Relevant bibliographies by topics / ISM: clouds

Academic literature on the topic 'ISM: clouds'

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Published: 4 June 2021
Last updated: 29 January 2023

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Journal articles on the topic "ISM: clouds"

1

Shull, Peter, John Dyson, and Franz Kahn. "A Model of SNR Evolution for an O-Star in a Cloudy ISM." International Astronomical Union Colloquium 101 (1988): 231–34. http://dx.doi.org/10.1017/s0252921100102416.

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AbstractWe present an analytical model of SNR evolution in a cloudy interstellar medium for a single progenitor star of spectral type 05 V. The model begins with the progenitor on the zero-age main sequence, includes the effects of the star’s wind and ionizing photons, and ends with the SNR’s assimilation by the ISM. We assume that the ISM consists of atomic clouds, molecular clouds, and a hot intercloud phase. The type of SNR that results bears a strong resemblance to N63A in the Large Magellanic Cloud.
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Subrahmanyam, K. V., and K. K. Kumar. "CloudSat observations of cloud-type distribution over the Indian summer monsoon region." Annales Geophysicae 31, no. 7 (July 3, 2013): 1155–62. http://dx.doi.org/10.5194/angeo-31-1155-2013.

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Abstract. The three-dimensional distribution of various cloud types over the Indian summer monsoon (ISM) region using five years (2006–2010) of CloudSat observations during June-July-August-September months is discussed for the first time. As the radiative properties, latent heat released and microphysical properties of clouds differ largely depending on the cloud type, it becomes important to know what types of clouds occur over which region. In this regard, the present analysis establishes the three-dimensional distribution of frequency of occurrence of stratus (St), stratocumulus (Sc), nimbostratus (Ns), cumulus (Cu), altocumulus (Ac), altostratus (As), cirrus (Ci) and deep convective (DC) clouds over the ISM region. The results show that the various cloud types preferentially occur over some regions of the ISM, which are consistent during all the years of observations. It is found that the DC clouds frequently occur over northeast of Bay of Bengal (BoB), Ci clouds over a wide region of south BoB–Indian peninsula–equatorial Indian Ocean, and Sc clouds over the north Arabian Sea. Ac clouds preferentially occur over land, and a large amount of As clouds are found over BoB. The occurrence of both St and Ns clouds over the study region is much lower than all other cloud types.The interannual variability of all these clouds including their vertical distribution is discussed. It is envisaged that the present study opens up possibilities to quantify the feedback of individual cloud type in the maintenance of the ISM through radiative forcing and latent heat release.
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Mckee, Christopher F. "CO and the Multiphase ISM." Symposium - International Astronomical Union 170 (1997): 25–32. http://dx.doi.org/10.1017/s0074180900234025.

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CO observations indicate that molecular clouds have a complex multiphase structure, and this is compared with the multiphase structure of the diffuse interstellar medium. The trace ionization within the molecular gas is governed primarily by UV photoionization. Magnetic fields contribute a significantly larger fraction of the pressure in molecular clouds than in the diffuse interstellar medium. Observations suggest that the total Alfvén Mach number, mAtot, of the turbulence in the diffuse ISM exceeds unity; Zeeman observations are consistent with mAtot ≲ 1 in molecular clouds, but more data are needed to verify this. Most molecular clouds are self-gravitating, and they can be modeled as multi-pressure polytropes with thermal, magnetic, and wave pressure. The pressure and density within self-gravitating clouds is regulated by the pressure in the surrounding diffuse ISM.
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Siebenmorgen, R., J. Krełowski, J. Smoker, G. Galazutdinov, and S. Bagnulo. "Dark dust and single-cloud sightlines in the ISM." Astronomy & Astrophysics 641 (September 2020): A35. http://dx.doi.org/10.1051/0004-6361/202037511.

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The precise characteristics of clouds and the nature of dust in the diffuse interstellar medium can only be extracted by inspecting the rare cases of single-cloud sightlines. In our nomenclature such objects are identified by interstellar lines, such as K I, that show at a resolving power of λ∕Δλ ~ 75 000 one dominating Doppler component that accounts for more than half of the observed column density. We searched for such sightlines using high-resolution spectroscopy towards reddened OB stars for which far-UV extinction curves are known. We compiled a sample of 186 spectra, 100 of which were obtained specifically for this project with UVES. In our sample we identified 65 single-cloud sightlines, about half of which were previously unknown. We used the CH/CH+ line ratio of our targets to establish whether the sightlines are dominated by warm or cold clouds. We found that CN is detected in all cold (CH/CH+ > 1) clouds, but is frequently absent in warm clouds. We inspected the WISE (3−22 μm) observed emission morphology around our sightlines and excluded a circumstellar nature for the observed dust extinction. We found that most sightlines are dominated by cold clouds that are located far away from the heating source. For 132 stars, we derived the spectral type and the associated spectral type-luminosity distance. We also applied the interstellar Ca II distance scale, and compared these two distance estimates with Gaia parallaxes. These distance estimates scatter by ~40%. By comparing spectral type-luminosity distances with those of Gaia, we detected a hidden dust component that amounts to a few mag of extinction for eight sightlines. This dark dust is populated by ≳ 1 μm large grains and predominately appears in the field of the cold interstellar medium.
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Mandal, Ankush, Christoph Federrath, and Bastian Körtgen. "Molecular cloud formation by compression of magnetized turbulent gas subjected to radiative cooling." Monthly Notices of the Royal Astronomical Society 493, no. 3 (February 17, 2020): 3098–113. http://dx.doi.org/10.1093/mnras/staa468.

