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  • LUNAR AND PLANETARY EXPLORATION  (3.867)
  • Engineering  (3.361)
  • 2015-2019  (40)
  • 1990-1994  (7.188)
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  • 1
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    История исследований и разработок орудий и техники лова лабораторией промышленного рыболовства ЮгНИРО (2018)
    Kerch Branch ("YugNIRO") of FSBSI "AzNIIRKH" | Kerch, Crimea
    Details
    Publikationsdatum: 2021-05-19
    Beschreibung: Наряду с исследованиями по определению сырьевой базы Азово-Черноморского бассейна, при создании института АзЧерНИРО в 1933 г. была сразу организована научно-исследовательская лаборатория техники лова рыбы. За все время функционирования этого подразделения такие специалисты, как С.С. Виннов, О.И. Саковец, С.Я. Наместников, Е.Е. Шапунов, В.М. Кириллов, В.Г. Герасимов, В.С. Долбиш, Н.Г. Думин, В.Г. Васильев, А.А. Яковлев, Е.С. Деньгин, В.И. Абакаров, В.Н. Миронов, В.В. Стрельцов, А.С. Вайнерман, В.К. Яшкин, Ю.В. Шишов, А.М. Стафикопуло в течение многих лет вносили огромный вклад в развитие рыболовства в Азово-Черноморском бассейне и Мировом океане. До 1950 г. траловый промысел в Черном море отсутствовал, хотя были известны попытки внедрить этот вид лова в черноморское рыболовство. Так, в начале 1909 г. в северо-западной части Черного моря работал траулер «Федя». К концу 1911 г. количество траулеров, которые работали в данном регионе моря, увеличилось до 9 судов. Уловы состояли на 98-99 % из осетровых и на 1-2 % из камбалы. Ввиду очень большого вылова молоди осетровых рыб траловый промысел вскоре был запрещен. В 1932 г. из Мурманска для выяснения эффективности тралового лова в Черном море был послан рыболовный траулер «Абрек». Почти у всего черноморского побережья пробовали ловить отечественным промысловым тралом, применяемым в Баренцевом море для добычи трески. При этом отмечалось, что уловы камбалы были очень низкими. Очевидно, одной из причин была неприспособленность самой конструкции трала для лова этого вида рыб. В конце 1933 г. траулер вернулся в Мурманск. В 1949 г. Черноморская научно-промысловая экспедиция возобновила работы по освоению тралового лова в Черном море. Перед экспедицией стояла задача всесторонне изучить ихтиофауну моря и выяснить возможности применения ряда поисковых орудий лова, в том числе донного трала. С этой целью было разработано и испытано несколько типов донных тралов. С конца 1949 г. были начаты исследования по разработке конструкции разноглубинного трала для Черного моря. К тому времени инженерами М.К. Кокоревым, В.Ф. Шушпановым и А.Н. Потехиным была разработана специальная подъемно-распорная система. В соответствии с ее техническими данными в дальнейшем проектировались сетные части трала. Первый проект опытного рыболовного разноглубинного морского трала разрабатывался для лова мелких черноморских пелагических рыб в толще воды, на глубинах от 0 до 100 м, с одного судна. Большой вклад в развитие тралового промысла в Черном море внес А.Н. Самарянов.
    Beschreibung: Published
    Schlagwort(e): Engineering ; Fishing gear ; Fishing fleet ; Fishing vessels ; Trawlers ; Anchovy fisheries ; Sprat fisheries ; Purse fishing ; Commercial species ; Mullets
    Repository-Name: AquaDocs
    Materialart: Conference Material , Non Refereed
    Format: pp.247-254
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  • 2
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    Leading specialist of fish processing industry, scientist and lecturer Vinnov Aleksey Sergeevich (2019)
    Details
    Publikationsdatum: 2021-05-19
    Beschreibung: Aleksey Sergeevich Vinnov (25.05.1958 – 04.06.2019) was a Candidate of Sciences (Engineering), an Associate Professor, a talented lecturer, a rector of the Kerch Maritime Technological Institute (KMTI) in 2000–2005, a Senior Researcher in the FSBSI “Southern Scientific Research Institute of Marine Fisheries and Oceanography” (YugNIRO), and a Deputy Head for Operation and Quality of the Limited Liability Company under the Laws of Russian Federation “Aquamarine”. A.S. Vinnov made a great contribution into the development of education and science in the field of fisheries. Aleksey Sergeevich began his professional life as a Junior Researcher in the Astrakhan Technical Institute of Fishing Industry and Economy and defended his Candidate's Thesis in 1988. He dedicated the major part of his working career to the Kerch State Maritime Technological University, where he had been employed for 21 years, taking positions from a senior lecturer of the Department of Fish Processing Technology, an Associate Professor, the Dean of the Technological Faculty, the vice-rector for academic affairs, to the rector of the University. A.S. Vinnov was known for his rational thinking and professional integrity; he was diplomatic and considerate, and proved to be a competent leader. Vinnov's research works were dedicated to the issues of development of production technology for canned fish and fish protein mass, of kinetics of enzymatic hydrolysis, and many other subjects. A.S. Vinnov was honored with several badges of distinction due to his high professional expertise and personal contribution to the development of fisheries field, particularly education.
