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Search Results: 1 - 10 of 389682 matches for " R. N. Misra "
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Neurocysticercosis presenting as Weber's syndrome: As short report
Singh N,Verma R,Pankaj B,Misra S
Neurology India , 2003,
Abstract: This case report describes a rare, non-epileptic manifestation of neurocysticercosis where a 22-year-old male presented with acute onset right 3rd nerve palsy with left hemiplegia (Weber syndrome). Computerized tomography and magnetic resonance imaging revealed cysticercus granuloma. The patient improved and became asymptomatic with steroid treatment. Recognizing this clinical entity would avoid unnecessary antituberculous treatment and surgical intervention.
Patient with limb girdle dystrophy presenting with dopa-responsive dystonia - A case report
Verma R,Misra S,Singh N,Kishore D
Neurology India , 2003,
Abstract: Dopa-responsive dystonias are rare. We report a 14-year-old male who was diagnosed as a case of limb girdle dystrophy and had features suggestive of dopa-responsive dystonia.
Cauda-conus syndrome resulting from neurocysticercosis
Singh N,Verma R,Pankaj B,Misra S
Neurology India , 2003,
Abstract: A 60-year-old male, presented with insidious onset, gradually progressive, burning paresthesia over the saddle area, sphincteric disturbance, impotence and paraparesis. Investigations revealed a ring-enhancing lesion in the conus medullaris suggestive of neurocysticercosis . This was supported by quantitative enzyme-linked immunosorbant assay from purified cell fraction of taenia solium cysticerci. On treatment with steroids he showed marked improvement.
Comprehensive Spectral Analysis of Cyg X-1 using RXTE Data
Rizwan Shahid,R. Misra,S. N. A. Jaaffrey
Physics , 2012, DOI: 10.1088/1674-4527/12/10/005
Abstract: We analyse a large number ($> 500$) pointed RXTE observations of Cyg X-1 and model the spectrum of each one. A subset of the observations for which there is simultaneous reliable measure of the hardness ratio by the All Sky Monitor, shows that the sample covers nearly all the spectral shapes of Cyg X-1. The relative strength, width of the Iron line and the reflection parameter are in general correlated with the high energy photon spectral index $\Gamma$. This is broadly consistent with a geometry where for the hard state (low $\Gamma \sim 1.7$) there is a hot inner Comptonizing region surrounded by a truncated cold disk. The inner edge of the disk moves inwards as the source becomes softer till finally in the soft state (high $\Gamma > 2.2$) the disk fills the inner region and active regions above the disk produce the Comptonized component. However, the reflection parameter shows non-monotonic behaviour near the transition region ($\Gamma \sim 2$), suggestive of a more complex geometry or physical state of the reflector. Additionally, the inner disk temperature, during the hard state, is on the average higher than in the soft one, albeit with large scatter. These inconsistencies could be due to limitations in the data and the empirical model used to fit them. The flux of each spectral component is well correlated with $\Gamma$ which shows that unlike some other black hole systems, Cyg X-1 does not show any hysteresis behaviour. In the soft state, the flux of the Comptonized component is always similar to the disk one, which confirms that the ultra-soft state (seen in other brighter black hole systems) is not exhibited by Cyg X-1. The rapid variation of the Compton Amplification factor with $\Gamma$, naturally explains the absence of spectra with $\Gamma < 1.6$, despite a large number having $\Gamma \sim 1.65$.
The Effect of Non-Thermal Protons on the High Energy Spectra of Black Hole Binaries
S. Bhattacharyya,N. Bhatt,R. Misra,C. L. Kaul
Physics , 2003, DOI: 10.1086/377328
Abstract: In the inner regions of an accretion disk around a black hole, the presence of non-thermal protons would via p-p collisions produce electrons, positrons and $\gamma$-rays. For such a scenario, the steady state electron-positron distribution is computed taking into account Compton cooling, $e^{-} e^{+}$ pair production (due to $\gamma-\gamma$ interactions) and pair annihilation. The resultant spectra has a broad feature around $1 - 10$ MeV which may be tested with observations by INTEGRAL and GLAST. Using the available OSSE data for the black hole system, GRS 1915+115 we illustrate that an upper limit on the non-thermal proton fraction can be obtained, which may put constraints on the acceleration process active in this system.
