Strange animal lifestyles Adbhut jeevjantu shailiyan chapter 10 bio immortality

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SantoshBhatnagar1

IT IS A FEATURE ON INTERESTING TOPIC OF BIO IMMORTALITY -MAN HAS BEEN YARNING FOR IT SINCE ANCIENT TIMES WITHOUT SUCCESS BUT TINY CREATURES LIKE JEELY FISHES AND HYDRA HAD ACQUIRED IT MILLION OF YEARS AGO AND WE ARE NOW TRYING TO LEARN THE SECRET FROM THEM .

Strange animal lifestyles

Strange animal lifestyles Adbhut jeevjantu shailiyan chapter 10 bio immortality

Strange animal lifestyles Adbhut jeevjantu shailiyan chapter 10 bio immortality

Strange animal lifestyles Adbhut jeevjantu shailiyan chapter 10 bio immortality

Strange animal lifestyles Adbhut jeevjantu shailiyan chapter 10 bio immortality

Strange animal lifestyles Adbhut jeevjantu shailiyan chapter 10 bio immortality

Strange animal lifestyles Adbhut jeevjantu shailiyan chapter 10 bio immortality

Strange animal lifestyles Adbhut jeevjantu shailiyan chapter 10 bio immortality

Strange animal lifestyles Adbhut jeevjantu shailiyan chapter 10 bio immortality

Strange animal lifestyles Adbhut jeevjantu shailiyan chapter 10 bio immortality

Strange animal lifestyles Adbhut jeevjantu shailiyan chapter 10 bio immortality

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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

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GBSN - Microbiology (Unit 1)

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Forensic Biology & Its biological significance.pdf

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Forensic Biology & Its biological significance.pdf

rohankumarsinghrore1

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RizalinePalanog2

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

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Isotopic evidence of long-lived volcanism on Io

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