    Beschreibung: Алексей Сергеевич Виннов (25.05.1958 – 04.06.2019 гг.) — кандидат технических наук, доцент, талантливый преподаватель, ректор Керченского морского технологического института с 2000 по 2005 г. (КМТИ), старший научный сотрудник ФГБНУ «Южный научно-исследовательский институт рыбного хозяйства и океанографии» (ЮгНИРО), заместитель директора по производству и качеству ООО «Аквамарин». А.С. Виннов внес огромный вклад в развитие образования и науки рыбной отрасли. Свою трудовую деятельность Алексей Сергеевич начал в должности младшего научного сотрудника Астраханского технического института рыбной промышленности и хозяйства, успешно защитив в 1988 г. кандидатскую диссертацию. Большую часть своей трудовой деятельности он посвятил Керченскому государственному морскому технологическому университету, проработав здесь 21 год в должностях от старшего преподавателя кафедры технологии рыбных продуктов, доцента, декана технологического факультета, проректора по учебной работе до ректора университета. А.С. Виннов обладал рациональным мышлением, был очень грамотным, тактичным человеком, умелым руководителем. Научная деятельность Алексея Сергеевича была посвящена изучению вопросов усовершенствования технологии рыбных консервов, рыбных белковых масс, кинетики ферментативного гидролиза, а также многим другим. За личный вклад в развитие образования и рыбной отрасли, за высокий профессионализм А.С. Виннов был удостоен ряда почетных знаков отличия.
    Beschreibung: Published
    Schlagwort(e): Researchers ; Engineering ; Fish processing ; Canned food ; Rector ; Proteins ; Hydrolysis
    Repository-Name: AquaDocs
    Materialart: Journal Contribution , Refereed
    Format: pp.91-95
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  • 3
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    Near-surface ice on Mercury and the Moon: A topographic thermal model (1994)
    In:  Other Sources
    Details
    Publikationsdatum: 2019-08-28
    Beschreibung: A thermal model that can be easily adapted to craters of arbitrary shape is developed and applied to high-latitude impact craters on Mercury and the Moon, Chao Meng Fu crater at -87.5 deg L on Mercury, an unnamed bowl-shaped crater at 86.7 deg L on Mercury, and Peary crater at 88.6 deg L on the Moon. For an assumed input topography and grid of surface elements, the model computes for each element the irradiation from direct insolation and reflected and emitted radiation from other elements, taking into account shadowing by walls of the crater, partial obscuration of the solar disk near the poles and the diurnal, orbital, and seasonal cycles. Temperatures are computed over the surface grid as functions of depth and time from the surface to a specified depth and over the pertinent astronomical cycles, including the effects of direct and indirect surface irradiation, infrared radiation, heat conduction, and interior heating. Vapor fluxes and ice recession times are computed as functions of ice depth over the surface grid. Temperatures profiles, vapor fluxes, and ice recession times were computed for flat surfaces not associated with craters near the poles of Mercury and the Moon. It was found that water ice could have existed throughout geologic time within the maximum radar detection depth of recent observation of Mercury (J. K. Harmon and M. A. Slade, 1992, Science 258, 640-643) poleward of approximately 87 - 88 deg L on Mercury and poleward of approximately 73 deg L on the Moon. For Chao Meng Fu crater it was found that approximately 40% of the crater floor is permanently shadowed from direct solar insolation, while the remainder of the crater floor is periodically illuminated by a partially obscured Sun. Temperatures at the upper levels of the south wall can slightly exceed 550 K. Surface temperatures in the permanently shadowed region of the crater floor are under approximately 130 K, which could have allowed water ice to exist throughout geologic time within the radar detection depth of recent observation of Mercury. For small bowl-shaped crater on Mercury, it was found that most of the crater is permanently shadowed from direct solar radiation, except for a narrow semicircular band bordering the north rim. However, temperatures in the permanently shadowed region periodically reach a maximum near approximately 315 K due to efficient heating of the small crater by thermal emission and reflection from the small sunlit region, which periodically reaches temperatures exceeding 630 K. Water ice could not have existed throughout geologic time anywhere in this crater within the radar detection depth. For Peary crater on the Moon, the entire crater floor is permanently shadowed from direct solar insolation with maximum temperature under 120 K. The upper level of the north wall periodically reaches a maximum temperature near 310 K. The low temperatures on the crater floor would have allowed water ice to exist near the surface throughout geologic time, provided that the Moon's obliquity was always as low as it is at present.
