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vinothiyagarajan1

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components of systemic defense - tissue and blood

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leptospirosis, salmonellosis, swine flu and avian flu

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components of host surface defense system

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components of systemic defense - tissue and blood

leptospirosis, salmonellosis, swine flu and avian flu

virulence assays - molecular diagnostic techniques

ouchterlony double diffusion method and immunoblotting

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components of host surface defense system

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The thermal continuum emission observed from accreting black holes across X-ray bands has the potential to be leveraged as a powerful probe of the mass and spin of the central black hole. The vast majority of existing ‘continuum fitting’ models neglect emission sourced at and within the innermost stable circular orbit (ISCO) of the black hole. Numerical simulations, however, find non-zero emission sourced from these regions. In this work, we extend existing techniques by including the emission sourced from within the plunging region, utilizing new analytical models that reproduce the properties of numerical accretion simulations. We show that in general the neglected intra-ISCO emission produces a hot-and-small quasi-blackbody component, but can also produce a weak power-law tail for more extreme parameter regions. A similar hot-and-small blackbody component has been added in by hand in an ad hoc manner to previous analyses of X-ray binary spectra. We show that the X-ray spectrum of MAXI J1820+070 in a soft-state outburst is extremely well described by a full Kerr black hole disc, while conventional models that neglect intra-ISCO emission are unable to reproduce the data. We believe this represents the first robust detection of intra-ISCO emission in the literature, and allows additional constraints to be placed on the MAXI J1820 + 070 black hole spin which must be low a• < 0.5 to allow a detectable intra-ISCO region. Emission from within the ISCO is the dominant emission component in the MAXI J1820 + 070 spectrum between 6 and 10 keV, highlighting the necessity of including this region. Our continuum fitting model is made publicly available.

Continuum emission from within the plunging region of black hole discs

Sérgio Sacani

In this work, we assess the potential detectability of solar panels made of silicon on an Earth-like exoplanet as a potential technosignature. Silicon-based photovoltaic cells have high reflectance in the UV-VIS and in the near-IR, within the wavelength range of a space-based flagship mission concept like the Habitable Worlds Observatory (HWO). Assuming that only solar energy is used to provide the 2022 human energy needs with a land cover of ∼ 2.4%, and projecting the future energy demand assuming various growth-rate scenarios, we assess the detectability with an 8 m HWO-like telescope. Assuming the most favorable viewing orientation, and focusing on the strong absorption edge in the ultraviolet-to-visible (0.34 − 0.52 µm), we find that several 100s of hours of observation time is needed to reach a SNR of 5 for an Earth-like planet around a Sun-like star at 10pc, even with a solar panel coverage of ∼ 23% land coverage of a future Earth. We discuss the necessity of concepts like Kardeshev Type I/II civilizations and Dyson spheres, which would aim to harness vast amounts of energy. Even with much larger populations than today, the total energy use of human civilization would be orders of magnitude below the threshold for causing direct thermal heating or reaching the scale of a Kardashev Type I civilization. Any extraterrrestrial civilization that likewise achieves sustainable population levels may also find a limit on its need to expand, which suggests that a galaxy-spanning civilization as imagined in the Fermi paradox may not exist.

Detectability of Solar Panels as a Technosignature

Sérgio Sacani

The concepts of plant disease management are primarily centered on identifying the disease and reducing damage or loss below the threshold of economic detriment. Whetzel (1919) was the first to define disease control approaches as Exclusion, Eradication, Protection, and Resistance, with two more methods added later: Avoidance and Therapy (National Science Academy, 1968). Thus, management methods refer to steps done to lower the incidence and intensity of the illness, limit the number of inoculums that originate and propagate the disease, and, eventually, minimize the disease's losses.

PLANT DISEASE MANAGEMENT PRINCIPLES AND ITS IMPORTANCE

TALAPATI ARUNA CHENNA VYDYANAD

GBSN - Microbiology Lab (Compound Microscope)

Areesha Ahmad

Recent observations of galaxy clusters and groups with misalignments between their central AGN jets and X-ray cavities, or with multiple misaligned cavities, have raised concerns about the jet – bubble connection in cooling cores, and the processes responsible for jet realignment. To investigate the frequency and causes of such misalignments, we construct a sample of 16 cool core galaxy clusters and groups. Using VLBA radio data we measure the parsec-scale position angle of the jets, and compare it with the position angle of the X-ray cavities detected in Chandra data. Using the overall sample and selected subsets, we consistently find that there is a 30% – 38% chance to find a misalignment larger than ∆Ψ = 45◦ when observing a cluster/group with a detected jet and at least one cavity. We determine that projection may account for an apparently large ∆Ψ only in a fraction of objects (∼35%), and given that gas dynamical disturbances (as sloshing) are found in both aligned and misaligned systems, we exclude environmental perturbation as the main driver of cavity – jet misalignment. Moreover, we find that large misalignments (up to ∼ 90◦ ) are favored over smaller ones (45◦ ≤ ∆Ψ ≤ 70◦ ), and that the change in jet direction can occur on timescales between one and a few tens of Myr. We conclude that misalignments are more likely related to actual reorientation of the jet axis, and we discuss several engine-based mechanisms that may cause these dramatic changes.

