IMPROVED PROCESS FOR THE PREPARATION OF 4-((4-METHYLPIPERAZIN-1-YL)METHYL)-3-(TRIFLUOROMETHYL)ANILINE

IMPROVED PROCESS FOR THE PREPARATION OF 4-((4-METHYLPIPERAZIN-1-YL)METHYL)-3-(TRIFLUOROMETHYL)ANILINE The present invention relates to an improved process for the preparation of 4-((4-methylpiperazin-1-yl)methyl)-3-(trifluoromethyl)aniline formula (1). Formula (1) 4-((4-methylpiperazin-1-yl)methyl)-3-(trifluoromethyl)aniline is used in the preparation of Ponatinib hydrochloride

IMPROVED PROCESS FOR THE PREPARATION OF LURBINECTEDIN

The present disclosure relates to an improved process for the preparation of Lurbinectedin of formula-1which is structurally shown as below: Formula-

The feedback of an HC HII region on its parental molecular core: The case of core A1 in the star-forming region G24.78+0.08

Context: G24.78+0.08 is a well known high-mass star-forming region, where several molecular cores harboring OB young stellar objects are found inside a clump of size ≈1 pc. This article focuses on the most prominent of these cores, A1, where an intense hypercompact (HC) HII region has been discovered by previous observations. Aims: Our aim is to determine the physical conditions and the kinematics of core A1, and study the interaction of the HII region with the parental molecular core. Methods: We combine ALMA 1.4 mm high-angular resolution (≈0.′′2) observations of continuum and line emission with multi-epoch Very Long Baseline Interferometry data of water 22 GHz and methanol 6.7 GHz masers. These observations allow us to study the gas kinematics on linear scales from 10 to 104 au, and to accurately map the physical conditions of the gas over core A1. Results: The 1.4 mm continuum is dominated by free-free emission from the intense HC HII region (size ≈1000 au) observed to the North of core A1 (region A1N). Analyzing the H30α line, we reveal a fast bipolar flow in the ionized gas, covering a range of LSR velocities (VLSR) of ≈60 km s−1. The amplitude of the VLSR gradient, 22 km s−1 mpc−1, is one of the highest so far observed towards HC HII regions. Water and methanol masers are distributed around the HC HII region in A1N, and the maser three-dimensional (3D) velocities clearly indicate that the ionized gas is expanding at high speed (≥200 km s−1) into the surrounding molecular gas. The temperature distribution (in the range 100–400 K) over core A1, traced with molecular (CH3OCHO, 13CH3CN, 13CH3OH, and CH3CH2CN) transitions with level energy in the range 30 K ≤ Eu/k ≤ 300 K, reflects the distribution of shocks produced by the fast-expansion of the ionized gas of the HII region. The high-energy (550 K ≤ Eu/k ≤ 800 K) transitions of vibrationally excited CH3CN are likely radiatively pumped, and their rotational temperature can significantly differ from the kinetic temperature of the gas. Over core A1, the VLSR maps from both the 1.4 mm molecular lines and the 6.7 GHz methanol masers consistently show a VLSR gradient (amplitude ≈0.3 km s−1 mpc−1) directed approximately S–N. Rather than gravitationally supported rotation of a massive toroid, we interpret this velocity gradient as a relatively slow expansion of core A1

Substructures in the Keplerian disc around the O-type (proto-)star G17.64+0.16

Contains fulltext : 205611.pdf (publisher's version ) (Open Access

Accelerating infall and rotational spin-up in the hot molecular core G31.41+0.31

As part of our effort to search for circumstellar disks around high-mass stellar objects, we observed the well-known core G31.41 +0.31 with ALMA at 1.4 mm with an angular resolution of ~0.′′22 (~1700 au). The dust continuum emission has been resolved into two cores namely Main and NE. The Main core, which has the stronger emission and is the more chemically rich, has a diameter of ~5300 au, and is associated with two free-free continuum sources. The Main core looks featureless and homogeneous in dust continuum emission and does not present any hint of fragmentation. Each transition of CH₃CN and CH₃OCHO, both ground and vibrationally excited, as well as those of CH₃CN isotopologues, shows a clear velocity gradient along the NE–SW direction, with velocity linearly increasing with distance from the center, consistent with solid-body rotation. However, when comparing the velocity field of transitions with different upper level energies, the rotation velocity increases with increasing energy of the transition, which suggests that the rotation speeds up toward the center. Spectral lines towardtoward the dust continuum peak show an inverse P-Cygni profile that supports the existence of infall in the core. The infall velocity increases with the energy of the transition suggesting that the infall is accelerating toward the center of the core, consistent with gravitational collapse. Despite the monolithic appearance of the Main core, the presence of red-shifted absorption, the existence of two embedded free-free sources at the center, and the rotational spin-up are consistent with an unstable core undergoing fragmentation with infall and differential rotation due to conservation of angular momentum. Therefore, the most likely explanation for the monolithic morphology is that the large opacity of the dust emission prevents the detection of any inhomogeneity in the core