    Schlagwort(e): LUNAR AND PLANETARY EXPLORATION
    Materialart: Icarus (ISSN 0019-1035); 111; 2; p. 441-455
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  • 4
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    Mars atmospheric loss and isotopic fractionation by solar-wind-induced sputtering and photochemical escape (1994)
    In:  Other Sources
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    Publikationsdatum: 2019-08-28
    Beschreibung: We examine the effects of the loss of Mars atmospheric constituents by solar-wind-induced sputtering and by photochemical escape during the past 3.8 billion years. Sputtering is capable of efficiently removing species from the upper atmosphere, including the light noble gases; nitrogen and oxygen are removed by photochemical processes as well. Due to diffusive separation (by mass) above the homopause, removal from the top of the atmosphere will fractionate the isotopes of each species, with the lighter mass being preferentially lost. For carbon and oxygen, this allows us to determine the size of nonatmospheric reservoirs which mix with the atmosphere; these reservoirs can be CO2 adsorbed in the regolith and H2O in the polar ice caps. We have constructed both simple analytical models and time-dependent models of the loss of volatiles from and supply to the martian atmosphere. Both argon and neon require continued replenishment from outgassing over geologic time. For argon, sputtering loss explains the fractionation of (Ar-36)/(Ar-38) without requiring a distinct epoch of hydrodynamic escape (although fractionation of Xe isotopes still requires very early hydrodynamic loss). For neon, the current (Ne-22)/(Ne-20) ratio represents a balance between loss to space and continued resupply from the interior; the similarity of the ratio to the terrestrial value is coincidental. For nitrogen, the loss by both sputtering and photochemical escape would produce a fractionation of (N-15)/(N-14) larger than observed; an early, thicker carbon dioxide atmosphere could mitigate the nitrogen loss and produce the observed fractionation, as could continued outgassing of juvenile nitorgen. Based on the isotopic constraints, the total amount of carbon dioxide lost over geologic time is probably on the order of tens of millibars rather than a substantial fraction of a bar. The total loss from solar-wind-induced sputtering and photochemical escape, therefore, does not seem able to explain the loss of a putative thick, early atmosphere withput requiring formation of extensive surface carbonate deposits or other nonatmospheric reservoirs for CO2.
    Schlagwort(e): LUNAR AND PLANETARY EXPLORATION
    Materialart: Icarus (ISSN 0019-1035); 111; 2; p. 271-288
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  • 5
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    Structural history of Maxwell Montes, Venus: Implications for Venusian mountain belt formation (1994)
    In:  Other Sources
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    Publikationsdatum: 2019-08-28
    Beschreibung: Models for Venusian mountain belt formation are important for understanding planetary geodynamic mechanisms. A range of data sets at various scales must be considered in geodynamic modelling. Long wavelength data, such as gravity and geoid to topography ratios, need constraints from smaller-scale observations of the surface. Pre-Magellan images of the Venusian surface were not of high enough resolution to observe details of surface deformation. High-resolution Magellan images of Maxwell Montes and the other deformation belts allow us to determine the nature of surface deformation. With these images we can begin to understand the constraints that surface deformation places on planetary dynamic models. Maxwell Montes and three other deformation belts (Akna, Freyja, and Danu montes) surround the highland plateau Lakshmi Planum in Venus' northern hemisphere. Maxwell, the highest of these belts, stands 11 km above mean planetary radius. We present a detailed structural and kinematic study of Maxwell Montes. Key observations include (1) dominant structure fabrics are broadly distributed and show little change in spacing relative to elevation changes of several kilometers; (2) the spacing, wavelength and inferred amplitude of mapped structures are small; (3) interpreted extensional structures occur only in areas of steep slope, with no extension at the highest topographic levels; and (4) deformation terminates abruptly at the base of steep slopes. One implications of these observations is that topography is independent of thin-skinned, broadly distributed, Maxwell deformation. Maxwell is apparently stable, with no observed extensional collapse. We propose a 'deformation-from-below' model for Maxwell, in which the crust deforms passively over structurally imbricated and thickened lower crust. This model may have implications for the other deformation belts.
