255 research outputs found
NANOEMULSION AS A NOVEL OPHTHALMIC DELIVERY SYSTEM FOR ACETAZOLAMIDE
Objective: The aim of this work was to formulate the antiglaucoma drug acetazolamide as ocular nanoemulsion of high therapeutic efficacy and prolonged effect.
Methods: Eighteen nanoemulsion formulaions consisting of different oils, surfactants and cosurfactants at various ratios and constant water content (39%) were prepared based on their constructed pseudoternary-phase diagrams. According to the In vitro release studies, three nanoemulsions which exhibited fast drug release were used to prepare acetazolamide nanoemulsions with higher water content (59%). The six nanoemulsions at either water content (39 or 59%) were evaluated for their physicochemical properties and ex- vivo corneal permeability. In addition, Draize rabbit eye irritation test was performed. Moreover, biological evaluation of acetazolamide nanoemulsions for their intraocular pressure lowering activity on glaucomatous albino rabbits was carried out.
Results: Isopropyl myristate nanoemulsion prepared with cremophor EL and transcutol P exhibited the fastest drug release among all isopropyl myristate nanoemulsions. Oleic acid nanoemulsion prepared with mixture of tween 80 and cremophor EL as surfactants together with transcutol P showed the fastest drug release among other oleic acid nanoemulsion formulae. Similar results were also observed for peanut oil nanoemulsions. The above mentioned formulations either at 39% or 59% water content showed acceptable physicochemical properties and higher acetazolamide permeability coefficient through goat corneas than that reported for the free drug. They also were non irritant to rabbit eye. Therapeutic efficacy testing revealed that peanut oil nanoemulsion at 39% water content showed better and prolonged intraocular pressure lowering effect relative to either commercial brinzolamide eye drops (Azopt®) or the commercial oral acetazolamide tablet (Cidamex®).
Conclusion: Acetazolamide was successfully formulated in nanoemulsion form which revealed high therapeutic efficacy in treatment of glaucoma together with a prolonged effect
Propositional calculus for adjointness lattices
Recently, Morsi has developed a complete syntax for the class of all
adjointness algebras . There, is a partially ordered set with top element , is a
conjunction on for which is a left identity
element, and the two implication-like binary operations and on
are adjoints of .
In this paper, we extend that formal system to one for the class of
all 9-tuples , called \emph{%
adjointness lattices}; in each of which is a bounded lattice, and is an
adjointness algebra. We call it \emph{Propositional Calculus for Adjointness
Lattices}, abbreviated . Our axiom scheme for features four
inference rules and thirteen axioms. We deduce enough theorems and
inferences in to establish its completeness for ; by means of
a quotient-algebra structure (a Lindenbaum type of algebra). We study two
negation-like unary operations in an adjointness lattice, defined by means
of together with and . We end by developing complete syntax for
all adjointness lattices whose implications are -type implications
Eficiencia de la extracción asistida por ultrasonido de pétalos de Delonix regia como antioxidante natural en la estabilidad oxidativa del aceite de girasol
The possibility of improving the oxidative stability of sunflower oil by enriching it with carotenoids from Delonix regia petals was studied. A combination of ultrasound-assisted extraction and stirring techniques was used. The optimal conditions were material/solvent ratio of 1:20 (w/v), ultrasonic power of 30 W and extraction time of 50 min. Under these conditions, the yield of total carotenoids was 503.0 μg/g dry weight. Increasing the acoustic power density degraded carotenoids. A HPLC analysis was used for the quantification of β-carotene in the extract. The DPPH radical scavenging activity and ferric reducing antioxidant power of the carotenoid-rich extract were found to be superior to the standard Butylated hydroxyl toluene (BHT). The enrichment of sunflower oil with carotenoid-rich extract at 67.46 mg carotenoids/kg oil improved its oxidative stability by more than 50% as measured by the Rancimat method. These results suggest that the investigated extract has the potential to be used as a bio-preservative in food products.Se estudió la