A CRITICAL REVIEW ON CONCEPT OF PRABHAVA

Ayurveda The science of life has been practiced in India from time immemorial and has stood test of time. This is due to the vast conceptual canvas and framework of Ayurveda. It is important to realize that, Ayurveda is not confined to medicines only, it tackles the whole subject of Life in its various ramifications. The basic fundamentals of Ayurveda are to be understood and thoroughly implemented to achieve the target of promotion of health in its true sense and complete cure from disease. According to Ayurvedic pharmacology the drug action is attributed to certain principles namely Rasa, Guna, Virya, Vipaka and Prabhava. It was observed that both the drugs as well as the living body have Panchabhutika composition in common and if the drugs are used sensibly, they can alter the body components accordingly. However if the Ayurvedic concepts are not properly understood and interpreted in globally accepted language; the tremendous efforts in research would go meaningless and futile. It is therefore strongly needed to utilize the tools derived from the advancement in technology in the new millennium for re-establishing concepts of Ayurveda in current perspectives. Although many Ayurvedic concepts described in the Samhitas seem very easy, but they are actually very difficult to understand, as the Samhitas presented everything in a concise form. There are certain concepts which need to be explored and evaluated through their practical applicability. One of such concepts is the concept of Prabhava. In a nutshell there is an urgent need to develop a process and scientific method to understand these principles. This review is an attempt to highlight the concept of Prabhava and its significance in present era

The underlying factors of occurrence of Mucormycosis in post-COVID-19 patients – A meta-analysis of case histories

Mucormycosis is a life-threatening fungal infection caused by fungi of the order Mucorales. It usually affects people with weakened immune systems, such as those with uncontrolled diabetes, acquired immunodeficiency syndrome, iatrogenic immunosuppression, and hematological malignancies, as well as individuals who have had organ transplants. The type of mucormycosis a person suffers from is often determined by their underlying conditions. The most common types are rhino-cerebral mucormycosis, pulmonary mucormycosis, cutaneous mucormycosis, cerebral mucormycosis, gastrointestinal mucormycosis, and disseminated mucormycosis. The incidence of mucormycosis has been increasing over the years, with an overall mortality rate of 54%. Recent cases have shown a correlation between COVID-19 and mucormycosis. Using anti-inflammatory drugs to combat the cytokine storm associated with COVID-19 can weaken the immune system, making individuals more susceptible to opportunistic fungal infections like mucormycosis. Underlying health conditions further exacerbate the condition. This study reviewing 198 cases of mucormycosis and conducting a meta-analysis found that post-COVID-19 patients most commonly developed rhino-orbital-cerebral mucormycosis, followed by pulmonary and gastrointestinal mucormycosis. The study also identified diabetes as the most common underlying factor contributing to the development of mucormycosis in post-COVID-19 patients, followed by hypertension and obesity. The study also examined the influence of age, affected organs, and the use of certain drugs on the development of mucormycosis. Age was found to be a significant factor in the infection. This meta-analysis is one of the first to compare post-COVID mucormycosis cases with those from the pre-COVID era. The hope is that this study and analysis will help identify the determinants of mucormycosis in post-COVID patients and aid the scientific community in finding a solution to this problem

First measurement of the Hubble Constant from a Dark Standard Siren using the Dark Energy Survey Galaxies and the LIGO/Virgo Binary–Black-hole Merger GW170814

International audienceWe present a multi-messenger measurement of the Hubble constant H 0 using the binary–black-hole merger GW170814 as a standard siren, combined with a photometric redshift catalog from the Dark Energy Survey (DES). The luminosity distance is obtained from the gravitational wave signal detected by the Laser Interferometer Gravitational-Wave Observatory (LIGO)/Virgo Collaboration (LVC) on 2017 August 14, and the redshift information is provided by the DES Year 3 data. Black hole mergers such as GW170814 are expected to lack bright electromagnetic emission to uniquely identify their host galaxies and build an object-by-object Hubble diagram. However, they are suitable for a statistical measurement, provided that a galaxy catalog of adequate depth and redshift completion is available. Here we present the first Hubble parameter measurement using a black hole merger. Our analysis results in , which is consistent with both SN Ia and cosmic microwave background measurements of the Hubble constant. The quoted 68% credible region comprises 60% of the uniform prior range [20, 140] km s−1 Mpc−1, and it depends on the assumed prior range. If we take a broader prior of [10, 220] km s−1 Mpc−1, we find (57% of the prior range). Although a weak constraint on the Hubble constant from a single event is expected using the dark siren method, a multifold increase in the LVC event rate is anticipated in the coming years and combinations of many sirens will lead to improved constraints on H 0