    Schlagwort(e): LUNAR AND PLANETARY EXPLORATION
    Materialart: Journal of Geophysical Research (ISSN 0148-0227); 99; E12; p. 26105-26028
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  • 6
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    Thermal and albedo mapping of the polar regions of Mars using Viking thermal mapper observations: 2. South polar region (1994)
    In:  Other Sources
    Details
    Publikationsdatum: 2019-08-28
    Beschreibung: We present the first maps of the apparent thermal inertia and albedo of the south polar region of Mars. The observations used to create these maps were acquired by the infrared thermal mapper (IRTM) instruments on the two Viking Orbiters over a 30-day period in 1977 during the Martian late southern summer season. The maps cover the region from 60 deg S to the south pole at a spatial resolution of 1 deg of latitude, thus completing the initial thermal mapping of the entire planet. The analysis and interpretation of these maps is aided by the results of a one-dimensional radiative convective model, which is used to calculate diurnal variations in surface and atmospheric temperatures, and brightness temperatures at the top of the atmosphere for a range of assumptions concerning dust optical properties and dust optical depths. The maps show that apparent thermal inertias of bare ground regions decrease systematically from 60 deg S to the south pole. In unfrosted regions close to the south pole, apparent thermal inertias are among the lowest observed anywhere on the planet. On the south residual cap, apparent thermal inertias are very high due to the presence of CO2 frost. In most other regions of Mars, best fit apparent albedos based on thermal emission measurements are generally in good agreement with actual surface albedos based on broadband solar reflectance measurements. The one-dimensional atmospheric model calculations also predict anomalously cold brightness temperatures close to the pole during late summer, and after considering a number of alternatives, it is concluded that the net surface cooling due to atmospheric dust is the best explanation for this phenomenon. The region of lowest apparent thermal inertia close to the pole, which includes the south polar layered deposits, is interpreted to be mantled by a continuous layer of aeolian material that must be at least a few millimeters thick. The low thermal inertias mapped in the south polar region imply an absence of surface water ice deposits, which is consistent with Viking Mars atmospheric water detector (MAWD) measurements which show low atmospheric water vapor abundances throughout the summer season.
    Schlagwort(e): LUNAR AND PLANETARY EXPLORATION
    Materialart: Journal of Geophysical Research (ISSN 0148-0227); 99; E12; p. 25993-26013
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  • 7
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    Carbonate-sulfate volcanism on Venus? (1994)
    In:  Other Sources
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    Publikationsdatum: 2019-08-28
    Beschreibung: Venusian canali, outflow channels, and associated volcanic deposits resemble fluvial landforms more than they resmeble volcanic features on Earth and Mars. Some canali have meandering habits and features indicative of channel migration that are very similar to meandering river channels and flood plains on Earth, venusian outflow channels closely resemble water-carved outflow channels on Mars and the Channeled Scabland in Washington, collapsed terrains at the sources of some venusian channels resemble chaotic terrains at the sources of martian outflow channels, venusian lava deltas are similar to bird's-foot deltas such as the Mississippi delta, and venusian valley networks indicate sapping. We have developed an alternative possibility that the lava had a water-like rheology and a melting point slightly greater than Venus' surface temperature, thus accounting for the unusual behavior of the lava. Unlike silicate lavas, some carbonatites (including carbonate-sulfate-rich liquids) have these properties; thus they can flow great distances while retaining a high fluidity, significant mechanical erosiveness, and substantial capacity to transport and deposit sediment. Venusian geochemistry and petrology are consistent with extensive eruptions of carbonatite lavas, which could have crustal and/or mantle origins. Venus' atmosphere (especially CO2, HCl, and HF abundances) and rocks may be in local chemical equilibrium, which suggests that the upper crust contains large amounts of calcite, anhydrite, and other salts. Chemical analyses indicate, according to some models, that Venusian rocks may contain 4-19% calcite and anhydrite. Mixtures of crustal salts could melt at temperatures a few tens to a few hundred Kelvins higher than Venus' surface temperature; hence, melting may be induced by modest endogenetic or impact heating. Salts may have many of the same geologic roles on Venus as water and ice have on Mars. A molten salt (carbonatite) 'aquifer' may exist beneath a few hundred meters to several kilometers of solidified salt-rich 'permafrost.' Many geologic features can be explained by carbonatite magmatism: (1) impact melting of crustal salts can explain crater outflows, (2) small, sustained eruptions from molten salt aquifers can explain sapping valleys, (3) large, sustained eruptions may explain canali and their flood plans, and (4) catastrophic outbursts amy have formed outflow channels and chaotic terrain. Landforms created by carbonate-rich lavas would be thermally stable on Venus' surface, though some minerals may weather to other solid substances.