posibilidad de mejorar la estabilidad oxidativa del aceite de girasol enriqueciéndolo con carotenoides de pétalos de Delonix regia. Se utilizaron técnicas combinadas de extracción asistida por ultrasonido y técnicas de agitación. Las condiciones óptimas fueron una relación material/ disolvente de 1:20 (p/v), una potencia ultrasónica de 30 W y un tiempo de extracción de 50 min. En estas condiciones, el rendimiento de carotenoides totales fue de 503,0 ?g/g de peso seco. El aumento de la densidad de potencia acústica degrada a los carotenoides. El análisis por HPLC se utilizó para la cuantificación de β-caroteno en el extracto. Se encontró que la actividad de captación de radicales DPPH y el poder antioxidante reductor férrico del extracto rico en carotenoides es superior al del butilhidroxitolueno estándar (BHT). El enriquecimiento de aceite de girasol con extracto rico en carotenoides a 67,46 mg de carotenoides/kg de aceite mejoró su estabilidad oxidativa en más del 50% según lo medido por el método de Rancimat. Estos resultados proponen que el extracto investigado tiene el potencial de ser utilizado como conservante biológico en productos alimenticios
Chandra Observations of G11.2-0.3: Implications for Pulsar Ages
We present Chandra X-ray Observatory imaging observations of the young
Galactic supernova remnant G11.2-0.3. The image shows that the previously known
young 65-ms X-ray pulsar is at position (J2000) RA 18h 11m 29.22s, DEC -19o 25'
27.''6, with 1 sigma error radius 0.''6. This is within 8'' of the geometric
center of the shell. This provides strong confirming evidence that the system
is younger, by a factor of ~12, than the characteristic age of the pulsar. The
age discrepancy suggests that pulsar characteristic ages can be poor age
estimators for young pulsars. Assuming conventional spin down with constant
magnetic field and braking index, the most likely explanation for the age
discrepancy in G11.2-0.3 is that the pulsar was born with a spin period of ~62
ms. The Chandra image also reveals, for the first time, the morphology of the
pulsar wind nebula. The elongated hard-X-ray structure can be interpreted as
either a jet or a Crab-like torus seen edge on. This adds to the growing list
of highly aspherical pulsar wind nebulae and argues that such structures are
common around young pulsars.Comment: 16 pages, 3 figures, Accepted for publication in ApJ. For a full
resolution version of Fig 1, see
http://www.physics.mcgill.ca/~vkaspi/G11.2-0.3/f1.ep
A Low Frequency Survey of the Galactic Plane Near l=11 degrees: Discovery of Three New Supernova Remnants
We have imaged a 1 deg^2 field centered on the known Galactic supernova
remnant (SNR) G11.2-0.3 at 74, 330, and 1465 MHz with the Very Large Array
radio telescope (VLA) and 235 MHz with the Giant Metrewave Radio Telescope
(GMRT). The 235, 330, and 1465 MHz data have a resolution of 25 arcsec, while
the 74 MHz data have a resolution of 100 arcsec. The addition of this low
frequency data has allowed us to confirm the previously reported low frequency
turnover in the radio continuum spectra of the two known SNRs in the field:
G11.2-0.3 and G11.4-0.1 with unprecedented precision. Such low frequency
turnovers are believed to arise from free-free absorption in ionized thermal
gas along the lines of site to the SNRs. Our data suggest that the 74 MHz
optical depths of the absorbing gas is 0.56 and 1.1 for G11.2-0.3 and
G11.4-0.1, respectively. In addition to adding much needed low frequency
integrated flux measurements for two known SNRs, we have also detected three
new SNRs: G11.15-0.71, G11.03-0.05, and G11.18+0.11. These new SNRs have
integrated spectral indices between -0.44 and -0.80. Because of confusion with
thermal sources, the high resolution (compared to previous Galactic radio
frequency surveys) and surface brightness sensitivity of our observations have
been essential to the identification of these new SNRs. With this study we have
more than doubled the number of SNRs within just a 1 deg^2 field of view in the
inner Galactic plane. This result suggests that future low frequency
observations of the Galactic plane of similar quality may go a long way toward
alleviating the long recognized incompleteness of Galactic SNR catalogs.Comment: 31 pages, 9 figures. Figure 7 is in color. Accepted to A
The Expansion and Radio Spectral Index of G21.5-0.9: Is PSR J1833-1034 the Youngest Pulsar?
