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This is a presentation on Indian denim brand Hard currency denim jeans brand. It contains all details regarding the denim brand.
Hard currency
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prince gupta
Student of Dezyne E’cole College ,www.dezyneecole.com Fashion design is a form of art dedicated to the creation of clothing and other lifestyle accessories. Modern fashion design is divided into two basic categories: haute couture and ready-to-wear. The haute couture collection is dedicated to certain customers and is custom sized to fit these customers exactly. In order to qualify as a haute couture house, a designer has to be part of the Syndical Chamber for Haute Couture and show a new collection twice a year presenting a minimum of 35 different outfits each time. Ready-to-wear collections are standard sized, not custom made, so they are more suitable for large production runs. They are also split into two categories: designer/createur and confection collections. Designer collections have a higher quality and finish as well as an unique design. They often represent a certain philosophy and are created to make a statement rather than for sale. Both ready-to-wear and haute-couture collections are presented on international catwalks.
Ruchika Sharma ,Fashion Designer Womens Wear
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dezyneecole
HOW BENEFICIAL IS KERALA HANDLOOMS FOR A CONSUMER OF CLOTHING PRODUCTS IS ....?
Kerala handlooms
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Chandran Kani
a ppt on kalasha tribe of pakishtan.
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prince gupta
This Project has been Developed by the Student of Dezyne E'cole College Doing Her Interior Design Studies Bachelor Degree Programme + 2Yr Residential & Commercial Design Diploma Programme www.dezyneecole.com
Srishti Sharma,,B.Sc-ID+ 2 Year Residential & Commercial Design Diploma
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dezyneecole
a ppt on kuchipudi dance
Kuchipudi
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phulkari of panjab kulture and its daily life impacts
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complete information about raymonds and park avenue based on retail unit. all the report is collected from retail house survey.
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This is a presentation on Indian denim brand Hard currency denim jeans brand. It contains all details regarding the denim brand.
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prince gupta
Student of Dezyne E’cole College ,www.dezyneecole.com Fashion design is a form of art dedicated to the creation of clothing and other lifestyle accessories. Modern fashion design is divided into two basic categories: haute couture and ready-to-wear. The haute couture collection is dedicated to certain customers and is custom sized to fit these customers exactly. In order to qualify as a haute couture house, a designer has to be part of the Syndical Chamber for Haute Couture and show a new collection twice a year presenting a minimum of 35 different outfits each time. Ready-to-wear collections are standard sized, not custom made, so they are more suitable for large production runs. They are also split into two categories: designer/createur and confection collections. Designer collections have a higher quality and finish as well as an unique design. They often represent a certain philosophy and are created to make a statement rather than for sale. Both ready-to-wear and haute-couture collections are presented on international catwalks.
Ruchika Sharma ,Fashion Designer Womens Wear
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dezyneecole
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phulkari of panjab kulture and its daily life impacts
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GUIDELINES ON SIMILAR BIOLOGICS Regulatory Requirements for Marketing Authori...
GUIDELINES ON SIMILAR BIOLOGICS Regulatory Requirements for Marketing Authori...
Lokesh Kothari
Understanding circumstellar disks is of prime importance in astrophysics, however, their birth process remains poorly constrained due to observational and numerical challenges. Recent numerical works have shown that the small-scale physics, often wrapped into a sub-grid model, play a crucial role in disk formation and evolution. This calls for a combined approach in which both the protostar and circumstellar disk are studied in concert. Aims. We aim to elucidate the small scale physics and constrain sub-grid parameters commonly chosen in the literature by resolving the star-disk interaction. Methods. We carry out a set of very high resolution 3D radiative-hydrodynamics simulations that self-consistently describe the collapse of a turbulent dense molecular cloud core to stellar densities. We study the birth of the protostar, the circumstellar disk, and its early evolution (< 6 yr after protostellar formation). Results. Following the second gravitational collapse, the nascent protostar quickly reaches breakup velocity and sheds its surface material, thus forming a hot (∼ 103 K), dense, and highly flared circumstellar disk. The protostar is embedded within the disk, such that material can flow without crossing any shock fronts. The circumstellar disk mass quickly exceeds that of the protostar, and its kinematics are dominated by self-gravity. Accretion onto the disk is highly anisotropic, and accretion onto the protostar mainly occurs through material that slides on the disk surface. The polar mass flux is negligible in comparison. The radiative behavior also displays a strong anisotropy, as the polar accretion shock is shown to be supercritical whereas its equatorial counterpart is subcritical. We also f ind a remarkable convergence of our results with respect to initial conditions. Conclusions. These results reveal the structure and kinematics in the smallest spatial scales relevant to protostellar and circumstellar disk evolution. They can be used to describe accretion onto regions commonly described by sub-grid models in simulations studying larger scale physics.