有限供水对小麦根系生长、水分利用和籽粒产量的影响
R.,K.,Misra,T.,N.,Chaudhary,唐永金
麦类作物学报 , 1987, DOI: 10.7606/j.issn.1009-1041.1987.02.033
Abstract: 小麦是印度的主要冬季作物,但大多数种麦区降雨量是有限的.为了最大限度地减少由蒸散(ET)亏缺引起的产量降低,实行可用水的限量灌溉是非常重要的.有证据表明,一定的蒸散亏缺的影响取决于亏缺发生的时间和它的强度(Hagan和Stewart,1972).由于小麦的根系分布和水分吸收模式密切相关(Chaudhary和Bhatnagar,1980),所以对供水有限的地区来说,根系分布广而深的植株可能是符合需要的.
A comparative study of flurbiprofen and piroxicam in osteoarthritis.
Misra N
Journal of Postgraduate Medicine , 1992,
Abstract: In this single-blind, multiple-dose study the efficacy and tolerability of flurbiprofen was compared with that of piroxicam in 60 adult patients suffering from osteoarthritis of the knee. The patients were randomly allocated to receive either flurbiprofen 100 mg twice daily or piroxicam 20 mg once daily for a period of four weeks. Clinical assessments w.r.t. pain, tenderness, stiffness, swelling and general activity of patient were carried out prior to initiation of trial therapy and thereafter at weekly intervals for four weeks. The findings were graded. Though significant improvements as compared to baseline data occurred in both the treatment groups, flurbiprofen was found to be superior to piroxicam in improving pain on movement and at rest (p < 0.05). The incidence of side effects was less in the group receiving flurbiprofen (6% compared to 47% observed with piroxicam).
Experimental lens induced uveitis in rat
Misra R
Indian Journal of Ophthalmology , 1981,
Abstract:
Orbital rhabdomyosarcoma
Misra R
Indian Journal of Ophthalmology , 1971,
Abstract:
Multi-wavelength imaging observations of plasma depletions over Kavalur, India
H. S. S. Sinha,P. K. Rajesh,R. N. Misra,N. Dutt
Annales Geophysicae (ANGEO) , 2003,
Abstract: Observations of ionospheric plasma depletions were made over Kavalur (12.56° N, 78.8° E, Mag. Lat 4.6° N), India during March–pril 1998 using an all sky optical imaging system operating at 630 nm, 777.4 nm and 557.7 nm. Out of 14 nights of observations, plasma depletions were seen only on 9 nights. Except for 21 March 1998, which was a magnetically disturbed period, all other nights belonged to a magnetically quiet period. Some of the important results obtained from these observations are: (a) After the onset of the equatorial spread F (ESF), plasma depletions take typically about 2 hrs 40 min to come to a fully developed state, (b) There are three distinct types of plasma depletions: type 1 have an east-west (e–w) extent of 250–350 km with an inter-depletion distance (IDD) of 125–300 km; Type 2 have an e–w extent of 100–150 km and IDD of 50–150 km; Type 3 have smallest the e–w extent (40–100 km) and IDD of 20–60 km, (c) Most of the observed plasma depletions (> 82%) had their eastward velocity in the range of 25–125 ms–1. Almost stationary plasma depletions (0–25 ms–1) were observed on one night, which was magnetically disturbed. These very slow moving depletions appear to be the result of a modification of the F-region dynamo field due to direct penetration of the electric field and/or changes in the neutral winds induced by the magnetic disturbance, (d) On the night of 21/22 March 1998, which was a magnetically disturbed period, plasma depletions could be seen simultaneously in all three observing wavelengths, i.e. in 630 nm, 777.4 nm and 557.7 nm. It is believed that this simultaneous occurrence was due to neutral density modifications as a result of enhanced magnetic activity. (e) Well developed brightness patterns were observed for the first time in 777.4 nm images. Earlier, such brightness patterns were observed only in 630 nm and 557.7 nm images. These brightness patterns initially appear as very small regions in the northern part of the image and then in about 90 min time, they attain their peak brightness and encompass the entire field-of-view in about 2 hrs 30 min. In some cases, brightness patterns contain one or two well developed plasma depletions within them. (f) The brightness patterns reported here differ from the earlier observations in that they do not show any differential behaviour in the direction of movement before and after the midnight, and that they are present for extended periods of time as large as 6 hrs. Key words. Atmospheric composition and structure (air-glow and aurora); Ionosphere (equatorial ionosphere; ionospheric ir
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