A Prospective Open Labelled Phase-II Non- Randomized Clinical Trial on “NERUNJI VER KUDINEER” for “KALLADAIPPU” (UROLITHIASIS)

KALLADAIPPU is the most common disease in our country. The evidence of the disease KALLADAIPPU was derived from YUGI VAIDHIYA CHINTHAMANI 800, by Dr.K.Anbarasu B.S.M.S (Page.No.283). The clinical features of KALLADAIPPU can be correlated with UROLITHIASIS in modern science. Urolithiasis is a term originated from three Greek words “ouron” for urine, “oros” for flow, and “lithos” for stone. It is the formation of calculi which are formed or located anywhere in the urinary system (i.e. kidneys, bladder, urethrae, and urinary tract). Many herbal and herbal-mineral formulations have been described in Siddha text books. One such drug NERUNJI VER KUDINEER mentioned in the book of AATHMARATCHAMIRTHAM ENNUM VAIDHYA SARASANGIRAGAM (Page.no:349). A total of 40 patients of both sex (20 OPD and 20 IPD) were selected and administered with the clinical trial medicine “NERUNJI VER KUDINEER” 100 ml BID at PG Department of Pothu Maruthuvam, Govt. Siddha Medical College and Hospital, Palayamkottai. The whole study period is between August 2018 and June 2019. The clinical trial medicine was subjected to Biochemical, Toxicity and Pharmacological studies. In clinical study 75% of out patients and 50% of in patients showed Good response. And 25% of Out patients and 45% In patients showed Moderate response. Poor response in 5% of IPD. No Adverse reaction was found in this clinical study. The statistical analysis showed good significant value (P<0.0001). The Nerunji ver Kudineer is safe and effective and affordable cost in the treatment of Kalladaippu Noi (Urolithiasis)

Small carbon chains in circumstellar envelopes

Observations were made for a number of carbon-rich circumstellar envelopes using the Phoenix spectrograph on the Gemini South telescope to determine the abundance of small carbon chain molecules. Vibration-rotation lines of the $\nu_{3}$ antisymmetric stretch of C$_{3}$ near 2040 cm$^{-1}$ (4.902 $\mu$m) have been used to determine the column density for four carbon-rich circumstellar envelopes: CRL 865, CRL 1922, CRL 2023 and IRC +10216. We additionally calculate the column density of C$_{5}$ for IRC +10216, and provide an upper limit for 5 more objects. An upper limit estimate for the C$_{7}$ column density is also provided for IRC+10216. A comparison of these column densities suggest a revision to current circumstellar chemical models may be needed

Molecular Opacities for Exoplanets

Spectroscopic observations of exoplanets are now possible by transit methods and direct emission. Spectroscopic requirements for exoplanets are reviewed based on existing measurements and model predictions for hot Jupiters and super-Earths. Molecular opacities needed to simulate astronomical observations can be obtained from laboratory measurements, ab initio calculations or a combination of the two approaches. This discussion article focuses mainly on laboratory measurements of hot molecules as needed for exoplanet spectroscopy

GPRD, A Database for the Spectral Properties of Diatomic Molecules of Atmospheric Interest

A short note describing the development of a database providing factual and numerical data on the spectral properties of diatomic molecules. This database is available online for the overall scientific community at the following adress: http://cfp.ist.utl.pt/radiation/Comment: 2 page

Hot methane line lists for exoplanet and brown dwarf atmospheres

We present comprehensive experimental line lists of methane (CH4) at high temperatures obtained by recording Fourier transform infrared emission spectra. Calibrated line lists are presented for the temperatures 300 - 1400 degC at twelve 100 degC intervals spanning the 960 - 5000 cm-1 (2.0 - 10.4 microns) region of the infrared. This range encompasses the dyad, pentad and octad regions, i.e., all fundamental vibrational modes along with a number of combination, overtone and hot bands. Using our CH4 spectra, we have estimated empirical lower state energies (Elow in cm-1) and our values have been incorporated into the line lists along with line positions (cm-1) and calibrated line intensities (S' in cm molecule-1). We expect our hot CH4 line lists to find direct application in the modeling of planetary atmospheres and brown dwarfs.Comment: Supplementary material is provided via the Astrophysical Journal referenc

ACE-FTS Observations of Acetonitrile in the Lower Stratosphere

This work reports the first infrared satellite remote-sensing measurements of acetonitrile (CH3CN) in the Earth\u27s atmosphere using solar occultation measurements made by the Atmospheric Chemistry Experiment Fourier transform spectrometer (ACE-FTS) between 2004 and 2011. The retrieval scheme uses new quantitative laboratory spectroscopic measurements of acetonitrile (Harrison and Bernath, 2012). Although individual ACE-FTS profile measurements are dominated by measurement noise, median profiles in 10 degrees latitude bins show a steady decline in volume mixing ratio from similar to 150 ppt (parts per trillion) at 11.5 km to \u3c 40 ppt at 25.5-29.5 km. These new measurements agree well with the scant available air-and balloon-borne data in the lower stratosphere. An acetonitrile stratospheric lifetime of 73 ± 20 yr has been determined

Fourier Transform Emission Spectroscopy of YH and YD: Observation of New A¹Δ and B¹Π Electronic States

The emission spectra of YH and YD molecules have been investigated in the 3600–12 000 cm−1 region using a Fourier transform spectrometer. Molecules were formed in an yttrium hollow cathode lamp operated with a continuous flow of a mixture of Ne and Ar gases, and YH and YD were observed together in the same spectra. A group of bands observed near 1 μm have been identified as 0-0 and 1-1 bands of the A1Δ-X1Σ+ and B1Π-X1Σ+ transitions of YH and the 0-0 bands of the same two transitions for YD. The A1Δ and B1Π states of YH are separated by only about 12 cm−1 and are involved in strong interactions. A perturbation analysis has been performed using the PGOPHER program to fit the two interacting electronic states and spectroscopic parameters for the A1Δ and B1Π states, including the interaction matrix elements, have been obtained for the first time

CH in stellar atmospheres: an extensive linelist

The advent of high-resolution spectrographs and detailed stellar atmosphere modelling has strengthened the need for accurate molecular data. Carbon-enhanced metal-poor (CEMP) stars spectra are interesting objects with which to study transitions from the CH molecule. We combine programs for spectral analysis of molecules and stellar-radiative transfer codes to build an extensive CH linelist, including predissociation broadening as well as newly identified levels. We show examples of strong predissociation CH lines in CEMP stars, and we stress the important role played by the CH features in the Bond-Neff feature depressing the spectra of barium stars by as much as 0.2 magnitudes in the $\lambda=$3000 -- 5500 \AA\ range. Because of the extreme thermodynamic conditions prevailing in stellar atmospheres (compared to the laboratory), molecular transitions with high energy levels can be observed. Stellar spectra can thus be used to constrain and improve molecular data.Comment: 33pages, 15 figures, accepted in A&A external data available at http://www.astro.ulb.ac.be/~spectrotools