Jet reorientation in central galaxies of clusters and groups: insights from V...

Sérgio Sacani

Aerodynamics. flippatterncn5tm5ttnj6nmnynyppt

sreddyrahul

Hadean zircons provide a potential record of Earth's earliest subduction 4.3 billion years ago. Itremains enigmatic how subduction could be initiated so soon after the presumably Moon‐forming giant impact(MGI). Earlier studies found an increase in Earth's core‐mantle boundary (CMB) temperature due to theaccumulation of the impactor's core, and our recent work shows Earth's lower mantle remains largely solid, withsome of the impactor's mantle potentially surviving as the large low‐shear velocity provinces (LLSVPs). Here,we show that a hot post‐impact CMB drives the initiation of strong mantle plumes that can induce subductioninitiation ∼200 Myr after the MGI. 2D and 3D thermomechanical computations show that a high CMBtemperature is the primary factor triggering early subduction, with enrichment of heat‐producing elements inLLSVPs as another potential factor. The models link the earliest subduction to the MGI with implications forunderstanding the diverse tectonic regimes of rocky planets.

A Giant Impact Origin for the First Subduction on Earth

Sérgio Sacani

NUMERICAL Proof Of TIme Electron Theory.

syedmuneemqadri

In-Pond Raceway Systems (IPRS) represent a cutting-edge method in pond aquaculture, effectively combining the advantages of confining fish in a restricted area within the pond with the efficiency of a flowing water system. This innovative approach facilitates water circulation within the pond, mimicking the natural flow found in riverine environments. By creating this dynamic water movement, IPRS significantly enhances the pond's productivity potential. The core principle of IPRS involves the installation of specific components that work in concert to circulate and refresh the water within the pond, all while preventing any discharge into the surrounding environment. This setup effectively utilizes a dividing partition, or baffle, to create a circular water flow pattern. As a result, the water undergoes continuous mixing and movement, optimizing conditions for fish growth and minimizing stagnation.

In-pond Race way systems for Aquaculture (IPRS).pptx

MAGOTI ERNEST

NuGOweek 2024 full programme - hosted by Ghent University

pablovgd

Alternative method of dissolution in-vitro in-vivo correlation and dissolutio...

Sahil Suleman

The magnetic dynamo cycle of the Sun features a distinct pattern: a propagating region of sunspot emergence appears around 30° latitude and vanishes near the equator every 11 years (ref. 1). Moreover, longitudinal flows called torsional oscillations closely shadow sunspot migration, undoubtedly sharing a common cause2. Contrary to theories suggesting deep origins of these phenomena, helioseismology pinpoints low-latitude torsional oscillations to the outer 5–10% of the Sun, the near-surface shear layer3,4. Within this zone, inwardly increasing differential rotation coupled with a poloidal magnetic field strongly implicates the magneto-rotational instability5,6, prominent in accretion-disk theory and observed in laboratory experiments7. Together, these two facts prompt the general question: whether the solar dynamo is possibly a near-surface instability. Here we report strong affirmative evidence in stark contrast to traditional models8 focusing on the deeper tachocline. Simple analytic estimates show that the near-surface magneto-rotational instability better explains the spatiotemporal scales of the torsional oscillations and inferred subsurface magnetic field amplitudes9. State-of-the-art numerical simulations corroborate these estimates and reproduce hemispherical magnetic current helicity laws10. The dynamo resulting from a well-understood near-surface phenomenon improves prospects for accurate predictions of full magnetic cycles and space weather, affecting the electromagnetic infrastructure of Earth.

The solar dynamo begins near the surface

Sérgio Sacani

Lubrication System in forced feed system

ADB online India

Tuberculosis (TB)-Notes.pdf microbiology notes

jyothisaisri

It should be no surprise that AI is treading a similar path to computing which began with single-purpose machines tasked for payroll calculations, banking transactions, or weapons targeting et al, but nothing more! It took decades for General Purpose Computing to emerge in the form of the now ubiquitous PC. Today, AI is still in a single-purpose/task-specific phase, and we have no general-purpose platforms, but their emergence is only a matter of time! Recent AI progress has seen a repeat of the media debate and alarmist warnings for our computing past, compounded by consequential advances in robotics. In turn, this has promoted numerous attempts to draw biological equivalences defining the time when machines will overtake humans. But without any workable definitions or framework that tend to little more than un/educated guesses. Recourse to IQ measures and the Touring test have proved to be irrelevant, and without a reference framework or formal characterisation, continued discussion and debate remain futile We therefore approach this AI problem from the bottom up by defining the simplest of machines and lifeforms to derive clues, pointers and basic boundary conditions . This sees a fundamental Entropic description emerge that is applicable to both machine and lifeforms. This presentation is suitable for professionals and the public alike, and is fully illustrated by high-quality graphics, animations and, movies. Inevitably, it contains some mathematics that non-practitioners will have to take on trust, but the focus is on defining the key characteristics, parameters, and important features of AI, our total dependence, and the future! Note: A 40 min session for a predominantly ley audience and not all the slides presented here were used on the day. Their inclusion here is in response to those audience members requesting more detail at the end of/during the event.

