542 research outputs found
Gastrointestinal motility in the immediate postoperative period after intestinal transplantation, with special reference to acute rejection
Intestinal neuromuscular function after preservation and transplantation
While it is well known that prolonged preservation of the intestinal graft causes severe mucosal damage after transplantation, little is known about the effect on neuromuscular function. The entire small intestine of adult hound dogs was flushed and preserved with cold lactated Ringer's solution and autotransplanted either immediately (n = 6) or after 24 hr (n = 6). Animals undergoing sham operation (n = 4) were used as a control. Fasting motility and the response of the intestinal smooth muscle and enteric nerves to bethanechol (100 μg/kg/0.5 hr, iv) and cisapride (0.5 mg/kg, iv) were determined by a multiple strain gauge method on Postoperative Days 2, 4, 7, 14, 21, and 28. Compared to the control, immediately transplanted grafts and those preserved for 24 hr developed delayed reappearance of migrating myoelectric complexes (MMC), hypercontractile activity, and reduced response to bethanechol and cisapride administration. Animals in the preservation group developed more abnormal fasting motility after transplantation, but responses to bethanechol and cisapride stimulation were not markedly different from those of the immediate group. The reappearance of MMC occurred 3 weeks postoperatively in the preservation group compared to 2 days in the immediate group. The results of our study indicate that intestinal dysmotility is augmented in prolonged-preservation grafts compared to those with brief preservation. The dysmotility was transient and normalized 3 to 4 weeks after surgery. Preservation and reperfusion injury to the neuromuscular system of intestinal grafts are reversible and are attenuated by simple hypothermia
042 EFFECTIVENESS OF VIDEO-BASED HOME EXERCISE FOR OSTEOARTHRITIS OF THE KNEE: A RANDOMIZED CONTROLLED TRIAL
The naked planet Earth: Most essential pre-requisite for the origin and evolution of life
AbstractOur blue planet Earth has long been regarded to carry full of nutrients for hosting life since the birth of the planet. Here we speculate the processes that led to the birth of early life on Earth and its aftermath, finally leading to the evolution of metazoans. We evaluate: (1) the source of nutrients, (2) the chemistry of primordial ocean, (3) the initial mass of ocean, and (4) the size of planet. Among the life-building nutrients, phosphorus and potassium play a key role. Only three types of rocks can serve as an adequate source of nutrients: (a) continent-forming TTG (granite), enabling the evolution of primitive life to metazoans; (b) primordial continents carrying anorthosite with KREEP (Potassium, Rare Earth Elements, and Phosphorus) basalts, which is a key to bear life; (c) carbonatite magma, enriched in radiogenic elements such as U and Th, which can cause mutation to speed up evolution and promote the birth of new species in continental rift settings. The second important factor is ocean chemistry. The primordial ocean was extremely acidic (pH = 1–2) and enriched in halogens (Cl, F and others), S, N and metallic elements (Cd, Cu, Zn, and others), inhibiting the birth of life. Plate tectonics cleaned up these elements which interfered with RNA. Blue ocean finally appeared in the Phanerozoic with pH = 7 through extensive interaction with surface continental crust by weathering, erosion and transportation into ocean. The initial ocean mass was also important. The birth of life and aftermath of evolution was possible in the habitable zone with 3–5 km deep ocean which was able to supply sufficient nutrients. Without a huge landmass, nutrients cannot be supplied into the ocean only by ridge-hydrothermal circulation in the Hadean. Finally, the size of the planet plays a crucial role. Cooling of massive planets is less efficient than smaller ones, so that return-flow of seawater into mantle does not occur until central stars finish their main sequence. Due to the suitable size of Earth, the dawn of Phanerozoic witnessed the initiation of return-flow of seawater into the mantle, leading to the emergence of huge landmass above sea-level, and the distribution of nutrients on a global scale. Oxygen pump also played a critical role to keep high-PO2 in atmosphere since then, leading to the emergence of ozone layer and enabling animals and plants to invade the land.To satisfy the tight conditions to make the Earth habitable, the formation mechanism of primordial Earth is an important factor. At first, a ‘dry Earth’ must be made through giant impact, followed by magma ocean to float nutrient-enriched primordial continents (anorthosite + KREEP). Late bombardment from asteroid belt supplied water to make 3–5 km thick ocean, and not from icy meteorites from Kuiper belt beyond cool Jupiter. It was essential to meet the above conditions that enabled the Earth as a habitable planet with evolved life forms. The tight constraints that we evaluate for birth and evolution of life on Earth would provide important guidelines for planetary scientists hunting for life in the exo-solar planets
