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Hemoglobin metabolism: C Kalyan & E. Muralinath

muralinath2

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

Cherry

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

GBSN - Microbiology Lab (Compound Microscope)

Areesha Ahmad

SCHISTOSOMA HEAMATOBIUM life cycle .pdf

DebdattaGhosh6

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

Mohamed Said

GBSN - Biochemistry (Unit 4) Chemistry of Carbohydrates

Areesha Ahmad

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 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

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

Mars is a particularly attractive candidate among known astronomical objects to potentially host life. Results from space exploration missions have provided insights into Martian geochemistry that indicate oxychlorine species, particularly perchlorate, are ubiquitous features of the Martian geochemical landscape. Perchlorate presents potential obstacles for known forms of life due to its toxicity. However, it can also provide potential benefits, such as producing brines by deliquescence, like those thought to exist on present-day Mars. Here we show perchlorate brines support folding and catalysis of functional RNAs, while inactivating representative protein enzymes. Additionally, we show perchlorate and other oxychlorine species enable ribozyme functions, including homeostasis-like regulatory behavior and ribozyme-catalyzed chlorination of organic molecules. We suggest nucleic acids are uniquely wellsuited to hypersaline Martian environments. Furthermore, Martian near- or subsurface oxychlorine brines, and brines found in potential lifeforms, could provide a unique niche for biomolecular evolution.

Emergent ribozyme behaviors in oxychlorine brines indicate a unique niche for...

Sérgio Sacani

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

Sahil Suleman

The highest priority recommendation of the Astro2020 Decadal Survey for space-based astronomy was the construction of an observatory capable of characterizing habitable worlds. In this paper series we explore the detectability of and interference from exomoons and exorings serendipitously observed with the proposed Habitable Worlds Observatory (HWO) as it seeks to characterize exoplanets, starting in this manuscript with Earth-Moon analog mutual events. Unlike transits, which only occur in systems viewed near edge-on, shadow (i.e., solar eclipse) and lunar eclipse mutual events occur in almost every star-planet-moon system. The cadence of these events can vary widely from ∼yearly to multiple events per day, as was the case in our younger Earth-Moon system. Leveraging previous space-based (EPOXI) lightcurves of a Moon transit and performance predictions from the LUVOIR-B concept, we derive the detectability of Moon analogs with HWO. We determine that Earth-Moon analogs are detectable with observation of ∼2-20 mutual events for systems within 10 pc, and larger moons should remain detectable out to 20 pc. We explore the extent to which exomoon mutual events can mimic planet features and weather. We find that HWO wavelength coverage in the near-IR, specifically in the 1.4 µm water band where large moons can outshine their host planet, will aid in differentiating exomoon signals from exoplanet variability. Finally, we predict that exomoons formed through collision processes akin to our Moon are more likely to be detected in younger systems, where shorter orbital periods and favorable geometry enhance the probability and frequency of mutual events.

Exomoons & Exorings with the Habitable Worlds Observatory I: On the Detection...

Sérgio Sacani

The recently reported observation of VFTS 243 is the first example of a massive black-hole binary system with negligible binary interaction following black-hole formation. The black-hole mass (≈10M⊙) and near-circular orbit (e ≈ 0.02) of VFTS 243 suggest that the progenitor star experienced complete collapse, with energy-momentum being lost predominantly through neutrinos. VFTS 243 enables us to constrain the natal kick and neutrino-emission asymmetry during black-hole formation. At 68% confidence level, the natal kick velocity (mass decrement) is ≲10 km=s (≲1.0M⊙), with a full probability distribution that peaks when ≈0.3M⊙ were ejected, presumably in neutrinos, and the black hole experienced a natal kick of 4 km=s. The neutrino-emission asymmetry is ≲4%, with best fit values of ∼0–0.2%. Such a small neutrino natal kick accompanying black-hole formation is in agreement with theoretical predictions.

Constraints on Neutrino Natal Kicks from Black-Hole Binary VFTS 243

Sérgio Sacani

Erythropoiesis- Dr.E. Muralinath-C Kalyan

muralinath2

Ostiguy & Panizza & Moffitt (eds.) - Populism in Global Perspective. A Perfor...

frank0071

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

Plasma proteins_ Dr.Muralinath_Dr.c. kalyan

muralinath2

Lec 1.b Totipotency and birth of tissue culture.ppt

asifali1111

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

Recently uploaded (20)

Hemoglobin metabolism: C Kalyan & E. Muralinath

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

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

GBSN - Microbiology Lab (Compound Microscope)

SCHISTOSOMA HEAMATOBIUM life cycle .pdf

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

GBSN - Biochemistry (Unit 4) Chemistry of Carbohydrates

Detectability of Solar Panels as a Technosignature

The solar dynamo begins near the surface

A Giant Impact Origin for the First Subduction on Earth

Emergent ribozyme behaviors in oxychlorine brines indicate a unique niche for...

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

Exomoons & Exorings with the Habitable Worlds Observatory I: On the Detection...

Constraints on Neutrino Natal Kicks from Black-Hole Binary VFTS 243

Erythropoiesis- Dr.E. Muralinath-C Kalyan

Ostiguy & Panizza & Moffitt (eds.) - Populism in Global Perspective. A Perfor...

Quantifying Artificial Intelligence and What Comes Next!

Plasma proteins_ Dr.Muralinath_Dr.c. kalyan

Lec 1.b Totipotency and birth of tissue culture.ppt

Continuum emission from within the plunging region of black hole discs