solar system, Io, we describe how sodium (Na i) and potassium (K i) gas ...could be a signature of the geological activity venting from an otherwise hidden exo-Io. Analyzing ∼a dozen close-in gas giants hosting robust alkaline detections, we show that an Io-sized satellite can be stable against orbital decay below a planetary tidal . This tidal energy is also focused into the satellite driving an ∼105 2 higher mass-loss rate than Io's supply to Jupiter's Na exosphere based on simple atmospheric loss estimates. The remarkable consequence is that several exo-Io column densities are, on average, more than sufficient to provide the ∼1010 1 Na cm−2 required by the equivalent width of exoplanet transmission spectra. Furthermore, the benchmark observations of both Jupiter's extended (∼1000 RJ) Na exosphere and Jupiter's atmosphere in transmission spectroscopy yield similar Na column densities that are purely exogenic in nature. As a proof of concept, we fit the "high-altitude" Na at WASP-49b with an ionization-limited cloud similar to the observed Na profile about Io. Moving forward, we strongly encourage time-dependent ingress and egress monitoring along with spectroscopic searches for other volcanic volatiles.
The standard in nipple reconstruction remains the autologous skin flap. Unfortunately, the results are not satisfying, with up to 75% loss of nipple projection over time. Existing studies ...investigated the use of primates as a source of implants. The authors hypothesized that the porcine nipple can serve as a perfect shape-supporting implant because of functional similarities to the human nipple. A decellularization protocol was developed to obtain an acellular nipple scaffold (ANS) for nipple reconstruction.
Tissue samples were collected from eight disease-free female Yorkshire pigs (60 to 70 kg) and then decellularized. The decellularization efficiency and extracellular matrix characterization was performed histologically and quantitatively (DNA, total collagen, elastin, and glycosaminoglycan content). In vitro and in vivo biocompatibility was determined by human dermal fibroblast culture and subcutaneous implantation of six ANSs in a single Yorkshire pig (60 to 70 kg), respectively. Inflammation and adverse events were monitored daily based on local clinical signs.
The authors showed that all cellular structures and 96% of DNA 321.7 ± 57.6 ng DNA/mg wet tissue versus 11.7 ± 10.9 ng DNA/mg wet tissue, in native and ANS, respectively ( P < 0.001) can be successfully removed. However, this was associated with a decrease in collagen 89.0 ± 11.4 and 58.8 ± 9.6 μg collagen/mg ( P < 0.001) and elastin 14.2 ± 1.6 and 7.9 ± 2.4 μg elastin/mg ( P < 0.05) and an increase in glycosaminoglycan content 5.0 ± 0.7 and 6.0 ± 0.8 ng/mg ( P < 0.05). ANS can support continuous cell growth in vitro and during preliminary biocompatibility tests in vivo.
This is a preliminary report of a novel promising ANS for nipple reconstruction, but more research is needed to validate results.
Breast cancer is very common among women. Treatment involves mastectomy, but its consequences affect patient mental well-being, and can lead to depression. Nipple-areola complex reconstruction is critical, and existing methods lead to unsatisfactory outcomes.
Spectroscopic observations of comet Hale-Boppwere undertaken near perihelion at millimetre wavelengths with the Institut de Radioastronomie Millimetrique (IRAM) telescopes at Plateau de Bure ...(France)and Pico Veleta (Spain). They resulted in the first detections of HCOOH,SO sub(2) , NH sub(2) CHO and HCOOCH sub(3) in a comet. HDO was detected through its3 sub(12) -2 sub(21) line at 225.897 GHz,complementing the observation of the 1 sub(01) -0 sub(00) line at 464.925 GHz at the James Clerk Maxwell Telescope (Meier et al., 1998,Science 279, 842).Several unidentified lines are present in the spectra. Observations of HC sub(3) N, HNCO, OCS, SO, CN, CO sub(+) , HCO sub(+) , in addition to more 'classical'species CO, HCN, HNC, CH sub(3) CN, CH sub(3) OH, H sub(2) CO, CS and H sub(2) S (Biveret al., this issue) permit us to make out an extensive inventory of the composition of the coma of comet Hale-Bopp at its perihelion. It presents strong analogies with gas-phase abundances measured in interstellar hot cores and bipolar flows, which are believed to reflect the composition of interstellar grains.
We review lattice results related to pion, kaon,
D
- and
B
-meson physics with the aim of making them easily accessible to the particle-physics community. More specifically, we report on the ...determination of the light-quark masses, the form factor
f
+
(
0
)
, arising in semileptonic
K
→
π
transition at zero momentum transfer, as well as the decay-constant ratio
f
K
/
f
π
of decay constants and its consequences for the CKM matrix elements
V
u
s
and
V
u
d
. Furthermore, we describe the results obtained on the lattice for some of the low-energy constants of
SU
(
2
)
L
×
SU
(
2
)
R
and
SU
(
3
)
L
×
SU
(
3
)
R
Chiral Perturbation Theory and review the determination of the
B
K
parameter of neutral kaon mixing. The inclusion of heavy-quark quantities significantly expands the FLAG scope with respect to the previous review. Therefore, we focus here on
D
- and
B
-meson decay constants, form factors, and mixing parameters, since these are most relevant for the determination of CKM matrix elements and the global CKM unitarity-triangle fit. In addition we review the status of lattice determinations of the strong coupling constant
α
s
.
