Optimization of High-Strength Hydrocarbon Biodegradation Using Respirometry

Laboratory respirometry experiments were conducted on mixtures of soil and oily sludge to estimate biodegradation rates by CO2 production rates and determine optimum conditions for biodegradation of high-strength hydrocarbon waste products. These experiments were used to determine a suitable range of total petroleum hydrocarbon (TPH) concentration for biological treatment and to optimize for nutrient addition and moisture content. CO2 production rates from biological respiration of hydrocarbon-contaminated soil were maximized at concentrations of 3-9% TPH (30,00090,000 mg/kg TPH). CO2 production rates decreased dramatically at concentrations above 9% TPH, indicating that either these concentrations are lethal to microbes present, or this high sludge content inhibits aeration of the soils. Addition of 120 mg/kg nitrogen, 40 mg/kg phosphorous, and 40 mg/kg potassium to the soils resulted in a three fold increase in CO2 production rates. No significant increase in CO2 production was observed when the nutrient addition was increased to 240 mg/kg nitrogen, 80 mg/kg phosphorous, and 80 mg/kg potassium. Maximum CO2 production rates were observed at 15-20% moisture content. CO2 production rates decreased significantly at and below 10% moisture and at and above 25% moisture. Maximum CO2 production rates observed for soil with 50,000 mg/kg TPH, with added nutrients at optimum moisture content, were 30-35 μL CO2/g/hr. Assuming all CO2 was generated from hydrocarbon degradation, this maximum CO2 production rate corresponds to a hydrocarbon biodegradation rate of approximately 500 mg TPH/kg/day (assuming 100% respiration for a conservative estimate). If ideal conditions are maintained and rates of respiration remain high, clay soil contaminated with 60,000 mg/kg TPH sludge could probably be remediated in 2 months

FORMULATION DEVELOPMENT AND EVALUATION OF GASTRORETENTIVE FLOATING TABLET OF CIPROFLOXACIN HYDROCHORIDE

Objective: The aim of formulating floating tablets of ciprofloxacin hydrochloride was to prolong the gastric residence time after oral administration to achieve the controlled release of drug. Ciprofloxacin hydrochloride, a broad-spectrum fluoroquinolone antibacterial agent and it is use in the treatment of bone and joint infections, diarrhoeal infection, lower respiratory tract infections, urinary tract infections and meningococcal prophylaxis.Methods: Floating tablets of Ciprofloxacin hydrochloride were prepared by wet granulation method using two different grades (K-100M & K-4M) of Hydroxyl Propyl Methyl Cellulose (HPMC) and Carbopol 934P using effervescent technique. Sodium bicarbonate was incorporated as a gas-generating agent. The floating tablets were evaluated for uniformity of weight, hardness, friability, drug content, in vitro buoyancy and dissolution studies. The effect of citric acid on drug release profile and floating properties was also investigated.Results: It was observed that tablet swelled radially and axially during in vitro buoyancy studies and remained buoyant for 10-14 h. The combination of sodium bicarbonate (70 mg) and citric acid (20 mg) was found to achieve the optimum in vitro buoyancy.Conclusion: In the present work it was concluded that the floating duration of was more in tablet with HPMC K-100 as compared with formulations containing HPMC K-4M. Drug ciprofloxacin hydrochloride release could be prolonged about 14 h in the GIT by using blend of HPMC-K 100M with sodium bicarbonate as gas generating agent and formulate it as a gastro retentive floating tablet.Keywords: Floating lag time, Ciprofloxacin hydrochloride, Total floating time, Hydroxyl Propyl Methyl Cellulos

DEVELOPMENT AND VALIDATION OF RP-HPLC METHOD FOR DETERMINATION OF HYDROCHLOROTHIAZIDE, OLMESARTAN MEDOXOMIL AND THEIR RELATED SUBSTANCES IN COMBINED TABLET DOSAGE FORM