Quantifying Artificial Intelligence and What Comes Next!

University of Hertfordshire

ManganesehasbeenobservedonMarsbytheNASACuriosityroverinavarietyofcontextsand isanimportantindicatorofredoxprocessesinhydrologicsystemsonEarth.WithintheMurrayformation,an ancientprimarilyfine‐grainedlacustrinesedimentarydeposit inGalecrater,Mars,haveobservedupto45× enrichmentinmanganeseandupto1.5×enrichmentinironwithincoarsergrainedbedrocktargetscomparedto themeanMurraysedimentcomposition.Thisenrichment inmanganesecoincideswiththetransitionbetween twostratigraphicunitswithintheMurray:SuttonIsland, interpretedasalakemarginenvironment,andBlunts Point,interpretedasalakeenvironment.OnEarth,lacustrineenvironmentsarecommonlocationsofmanganese precipitationduetohighlyoxidizingconditionsinthelakes.Here,weexplorethreemechanismsfor ferromanganeseoxideprecipitationatthislocation:authigenicprecipitationfromlakewateralongalakeshore, authigenicprecipitationfromreducedgroundwaterdischargingthroughporoussandsalongalakeshore,and earlydiageneticprecipitationfromgroundwaterthroughporoussands.All threescenariosrequirehighly oxidizingconditionsandwediscussoxidantsthatmayberesponsiblefortheoxidationandprecipitationof manganeseoxides.Thisworkhasimportant implicationsforthehabitabilityofMarstomicrobesthatcould haveusedMnredoxreactions,owingtoitsmultipleredoxstates,asanenergysourceformetabolism.

Manganese‐RichSandstonesasanIndicatorofAncientOxic LakeWaterConditionsinGale...

Sérgio Sacani

Studying the escaping atmospheres of highly irradiated exoplanets is critical for understanding the physical mechanisms that shape the demographics of close-in planets. A number of planetary outflows have been observed as excess H/He absorption during/after transit. Such an outflow has been observed for WASP-69b by multiple groups that disagree on the geometry and velocity structure of the outflow. Here, we report the detection of this planet’s outflow using Keck/NIRSPEC for the first time. We observed the outflow 1.28 hr after egress until the target set, demonstrating the outflow extends at least 5.8 × 105 km or 7.5 Rp This detection is significantly longer than previous observations, which report an outflow extending ∼2.2 planet radii just 1 yr prior. The outflow is blueshifted by −23 km s−1 in the planetary rest frame. We estimate a current mass-loss rate of 1 M⊕ Gyr−1 . Our observations are most consistent with an outflow that is strongly sculpted by ram pressure from the stellar wind. However, potential variability in the outflow could be due to time-varying interactions with the stellar wind or differences in instrumental precision.

WASP-69b’s Escaping Envelope Is Confined to a Tail Extending at Least 7 Rp

Sérgio Sacani

Factor Causing low production and physiology of mamary Gland

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The Scientific names of some important families of Industrial plants .pdf

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Continuum emission from within the plunging region of black hole discs

Detectability of Solar Panels as a Technosignature

PLANT DISEASE MANAGEMENT PRINCIPLES AND ITS IMPORTANCE

GBSN - Microbiology Lab (Compound Microscope)

Jet reorientation in central galaxies of clusters and groups: insights from V...

Aerodynamics. flippatterncn5tm5ttnj6nmnynyppt

A Giant Impact Origin for the First Subduction on Earth

NUMERICAL Proof Of TIme Electron Theory.

In-pond Race way systems for Aquaculture (IPRS).pptx

NuGOweek 2024 full programme - hosted by Ghent University

Alternative method of dissolution in-vitro in-vivo correlation and dissolutio...

The solar dynamo begins near the surface

Lubrication System in forced feed system

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Manganese‐RichSandstonesasanIndicatorofAncientOxic LakeWaterConditionsinGale...

WASP-69b’s Escaping Envelope Is Confined to a Tail Extending at Least 7 Rp

Factor Causing low production and physiology of mamary Gland

Triploidy ...............................pptx

The Scientific names of some important families of Industrial plants .pdf

components of host surface defense system

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components of host surface defense system