Production of N2 Vegard-Kaplan and Lyman-Birge-Hopfield emissions on Pluto

We have developed a model to calculate the emission intensities of various vibrational transitions of N$_2$ triplet band and Lyman-Birge-Hopfield (LBH) band emissions in the dayglow of Pluto for solar minimum, moderate, and maximum conditions. The calculated overhead intensities of Vegard-Kaplan ($A^3\Sigma_u^+ - X^1\Sigma^+_g$), First Positive ($B^3\Pi_g - A^3\Sigma^+_u$), Second Positive ($C^3\Pi_u - B^3\Pi_g$), Wu-Benesch ($W^3\Delta_u - B^3\Pi_g$), Reverse First Positive, and LBH ($a^1\Pi_g$-- $X^1\Sigma^+_g$) bands of N$_2$ are 17 (74), 14.8 (64), 2.4 (10.8), 2.9 (12.7), 2.9 (12.5), and 2.3 (10) R, respectively, for solar minimum (maximum) condition. We have predicted the overhead and limb intensities of VK (150-190 nm) and LBH (120-190 nm) bands of N$_2$ on Pluto for the New Horizons (NH) flyby condition that can be observed by Alice: the ultraviolet imaging spectrograph also know as P-Alice. The predicted limb intensities of VK and LBH bands peak at radial distance of $\sim$2000 km with the value of about 5 (13) and 9.5 (22) R for solar zenith angle 60$^\circ$ (0$^\circ$), respectively. We have also calculated overhead and limp intensities of few prominent transition of CO Fourth Positive bands for NH flyby condition.Comment: 7 pages, 5 figures, 2 table

Production of N2 Vegard-Kaplan and other triplet band emissions in the dayglow of Titan

Recently the Cassini Ultraviolet Imaging Spectrograph has revealed the presence of N2 Vegard-Kaplan band emissions in Titan's dayglow limb observation. We present model calculations for the production of various N2 triplet states in the upper atmosphere of Titan. The Analytical Yield Spectra technique is used to calculate steady state photoelectron fluxes in Titan's atmosphere, which are in agreement with those observed by the Cassini's CAPS instrument. Considering direct electron impact excitation, inter-state cascading, and quenching effects, the population of different levels of N2 triplet states are calculated under statistical equilibrium. Densities of all vibrational levels of each triplet state and volume production rates for various triplet states are calculated in the model. Vertically integrated overhead intensities for the same date and lighting conditions as the reported by UVIS observations for N2 VK, 1P, 2P, Wu-Benesch, and Reverse First Positive bands of N2 are found to be 132, 114, 19, 22, and 22 R, respectively. Overhead intensities are calculated for each vibrational transition of all the triplet band emissions of N2, which span a wider spectrum of wavelengths from ultraviolet to infrared. The calculated limb intensities of total and prominent transitions of VK band are presented. The model limb intensity of VK emission within the 150-190 nm wavelength region is in good agreement with the Cassini UVIS observed limb profile. An assessment of the impact of solar EUV flux on the N2 triplet band emission intensity has been made by using three different solar flux models, viz., Solar EUV Experiment, SOLAR2000 model of Tobiska (2004), and HEUVAC model of Richards et al, (2006). The calculated N2 VK band intensity at the peak of limb intensity due to S2K and HEUVAC solar flux models is a factor of 1.2 and 0.9, respectively, of that obtained using SEE solar EUV flux.Comment: 25 pages, 11 figures; Icarus, 201

BRIDGING THE GAP BETWEEN R&D AND COMMERCIALIZATION IN PHARMACEUTICAL INDUSTRY: ROLE OF MEDICAL AFFAIRS AND MEDICAL COMMUNICATIONS

The launch of a new drug into the market requires a unique and complex process initiating from development (R&D) to its commercialization (marketing authorization and selling of these products). Due to increased burden by regulatory authorities, the medical affairs evolved as separate medical organization to bifurcate medical and commercial functions. It is closely associated with development but works mainly on post-approval activities by providing both the scientific and clinical expertise. The core functional areas of medical affairs (MA) include: medical communications/publications, medical science liaisons (MSLs) and medical information. In the recent years ethical and evidence-based medical communications has attained increasing importance in emerging pharmaceutical markets. A successful product launch is based on both promotional (medico-marketing) and non-promotional (medical information services, publications) material to support the product and to report clinical trials in peer-reviewed international journals. Local clinical or observational studies and medical surveys can provide sufficient information about the product. Besides, a number of medical communication like product monographs, brochures, slide kits, leave behind literature (LBL), continuous medical education (CME) slides, training modules, key opinion leader documents(promotional inputs) and conference posters, abstracts, and journal articles (research based inputs)are other ways to aid in an effective product launch. In the last 10 years medical writers in India have developed the capability to meet this challenge through their training and work experience making India hub for medical communications services. KEYWORDS: Key opinion leaders; Medical affairs; Medical communications; Medical science liaisons; Medical writing

