CIP Genebank DOIS Data Management

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DOIS Data Management and GRIN-Global

GLOBAL INFORMATION SYSTEM
GLIS
GENEBANK GENESYS-PGR GENEBANK Website
GRIN-Global
PUBLIC USER INTERNATIONAL
TREATY, Easy-SMTA
DOIS DATA MANAGEMENT
Record and
maintain DOI
forever
Accession
passport data
Register PGRFA in
GLIS, mint DOI if
not provided
Publish DOI
Publish DOI
Data Synchronization
between GLIS &
Genesys
DOIRegistrationUsingDOIinSMTA
Request
Germplasm
Search &
Register
Request
Process
Request: Use
DOIs in labels
and paper list Generate
SMTA with
DOIs
Receive
Germplasm
with DOIs in
labels, paper
list and SMTA
Process
Request: Store
SMTA
Report SMTA
with DOIs
Optionally publish DOIs if
new varieties are generated

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Nanoparticles synthesis and characterization

Nanoparticles synthesis and characterization

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kaibalyasahoo82800

We explore different scenarios to explain the chemical difference found in the remarkable giant-giant binary system HD138202+CD−3012303. For the first time, we suggest how to distinguish these scenarios by taking advantage of the extensive convective envelopes of giant stars. Methods. We carried out a high-precision determination of stellar parameters and abundances by applying a full line-by-line differential analysis on GHOST high-resolution spectra. We used the FUNDPAR program with ATLAS12 model atmospheres and specific opacities calculated for an arbitrary composition through a doubly iterated method. Physical parameters were estimated with the isochrones package and evolutionary tracks were calculated via MIST models. Results. We found a significant chemical difference between the two stars (∆[Fe/H]∼0.08dex), which is largely unexpected considering the insensitivity of giant stars to planetary ingestion and diffusion effects. We tested the possibility of engulfment events by using several different combinations of stellar mass, ingested mass, metallicity of the engulfed object and different convective envelopes. However, the planetary ingestion scenario does not seem to explain the observed differences. For the first time, we distinguished the source of chemical differences using a giant-giant binary system. By ruling out other possible scenarios such as planet formation and evolutionary effects between the two stars, we suggest that primordial inhomogeneities might explain the observed differences. This remarkable result implies that the metallicity differences that were observed in at least some main-sequence binary systems might be related to primordial inhomogeneities rather than engulfment events. We also discuss the important implications of finding primordial inhomogeneities, which affect chemical tagging and other fields such as planet formation. We strongly encourage the use of giantgiant pairs. They are a relevant complement to main-sequence pairs for determining the origin of the observed chemical differences in multiple systems.

Disentangling the origin of chemical differences using GHOST

Disentangling the origin of chemical differences using GHOST

Disentangling the origin of chemical differences using GHOST

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

Nightside clouds and disequilibrium chemistry on the hot Jupiter WASP-43b

Chemistry is the scientific study of matter, its properties, composition, structure, and the changes it undergoes. It's often divided into various sub-disciplines such as organic chemistry, inorganic chemistry, physical chemistry, analytical chemistry, and biochemistry. Chemistry plays a crucial role in understanding the world around us and has applications in various fields such as medicine, materials science, environmental science, and industry.

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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

Asymmetry in the atmosphere of the ultra-hot Jupiter WASP-76 b

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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

