oalib

OALib Journal期刊

ISSN: 2333-9721

费用:99美元

投稿

时间不限

2017 ( 157 )

2016 ( 252 )

2015 ( 5107 )

2014 ( 6147 )

自定义范围…

匹配条件: “F. Remus” ,找到相关结果约144107条。
列表显示的所有文章,均可免费获取
第1页/共144107条
每页显示
Ecoturismo en la Región de la uva y el vino: Brasil
Fávero,Ivane Remus; Rotta Antunes,Janete;
Estudios y perspectivas en turismo , 2007,
Abstract: this article presents the preliminary results of an inventory on wine tourism conducted in the grape and wine region of the serra gaúcha, in southern brazil. it analyzes the wineries of the municipalities of bento gon?alves, garibaldi, monte belo do sul, veranópolis, cotipor?, vila flores, fagundes varela, caxias do sul, flores da cunha, nova pádua and farroupilha. wineries which are open to tourist and those who are starting to develop wine tourism were the universe of the study.
Ecoturismo en la Región de la uva y el vino: Brasil Wine Tourism in Southern Brazil
Ivane Remus Fávero,Janete Rotta Antunes
Estudios y perspectivas en turismo , 2007,
Abstract: Este artículo presenta los resultados preliminares del inventario de enoturismo en la Región Uva y Vino ubicada en la Sierra Gaucha - Río Grande do Sul, Brasil. El trabajo analiza las bodegas situadas en los municipios de Bento Gon alves, Garibaldi, Monte Belo do Sul, Veranópolis, Cotipor , Vila Flores, Fagundes Varela, Caxias do Sul, Flores da Cunha, Nova Pádua y Farroupilha. El universo de estudio se centra en las bodegas que cuentan con infraestructura turística y reciben visitantes y en aquellas que se están iniciando en el enoturismo. This article presents the preliminary results of an inventory on wine tourism conducted in the Grape and Wine Region of the Serra Gaúcha, in Southern Brazil. It analyzes the wineries of the municipalities of Bento Gon alves, Garibaldi, Monte Belo do Sul, Veranópolis, Cotipor , Vila Flores, Fagundes Varela, Caxias do Sul, Flores da Cunha, Nova Pádua and Farroupilha. Wineries which are open to tourist and those who are starting to develop wine tourism were the universe of the study.
The equilibrium tide in stars and giant planets: I - the coplanar case
F. Remus,S. Mathis,J. -P. Zahn
Physics , 2012, DOI: 10.1051/0004-6361/201118160
Abstract: Since 1995, more than 500 extrasolar planets have been discovered orbiting very close to their parent star, where they experience strong tidal interactions. Their orbital evolution depends on the physical mechanisms that cause tidal dissipation, and these are still not well understood. We refine the theory of the equilibrium tide in fluid bodies that are partly or entirely convective, to predict the dynamical evolution of the systems. In particular, we examine the validity of modeling the tidal dissipation by the quality factor Q, as is commonly done. We consider here the simplest case where the considered star or planet rotates uniformly, all spins are aligned, and the companion is reduced to a point-mass. The first manifestation of the tide is to distort the shape of the star or planet adiabatically along the line of centers. This generates the divergence-free velocity field of the adiabatic equilibrium tide which is decoupled from the dynamical tide. The tidal kinetic energy is dissipated into heat through turbulent friction, which is modeled here as an eddy-viscosity acting on the adiabatic tidal flow. This dissipation induces a second velocity field, the dissipative equilibrium tide, which is in quadrature with the exciting potential; it is responsible for the imaginary part of the disturbing function, which is implemented in the dynamical evolution equations, from which one derives characteristic evolution times. The rate at which the system evolves depends on the physical properties of tidal dissipation, and specifically on how the eddy viscosity varies with tidal frequency and on the thickness of the convective envelope for the fluid equilibrium tide. At low frequency, this tide retards by a constant time delay, whereas it lags by a constant angle when the tidal frequency exceeds the convective turnover rate.
Understanding tidal dissipation in gaseous giant planets : the respective contributions of their core and envelope
M. Guenel,S. Mathis,F. Remus
Physics , 2014,
Abstract: Tidal dissipation in planetary interiors is one of the key physical mechanisms that drive the evolution of star-planet and planet-moon systems. New constraints are now obtained both in the Solar and exoplanetary systems. Tidal dissipation in planets is intrinsically related to their internal structure. In particular, fluid and solid layers behave differently under tidal forcing. Therefore, their respective dissipation reservoirs have to be compared. In this work, we compute separately the contributions of the potential dense rocky/icy core and of the convective fluid envelope of gaseous giant planets, as a function of core size and mass. We then compare the associated dissipation reservoirs, by evaluating the frequency-average of the imaginary part of the Love numbers $k^2_2$ in each region. We demonstrate that in general both mechanisms must be taken into account.
Understanding tidal dissipation in gaseous giant planets from their core to their surface
M. Guenel,S. Mathis,F. Remus
Physics , 2014, DOI: 10.1051/epjconf/201510106029
Abstract: Tidal dissipation in planetary interiors is one of the key physical mechanisms that drive the evolution of star-planet and planet-moon systems. Tidal dissipation in planets is intrinsically related to their internal structure. In particular, fluid and solid layers behave differently under tidal forcing. Therefore, their respective dissipation reservoirs have to be compared. In this work, we compute separately the contributions of the potential dense rocky/icy core and of the convective fluid envelope of gaseous giant planets, as a function of core size and mass. We demonstrate that in general both mechanisms must be taken into account.
The Geographical and Socio-Cultural Aspects of the Minority of Ukrainians in Romania
Viorica Banciu,Remus Eugen F?ldvari,Bianca Dana Albu?
International Journal of Social Science and Humanity , 2013, DOI: 10.7763/ijssh.2013.v3.236
Abstract: Migrations have been seen throughout ancient and modern history. This mass movement represents a last resort to hardships that people endure in their own country. Like many other peoples many Ukrainians have seen in migration the best solution to the historical context they were undergoing. Some of them chose as their new home, primarily, the region of Maramures in the North of Romania. Most of the emigrants, bought land, settled down, established families and communities and have been peacefully coexisting with the Romanian population.