    Schlagwort(e): LUNAR AND PLANETARY EXPLORATION
    Materialart: Icarus (ISSN 0019-1035); 112; 1; p. 219-252
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  • 8
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    The isostatic state of Mead crater (1994)
    In:  Other Sources
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    Publikationsdatum: 2019-08-28
    Beschreibung: We have analyzed high-resolution Magellan Doppler tracking data over Mead crater, using both line-of-sight and spherical harmonic methods, and have found a negative gravity anomaly of about 4-5 mgal (at spacecraft altitude, 182 km). This is consistent with no isostatic compensation of the present topography; the uncertainty in the analysis allows perhaps as much as 30% compensation at shallow dpeths (approximately 25 km). This is similar to observations of large craters on Earth, which are not generally compensated, but contrasts with at least some lunar basins which are inferred to have large Moho uplifts and corresponding positive Bouguer anomalies. An uncompensated load of this size requires a lithosphere with an effective elastic lithosphere thickness greater than 30 km. In order for the crust-mantle boundary not to have participated in the deformation associated with the collapse of the transient cavity during the creation of the crater, the yield strength near the top of the mantle must have been significantly higher on Earth and Venus than on the Moon at the time of basin formation. This might be due to increased strength against frictional sliding at the higher confining pressures within the larger planets. Alternatively, the thinner crusts of Earth and Venus compared to that of the Moon may result in higher creep strength of the upper mantle at shallower depths.
    Schlagwort(e): LUNAR AND PLANETARY EXPLORATION
    Materialart: Icarus (ISSN 0019-1035); 112; 1; p. 117-129
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  • 9
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    Gravitational tides on Jupiter. 3: Atmospheric response and mean flow acceleration (1994)
    In:  Other Sources
    Details
    Publikationsdatum: 2019-08-28
    Beschreibung: The gravitational tidal response at the visible cloud level of Jupiter is obtained as a function of static stability in the planetary interior. It is suggested that confirmation of the presence of static stability in the planetary interior could be achieved by observing tidal fields at cloud level. We also calculate the mean flow acceleration induced by tidal fields and suggest that, if the interior is even marginally statically stable, the tides may provide the momentum source maintaining the alternating zonal jets observed at the cloud level of the planet.
    Schlagwort(e): LUNAR AND PLANETARY EXPLORATION
    Materialart: Astrophysical Journal, Part 1 (ISSN 0004-637X); 424; 2; p. 1005-1013
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  • 10
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    State of stress, faulting, and eruption characteristics of large volcanoes on Mars (1993)
    In:  Other Sources
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    Publikationsdatum: 2019-08-28
    Beschreibung: The formation of a large volcano loads the underlying lithospheric plate and can lead to lithospheric flexure and faulting. In turn, lithospheric deformation affects the stress field beneath and within the volcanic edifice and can influence magma transport. Modeling the interaction of these processes is crucial to an understanding of the history of eruption characteristics and tectonic deformation of large volcanoes. We develop models of time-dependent stress and deformation for the Tharsis volcanoes on Mars. By means of a finite element code, we calculate stresses and displacements due to a volcano-shaped load emplaced on an elastic plate overlying a viscoelastic mantle. Models variously incorporate growth of the volcanic load with time and a detachment between volcano and lithosphere. The models illustrate the manner in which time-dependent stresses induced by lithospheric plate flexure beneath the volcanic load may affect eruption histories, and the derived stress fields can be related to tectonic features on and surrounding Martian volcanoes. As a result of flexure there are three regions where stresses become sufficiently large to cause failure by faulting, according to the Mohr-Coulomb criterion: at the surface of the plate just outward of the volcano, near the base of the elastic lithosphere beneath the center of the volcano, and on the upper flanks of the volcano early in its growth history.
    Schlagwort(e): LUNAR AND PLANETARY EXPLORATION
    Materialart: Journal of Geophysical Research (ISSN 0148-0227); 98; E12; p. 23,553-23,579
    Format: text
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