We report on new 5-GHz VLA radio observations of the pulsar-powered supernova
remnant G21.5-0.9. These observations have allowed us to make a high-quality
radio image of this remnant with a resolution of ~0.7". It has a filamentary
structure similar to that seen in the Crab Nebula. Radio structure suggestive
of the torus seen around the Crab pulsar is tentatively identified. We also
compared the new image with one taken ~15 yr earlier at 1.5 GHz, both to find
the expansion speed of the remnant and to make a spectral index image. Between
1991 and 2006, we find that the average expansion rate of the remnant is 0.11
+/- 0.02 %/year, corresponding, for a distance of 5 kpc, to a speed of 910 +/-
160 km/s wrt. the centre of the nebula. Assuming undecelerated expansion, this
expansion speed implies that the age of G21.5-0.9 is 870 (+200,-150) yr, which
makes PSR J1833-1034 one of the youngest, if not the youngest, known pulsars in
the Galaxy.Comment: Accepted for publication in the MNRAS. 8 pages; For an animation
showing the expansion of G21.5-0.9, see
http://www.yorku.ca/bartel/G21new.html . (The only change in V3 of the
preprint is to add the above url
The Deepest Radio Study of the Pulsar Wind Nebula G21.5-0.9: Still No Evidence for the Supernova Shell
We report on sensitive new 1.4-GHz VLA radio observations of the pulsar wind
nebula G21.5-0.9, powered by PSR J1833-1034, and its environs. Our observations
were targeted at searching for the radio counterpart of the shell-like
structure seen surrounding the pulsar wind nebula in X-rays. Some such radio
emission might be expected as the ejecta from the <~ 1000 yr old supernova
expand and interact with the surrounding medium. We find, however, no radio
emission from the shell, and can place a conservative 3-sigma upper limit on
its 1-GHz surface brightness of 7 x 10^-22 W/m^2/Hz/sr, comparable to the
lowest limits obtained for radio emission from shells around other pulsar-wind
nebulae. Our widefield radio image also shows the presence of two extended
objects of low-surface brightness. We re-examine previous 327-MHz images, on
which both the new objects are visible. We identify the first, G21.64-0.84, as
a new shell-type supernova remnant, with a diameter of ~13' and an unusual
double-shell structure. The second, G21.45-0.59, ~1' in diameter, is likely an
HII region.Comment: 8 Pages, submitted to MNRA
Seven-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Planets and Celestial Calibration Sources
(Abridged) We present WMAP seven-year observations of bright sources which
are often used as calibrators at microwave frequencies. Ten objects are studied
in five frequency bands (23 - 94 GHz): the outer planets (Mars, Jupiter,
Saturn, Uranus and Neptune) and five fixed celestial sources (Cas A, Tau A, Cyg
A, 3C274 and 3C58). The seven-year analysis of Jupiter provides temperatures
which are within 1-sigma of the previously published WMAP five-year values,
with slightly tighter constraints on variability with orbital phase, and limits
(but no detections) on linear polarization. Scaling factors are provided which,
when multiplied by the Wright Mars thermal model predictions at 350 micron,
reproduce WMAP seasonally averaged observations of Mars within ~2%. An
empirical model is described which fits brightness variations of Saturn due to
geometrical effects and can be used to predict the WMAP observations to within
3%. Seven-year mean temperatures for Uranus and Neptune are also tabulated.
Uncertainties in Uranus temperatures are 3%-4% in the 41, 61 and 94 GHz bands;
the smallest uncertainty for Neptune is ~8% for the 94 GHz band. Intriguingly,
the spectrum of Uranus appears to show a dip at ~30 GHz of unidentified origin,
although the feature is not of high statistical significance. Flux densities
for the five selected fixed celestial sources are derived from the seven-year
WMAP sky maps, and are tabulated for Stokes I, Q and U, along with polarization
fraction and position angle. Fractional uncertainties for the Stokes I fluxes
are typically 1% to 3%. Source variability over the seven-year baseline is also
estimated. Significant secular decrease is seen for Cas A and Tau A: our
results are consistent with a frequency independent decrease of about 0.53% per
year for Cas A and 0.22% per year for Tau A.Comment: 72 pages, 21 figures; accepted to ApJS; (v2) corrected Mars model
scaling factors, added figure 21, added text to Mars, Saturn and celestial
sources section
Fermi-LAT Search for Pulsar Wind Nebulae around gamma-ray Pulsars
The high sensitivity of the Fermi-LAT (Large Area Telescope) offers the first
opportunity to study faint and extended GeV sources such as pulsar wind nebulae
(PWNe). After one year of observation the LAT detected and identified three
pulsar wind nebulae: the Crab Nebula, Vela-X and the PWN inside MSH 15-52. In
the meantime, the list of LAT detected pulsars increased steadily. These
pulsars are characterized by high energy loss rates from ~3 \times 10^{33} erg
s to 5 \times 10 erg s and are therefore likely to power a
PWN. This paper summarizes the search for PWNe in the off-pulse windows of 54
LAT-detected pulsars using 16 months of survey observations. Ten sources show
significant emission, seven of these likely being of magnetospheric origin. The
detection of significant emission in the off-pulse interval offers new
constraints on the gamma-ray emitting regions in pulsar magnetospheres. The
three other sources with significant emission are the Crab Nebula, Vela-X and a
new pulsar wind nebula candidate associated with the LAT pulsar PSR J1023-5746,
coincident with the TeV source HESS J1023-575. We further explore the
association between the H.E.S.S. and the Fermi source by modeling its spectral
energy distribution. Flux upper limits derived for the 44 remaining sources are
used to provide new constraints on famous PWNe that have been detected at keV
and/or TeV energies.Comment: Accepted for publication in Astrophysical Journal, 42 pages, 17
figure
Implicator-conjunctor based models of fuzzy rough sets: definitions and properties
Ever since the first hybrid fuzzy rough set model was proposed in the early 1990' s, many researchers have focused on the definition of the lower and upper approximation of a fuzzy set by means of a fuzzy relation. In this paper, we review those proposals which generalize the logical connectives and quantifiers present in the rough set approximations by means of corresponding fuzzy logic operations. We introduce a general model which encapsulates all of these proposals, evaluate it w.r.t. a number of desirable properties, and refine the existing axiomatic approach to characterize lower and upper approximation operators
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