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ABSTRACT Complex turbulent motions of magnetized gas are ubiquitous in the interstellar medium (ISM). The source of this turbulence, however, is still poorly understood. Previous work suggests that compression caused by supernova shockwaves, gravity, or cloud collisions, may drive the turbulence to some extent. In this work, we present three-dimensional (3D) magnetohydrodynamic (MHD) simulations of contraction in turbulent, magnetized clouds from the warm neutral medium of the ISM to the formation of cold dense molecular clouds, including radiative heating and cooling. We study different contraction rates and find that observed molecular cloud properties, such as the temperature, density, Mach number, and magnetic field strength, and their respective scaling relations, are best reproduced when the contraction rate equals the turbulent turnover rate. In contrast, if the contraction rate is significantly larger (smaller) than the turnover rate, the compression drives too much (too little) turbulence, producing unrealistic cloud properties. We find that the density probability distribution function evolves from a double lognormal representing the two-phase ISM, to a skewed, single lognormal in the dense, cold phase. For purely hydrodynamical simulations, we find that the effective driving parameter of contracting cloud turbulence is natural to mildly compressive (b ∼ 0.4–0.5), while for MHD turbulence, we find b ∼ 0.3–0.4, i.e. solenoidal to naturally mixed. Overall, the physical properties of the simulated clouds that contract at a rate equal to the turbulent turnover rate, indicate that large-scale contraction may explain the origin and evolution of turbulence in the ISM.
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Franchetto, Andrea, Stephanie Tonnesen, Bianca M. Poggianti, Benedetta Vulcani, Marco Gullieuszik, Alessia Moretti, Rory Smith, et al. "Evidence for Mixing between ICM and Stripped ISM by the Analysis of the Gas Metallicity in the Tails of Jellyfish Galaxies." Astrophysical Journal Letters 922, no. 1 (November 1, 2021): L6. http://dx.doi.org/10.3847/2041-8213/ac3664.

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Abstract Hydrodynamical simulations show that the ram pressure stripping in galaxy clusters fosters a strong interaction between stripped interstellar medium (ISM) and the surrounding medium, with the possibility of intracluster medium (ICM) cooling into cold gas clouds. Exploiting the MUSE observation of three jellyfish galaxies from the GAs Stripping Phenomena in galaxies with MUSE (GASP) survey, we explore the gas metallicity of star-forming clumps in their gas tails. We find that the oxygen abundance of the stripped gas decreases as a function of the distance from the parent galaxy disk; the observed metallicity profiles indicate that more than 40% of the most metal-poor stripped clouds are constituted by cooled ICM, in qualitative agreement with simulations that predict mixing between the metal-rich ISM and the metal-poor ICM.
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Matsuura, Mikako. "Global Dust Budgets of the Magellanic Clouds." Proceedings of the International Astronomical Union 8, S292 (August 2012): 267–70. http://dx.doi.org/10.1017/s1743921313001336.

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AbstractWithin galaxies, gas and dust are constantly exchanged between stars and the interstellar medium (ISM). The life-cycle of gas and dust is the key to the evolution of galaxies. Despite its importance, it is has been very difficult to trace the life-cycle of gas and dust via observations. The Spitzer Space Telescope and Herschel Space Observatory have provided a great opportunity to study the life-cycle of the gas and dust in very nearby galaxies, the Magellanic Clouds. AGB stars are more important contributors to the dust budget in the Large Magellanic Cloud (LMC), while in the Small Magellanic Cloud (SMC), SNe are dominant. However, it seems that the current estimates of the total dust production from AGB stars is insufficient to account for dust present in the ISM. Other dust sources are needed, and supernovae are promising sources. Alternatively the time scale of dust lifetime itself needs some revisions, potentially because they could be unevenly distributed in the ISM or clumps.
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Linsky, J. L., S. Redfield, and B. Wood. "Components of the Local Interstellar Medium." Symposium - International Astronomical Union 203 (2001): 595–98. http://dx.doi.org/10.1017/s007418090022007x.

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HST, EUVE, and Ca II spectra are providing critical velocity and column density data needed to identify individual stuctures (clouds) of warm gas in the local ISM. The Sun is located very close to the edge of and will soon leave the Local Interstellar Cloud (LIC). We will summarize the properties of the LIC and other nearby warm clouds.
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Ferrara, Andrea. "Probing ISM Models with Hα Observations." Publications of the Astronomical Society of Australia 15, no. 1 (1998): 19–23. http://dx.doi.org/10.1071/as98019.

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AbstractI review the capabilities of Hα observations to constrain some aspects of the current models of the interstellar medium. In particular, it is shown that turbulence is a necessary ingredient of any viable model, since most of the energy produced by supernova explosions and ionising radiation is stored in kinetic form in the ISM. Various forms of turbulent energy dissipation, including cloud collisions, are analysed. Two additional aspects, concerning the existence of galactic fountains and their relation with high-velocity Clouds, and the extended ionised layer of spiral galaxies are discussed; some crucial experiments are suggested.
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Mandal, Ankush, Dipanjan Mukherjee, Christoph Federrath, Nicole P. H. Nesvadba, Geoffrey V. Bicknell, Alexander Y. Wagner, and Moun Meenakshi. "Impact of relativistic jets on the star formation rate: a turbulence-regulated framework." Monthly Notices of the Royal Astronomical Society 508, no. 4 (October 2, 2021): 4738–57. http://dx.doi.org/10.1093/mnras/stab2822.

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ABSTRACT We apply a turbulence-regulated model of star formation to calculate the star formation rate (SFR) of dense star-forming clouds in simulations of jet–interstellar medium (ISM) interactions. The method isolates individual clumps and accounts for the impact of virial parameter and Mach number of the clumps on the star formation activity. This improves upon other estimates of the SFR in simulations of jet–ISM interactions, which are often solely based on local gas density, neglecting the impact of turbulence. We apply this framework to the results of a suite of jet–ISM interaction simulations to study how the jet regulates the SFR both globally and on the scale of individual star-forming clouds. We find that the jet strongly affects the multiphase ISM in the galaxy, inducing turbulence and increasing the velocity dispersion within the clouds. This causes a global reduction in the SFR compared to a simulation without a jet. The shocks driven into clouds by the jet also compress the gas to higher densities, resulting in local enhancements of the SFR. However, the velocity dispersion in such clouds is also comparably high, which results in a lower SFR than would be observed in galaxies with similar gas mass surface densities and without powerful radio jets. We thus show that both local negative and positive jet feedback can occur in a single system during a single jet event, and that the SFR in the ISM varies in a complicated manner that depends on the strength of the jet–ISM coupling and the jet break-out time-scale.
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Dissertations / Theses on the topic "ISM: clouds"

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Harju, J., F. Daniel, O. Sipilae, P. Caselli, J. E. Pineda, R. K. Friesen, A. Punanova, et al. "Deuteration of ammonia in the starless core Ophiuchus/H-MM1." EDP SCIENCES S A, 2017. http://hdl.handle.net/10150/624367.

