879 research outputs found
A Prospective Open Labelled Phase-II Non- Randomized Clinical Trial on âNERUNJI VER KUDINEERâ for âKALLADAIPPUâ (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 âouronâ for urine, âorosâ for flow, and âlithosâ 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 âNERUNJI VER KUDINEERâ 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
antisymmetric stretch of C near 2040 cm (4.902 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 for IRC +10216, and
provide an upper limit for 5 more objects. An upper limit estimate for the
C 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
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 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
Fourier Transform Emission Spectroscopy of YH and YD: Observation of New AÂčÎ and BÂčÎ Electronic States
The emission spectra of YH and YD molecules have been investigated in the 3600â12 000 cmâ1 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 ÎŒm have been identified as 0-0 and 1-1 bands of the A1Î-X1ÎŁ+ and B1Î -X1ÎŁ+ transitions of YH and the 0-0 bands of the same two transitions for YD. The A1Î and B1Î states of YH are separated by only about 12 cmâ1 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 A1Î and B1Î states, including the interaction matrix elements, have been obtained for the first time
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