Blood perfusion quality of a flap is the main prognostic factor for success. Microvascular evaluation remains mostly inaccessible. We aimed to evaluate the microflow imaging mode, MV-Flow, in ...assessing flap microvascularization in a pig model of the fascio-cutaneous flap.
On five pigs, bilateral saphenous fascio-cutaneous flaps were procured on the superficial femoral vessels. A conventional ultrasound evaluation in pulsed Doppler and color Doppler was conducted on the ten flaps allowing for the calculation of the saphenous artery flow rate. The MV-Flow mode was then applied: for qualitative analysis, with identification of saphenous artery collaterals; then quantitative, with repeated measurements of the Vascularity Index (VI), percentage of pixels where flow is detected relative to the total ultrasound view area. The measurements were then repeated after increasing arterial flow by clamping the distal femoral artery.
The MV-Flow mode allowed a better follow-up of the saphenous artery's collaterals and detected microflows not seen with the color Doppler. The VI was correlated to the saphenous artery flow rate (Spearman rho of 0.64;
= 0.002) and allowed to monitor the flap perfusion variations.
Ultrasound imaging of microvascularization by MV-Flow mode and its quantification by VI provides valuable information in evaluating the microvascularization of flaps.
We review the present status of the Standard Model calculation of the anomalous magnetic moment of the muon. This is performed in a perturbative expansion in the fine-structure constant α and is ...broken down into pure QED, electroweak, and hadronic contributions. The pure QED contribution is by far the largest and has been evaluated up to and including O(α5) with negligible numerical uncertainty. The electroweak contribution is suppressed by (mμ∕MW)2 and only shows up at the level of the seventh significant digit. It has been evaluated up to two loops and is known to better than one percent. Hadronic contributions are the most difficult to calculate and are responsible for almost all of the theoretical uncertainty. The leading hadronic contribution appears at O(α2) and is due to hadronic vacuum polarization, whereas at O(α3) the hadronic light-by-light scattering contribution appears. Given the low characteristic scale of this observable, these contributions have to be calculated with nonperturbative methods, in particular, dispersion relations and the lattice approach to QCD. The largest part of this review is dedicated to a detailed account of recent efforts to improve the calculation of these two contributions with either a data-driven, dispersive approach, or a first-principle, lattice-QCD approach. The final result reads aμSM=116591810(43)×10−11 and is smaller than the Brookhaven measurement by 3.7σ. The experimental uncertainty will soon be reduced by up to a factor four by the new experiment currently running at Fermilab, and also by the future J-PARC experiment. This and the prospects to further reduce the theoretical uncertainty in the near future – which are also discussed here – make this quantity one of the most promising places to look for evidence of new physics.
Spectra of comet C/1995 O1 (Hale-Bopp) were obtained with the Infrared Space Observatory (ISO) at medium resolution with the grating spectrometer in the photometer (PHT-S) and/or at high resolution ...with the short wavelength spectrometer (SWS) and long wavelength spectrometer (LWS) in April 1996 (Crovisier et al., 1996), September-October 1996 (Crovisier et al., 1997a, b) and December 1997, at distances from the Sun of 4.6, 2.9 and 3.9 AU, respectively. For the first time, high-resolution spectra of a comet covering the entire 2.4 to 200 km spectral range were obtained. The vibrational bands of H sub(2) O, CO sub(2) and CO are detected in emission with PHT-S. Relative production rates of 100:22:70 are derived for H sub(2) O:CO sub(2) :CO at 3 AU pre-perihelion. H sub(2) O is observed at high spectral resolution in the sub(3) group of bands around 2.7 km and the sub(2) group around 6 km with SWS, and in several rotational lines in the 100-180 km region with LWS. The high signal-to-noise ratio of the sub(3) band observed on September-October 1996 allows accurate determinations of the water rotational temperature (28 K) and of its ortho-to-para ratio(2.45 c 0.10, which significantly differs from the high temperature limit and corresponds to a spin temperature of 25 K). Longward of 6 km the spectrum is dominated by dust thermal continuum emission, upon which broad emission features are superimposed. The wavelengths of the emission peaks correspond to those of Mg-rich crystalline olivine (forsterite). In the September-October 1996 spectra, emission features at 45 and 65 km and possible absorption at 2.9-3.2 km suggest that grains of water ice were present at 3 AU from the Sun. The observations made post-perihelion in late December 1997 led to the detections of H sub(2) O, CO sub(2) and CO at 3.9 AU from the Sun (Figures 1 and 2). The production rates were -3.0 10 super(28) ,3.5 10 super(28) and -1.5 10 super(29) s super(-1) , respectively. This corresponds to H sub(2) O:CO sub(2) :CO = 100:110:500 and confirms that at such distances from the Sun, cometary activity is dominated by sublimation of CO and CO sub(2) rather than by H sub(2) O.
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