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Context. Ammonia and its deuterated isotopologues probe physical conditions in dense molecular cloud cores. The time-dependence of deuterium fractionation and the relative abundances of different nuclear spin modifications are supposed to provide a means of determining the evolutionary stages of these objects. Aims. We aim to test the current understanding of spin-state chemistry of deuterated species by determining the abundances and spin ratios of NH2D, NHD2 and ND3 in a quiescent, dense cloud. Methods. Spectral lines of NH3, NH2D, NHD2, ND3 and N2D+ were observed towards a dense, starless core in Ophiuchus with the APEX, GBT and IRAM 30-m telescopes. The observations were interpreted using a gas-grain chemistry model combined with radiative transfer calculations. The chemistry model distinguishes between the different nuclear spin states of light hydrogen molecules, ammonia and their deuterated forms. Different desorption schemes can be considered. Results. High deuterium fractionation ratios with NH2D = NH3 similar to 0 : 4, NHD2 = NH2D similar to 0 : 2 and ND3 = NHD2 similar to 0 : 06 are found in the core. The observed ortho/para ratios of NH2D and NHD2 are close to the corresponding nuclear spin statistical weights. The chemistry model can approximately reproduce the observed abundances, but consistently predicts too low ortho/para-NH2D, and too large ortho/para-NHD2 ratios. The longevity of N2H+ and NH3 in dense gas, which is prerequisite to their strong deuteration, can be attributed to the chemical inertia of N-2 on grain surfaces. Conclusions. The discrepancies between the chemistry model and the observations are likely to be caused by the fact that the model assumes complete scrambling in principal gas-phase deuteration reactions of ammonia, which means that all the nuclei are mixed in reactive collisions. If, instead, these reactions occur through proton hop/hydrogen abstraction processes, statistical spin ratios are to be expected. The present results suggest that while the deuteration of ammonia changes with physical conditions and time, the nuclear spin ratios of ammonia isotopologues do not probe the evolutionary stage of a cloud.
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Thom, Christopher, and na. "High velocity clouds and the Milky Way Halo." Swinburne University of Technology, 2006. http://adt.lib.swin.edu.au./public/adt-VSWT20060920.101419.

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This thesis presents an exploration of stars and gas in the halo of our Galaxy. A sample of 8321 field horizontal branch (FHB) stars was selected from the Hamburg/ESO Survey. The stars make excellent tracers of the Milky Way halo, and we studied the kinematics of a subset of the HES FHB stars, comparing their velocity dispersions to those predicted by several models. Since these stars are intrinsically luminous, hot and numerous they make ideal probes of the distances to high-velocity clouds (HVCs) - clouds of neutral hydrogen gas whose distances are largely unknown and which do not fit simple models of Galaxy rotation. A catalogue of stars which align with the HVCs was developed. High resolution spectroscopy of 16 such HVC probes with the Magellan telescope has yielded a remarkably tight distance constraint to complex WB. This is one of only a handful of such distance limits so far established. Lower distance limits were set for several other clouds. Finally, we have suggested that some of the HVCs may be associated with the accretion onto the MilkyWay of the Sagittarius dwarf galaxy.
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Bieging, John H., Saahil Patel, William L. Peters, L. Viktor Toth, Gábor Marton, and Sarolta Zahorecz. "THE ARIZONA RADIO OBSERVATORY CO MAPPING SURVEY OF GALACTIC MOLECULAR CLOUDS. V. THE SH2-235 CLOUD IN CO J = 2 − 1, 13 CO J = 2 − 1, AND CO J = 3 − 2." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/621984.

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We present the results of a program to map the Sh2-235 molecular cloud complex in the CO and (CO)-C-13 J = 2 - 1 transitions using the Heinrich Hertz Submillimeter Telescope. The map resolution is 38 '' (FWHM), with an rms noise of 0.12K brightness temperature, for a velocity resolution of 0.34 km s(-1). With the same telescope, we also mapped the CO J = 3 - 2 line at a frequency of 345 GHz, using a 64 beam focal plane array of heterodyne mixers, achieving a typical rms noise of 0.5 K brightness temperature with a velocity resolution of 0.23 km s(-1). The three spectral line data cubes are available for download. Much of the cloud appears to be slightly sub-thermally excited in the J = 3 level, except for in the vicinity of the warmest and highest column density areas, which are currently forming stars. Using the CO and (CO)-C-13. J = 2 - 1 lines, we employ an LTE model to derive the gas column density over the entire mapped region. Examining a 125 pc(2). region centered on the most active star formation in the vicinity of Sh2-235, we find that the young stellar object surface density scales as approximately the 1.6-power of the gas column density. The area distribution function of the gas is a steeply declining exponential function of gas column density. Comparison of the morphology of ionized and molecular gas suggests that the cloud is being substantially disrupted by expansion of the H II regions, which may be triggering current star formation.
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Svoboda, Brian E., Yancy L. Shirley, Cara Battersby, Erik W. Rosolowsky, Adam G. Ginsburg, Timothy P. Ellsworth-Bowers, Michele R. Pestalozzi, et al. "THE BOLOCAM GALACTIC PLANE SURVEY. XIV. PHYSICAL PROPERTIES OF MASSIVE STARLESS AND STAR-FORMING CLUMPS." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/621258.