Formation of low mass protostars and their circumstellar disks
Formation of low mass protostars and their circumstellar disks
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This ppt is based on Bioinformatics topic American Type Culture Collection (ATCC)
American Type Culture Collection (ATCC).pptx
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abhishekdhamu51
Nanoparticles synthesis and characterization
Nanoparticles synthesis and characterization
Nanoparticles synthesis and characterization
kaibalyasahoo82800
Microbiology
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Bacterial Identification and Classifications
Areesha Ahmad
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Zoology is the branch of biology that focuses on the study of animals, including their behavior, physiology, anatomy, evolution, and distribution. It's a diverse field that encompasses everything from microscopic organisms to complex vertebrates.
Zoology 4th semester series (krishna).pdf
Zoology 4th semester series (krishna).pdf
Sumit Kumar yadav
Proposed feature alignment using Sinkhorn divergence as a representation learning approach for domain generalization in time-series forecasting, with a specific focus on N-BEATS and its variants.
Feature-aligned N-BEATS with Sinkhorn divergence (ICLR '24)
Feature-aligned N-BEATS with Sinkhorn divergence (ICLR '24)
Joonhun Lee
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Presentation from the "Opening up Research" conference organised by the University of Manchester's Office for Open Research. 24 April 2024 https://www.openresearch.manchester.ac.uk/ https://fairspectra.net https://alexhenderson.info
FAIRSpectra - Enabling the FAIRification of Spectroscopy and Spectrometry
FAIRSpectra - Enabling the FAIRification of Spectroscopy and Spectrometry
Alex Henderson
Wepresent Atacama Large Millimeter/submillimeter Array 12-m, 7-m, and Total Power Array observations of the FUOrionis outbursting system, covering spatial scales ranging from 160 to 25,000 au. The high-resolution interferometric data reveal an elongated 12CO(2–1) feature previously observed at lower resolution in 12CO(3–2). Kinematic modeling indicates that this feature can be interpreted as an accretion streamer feeding the binary system. The mass infall rate provided by the streamer is significantly lower than the typical stellar accretion rates (even in quiescent states), suggesting that this streamer alone is not massive enough to sustain the enhanced accretion rates characteristic of the outbursting class prototype. The observed streamer may not be directly linked to the current outburst, but rather a remnant of a previous, more massive streamer that may have contributed enough to the disk mass to render it unstable and trigger the FU Orionis outburst. The new data detect, for the first time, a vast, slow-moving carbon monoxide molecular outflow emerging from this object. To accurately assess the outflow properties (mass, momentum, and kinetic energy), we employ 13CO(2–1) data to correct for optical depth effects. The analysis indicates that the outflow corresponds to swept-up material not associated with the current outburst, similar to the slow molecular outflows observed around other FUor and Class I protostellar objects.
Discovery of an Accretion Streamer and a Slow Wide-angle Outflow around FUOri...
Discovery of an Accretion Streamer and a Slow Wide-angle Outflow around FUOri...
Sérgio Sacani
Clean In Place
Clean In Place(CIP).pptx .
Clean In Place(CIP).pptx .
Poonam Aher Patil
Site Acceptance test
Site Acceptance Test .
Site Acceptance Test .
Poonam Aher Patil
Context. WASP-76 b has been a recurrent subject of study since the detection of a signature in high-resolution transit spectroscopy data indicating an asymmetry between the two limbs of the planet. The existence of this asymmetric signature has been confirmed by multiple studies, but its physical origin is still under debate. In addition, it contrasts with the absence of asymmetry reported in the infrared (IR) phase curve. Aims. We provide a more comprehensive dataset of WASP-76 b with the goal of drawing a complete view of the physical processes at work in this atmosphere. In particular, we attempt to reconcile visible high-resolution transit spectroscopy data and IR broadband phase curves. Methods. We gathered 3 phase curves, 20 occultations, and 6 transits for WASP-76 b in the visible with the CHEOPS space telescope. We also report the analysis of three unpublished sectors observed by the TESS space telescope (also in the visible), which represents 34 phase curves. Results. WASP-76 b displays an occultation of 260±11 and 152±10 ppm in TESS and CHEOPS bandpasses respectively. Depending on the composition assumed for the atmosphere and the data reduction used for the IR data, we derived geometric albedo estimates that range from 0.05 ± 0.023 to 0.146 ± 0.013 and from <0.13 to 0.189 ± 0.017 in the CHEOPS and TESS bandpasses, respectively. As expected from the IR phase curves, a low-order model of the phase curves does not yield any detectable asymmetry in the visible either. However, an empirical model allowing for sharper phase curve variations offers a hint of a flux excess before the occultation, with an amplitude of ∼40 ppm, an orbital offset of ∼−30◦ , and a width of ∼20◦ . We also constrained the orbital eccentricity of WASP-76 b to a value lower than 0.0067, with a 99.7% confidence level. This result contradicts earlier proposed scenarios aimed at explaining the asymmetry observed in high-resolution transit spectroscopy. Conclusions. In light of these findings, we hypothesise that WASP-76 b could have night-side clouds that extend predominantly towards its eastern limb. At this limb, the clouds would be associated with spherical droplets or spherically shaped aerosols of an unknown species, which would be responsible for a glory effect in the visible phase curves.
