Mythologos

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The document discusses the benefits of meditation for reducing stress and anxiety. Regular meditation practice can help calm the mind and body by lowering heart rate and blood pressure. Making meditation a part of a daily routine, even if just 10-15 minutes per day, can have mental and physical health benefits over time by helping people feel more relaxed and focused.

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PESTS OF SUGARCANE - BORERS BORERS 1. Early shoot borer, Chilo infuscatellus, Crambidae, Lepidoptera Symptom of damage: Deadheart in 1-3 month old crop, which can be easily pulled out, rotten portion of the straw coloured dead-heart emits an offensive odour. A number of bore holes at the base of the shoot just above the ground level. Nature of damage: Caterpillar bores into the central shoot and feeds on the internal tissue. This cause interference in the translocation of plant sap and damage the sugar storing tissues. Egg: Flat-scale like eggs are laid in 3-5 rows on the lower surface of leaves in masses of 4-100. The masses are slightly overlapping like tiles. Larva: Larva is dirty white with five dark violet longitudinal stripes and dark brown head. Pupa: Pupation takes place within the tunnel. Caterpillar before pupating makes a large exit hole in the stem and blocks the opening with silken discs. Adult: Pale greyish brown moth with black dots near the costal margin of the forewings and with white hindwings. 2. Internode borer, Chilo sacchariphagus indicus, Crambidae, Lepidoptera Symptom of damage: Internodes constricted and shortened, with a number of boreholes and fresh excreta in the nodal region. Affected tissues reddened. Nature of damage: Caterpillars attack sugarcane plants after 3 months of planting. They bore into the canes near the nodes; entry holes are plugged with excreta. Entry is generally confined to the first five internodes. Egg: Scale-like white eggs are laid by female moths in batches of 9-11, near the midribs, on leaf sheaths or on stem. Larva: White larva with four violet longitudinal stripes and light brown head. Pupa: Pupation takes place in semi-dried leaf sheath. Adult: Pale brown with white hind wings. 3. Top borer, Scirpophaga excerptalis, Pyralidae, Lepidoptera Symptom of damage: Deadheart in grownup canes, which cannot be easily pulled; deadheart reddish brown in colour; parallel row of shot holes in the emerging leaves and red tunnels in the midribs of leaves; bunchy tip due to the growth of side shoots. Nature of damage: Caterpillars are mainly found in the apical portion of the canes, boring through the growing point and down the upper joints until it reaches the sappy portion of the stem, there it feeds on the tissues and destroys the cane. They also bore into the unfolded leaves preferably into the midrib, mining its way to the base. Egg: Eggs are laid on the lower surface of top leaves in clusters particularly near midribs. The clusters are covered with buff coloured hairs. Larva :Smooth, white or cream coloured with a red coloured mid-dorsal line and yellow head. Pupa: Pupation takes place within the larval tunnel in a chamber with an exit hole constructed by the caterpillar. Adult: White coloured moth (with a buff coloured anal tuft in the abdominal tip of female).

Pests of sugarcane_Binomics_IPM_Dr.UPR.pdf

PirithiRaju

Within the uncertainties of involved astronomical and biological parameters, the Drake Equation typically predicts that there should be many exoplanets in our galaxy hosting active, communicative civilizations (ACCs). These optimistic calculations are however not supported by evidence, which is often referred to as the Fermi Paradox. Here, we elaborate on this long-standing enigma by showing the importance of planetary tectonic style for biological evolution. We summarize growing evidence that a prolonged transition from Mesoproterozoic active single lid tectonics (1.6 to 1.0 Ga) to modern plate tectonics occurred in the Neoproterozoic Era (1.0 to 0.541 Ga), which dramatically accelerated emergence and evolution of complex species. We further suggest that both continents and oceans are required for ACCs because early evolution of simple life must happen in water but late evolution of advanced life capable of creating technology must happen on land. We resolve the Fermi Paradox (1) by adding two additional terms to the Drake Equation: foc (the fraction of habitable exoplanets with significant continents and oceans) and fpt (the fraction of habitable exoplanets with significant continents and oceans that have had plate tectonics operating for at least 0.5 Ga); and (2) by demonstrating that the product of foc and fpt is very small (< 0.00003–0.002). We propose that the lack of evidence for ACCs reflects the scarcity of long-lived plate tectonics and/or continents and oceans on exoplanets with primitive life.

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Sérgio Sacani

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

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.

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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.

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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.

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Cyanobacteria (also known as blue-green algae) are ubiquitous photosynthetic microorganisms found in diverse habitats such as fresh water, marine water, moist rocks, etc. The photosynthetic mode of nutrition makes them significant global oxygen producers along with nitrogen-fixing ability of heterocyst and carbon sequestration. Some cyanobacterial species have the ability to perform a dual mode of nutritional procurement. This unique capability of cyanobacteria to utilize both organic (heterotrophic) and inorganic (autotrophic) carbon sources for energy production and growth is termed as mixotrophy which impart nutritional flexibility and competitive ability to them. Cyanobacterial mixotrophy provides the promising avenues in biotechnological applications such as wastewater treatment, bioremediation, pharmaceuticals, food supplements, biofertilizer, coloring agents, synthesis of bioactive compounds and as an agent for eco-friendly bio-fuels generation, etc Mixotrophically grown cyanobacteria, demonstrate significant potential for efficient and economical applications beyond their conventional agricultural application, thereby offering a versatile and impactful resource for future technological and environmental challenges.

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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.

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