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We sort 4683 molecular clouds between 10 degrees < l < 65 degrees from the Bolocam Galactic Plane Survey based on observational diagnostics of star formation activity: compact 70 mu m sources, mid-IR color-selected YSOs, H2O and CH3OH masers, and UCH II. regions. We also present a combined NH3-derived gas kinetic temperature and H2O maser catalog for 1788 clumps from our own GBT 100 m observations and from the literature. We identify a subsample of 2223 (47.5%) starless clump candidates (SCCs), the largest and most robust sample identified from a blind survey to date. Distributions of flux density, flux concentration, solid angle, kinetic temperature, column density, radius, and mass show strong (>1 dex) progressions when sorted by star formation indicator. The median SCC is marginally subvirial (alpha similar to 0.7) with >75% of clumps with known distance being gravitationally bound (alpha < 2). These samples show a statistically significant increase in the median clump mass of Delta M similar to 170-370 M-circle dot from the starless candidates to clumps associated with protostars. This trend could be due to (i) mass growth of the clumps at (M) over dot similar to 200-440 M-circle dot Myr(-1) for an average freefall 0.8 Myr timescale, (ii) a systematic factor of two increase in dust opacity from starless to protostellar phases, and/or (iii). a variation in the ratio of starless to protostellar clump lifetime that scales as similar to M-0.4. By comparing to the observed number of CH3OH maser containing clumps, we estimate the phase. lifetime of massive (M > 10(3) M-circle dot) starless clumps to be 0.37 +/- 0.08 Myr (M/10(3) M-circle dot)(-1); the majority (M < 450 M-circle dot) have phase. lifetimes longer than their average freefall time.
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Seo, Youngmin, and Youngmin Seo. "The L1495-B218 Filaments in Taurus Seen in NH₃ & CCS and Dynamical Stability of Filaments and Dense Cores." Diss., The University of Arizona, 2016. http://hdl.handle.net/10150/621572.

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We present deep NH₃ and CCS maps of L1495-B218 filaments and the dense cores embedded within the filaments in Taurus. The L1495-B218 filaments form an interconnected, nearby, large complex extending over 8 pc. We observed the filaments in NH₃ (1,1)&(2,2), CCS Nⱼ = 1₂-0₁, and HC₇N J = 21-20 with spectral resolution of 0.038 km/s and spatial resolution of 31". The CSAR algorithm, which is a hybrid of seeded-watershed and binary dendrogram algorithm, identifies 39 leaves and 16 branches in NH₃ (1,1). Applying a virial analysis for the 39 NH₃ leaves, we find only 9 out of 39 leaves are gravitationally bound, and 12 out of 30 gravitationally unbound leaves are pressure-confined. Our analysis suggests that a dense core may form as a pressure-confined structure, evolve to a gravitationally bound core, and then undergo collapse to form a protostar. We find that the L1495A, B213E, and B216 regions have strong CCS emission and the B211 and B218 regions have weak CCS emission. Analysis of CCS emission with NH₃ (1,1) and dust continuum emission shows that CCS is not a good tracer for starless core evolution. On the other hand, CCS appears to trace recently accreted gas in L1495A and L1521D. We also present more realistic dynamic stability conditions for dense cores and filaments. In a new analysis of stability conditions we account for converging motions which have been modeled toward starless cores and take the effect of radiation fields. We find that the critical size of a dense core having a homologous converging motion with its peak speed being the sound speed is roughly half of the critical size of the Bonnor-Ebert sphere. We also find the critical mass/line density of a dense core/filament irradiated by radiation to be considerably smaller than that of the Bonnor-Ebert sphere/isothermal cylinder when the radiation pressure is stronger than the central gas pressure of dense core/isothermal cylinder. For regions in the inner Galaxy and near OB associations, the critical mass/line density of a dense structure may be less than 20% of the critical mass/line density of Bonnor-Ebert sphere/isothermal cylinder.
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Olofsson, Sven. "Extinction in Molecular Clouds : Case of Barnard 335." Doctoral thesis, Stockholms universitet, Institutionen för astronomi, 2012. http://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-72523.

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The Bok globule B335 is a small molecular cloud in the solar neighbourhood near the galactic plane. The aim for this three-paper-study is to construct and analyze the extinction for this globule. The method we apply is to use the light from field stars behind the cloud in broadband filters ranging from UV to the mid-infrared. We have observations performed at the ESO telescopes at La Silla and Paranal as well as at the Nordic 2.5 m telescope at La Palma. Together with images and spectra from 2MASS-, ISO- and Spitzer-archives we are able to cover the wavelength range from 0.35 to 24 μm. An important tool to analyze these observations results in order to get the extinction is the grid of synthetic stellar atmospheric spectra provided by Hauschildt (2005). The extinction so received is a result in itself. From the analysis of the extinction wavelength dependence we derive properties of the dust, especially its composition and grain size distribution. By modeling the grain size distribution we are able to find the extinction from the reddening of the stars. We find that the extinction in the optical wavelength 0.35 to 2 μm range nicely follows the functional form described by Cardelli et al. (1989). Our result from the wavelength range redward of 2 μm show an extinction dependent on the part of the cloud examined. For the rim of the cloud we get an extinction similar to that reported earlier for the diffuse interstellar medium. From the central parts of the cloud, however, a higher extinction was found. Our grain size model contains a carbonaceous particle distribution and a silicate one. The result can be explained by depletion of carbon onto carbonaceous grains and also by carbon onto all grains including the silicates. Our modeling of the extinction and our classification of the background stars allow us to - determine the distance to the globule - estimate the gas column density ratio - estimate the mass of globule - get a handle on the dust conversion processes through the grain size distribution   From the water- and CO-ice spectra we are able to estimate the ice column densities. We find similar ice column densities for the two ices. The estimates differ, when calculated from band strengths or from Lorenz-Mie calculations of ice mantles on the grain size distribution, by a factor of two.
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Wu, Ya-Lin, Kazushi Sakamoto, and Hsi-An Pan. "Submillimeter Array 12CO (2-1) Imaging of the NGC 6946 Giant Molecular Clouds." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/623951.