Formation of low mass protostars and their circumstellar disks

Context. Determining the size distribution of asteroids is key to understanding the collisional history and evolution of the inner Solar System. Aims. We aim to improve our knowledge of the size distribution of small asteroids in the main belt by determining the parallaxes of newly detected asteroids in the Hubble Space Telescope (HST) archive and subsequently their absolute magnitudes and sizes. Methods. Asteroids appear as curved trails in HST images because of the parallax induced by the fast orbital motion of the spacecraft. Taking into account the trajectory of this latter, the parallax effect can be computed to obtain the distance to the asteroids by fitting simulated trajectories to the observed trails. Using distance, we can obtain the absolute magnitude of an object and an estimation of its size assuming an albedo value, along with some boundaries for its orbital parameters. Results. In this work, we analyse a set of 632 serendipitously imaged asteroids found in the ESA HST archive. Images were captured with the ACS/WFC and WFC3/UVIS instruments. A machine learning algorithm (trained with the results of a citizen science project) was used to detect objects in these images as part of a previous study. Our raw data consist of 1031 asteroid trails from unknown objects, not matching any entries in the Minor Planet Center (MPC) database using their coordinates and imaging time. We also found 670 trails from known objects (objects featuring matching entries in the MPC). After an accuracy assessment and filtering process, our analysed HST asteroid set consists of 454 unknown objects and 178 known objects. We obtain a sample dominated by potential main belt objects featuring absolute magnitudes (H) mostly between 15 and 22 mag. The absolute magnitude cumulative distribution logN(H > H0) ∝ αlog(H0) confirms the previously reported slope change for 15 < H < 18, from α ≈ 0.56 to α ≈ 0.26, maintained in our case down to absolute magnitudes of around H ≈ 20, and therefore expanding the previous result by approximately two magnitudes. Conclusions. HST archival observations can be used as an asteroid survey because the telescope pointings are statistically randomly oriented in the sky and cover long periods of time. They allow us to expand the current best samples of astronomical objects at no extra cost in regard to telescope time.

Hubble Asteroid Hunter III. Physical properties of newly found asteroids

Hubble Asteroid Hunter III. Physical properties of newly found asteroids

Hubble Asteroid Hunter III. Physical properties of newly found asteroids

Past civilisations have nurtured small populations of those trying to understand and manipulate nature to some advantage in materials, tools, weapons, food, and wealth. However, they never formed communities and lacked the means of recording, communicating, and sharing successes and failures. They also lacked a common framework/philosophy to qualify them as scientists, but that all began to change in the 16th Century. In this lecture we consider the progression to a philosophy of science, and the underlying principles and assumptions that now guide scientific inquiry.We also examines the nature of scientific knowledge, the methods of acquisition, evolution, and significance over past centuries, and reflect on the value to society. In the struggle to solve problems, deliver understanding, and reveal the truth about our universe, science had to suffer and survive: ignorance, bigotry, established superstitions, and the ‘diktats’ of religions and politics, and latterly, falling education standards mired by social media. We chart that ‘scientific’ journey emphasising the importance of observation, experimentation, and the search for universal laws. Ultimately, this essentially Aristotelian perspective was challenged and overtaken by the rise of empiricism, which emphasised the importance of sensory experience and the limitations of human knowledge. Science continues to evolve and provide us with the best truths attainable with our leading edge technologies of observation and experimentation. Today, it stands as the greatest and richest contributor to human knowledge, understanding, progress, and wellbeing. In turn, debates and controversies are ongoing, shaping the field and philosophy which remains essential for understanding the nature of scientific knowledge and the models it creates. But unlike any belief system, the answers and models furnishers by science are not certain and invariant, they tend to be stochastic and incomplete - ‘the best we can do’ at a given time.

The Philosophy of Science

The Philosophy of Science

The Philosophy of Science

University of Hertfordshire

TEST BANK For Radiologic Science for Technologists, 12th Edition by Stewart C...

TEST BANK For Radiologic Science for Technologists, 12th Edition by Stewart C...

TEST BANK For Radiologic Science for Technologists, 12th Edition by Stewart C...

A botany file is similar to a chemistry practical file but specifically focuses on experiments and observations related to plants. It typically includes detailed descriptions of plant-related experiments, such as germination studies, growth experiments, tissue culture techniques, plant anatomy investigations, and ecological surveys. The file may contain records of plant specimens collected, their classification, characteristics, and ecological significance. Additionally, it may include diagrams, photographs, drawings, tables, and data analysis related to plant research. Like a chemistry practical file, a botany file serves as a documentation of practical work conducted in the field of botany and is often used for assessment and educational purposes.