Chasing discs around O-type (proto)stars: ALMA evidence for an SiO disc and disc wind from G17.64+0.16★

We present high angular resolution (~0.2″) continuum and molecular emission line Atacama Large Millimeter/sub-millimeter Array (ALMA) observations of G17.64+0.16 in Band 6 (220−230 GHz) taken as part of a campaign in search of circumstellar discs around (proto)-O-stars. At a resolution of ~400 au the main continuum core is essentially unresolved and isolated from other strong and compact emission peaks. We detect SiO (5–4) emission that is marginally resolved and elongated in a direction perpendicular to the large-scale outflow seen in the 13 CO (2−1) line using the main ALMA array in conjunction with the Atacama Compact Array (ACA). Morphologically, the SiO appearsto represent a disc-like structure. Using parametric models we show that the position-velocity profile of the SiO is consistent with the Keplerian rotation of a disc around an object between 10 and 30 M⊙ in mass, only if there is also radial expansion from a separate structure. The radial motion component can be interpreted as a disc wind from the disc surface. Models with a central stellar object mass between 20 and 30 M⊙ are the most consistent with the stellar luminosity (1 × 105 L⊙) and indicative of an O-type star. The H30α millimetre recombination line (231.9 GHz) is also detected, but spatially unresolved, and is indicative of a very compact, hot, ionised region co-spatial with the dust continuum core. The broad line-width of the H30α emission (full-width-half-maximum = 81.9 km s−1) is not dominated by pressure-broadening but is consistent with underlying bulk motions. These velocities match those required for shocks to release silicon from dust grains into the gas phase. CH3 CN and CH3 OH thermal emission also shows two arc shaped plumes that curve away from the disc plane. Their coincidence with OH maser emission suggests that they could trace the inner working surfaces of a wide-angle wind driven by G17.64 which impacts the diffuse remnant natal cloud before being redirected into the large-scale outflow direction. Accounting for all observables, we suggest that G17.64 is consistent with a O-type young stellar object in the final stages of protostellar assembly, driving a wind, but that has not yet developed into a compact H II region. The existance and detection of the disc in G17.64 is likely related to its isolated and possibly more evolved nature, traits which may underpin discs in similar sources

Additional file 2: of Is adjunctive naturopathy associated with improved glycaemic control and a reduction in need for medications among type 2 Diabetes patients? A prospective cohort study from India

Dataset. (XLS 57 kb

Additional file 1: of Is adjunctive naturopathy associated with improved glycaemic control and a reduction in need for medications among type 2 Diabetes patients? A prospective cohort study from India

Codebook. (TXT 8 kb

Infant & Child Mortality in Pakistan and its Determinants: A Review

Over the years, several developing countries have been suffering from high infant and child mortality rates, however, according to the recent statistics, Pakistan falls high on the list. Our narrative review of copious research on this topic highlights that several factors, such as complications associated with premature births, high prevalence of birth defects, lack of vaccination, unsafe deliveries, poor breastfeeding practices, complications during delivery, sudden infant death syndrome (SIDS), poor socioeconomic conditions, and a struggling healthcare system, have influenced these rates. Bearing in mind the urgency of addressing the increased infant and child mortality rate in Pakistan, multiple steps must be taken in order to prevent unnecessary deaths. An effective initiative could be spreading awareness and education among women, as a lack of education among women has been indirectly linked to increased child mortality in Pakistan across many researches conducted on the issue. Furthermore, the government should invest in healthcare by hiring more physicians and providing better supplies and improving infrastructure, especially in underdeveloped areas, to decrease child mortality due to lack of clean water and poor hygiene. Lastly, telemedicine should be made common in order to provide easy access to women who cannot visit the hospital