Asymmetry in the atmosphere of the ultra-hot Jupiter WASP-76 b
Asymmetry in the atmosphere of the ultra-hot Jupiter WASP-76 b
Sérgio Sacani
Factory Acceptance Test( FAT)
Factory Acceptance Test( FAT).pptx .
Factory Acceptance Test( FAT).pptx .
Poonam Aher Patil
HotJupiters are amongthebest-studied exoplanets, but it is still poorly understood how their chemical composition and cloud properties vary with longitude. Theoretical models predict that clouds may condense on the nightside and that molecular abundances can be driven out of equilibrium by zonal winds. Here we report a phase-resolved emission spectrum of the hot Jupiter WASP-43b measured from 5–12µ 5–12µ 5–12µm with JWST’s Mid-Infrared Instrument (MIRI). 1524 ±35 1524 ±35 and 863±23 The spectra reveal a large day–night temperature contrast (with average brightness temperatures of 1524 ± 35 863 ±23 863 ±23Kelvin, respectively) and evidence for water absorption at all orbital phases. Comparisons with three-dimensional atmospheric models show that both the phase curve shape and emission spectra strongly suggest the presence of nightside clouds which become optically thick to thermal emission at pressures greater than ∼100mbar. The dayside is consistent with a cloudless atmosphere above the mid-infrared photosphere. Con3trary to expectations from equilibrium chemistry but consistent with disequilibrium kinetics models, methane is not detected on the nightside (2σ upper limit of 1–6 parts per million, depending on model assumptions).
Nightside clouds and disequilibrium chemistry on the hot Jupiter WASP-43b
Nightside clouds and disequilibrium chemistry on the hot Jupiter WASP-43b
Sérgio Sacani
Proteome is a set of proteins produced in an organism, system, or biological context or entire set of proteins that is, or can be, expressed by a genome, cell, tissue, or organism at a certain expressed time in a given set of condition. Proteomics is the study of all the proteins produced by a cell.
Proteomics: types, protein profiling steps etc.
Proteomics: types, protein profiling steps etc.
Silpa
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Formation of low mass protostars and their circumstellar disks
Formation of low mass protostars and their circumstellar disks
American Type Culture Collection (ATCC).pptx
American Type Culture Collection (ATCC).pptx
Nanoparticles synthesis and characterization
Nanoparticles synthesis and characterization
Bacterial Identification and Classifications
Bacterial Identification and Classifications
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Zoology 4th semester series (krishna).pdf
Zoology 4th semester series (krishna).pdf
Feature-aligned N-BEATS with Sinkhorn divergence (ICLR '24)
Feature-aligned N-BEATS with Sinkhorn divergence (ICLR '24)
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FAIRSpectra - Enabling the FAIRification of Spectroscopy and Spectrometry
FAIRSpectra - Enabling the FAIRification of Spectroscopy and Spectrometry
Discovery of an Accretion Streamer and a Slow Wide-angle Outflow around FUOri...
Discovery of an Accretion Streamer and a Slow Wide-angle Outflow around FUOri...
Clean In Place(CIP).pptx .
Clean In Place(CIP).pptx .
Site Acceptance Test .
Site Acceptance Test .
Asymmetry in the atmosphere of the ultra-hot Jupiter WASP-76 b
Asymmetry in the atmosphere of the ultra-hot Jupiter WASP-76 b
Factory Acceptance Test( FAT).pptx .
Factory Acceptance Test( FAT).pptx .
Nightside clouds and disequilibrium chemistry on the hot Jupiter WASP-43b
Nightside clouds and disequilibrium chemistry on the hot Jupiter WASP-43b
Proteomics: types, protein profiling steps etc.
Proteomics: types, protein profiling steps etc.
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