Searches for gravitational waves from known pulsars at two harmonics in 2015-2017 LIGO data

International audienceWe present a search for gravitational waves from 222 pulsars with rotation frequencies ≳10 Hz. We use advanced LIGO data from its first and second observing runs spanning 2015–2017, which provides the highest-sensitivity gravitational-wave data so far obtained. In this search we target emission from both the l = m = 2 mass quadrupole mode, with a frequency at twice that of the pulsar’s rotation, and the l = 2, m = 1 mode, with a frequency at the pulsar rotation frequency. The search finds no evidence for gravitational-wave emission from any pulsar at either frequency. For the l = m = 2 mode search, we provide updated upper limits on the gravitational-wave amplitude, mass quadrupole moment, and fiducial ellipticity for 167 pulsars, and the first such limits for a further 55. For 20 young pulsars these results give limits that are below those inferred from the pulsars’ spin-down. For the Crab and Vela pulsars our results constrain gravitational-wave emission to account for less than 0.017% and 0.18% of the spin-down luminosity, respectively. For the recycled millisecond pulsar J0711−6830 our limits are only a factor of 1.3 above the spin-down limit, assuming the canonical value of 1038 kg m2 for the star’s moment of inertia, and imply a gravitational-wave-derived upper limit on the star’s ellipticity of 1.2 × 10−8. We also place new limits on the emission amplitude at the rotation frequency of the pulsars

Search for the isotropic stochastic background using data from Advanced LIGO's second observing run

The stochastic gravitational-wave background is a superposition of sources that are either too weak or too numerous to detect individually. In this study, we present the results from a cross-correlation analysis on data from Advanced LIGO’s second observing run (O2), which we combine with the results of the first observing run (O1). We do not find evidence for a stochastic background, so we place upper limits on the normalized energy density in gravitational waves at the 95% credible level of Ω GW < 6.0 × 10 − 8 for a frequency-independent (flat) background and Ω GW < 4.8 × 10 − 8 at 25 Hz for a background of compact binary coalescences. The upper limit improves over the O1 result by a factor of 2.8. Additionally, we place upper limits on the energy density in an isotropic background of scalar- and vector-polarized gravitational waves, and we discuss the implication of these results for models of compact binaries and cosmic string backgrounds. Finally, we present a conservative estimate of the correlated broadband noise due to the magnetic Schumann resonances in O2, based on magnetometer measurements at both the LIGO Hanford and LIGO Livingston observatories. We find that correlated noise is well below the O2 sensitivity

Search for Gravitational-wave Signals Associated with Gamma-Ray Bursts during the Second Observing Run of Advanced LIGO and Advanced Virgo

We present the results of targeted searches for gravitational-wave transients associated with gamma-ray bursts during the second observing run of Advanced LIGO and Advanced Virgo, which took place from 2016 November to 2017 August. We have analyzed 98 gamma-ray bursts using an unmodeled search method that searches for generic transient gravitational waves and 42 with a modeled search method that targets compact-binary mergers as progenitors of short gamma-ray bursts. Both methods clearly detect the previously reported binary merger signal GW170817, with p-values of <9.38 × 10−6 (modeled) and 3.1 × 10−4 (unmodeled). We do not find any significant evidence for gravitational-wave signals associated with the other gamma-ray bursts analyzed, and therefore we report lower bounds on the distance to each of these, assuming various source types and signal morphologies. Using our final modeled search results, short gamma-ray burst observations, and assuming binary neutron star progenitors, we place bounds on the rate of short gamma-ray bursts as a function of redshift for z ≤ 1. We estimate 0.07─1.80 joint detections with Fermi-GBM per year for the 2019─20 LIGO-Virgo observing run and 0.15─3.90 per year when current gravitational-wave detectors are operating at their design sensitivities