Botany 4th semester file By Sumit Kumar yadav.pdf

Botany 4th semester file By Sumit Kumar yadav.pdf

Botany 4th semester file By Sumit Kumar yadav.pdf

Sumit Kumar yadav

The primary distinction between a test cross and a backcross is that a test cross is used to determine the genotype of a phenotypically dominant individual, whereas a backcross is used to recover a dominant genotype from a parent who has an extreme genotype. The hybrids that are backcrossed are known as 'BC' hybrids. For example, a BC1 hybrid is an F1 hybrid that was crossed with one of its parents or a genetically similar species. The BC2 hybrid is defined as a BC1 hybrid that has been crossed with the same parent or genetically similar species. Other instances include backcrossing in animals. A system of breeding in which repeated backcrosses are made to transfer a specific character to a well-adapted variety for which the variety is deficient is referred to as backcross breeding This approach is infrequently utilized in vegetatively propagated crops such as sugarcane and potatoes, and only with slight alterations. A test cross is a genetic technique for determining an unknown genotype in a dominant person. It is a breeding procedure in which a (known genotype) homozygous recessive individual is paired with an individual of the opposite mating type who has an unknown dominant genotype. The phenotypic characteristics of the resulting children are investigated, and the genotype of the examined individual is determined appropriately. If all of the progeny from the test cross are dominant, we may conclude that the genotype of the tested unknown person is homozygous dominant. If 50% of kids exhibit dominant traits and the remaining 50% exhibit recessive traits, we may conclude that the genotype of the tested unknown individual is heterozygous dominant. #genetics #backcross #testcross #mendel #crosses #monohybridtestcross #backcrossandtestcross #typesofcross #dihybridtestcross #limitationsofcross #applicationsofcross #mscbotany #botany

DIFFERENCE IN BACK CROSS AND TEST CROSS

DIFFERENCE IN BACK CROSS AND TEST CROSS

DIFFERENCE IN BACK CROSS AND TEST CROSS

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Chromatin Structure | EUCHROMATIN | HETEROCHROMATIN

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sankalpkumarsahoo174

Jupiter’s moon Io hosts extensive volcanism, driven by tidal heating. The isotopic composition of Io's inventory of volatile chemical elements, including sulfur and chlorine, reflects its outgassing and mass loss history, and thus records information about its evolution. We used millimeter observations of Io’s atmosphere to measure sulfur isotopes in gaseous SO2 and SO, and chlorine isotopes in gaseous NaCl and KCl. We find 34S/32S = 0.0595 ± 0.0038 (equivalent to δ34S = +347 ± 86‰), which is highly enriched compared to average Solar System values and indicates that Io has lost 94 to 99% of its available sulfur. Our measurement of 37Cl/35Cl = 0.403 ± 0.028 (δ37Cl = +263 ± 88‰) shows that chlorine is similarly enriched. These results indicate that Io has been volcanically active for most (or all) of its history, with potentially higher outgassing and mass-loss rates at earlier times.

Isotopic evidence of long-lived volcanism on Io

Isotopic evidence of long-lived volcanism on Io

Isotopic evidence of long-lived volcanism on Io

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Recently uploaded (20)

Nanoparticles synthesis and characterization

Nanoparticles synthesis and characterization

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Disentangling the origin of chemical differences using GHOST

Disentangling the origin of chemical differences using GHOST

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Nightside clouds and disequilibrium chemistry on the hot Jupiter WASP-43b

Nightside clouds and disequilibrium chemistry on the hot Jupiter WASP-43b

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Chemistry 4th semester series (krishna).pdf

Chemistry 4th semester series (krishna).pdf

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Zoology 4th semester series (krishna).pdf

Zoology 4th semester series (krishna).pdf

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Asymmetry in the atmosphere of the ultra-hot Jupiter WASP-76 b

Asymmetry in the atmosphere of the ultra-hot Jupiter WASP-76 b

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Labelling Requirements and Label Claims for Dietary Supplements and Recommend...

Labelling Requirements and Label Claims for Dietary Supplements and Recommend...

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Formation of low mass protostars and their circumstellar disks

Formation of low mass protostars and their circumstellar disks

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Hubble Asteroid Hunter III. Physical properties of newly found asteroids

Hubble Asteroid Hunter III. Physical properties of newly found asteroids

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The Philosophy of Science

The Philosophy of Science

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DIFFERENCE IN BACK CROSS AND TEST CROSS

DIFFERENCE IN BACK CROSS AND TEST CROSS

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Isotopic evidence of long-lived volcanism on Io

Isotopic evidence of long-lived volcanism on Io

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Biopesticide (2).pptx .This slides helps to know the different types of biop...

Biopesticide (2).pptx .This slides helps to know the different types of biop...

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Green chemistry and Sustainable development.pptx

Green chemistry and Sustainable development.pptx

CIP Genebank DOIS Data Management

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