Objective: Development of RP-HPLC method for determination of Hydrochlorothiazide (HCTZ), Olmesartan medoxomil (OLM) and their related substances in combined tablet dosage form and validation of the developed method. Methods: Gradient mobile phase system was used for estimation of drug contents and their related substances. Mobile phase A contained the mixture of Acetonitrile and 15 mM Phosphate buffer (pH adjusted to 3.4 with orthophosphoric acid) in the ratio of 20:80. Mobile phase B contained the same mixture in the ratio of 80:20. Chromatographic separation was carried out at the mobile phase flow rate of 0.8 mL/min using C18 Phenomenax inplace of Enable (250 × 4.6 mm) 5 μm column and detection was made at 254 nm. Results: The linearity of developed method was tested in the range of 62.5-187.5 μg/mL for Hydrochlorothiazide, 100-300 μg/mL for Olmesartan medoxomil, 1-1.8 μg/mL for Hydrochlorothiazide. The % recovery was found to be 99.88-100.67 % (HCTZ), 99.14-99.91 % (OLM), 99.11-100.71% (HCTZ-IMP) and 98.13-100.83% (OLM-IMP). The assay of marketed formulation was found to be 99.78% (HCTZ) and 99.26% (OLM). Conclusion: A simple, precise and accurate RP-HPLC method was developed for determination of Hydrochlorothiazide, Olmesartan medoxomil and their related substances

The opacity of grains in protoplanetary atmospheres

We have computed the size distribution of silicate grains in the outer radiative region of the envelope of a protoplanet evolving according to the scenario of Pollack et al. (1996). Our computation includes grain growth due to Brownian motion and overtake of smaller grains by larger ones. We also include the input of new grains due to the breakup of planetesimals in the atmosphere. We follow the procedure of Podolak (2003), but have speeded it up significantly. This allows us to test the sensitivity of the code to various parameters. We have also made a more careful estimate of the resulting grain opacity. We find that the grain opacity is of the order of $10^{-2}\ \mathrm{cm^2 g^{-1}}$throughout most of the outer radiative zone as Hubickyj et al. (2005) assumed for their low opacity case, but near the outer edge of the envelope, the opacity can increase to$\sim{1} \mathrm{cm^2 g^{-1}}$. We discuss the effect of this on the evolution of the models.Comment: 28 pages, 13 Figs., to be published in Icarus (accepted Sep. 2007

Dust coagulation in ISM

Coagulation is an important mechanism in the growth of interstellar and interplanetary dust particles. The microphysics of the coagulation process was theoretically analyzed as a function of the physical properties of the coagulating grains, i.e., their size, relative velocities, temperature, elastic properties, and the van der Waal interaction. Numerical calculations of collisions between linear chains provide the wave energy in individual particles and the spectrum of the mechanical vibrations set up in colliding particles. Sticking probabilities are then calculated using simple estimates for elastic deformation energies and for the attenuation of the wave energy due to absorption and scattering processes

QSO's from Galaxy Collisions with Naked Black Holes

In the now well established conventional view (see Rees [1] and references therein), quasi-stellar objects (QSOs) and related active galactic nuclei (AGN) phenomena are explained as the result of accretion of plasma onto giant black holes which are postulated to form via gravitational collapse of the high density regions in the centers of massive host galaxies. This model is supported by a wide variety of indirect evidence and seems quite likely to apply at least to some observed AGN phenomena. However, one surprising set of new Hubble Space Telescope (HST) observations [2-4] directly challenges the conventional model, and the well known evolution of the QSO population raises some additional, though not widely recognized, difficulties. We propose here an alternative possibility: the Universe contains a substantial independent population of super-massive black holes, and QSO's are a phenomenon that occurs due to their collisions with galaxies or gas clouds in the intergalactic medium (IGM). This hypothesis would naturally explain why the QSO population declines very rapidly towards low redshift, as well as the new HST data.Comment: plain TeX file, no figures, submitted to Natur

The black hole mass distribution in early-type galaxies: cusps in HST photometry interpreted through adiabatic black hole growth