Anelastic tidal dissipation in multi-layer planets
F. Remus,S. Mathis,J. -P. Zahn,V. Lainey
Physics , 2012, DOI: 10.1051/0004-6361/201118595
Abstract: Earth-like planets have viscoelastic mantles, whereas giant planets may have viscoelastic cores. The tidal dissipation of such solid regions, gravitationally perturbed by a companion body, highly depends on their rheology and on the tidal frequency. Therefore, modelling tidal interactions presents a high interest to provide constraints on planets' properties and to understand their history and their evolution, in our Solar System or in exoplanetary systems. We examine the equilibrium tide in the anelastic parts of a planet whatever the rheology, taking into account the presence of a fluid envelope of constant density. We show how to obtain the different Love numbers that describe its tidal deformation. Thus, we discuss how the tidal dissipation in solid parts depends on the planet's internal structure and rheology. Finally, we show how the results may be implemented to describe the dynamical evolution of planetary systems. The first manifestation of the tide is to distort the shape of the planet adiabatically along the line of centers. Then, the response potential of the body to the tidal potential defines the complex Love numbers whose real part corresponds to the purely adiabatic elastic deformation, while its imaginary part accounts for dissipation. This dissipation is responsible for the imaginary part of the disturbing function, which is implemented in the dynamical evolution equations, from which we derive the characteristic evolution times. The rate at which the system evolves depends on the physical properties of tidal dissipation, and specifically on how the shear modulus varies with tidal frequency, on the radius and also the rheological properties of the solid core. The quantification of the tidal dissipation in solid cores of giant planets reveals a possible high dissipation which may compete with dissipation in fluid layers.
The surface signature of the tidal dissipation of the core in a two-layer planet
F. Remus,S. Mathis,J. -P. Zahn,V. Lainey
Physics , 2014, DOI: 10.1051/0004-6361/201424472
Abstract: Tidal dissipation, which is directly linked to internal structure, is one of the key physical mechanisms that drive systems evolution and govern their architecture. A robust evaluation of its amplitude is thus needed to predict evolution time for spins and orbits and their final states. The purpose of this paper is to refine recent model of the anelastic tidal dissipation in the central dense region of giant planets, commonly assumed to retain a large amount of heavy elements, which constitute an important source of dissipation. The previous paper evaluated the impact of the presence of the static fluid envelope on the tidal deformation of the core and on the associated anelastic tidal dissipation, through the tidal quality factor Qc. We examine here its impact on the corresponding effective anelastic tidal dissipation, through the effective tidal quality factor Qp. We show that the strength of this mechanism mainly depends on mass concentration. In the case of Jupiter- and Saturn-like planets, it can increase their effective tidal dissipation by, around, a factor 2.4 and 2 respectively. In particular, the range of the rheologies compatible with the observations is enlarged compared to the results issued from previous formulations. We derive here an improved expression of the tidal effective factor Qp in terms of the tidal dissipation factor of the core Qc, without assuming the commonly used assumptions. When applied to giant planets, the formulation obtained here allows a better match between the an elastic core's tidal dissipation of a two-layer model and the observations.
The anelastic equilibrium tide in exoplanetary systems
F. Remus,S. Mathis,J. -P. Zahn,V. Lainey
Physics , 2012,
Abstract: Earth-like planets have anelastic mantles, whereas giant planets may have anelastic cores. As for the fluid parts of a body, the tidal dissipation of such solid regions, gravitationally perturbed by a companion body, highly depends on its internal friction, and thus on its internal structure. Therefore, modelling this kind of interaction presents a high interest to provide constraints on planet interiors, whose properties are still quite uncertain. Here, we examine the equilibrium tide in the solid central region of a planet, taking into account the presence of a fluid envelope. We first present the equations governing the problem, and show how to obtain the different Love numbers that describe its deformation. We discuss how the quality factor Q depends on the rheological parameters, and the size of the core. Taking plausible values for the anelastic parameters, and examinig the frequency-dependence of the solid dissipation, we show how this mechanism may compete with the dissipation in fluid layers, when applied to Jupiter- and Saturn-like planets. We also discuss the case of the icy giants Uranus and Neptune.
POLICY DIALOG: THE MISSING LINK IN THE 2008 ROMANIAN HUMAN PAPILLOMAVIRUS (HPV) VACCINATION PROGRAM
Remus PRICOPIE
Transylvanian Review of Administrative Sciences , 2009,
Abstract: The model of the traditional decision-making deciding behind the closed doors of power is strongly eroded by the new perception of democracy, as it is gradually replaced by a model dominated not by managers, but by the management of decision. This article analyzes from the social sciences perspective a) why the Romanian 2008 HPV vaccination campaign turned out to be a failure, b) what generated the strong public rejection of a policy that the Ministry of Public Health supposed would be easily accepted by the population, and especially by the targeted group – the 10-11 years old girls and their parents. The article also seeks to offer recommendations, from the public communication perspective, regarding how policy dialogue and public participation might support the promotion of large-scale policies by involving the stakeholders at all stages of the decision-making process, and hence, avoiding unfounded social tensions and waste of valuable resources.
第1页/共144107条
每页显示


Home
Copyright © 2008-2017 Open Access Library. All rights reserved.