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We present a (CO)-C-12 (2-1) mosaic map of the spiral galaxy NGC 6946 by combining data from the Submillimeter Array and the IRAM 30m telescope. We identify 390 giant molecular clouds (GMCs) from the nucleus to 4.5 kpc in the disk. GMCs in the inner 1 kpc are generally more luminous and turbulent, some of which have luminosities > 10(6)K. km. s(-1) pc(2) and velocity dispersions > 10. km s(-1). Large-scale bar-driven dynamics likely regulate GMC properties in the nuclear region. Similar to the MilkyWay and other disk galaxies, GMC mass function of NGC 6946 has a shallower slope (index > -2) in the inner region, and a steeper slope (index < -2) in the outer region. This difference in mass spectra may be indicative of different cloud formation pathways: gravitational instabilities might play a major role in the nuclear region, while cloud coalescence might be dominant in the outer disk. Finally, the NGC 6946 clouds are similar to those inM33 in terms of statistical properties, but they are generally less luminous and turbulent than the M51 clouds.
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Seo, Young Min, and Andrew N. Youdin. "The role of non-ionizing radiation pressure in star formation: the stability of cores and filaments." OXFORD UNIV PRESS, 2016. http://hdl.handle.net/10150/621725.

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Stars form when filaments and dense cores in molecular clouds fragment and collapse due to self-gravity. In the most basic analyses of gravitational stability, the competition between self-gravity and thermal pressure sets the critical (i.e. maximum stable) mass of spheres and the critical line density of cylinders. Previous work has considered additional support from magnetic fields and turbulence. Here, we consider the effects of non-ionizing radiation, specifically the inward radiation pressure force that acts on dense structures embedded in an isotropic radiation field. Using hydrostatic, isothermal models, we find that irradiation lowers the critical mass and line density for gravitational collapse, and can thus act as a trigger for star formation. For structures with moderate central densities, similar to 10(3) cm(-3), the interstellar radiation field in the Solar vicinity has an order unity effect on stability thresholds. For more evolved objects with higher central densities, a significant lowering of stability thresholds requires stronger irradiation, as can be found closer to the Galactic centre or near stellar associations. Even when strong sources of ionizing radiation are absent or extincted, our study shows that interstellar irradiation can significantly influence the star formation process.
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Stanimirović, Snežana. "The complex nature of the ISM in the SMC : an HI and infrared study /." View thesis, 1999. http://library.uws.edu.au/adt-NUWS/public/adt-NUWS20030826.143835/index.html.

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Thesis (PhD) -- University of Western Sydney, Nepean, 1999.
"A thesis submitted for the degree of Doctor of Philosophy at the University of Western Sydney Nepean" "July, 1999" Bibliography : p. 177-185.
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Imara, Nia, Charles Lada, John Lewis, John H. Bieging, Shuo Kong, Marco Lombardi, and Joao Alves. "X Marks the Spot: Nexus of Filaments, Cores, and Outflows in a Young Star-forming Region." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/624336.

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We present a multiwavelength investigation of a region of a nearby giant molecular cloud that is distinguished by a minimal level of star formation activity. With our new (CO)-C-12(J = 2-1) and (CO)-C-13(J = 2-1) observations of a remote region within the middle of the California molecular cloud, we aim to investigate the relationship between filaments, cores, and a molecular outflow in a relatively pristine environment. An extinction map of the region from Herschel Space Observatory observations reveals the presence of two 2 pc long filaments radiating from a highextinction clump. Using the (CO)-C-13 observations, we show that the filaments have coherent velocity gradients and that their mass-per-unit-lengths may exceed the critical value above which filaments are gravitationally unstable. The region exhibits structure with eight cores, at least one of which is a starless, prestellar core. We identify a low-velocity, low-mass molecular outflow that may be driven by a flat spectrum protostar. The outflow does not appear to be responsible for driving the turbulence in the core with which it is associated, nor does it provide significant support against gravitational collapse.
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Books on the topic "ISM: clouds"

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Huché, Thierry. Cloud computing infrastructure on IBM Power Systems: Getting started with ISDM. Poughkeepsie, N.Y: IBM Corp., International Technical Support Organization, 2012.

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Matthew, Holm, ed. I'm grumpy. New York, NY: Random House Children's Books, 2016.

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Dai, Owen, ed. Isi a'r cloc. Caerdydd: Dref Wen, 2003.

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Ryan, Ken. Computer anxiety?: Instant relief! : an easy-to-read introduction to IBM PCs, compatibles, and clones. Anchorage, AK: Castle Mountain Press, 1991.

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Ryan, Ken. Computer anxiety?: Instant relief! : an easy-to-read introduction to IBM PCs, compatibles, and clones. 2nd ed. Anchorage, AK: Castle Mountain Press, 1992.

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Silver, Gerald A. Simplified BASIC programming for IBM PCs, PS/2s, compatibles & clones. 2nd ed. New York: Ardsley House Publishers, 1988.

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International Business Machines Corporation. International Technical Support Organization, ed. Multitenant utility computing on IBM Power Systems running AIX. [Poughkeepse, NY]: IBM, International Technical Support Organization, 2009.

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O'Hara, Brian T., and Ben Malisow. CCSP® (ISC)2® Certified Cloud Security Professional Official Study Guide. Hoboken, NJ, USA: John Wiley & Sons, Inc., 2017. http://dx.doi.org/10.1002/9781119419372.

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I'm just moving clouds today, tomorrow I'll try mountains: And other more or less blissfully Brilliant thoughts. Santa Barbara, Calif: Woodbridge Press, 1998.

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David, Warren. Desktop personal computer markets: Focus on IBM, the clones, and scenarios. Palo Alto, CA: Market Intelligence Research Co., 1987.

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Book chapters on the topic "ISM: clouds"

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Pettini, Max. "Studies of the ISM in the LMC Using SN1987A." In The Magellanic Clouds, 431. Dordrecht: Springer Netherlands, 1991. http://dx.doi.org/10.1007/978-94-011-3432-3_114.

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Braun, Robert, and Nissim Kanekar. "Tiny HI Clouds in the Local ISM." In The Initial Mass Function 50 Years Later, 303–8. Dordrecht: Springer Netherlands, 2005. http://dx.doi.org/10.1007/978-1-4020-3407-7_58.