Evaluation of lipid profile and apolipoproteins in cord blood from Tribal and nontribal population of Udaipur region, India

Background: Cardiovascular diseases are the leading cause of mortality in India. The important factor associated is dyslipidemia. A strong relationship has been seen in epidemiological studies between cholesterol and cardiovascular disease. The present study was planned to analyze cord blood lipid profile, apolipoproteins and atherogenic index in tribal and nontribal population and compare them gender wise.Methods: Our study group consisted of 250 healthy full-term newborn. The cord blood was collected immediately after a normal delivery. The blood was tested to determine lipid profile, apolipoproteins and atherogenic index. Results: The results showed that the levels of lipid profile, apolipoproteins and ratio (TC/HDL, TC/LDL, HDL/LDL, and LDL/HDL) were higher in non-tribal population than tribal ones. Gender wise comparison revealed higher levels in male non-tribal neonates as compared to female non-tribal neonates. The apolipoproteinB and Atherogenic index (ApoB/ApoA-1) were higher in females than male non-tribal neonates in cord blood. The trends were reversed in the tribal population.Conclusions: The result concluded that tribal and non-tribal population, also female and male neonates have genetic variation and difference in lipid metabolism

Calculations of N2 triplet states vibrational populations and band emissions in Venusian dayglow

A model for N2 triplet states band emissions in the Venusian dayglow has been developed for low and high solar activity conditions. Steady state photoelectron fluxes and volume excitation rates for N2 triplet states have been calculated using the Analytical Yield Spectra (AYS) technique. Model calculated photoelectron flux is in good agreement with Pioneer Venus Orbiter-observed electron flux. Since inter-state cascading is important for the triplet states of N2, populations of different levels of N2 triplet states are calculated under statistical equilibrium considering direct electron impact excitation, and cascading and quenching effects. Densities of all vibrational levels of each triplet state are calculated in the model. Height-integrated overhead intensities of N2 triplet band emissions are calculated, the values for Vegard-Kaplan (A^3Sigma_u^+ - X^1Pi_g^+), First Positive (B^3Pi_g - A^3Sigma_u^+), Second Positive (C^3Pi_u - B^3Pi_g), and Wu-Benesch (W^3Delta_u - B^3Pi_g) bands of N2, are 1.9 (3.2), 3 (6), 0.4 (0.8), and 0.5 (1.1) kR, respectively, for solar minimum (maximum) conditions. The intensities of the three strong Vegard-Kaplan bands (0, 5), (0, 6), and (0, 7) are 94 (160), 120 (204), and 114 (194) R, respectively, for solar minimum (maximum) conditions. Limb profiles are calculated for VK (0, 4), (0, 5), (0, 6) and (0, 7) bands. The calculated intensities on Venus are about a factor 10 higher than those on Mars. The present study provides a motivation for a search of N2 triplet band emissions in the dayglow of Venus.Comment: Icarus, 201

Impact of solar EUV flux on CO Cameron band and CO2+ UV doublet emissions in the dayglow of Mars

This study is aimed at making a calculation about the impact of the two most commonly used solar EUV flux models -- SOLAR2000 (S2K) of \cite{Tobiska04} and EUVAC model of \cite{Richards94} -- on photoelectron fluxes, volume emission rates, ion densities and CO Cameron and CO$_2^+$ UV doublet band dayglow emissions on Mars in three solar activity conditions: minimum, moderate, and maximum. Calculated limb intensities profiles are compared with SPICAM/Mars Express and Mariner observations. Analytical yield spectrum (AYS) approach has been used to calculate photoelectron fluxes in Martian upper atmosphere. Densities of prominent ions and CO molecule in excited triplet a$^3\Pi$ state are calculated using major ion-neutral reactions. Volume emission rates of CO Cameron and CO$_2^+$ UV doublet bands have been calculated for dif{}ferent observations (Viking condition, Mariner and Mars Express SPICAM observations) on Mars. For the low solar activity condition, dayglow intensities calculated using the S2K model are $\sim$40% higher than those calculated using the EUVAC model. During high solar activity, due to the higher EUV fluxes at wavelengths below 250 \AA\ in the EUVAC model, intensities calculated using EUVAC model are slightly higher ($\sim$20%) than those calculated using S2K model. Irrespective of the solar activity condition, production of Cameron band due to photodissociative excitation of CO$_2$ is around 50% higher when S2K model is used. Altitude of peak limb brightness of CO Cameron and CO$_2^+$ UV doublet band is found to be independent of solar EUV flux models. Calculated limb intensities of CO Cameron and CO$_2^+$ UV doublet bands are on an average a factor of $\sim$2 and $\sim$1.5, respectively, higher than the SPICAM Mars Express observation, while they are consistent with the Mariner observations.Comment: 27 Pages, 12 Figures; Planetary and Space Science, 201