The surface brightness profiles of early-type galaxies have central cusps. Two characteristic profile types are observed with HST: `core' profiles have a break at a resolved radius and logarithmic cusp slope gamma < 0.3 inside that radius; `power-law' profiles have no clear break and gamma > 0.3. With few exceptions, galaxies with M_V -20.5 have power-law profiles. Both profile types occur in galaxies with -22 < M_V < -20.5. We show that these results are consistent with the hypothesis that: (i) all early-type galaxies have black holes (BHs) that grew adiabatically in homogeneous isothermal cores; and (ii) these `progenitor' cores followed scaling relations similar to those of the fundamental plane. The models studied here are the ones first proposed by Young. Models with BH masses and progenitor cores that obey established scaling relations predict (at Virgo) that galaxies with M_V < -21.2 have core profiles and galaxies with M_V > -21.2 have power-law profiles. This reproduces both the sense and the absolute magnitude of the observed transition. Intrinsic scatter in BH and galaxy properties can explain why both types of galaxies are observed around the transition magnitude. The observed bimodality in cusp slopes may be due to a bimodality in M_bh/L, with rapidly rotating disky galaxies having larger M_bh/L than slowly rotating boxy galaxies. Application to individual galaxies with HST photometry yields a roughly linear correlation between BH mass and V-band galaxy luminosity, log M_bh = -1.83 + log L (solar units). This agrees with the average relation for nearby galaxies with kinematically determined BH masses, and also with predictions from quasar statistics (shortened abstract).Comment: 41 pages, LaTeX, with 11 PostScript figures. Submitted to the Astronomical Journal. Postscript version also available from http://sol.stsci.edu/~marel/abstracts/abs_R23.htm

Contrasting histoarchitecture of calcified leaflets from stenotic bicuspid versus stenotic tricuspid aortic valves

AbstractPreliminary findings from clinical trials of percutaneous balloon aortic valvuloplasty and intraoperative debridement of calcific deposits in patients with aortic stenosis have suggested that calcified, congenitally bicuspid aortic valves may be less amenable to these techniques than are calcified tricuspid aortic valves. Accordingly, we evaluated the histoarchitecture of calcific deposits in 30 operatively excised aortic valves. Light microscopic sections taken through the calcified aortic valve leaflets disclosed two principal types of histoarchitectitre. In 11 aortic valves nodular calcific deposits were superimposed on an underlying fibrotic aortic valve leaflet (type A); in 17 valves calcific deposits were diffusely distributed throughout the body (spongiosa) of the aortic valve leaflets (type B). Two aortic valves could not be classified histologically.These histologic subtypes were not randomly distributed with regard to gross valvular morphology. All 14 bicuspid valves (100%) were type B; in contrast, 11 (69%) of 16 tricuspld aortic valves were type A, and only 3 (19%) of 16 tricuspid valves were type B (p < 0.01). Both valves with nonclassifiable histologic features were tricuspid on the basis of gross examination.Thus, the histoarchitectural distribution of calcific deposits is different for bicuspid than for tricuspid stenotic aortic valves. The more diffuse distribution of calcium throughout the body of calcified bicuspid aortic valve leaflets may render these valves less amenable to operative and percutaneous valvuloplasty than are calcified tricuspid aortic valve leaflets on which calcific deposits are typically superimposed in nodular form

Young stars and non-stellar emission in the aligned radio galaxy 3C 256

We present ground-based images of the z=1.824 radio galaxy 3C 256 in the standard BVRIJHK filters and an interference filter centered at 8800A, a Hubble Space Telescope image in a filter dominated by Ly-alpha emission (F336W), and spectra covering rest-frame wavelengths from Ly-alpha to [O III] 5007. Together with published polarimetry observations, we use these to decompose the overall spectral energy distribution into nebular continuum emission, scattered quasar light, and stellar emission. The nebular continuum and scattered light together comprise half (one third) of the V-band (K-band) light within a 4-arcsec aperture, and are responsible for the strong alignment between the optical/near-infrared light and the radio emission. The stellar emission is dominated by a population estimated to be 100-200 Myr old (assuming a Salpeter IMF), and formed in a short burst with a peak star formation rate of 1-4x10^3 Msun/yr. The total stellar mass is estimated to be no more than 2x10^{11} Msun, which is far less than other luminous radio galaxies at similar redshifts, and suggests that 3C 256 will undergo further star formation or mergers.Comment: 35 pages including 10 figures; to appear in Nov 10 Ap

The Cosmic Density of Massive Black Holes from Galaxy Velocity Dispersions

Supermassive black holes are thought to be relics of quasars, and their numbers and masses are therefore related to the quasar luminosity function and its evolution with redshift. We have used the relationship between black hole mass and bulge velocity dispersion (the M_bullet - sigma relation) to make an improved estimate of the mass density and mass spectrum of supermassive black holes. Uncertainties in the M_bullet - sigma relation have little effect on the mass density. We find a mass density of (4.8 +/- 1.6) h^2 x 10^5 M_sun Mpc^-3. Some of the variance in published density estimates comes from the use of different values of the Hubble constant.Comment: To appear in the December 2002 issue of The Astronomical Journa