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Kegel, Wilhelm H. "Fluctuations in the ISM Due to the Gravitational Interaction with the System of Stars." In Physical Processes in Interstellar Clouds, 125–36. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-3945-5_11.

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Kegel, Wilhelm H. "The Large-Scale Motion of the ISM and the Interaction with the System of Stars." In Physical Processes in Interstellar Clouds, 115–24. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-3945-5_10.

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Ballesteros-Paredes, Javier. "Molecular Clouds: Formation and Disruption." In From Observations to Self-Consistent Modelling of the ISM in Galaxies, 67–78. Dordrecht: Springer Netherlands, 2004. http://dx.doi.org/10.1007/978-94-007-0979-9_10.

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Wakker, Bart P. "Recent Developments Concerning High-Velocity Clouds." In From Observations to Self-Consistent Modelling of the ISM in Galaxies, 205–14. Dordrecht: Springer Netherlands, 2004. http://dx.doi.org/10.1007/978-94-007-0979-9_30.

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Konz, Christian, Guido T. Birk, and Harald Lesch. "Dynamical Evolution of High Velocity Clouds." In From Observations to Self-Consistent Modelling of the ISM in Galaxies, 215–18. Dordrecht: Springer Netherlands, 2004. http://dx.doi.org/10.1007/978-94-007-0979-9_31.

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Smith, Michael D., Georgi Pavlovski, Mordecai-Mark Maclow, Alexander Rosen, Tigran Khanzadyan, Roland Gredel, and Thomas Stanke. "Molecule Destruction and Formation in Molecular Clouds." In From Observations to Self-Consistent Modelling of the ISM in Galaxies, 157–60. Dordrecht: Springer Netherlands, 2004. http://dx.doi.org/10.1007/978-94-007-0979-9_23.

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Alves, J. "The Structure of Molecular Clouds from PC to AU Scale." In From Observations to Self-Consistent Modelling of the ISM in Galaxies, 83–87. Dordrecht: Springer Netherlands, 2004. http://dx.doi.org/10.1007/978-94-007-0979-9_12.

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Brüll, M., C. Kramer, V. Ossenkopf, R. Simon, and J. Stutzki. "The KOSMA Large-Scale CO Survey of Clouds in the Galactic Molecular Ring." In From Observations to Self-Consistent Modelling of the ISM in Galaxies, 79–82. Dordrecht: Springer Netherlands, 2004. http://dx.doi.org/10.1007/978-94-007-0979-9_11.

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Conference papers on the topic "ISM: clouds"

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Park, Minwoo, Dhiraj Joshi, and Alexander Loui. "Tag Cloud++ - Scalable Tag Clouds for Arbitrary Layouts." In 2012 IEEE International Symposium on Multimedia (ISM). IEEE, 2012. http://dx.doi.org/10.1109/ism.2012.66.

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Anderson, L. D., T. M. Bania, S. L. Snowden, Randall K. Smith, Steven L. Snowden, and K. D. Kuntz. "Mapping the Hot ISM Using X-Ray Shadowing Towards Infrared Dark Clouds." In THE LOCAL BUBBLE AND BEYOND II: Proceedings of the International Conference. AIP, 2009. http://dx.doi.org/10.1063/1.3211830.

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Kim, Taehoon, Kyoung-Sook Kim, Jun Lee, and Akiyoshi Matono. "Dotloom: Toward a Decentralized Data Platform for Massive Three-Dimensional Point Clouds." In 2019 IEEE International Symposium on Multimedia (ISM). IEEE, 2019. http://dx.doi.org/10.1109/ism46123.2019.00059.

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Shao, Wanpeng, Ken'Ichi Kakizaki, Shunsuke Araki, and Tomohisa Mukai. "Damage Detection of the RC Building in TLS Point Clouds Using 3D Deep Neural Network PointNet++." In 2021 IEEE International Symposium on Multimedia (ISM). IEEE, 2021. http://dx.doi.org/10.1109/ism52913.2021.00015.

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Trapero, Joaquin, John E. Beckman, Ricardo Génova, Conal D. McKeith, and Ingemar Lundström. "The cool neutral phase of the local ISM: compact clouds carry a major fraction of the mass." In Back to the Galaxy. AIP, 1992. http://dx.doi.org/10.1063/1.44010.

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Kazdagli, Mikhail, Mohit Tiwari, and Akshat Kumar. "Using Constraint Programming and Graph Representation Learning for Generating Interpretable Cloud Security Policies." In Thirty-First International Joint Conference on Artificial Intelligence {IJCAI-22}. California: International Joint Conferences on Artificial Intelligence Organization, 2022. http://dx.doi.org/10.24963/ijcai.2022/257.

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Modern software systems rely on mining insights from business sensitive data stored in public clouds. A data breach usually incurs significant (monetary) loss for a commercial organization. Conceptually, cloud security heavily relies on Identity Access Management (IAM) policies that IT admins need to properly configure and periodically update. Security negligence and human errors often lead to misconfiguring IAM policies which may open a backdoor for attackers. To address these challenges, first, we develop a novel framework that encodes generating optimal IAM policies using constraint programming (CP). We identify reducing dormant permissions of cloud users as an optimality criterion, which intuitively implies minimizing unnecessary datastore access permissions. Second, to make IAM policies interpretable, we use graph representation learning applied to historical access patterns of users to augment our CP model with similarity constraints: similar users should be grouped together and share common IAM policies. Third, we describe multiple attack models and show that our optimized IAM policies significantly reduce the impact of security attacks using real data from 8 commercial organizations, and synthetic instances.
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Baig, Roger, Rodrigo Carbajales, Pau Escrich, Jorge Florit, Felix Freitag, Agusti Moll, Leandro Navarro, et al. "The cloudy distribution in community network clouds in Guifi.net." In 2015 IFIP/IEEE International Symposium on Integrated Network Management (IM). IEEE, 2015. http://dx.doi.org/10.1109/inm.2015.7140459.

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Karam, Y., T. Baker, and A. T. Bendiab. "Oblivious Clouds: Towards Self-Conscious Cloud Based Application Development." In 2013 Fourth International Conference on Intelligent Systems, Modelling and Simulation (ISMS 2013). IEEE, 2013. http://dx.doi.org/10.1109/isms.2013.42.

