Introductory meteorology & climatic change AMET5311 NOTES IGKV

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The document discusses the results of a study on the impact of COVID-19 lockdowns on air pollution. Researchers found that lockdowns led to significant short-term reductions in nitrogen dioxide and fine particulate matter pollution globally as economic activities slowed. However, the impacts on greenhouse gases and long-term air quality improvements remain uncertain without permanent behavior and economic changes.

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

Introductory meteorology & climatic change AMET5311 NOTES IGKV

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RizalinePalanog2

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

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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...

COST ESTIMATION FOR A RESEARCH PROJECT.pptx

COST ESTIMATION FOR A RESEARCH PROJECT.pptx

COST ESTIMATION FOR A RESEARCH PROJECT.pptx

FarihaAbdulRasheed

RecoveringancientrecordsofEarth'smagneticfieldisessentialfordeterminingtheroleofthemagnetosphereinprotectingearlyEarthfromcosmicradiationandatmosphericescape.WepresentpaleomagneticfieldtestshintingthatarecordofEarth's3.7‐billion‐year(Ga)oldmagneticfieldmaybepreservedinthenortheasternIsuaSupracrustalBeltasachemicalremanentmagnetizationacquiredduringamphibolite‐grademetamorphisminthebandedironformation.MultiplepetrologicalandgeochronologicallinesofevidenceindicatethatthenorthernmostpartofIsuahasnotexperiencedmetamorphictemperaturesexceeding380°CsincetheEoarchean,suggestingtherockshavenotbeensignificantlyheatedsincemagnetizationwasacquired.Weuse“pseudo”bakedcontacttests(intrusionsemplaced3.26–3.5Gaago)andafoldtest(folding3.6Gaago)todemonstratethatsomesamplespreserveaca.3.7Garecordofthemagneticfield.Werecoverafieldstrengthof>15μT.ThissuggeststhatEarth'smagneticfieldmayhavebeenweakenoughtoenhanceatmosphericescapeduringtheArchean

PossibleEoarcheanRecordsoftheGeomagneticFieldPreservedintheIsuaSupracrustalBe...

PossibleEoarcheanRecordsoftheGeomagneticFieldPreservedintheIsuaSupracrustalBe...

PossibleEoarcheanRecordsoftheGeomagneticFieldPreservedintheIsuaSupracrustalBe...

CELL -Structural and Functional unit of life.pdf

CELL -Structural and Functional unit of life.pdf

CELL -Structural and Functional unit of life.pdf

Nistarini College, Purulia (W.B) India

Pulmonary drug delivery system M.pharm -2nd sem P'ceutics

Pulmonary drug delivery system M.pharm -2nd sem P'ceutics

Pulmonary drug delivery system M.pharm -2nd sem P'ceutics

Recombination DNA Technology (Nucleic Acid Hybridization )

Recombination DNA Technology (Nucleic Acid Hybridization )

Recombination DNA Technology (Nucleic Acid Hybridization )

aarthirajkumar25

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High Class Escorts in Hyderabad ₹7.5k Pick Up & Drop With Cash Payment 969456...

High Class Escorts in Hyderabad ₹7.5k Pick Up & Drop With Cash Payment 969456...

Nanoparticles synthesis and characterization

Nanoparticles synthesis and characterization

Nanoparticles synthesis and characterization

kaibalyasahoo82800

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

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

Bacterial Identification and Classifications

Bacterial Identification and Classifications

Bacterial Identification and Classifications

GBSN - Microbiology (Unit 2)

GBSN - Microbiology (Unit 2)

GBSN - Microbiology (Unit 2)

Zoology 4th semester series (krishna).pdf

Zoology 4th semester series (krishna).pdf

Zoology 4th semester series (krishna).pdf

Sumit Kumar yadav

Chemical Tests; flame test, positive and negative ions test Edexcel Internati...

Chemical Tests; flame test, positive and negative ions test Edexcel Internati...

Chemical Tests; flame test, positive and negative ions test Edexcel Internati...

Seismic Method Estimate velocity from seismic data.pptx

Seismic Method Estimate velocity from seismic data.pptx

Seismic Method Estimate velocity from seismic data.pptx

Theoretical predictions and observational data indicate a class of sub-Neptune exoplanets may have water-rich interiors covered by hydrogen-dominated atmospheres. Provided suitable climate conditions, such planets could host surface liquid oceans. Motivated by recent JWST observations of K2-18 b, we self-consistently model the photochemistry and potential detectability of biogenic sulfur gases in the atmospheres of temperate sub-Neptune waterworlds for the first time. On Earth today, organic sulfur compounds produced by marine biota are rapidly destroyed by photochemical processes before they can accumulate to significant levels. Domagal-Goldman et al. suggest that detectable biogenic sulfur signatures could emerge in Archean-like atmospheres with higher biological production or low UV flux. In this study, we explore biogenic sulfur across a wide range of biological fluxes and stellar UV environments. Critically, the main photochemical sinks are absent on the nightside of tidally locked planets. To address this, we further perform experiments with a 3D general circulation model and a 2D photochemical model (VULCAN 2D) to simulate the global distribution of biogenic gases to investigate their terminator concentrations as seen via transmission spectroscopy. Our models indicate that biogenic sulfur gases can rise to potentially detectable levels on hydrogen-rich water worlds, but only for enhanced global biosulfur flux (20 times modern Earth’s flux). We find that it is challenging to identify DMS at 3.4 μm where it strongly overlaps with CH4, whereas it is more plausible to detect DMS and companion byproducts, ethylene (C2H4) and ethane (C2H6), in the mid-infrared between 9 and 13 μm. Unified Astronomy Thesaurus concepts: Exoplanet atmospheres (487); Exoplanet

Biogenic Sulfur Gases as Biosignatures on Temperate Sub-Neptune Waterworlds

Biogenic Sulfur Gases as Biosignatures on Temperate Sub-Neptune Waterworlds

Biogenic Sulfur Gases as Biosignatures on Temperate Sub-Neptune Waterworlds

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Disentangling the origin of chemical differences using GHOST

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Biogenic Sulfur Gases as Biosignatures on Temperate Sub-Neptune Waterworlds

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