Long-term effect of jejunoileal autotransplantation on motility and transit time in canine small bowel
Development of a novel integrated iontophoresis electrode consisting of metallic and drug-loaded layers
On the Origin of HD149026b
The high density of the close-in extrasolar planet HD149026b suggests the
presence of a huge core in the planet, which challenges planet formation
theory. We first derive constraints on the amount of heavy elements and
hydrogen/helium present in the planet: We find that preferred values of the
core mass are between 50 and 80 M_E. We then investigate the possibility of
subcritical core accretion as envisioned for Uranus and Neptune and find that
the subcritical accretion scenario is unlikely in the case of HD149026b for at
least two reasons: (i) Subcritical planets are such that the ratio of their
core mass to their total mass is above ~0.7, in contradiction with constraints
for all but the most extreme interior models of HD149026b; (ii) High accretion
rates and large isolation mass required for the formation of a subcritical core
of 30 M_E are possible only at specific orbital distances in a disk with a
surface density of dust equal to at least 10 times that of the minimum mass
solar nebula. This value climbs to 30 when considering a 50 M_E core. These
facts point toward two main routes for the formation of this planet: (i) Gas
accretion that is limited by a slow viscous inflow of gas in an evaporating
disk; (ii) A significant modification of the composition of the planet after as
accretion has stopped. These two routes are not mutually exclusive.
Illustrating the second route, we show that for a wide range of impact
parameters, giant impacts lead to a loss of the gas component of the planet and
thus may lead to planets that are highly enriched in heavy elements. In the
giant impact scenario, we expect an outer giant planet to be present.
Observational studies by imaging, astrometry and long term interferometry of
this system are needed to better narrow down the ensemble of possibilities.Comment: 29 pages, 8 figures, to appear in the 10 October 2006 issue of Ap
Origin of the Different Architectures of the Jovian and Saturnian Satellite Systems
The Jovian regular satellite system mainly consists of four Galilean
satellites that have similar masses and are trapped in mutual mean motion
resonances except for the outer satellite, Callisto. On the other hand, the
Saturnian regular satellite system has only one big icy body, Titan, and a
population of much smaller icy moons. We have investigated the origin of these
major differences between the Jovian and Saturnian satellite systems by
semi-analytically simulating the growth and orbital migration of
proto-satellites in an accreting proto-satellite disk. We set up two different
disk evolution/structure models that correspond to Jovian and Saturnian
systems, by building upon previously developed models of an actively-supplied
proto-satellite disk, the formation of gas giants, and observations of young
stars. Our simulations extend previous models by including the (1) different
termination timescales of gas infall onto the proto-satellite disk and (2)
different evolution of a cavity in the disk, between the Jovian and Saturnian
systems. We have performed Monte Carlo simulations and show that in the case of
the Jovian systems, four to five similar-mass satellites are likely to remain
trapped in mean motion resonances. This orbital configuration is formed by type
I migration, temporal stopping of the migration near the disk inner edge, and
quick truncation of gas infall caused by Jupiter opening a gap in the Solar
nebula. The Saturnian systems tend to end up with one dominant body in the
outer regions caused by the slower decay of gas infall associated with global
depletion of the Solar nebula. The total mass and compositional zoning of the
predicted Jovian and Saturnian satellite systems are consistent with the
observed satellite systems.Comment: Accepted to ApJ, 33pages, 6figures, 2table
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