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Kaur, Bhajneet, Laxmi Ahuja, and Vinay Kumar. "Applications of ISM and TISM: Model Building Techniques." In 2019 International Conference on Machine Learning, Big Data, Cloud and Parallel Computing (COMITCon). IEEE, 2019. http://dx.doi.org/10.1109/comitcon.2019.8862177.

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Khanna, Rashmi. "IBM SmartCloud Cost Management with IBM Cloud Orchestrator Cost Management on the Cloud." In 2016 IEEE International Conference on Cloud Computing in Emerging Markets (CCEM). IEEE, 2016. http://dx.doi.org/10.1109/ccem.2016.040.

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Reports on the topic "ISM: clouds"

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Wehr, Tobias, ed. EarthCARE Mission Requirements Document. European Space Agency, November 2006. http://dx.doi.org/10.5270/esa.earthcare-mrd.2006.

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ESA's EarthCARE (Cloud, Aerosol and Radiation Explorer) mission - scheduled to be launched in 2024 - is the largest and most complex Earth Explorer to date and will advance our understanding of the role that clouds and aerosols play in reflecting incident solar radiation back into space and trapping infrared radiation emitted from Earth's surface. The mission is being implemented in cooperation with JAXA (Japan Aerospace Exploration Agency). It carries four scientific instruments. The Atmospheric Lidar (ATLID), operating at 355 nm wavelength and equipped with a high-spectral resolution and depolarisation receiver, measures profiles of aerosols and thin clouds. The Cloud Profiling Radar (CPR, contribution of JAXA), operates at 94 GHz to measure clouds and precipitation, as well as vertical motion through its Doppler functionality. The Multi-Spectral Imager provides across-track information of clouds and aerosols. The Broad-Band Radiometer (BBR) measures the outgoing reflected solar and emitted thermal radiation in order to derive broad-band radiative fluxes at the top of atmosphere. The Mission Requirement Document defines the scientific mission objectives and observational requirements of EarthCARE. The document has been written by the ESA-JAXA Joint Mission Advisory Group for EarthCARE.
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Walker, Andrew Charles. ISR-1 Seminar: Nuclear Cloud Lofting. Office of Scientific and Technical Information (OSTI), April 2016. http://dx.doi.org/10.2172/1248115.

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Shyshkina, Mariya P. Сервісні моделі формування хмаро орієнтованого середовища вищого навчального закладу. [б. в.], August 2018. http://dx.doi.org/10.31812/0564/2449.

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The article is devoted to creating and development of the cloud based educational and scientific environment of higher education institutions, using modern approaches to the ICT infrastructure design, based on the different types of service models, including public, corporate or hybrid clouds. Object of the study: to conduct the theoretical analysis of the research trends of the cloud based higher education institution ICT infrastructure modeling in the context of the tendencies of the ICT development and standardization. Object of the study: the process of formation and development of the educational and research environment in the higher education institution. The purpose of the article: to reveal the current trends of the cloud-based service models of the learning environment design and implementation. The methods of the study: The analysis of scientific and educational literature on pro-research problems; domestic and foreign experience on the emerging ICT implementation in the learning process. Results: The main types of the service models of design and deploy the cloud-based infrastructure of the educational institution are revealed; the advantages and disadvantages of the cloud-based approach are considered; the promising ways of implementation are considered. Conclusions: there are promising ways of the learning environment cloud-based service models design and application, taking into consideration its preferences and disadvantages for the certain case study.
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Hochstein, Lorin. High Performance Computing (HPC) Innovation Service Portal Pilots Cloud Computing (HPC-ISP Pilot Cloud Computing). Fort Belvoir, VA: Defense Technical Information Center, August 2011. http://dx.doi.org/10.21236/ada549202.

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Meacham, Janette, Paul Meacham, Cynthia Huber, and Erica Grong. Adaptation of the NWM Cloud Environment for an ISF Project. Office of Scientific and Technical Information (OSTI), September 2021. http://dx.doi.org/10.2172/1822280.

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Berney, Ernest, Naveen Ganesh, Andrew Ward, J. Newman, and John Rushing. Methodology for remote assessment of pavement distresses from point cloud analysis. Engineer Research and Development Center (U.S.), April 2021. http://dx.doi.org/10.21079/11681/40401.

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The ability to remotely assess road and airfield pavement condition is critical to dynamic basing, contingency deployment, convoy entry and sustainment, and post-attack reconnaissance. Current Army processes to evaluate surface condition are time-consuming and require Soldier presence. Recent developments in the area of photogrammetry and light detection and ranging (LiDAR) enable rapid generation of three-dimensional point cloud models of the pavement surface. Point clouds were generated from data collected on a series of asphalt, concrete, and unsurfaced pavements using ground- and aerial-based sensors. ERDC-developed algorithms automatically discretize the pavement surface into cross- and grid-based sections to identify physical surface distresses such as depressions, ruts, and cracks. Depressions can be sized from the point-to-point distances bounding each depression, and surface roughness is determined based on the point heights along a given cross section. Noted distresses are exported to a distress map file containing only the distress points and their locations for later visualization and quality control along with classification and quantification. Further research and automation into point cloud analysis is ongoing with the goal of enabling Soldiers with limited training the capability to rapidly assess pavement surface condition from a remote platform.
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Shomer, Ilan, Louise Wicker, Uzi Merin, and William L. Kerr. Interactions of Cloud Proteins, Pectins and Pectinesterases in Flocculation of Citrus Cloud. United States Department of Agriculture, February 2002. http://dx.doi.org/10.32747/2002.7580669.bard.

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The overall objective was to understand the cloud flocculation of citrus juice by characterization of the interactions between proteins and pectins, and to determine the role of PE isozymes in catalyzing this phenomenon. Specific objectives were to: 1. identify/characterize cloud-proteins in relation to their coagulable properties and affinity to pectins; 2. to determine structural changes of PME and other proteins induced by cation/pectin interactions; 3. localize cloud proteins, PME and bound protein/pectates in unheated and pasteurized juices; 4. to create "sensitized" pectins and determine their effect on clarification. The original objectives were not changed but the methods and approach were modified due to specific research requirements. Two i postulates were: 1. there is a specific interaction of cloud proteins with de-esterified regions of ! pectin and this contributes to cloud loss; 2. isozymes of pectin-methyl-esterase (PME) vary in efficiency to create sensitized pectins. The appearance of citrus fruit juice is an important quality factor and is determined by the color and turbidity that .are conferred by the suspended particles, i.e., by the cloud and its homogeneity. Under some circumstances the cloud tend to flocculate and the juice clarifies. The accepted approach to explain the clarification is based on pectin demethoxylation by PME that promotes formation of Ca-pectate. Therefore, the juice includes immediate heat-inactivation upon ~ squeezing. Protein coagulation also promotes cloud instability of citrus fruit extracts. However, the clarification mechanism is not fully understood. Information accumulated from several laboratories indicates that clarification is a more complex process than can be explained by a single mechanism. The increasing trend to consume natural-fresh juice emphasizing the importance of the knowledge to assure homogeneity of fresh juice. The research included complementary directions: Conditions that induce cloud-instability of natural- juice [IL]. Evaluate purification schemes of protein [USA]. Identifications of proteins, pectin and neutral sugars ([IL]; Structure of the cloud components using light and electron microscopy and immuno-labeling of PME, high-methoxyl-pectin (HMP) and low-methoxyl-pectin (LMP); Molecular weight of calcium sensitized pectins [US]; Evaluation of the products of PME activity [US]. Fractions and size distribution and cloud components [IL-US]. The optimal pH activity of PME is 7 and the flocculation pH of the cloud is 3-4. Thus, the c roles of PME, proteins and pectins in the cloud instability, were studied in pH ranges of 2- 7. The experiments led to establish firstly repeatable simulate conditions for cloud instability [IL]. Thermostable PME (TS-PE) known to induce cloud instability, but also thermolabile forms of PME (TL-PE) caused clarification, most likely due to the formation and dissolution of inactive :. PE-pectin complexes and displacement of a protective colloid from the cloud surface [US]. Furthermore, elimination of non-PME protein increases TS-PE activity, indicating that non-PME proteins moderate PME activity [US]. Other experiments Concomitantly with the study of the PME activity but promotes the association of cloud-proteins to pectin. Adjusting of the juice pH to f 7 retains the cloud stability and re-adjusting of the pH to 40% DE reacts to immuno-labeling in the cloud fragments, whereas
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Popel, Maiia V., and Mariya P. Shyshkina. The areas of educational studies of the cloud-based learning systems. [б. в.], September 2019. http://dx.doi.org/10.31812/123456789/3245.

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The article analyzes the current stage of educational studies of the cloud-based learning systems. The relationship between the notions of the cloud-based learning system and the cloud-based learning environment are investigated. It was found that the researchers paid most attention to the design of a cloud-based learning environment. However, in the process of a cloud-based environment design, the researchers consider a cloud-based system as a component within the cloud-based learning environment of as a stage in the process of design. It is shown that in the research literature there is no single interpretation of the concept of a cloud-based system for educational purposes. Still the number of basic approaches to the interpretation of the concept under investigation are revealed. The first approach is based on the understanding of the system, as a set of cloud services or cloud-based technologies. The second approach is to consider a separate cloud service as a cloud-based learning system. In this case, the cloud service tools should include such components that cover the content, the tools, the forms and the methods of learning. The structure of the cloud-based learning system within the interpretation of the latest works of Ukrainian researchers is considered.
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Iatsyshyn, Anna V., Valeriia O. Kovach, Yevhen O. Romanenko, and Andrii V. Iatsyshyn. Cloud services application ways for preparation of future PhD. [б. в.], September 2019. http://dx.doi.org/10.31812/123456789/3248.

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Currently, it is important in Ukraine to harmonize cloud technologies application with European and world scientific initiatives. Need to modernize preparation of future PhDs is caused by challenges of new information, globalized society and digital transformation of all spheres of life, including education and science. The research was aimed to determine features of cloud services application in preparation of future PhDs. Concepts of “cloud computing”, “cloud technologies”, “cloud learning technologies”, “cloud services”, “cloud oriented environment” were analyzed. Experience of cloud technologies and their services application in educational and scientific space in researches of foreign and Ukrainian students was considered. Ukrainian experience in preparation of future PhD of various specialties with cloud services application was analyzed. It was emphasized that approaches improving to preparation of future PhDs based on cloud services application would increase their level of digital competence. It is recommended to include a separate course or module of specific discipline on work with cloud technologies and services during preparation of future PhDs. It is important to improve disciplines and tools content to support education process. It can be learning of disciplines using cloud technologies or services by future PhD’s. Also, cloud services application to support scientific and scientific-organizational activities will increase level of organization and implementation of scientific research. It is important to create cloud-oriented environment for preparation of future PhDs in higher education and research institutions. Making cloud-oriented educational and scientific environment should be based on principles of open education. It is recommended to use cloud-based platforms and services (G Suite for Education; Microsoft Office 365; specialized SaaS (CoCalc or other)).
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Valko, Nataliia V., Nataliya O. Kushnir, and Viacheslav V. Osadchyi. Cloud technologies for STEM education. [б. в.], July 2020. http://dx.doi.org/10.31812/123456789/3882.

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Cloud technologies being used in STEM education for providing robotics studying are highlighted in this article. Developing cloud robotic systems have not been used to their fullest degree in education but are applied by limited specialists’ number. Advantages given by cloud robotics (an access to big data, open systems, open environments development) lead to work with mentioned systems interfaces improving and having them more accessible. The potential represented by these technologies make them worth being shown to the majority of teachers. Benefits of cloud technologies for robotics and automatization systems are defined. An integrated approach to knowledge assimilation is STEM education basis. The demanded stages for robotics system development are shown and cloud sources which could be possibly used are analyzed in this article.
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