scholarly journals Secular Evolution of Satellites by Tidal Effect

Space Science ◽  
10.5772/36563 ◽  
2012 ◽  
Author(s):  
Alexandre C. M. Correia
Keyword(s):  
Tidal Effect ◽  
Secular Evolution

scholarly journals Joint Discussion 8: Stellar Evolution in Real Time, Part IV Miscellany

1998 ◽  
Vol 11 (1) ◽  
pp. 377-377
Keyword(s):  
Real Time ◽  
Stellar Evolution ◽  
Main Theme ◽  
Secular Evolution ◽  
Time Part

For a number of interesting contributed papers at the JD8 it was not obvious at the meeting or later that their contents and conclusions are germane to the main theme of secular evolution evidences. The editors have decided that these papers should be listed by title only. They appear below in alphabetized order by (first or only) author.

scholarly journals Evidence for Secular Evolution in Late-Type Spirals

1996 ◽  
Vol 457 (2) ◽  
Author(s):  
Stéphane Courteau ◽  
Roelof S. de Jong ◽  
Adrick H. Broeils
Keyword(s):  
Late Type ◽  
Secular Evolution

Temporal evolution of reactive and resistive nonlinear instabilities

1987 ◽  
Vol 38 (3) ◽  
pp. 473-481 ◽  
Author(s):  
D. B. Melrose
Keyword(s):  
Electron Number Density ◽  
Temporal Evolution ◽  
Random Phase ◽  
Low Frequency ◽  
Rate Of Change ◽  
Number Density ◽  
Wave Instability ◽  
Langmuir Waves ◽  
Secular Evolution ◽  
Coherent Wave

A kinetic theory for nonlinear processes involving Langmuir waves, developed in an earlier paper, is extended through consideration of three aspects of the temporal evolution, (i) Following Falk & Tsytovich (1975). the dynamic equation for the rate of change of one amplitude at t is expressed as an integral over T of the product of two amplitudes at t – T and a kernel functionf(T); two generalizations of Falk & Tsytovich's form (f(T) ∝ T) that satisfy the requirement f(∞) = 0 are identified, (ii) It is shown that the low-frequency or beat disturbance may be described in terms of fluctuations in the electron number density, and that its time evolution involves an operator that is essentially the inverse of f(t). (iii) The transition from oscillatory evolution in the reactive or ‘coherent-wave’ version of the three-wave instability to the secular evolution of the resistive or ‘random-phase’ version is discussed qualitatively.

scholarly journals Galaxy Dynamics: Secular Evolution and Accretion

2010 ◽  
Vol 6 (S271) ◽  
pp. 119-126 ◽  
Author(s):  
Francoise Combes
Keyword(s):  
Angular Momentum ◽  
Galaxy Evolution ◽  
Resonant Scattering ◽  
Relative Role ◽  
Radial Migration ◽  
Galaxy Dynamics ◽  
Secular Evolution ◽  
Minor Mergers ◽  
Gas Accretion

AbstractRecent results are reviewed on galaxy dynamics, bar evolution, destruction and re-formation, cold gas accretion, gas radial flows and AGN fueling, minor mergers. Some problems of galaxy evolution are discussed in particular, exchange of angular momentum, radial migration through resonant scattering, and consequences on abundance gradients, the frequency of bulgeless galaxies, and the relative role of secular evolution and hierarchical formation.

Water and the Oxidation State of Subduction Zone Magmas

Science ◽  
2009 ◽  
Vol 325 (5940) ◽  
pp. 605-607 ◽  
Author(s):  
Katherine A. Kelley ◽  
Elizabeth Cottrell
Keyword(s):  
Oxygen Fugacity ◽  
Subduction Zones ◽  
Melt Inclusions ◽  
Primary Control ◽  
Edge Structure ◽  
Secular Evolution ◽  
Oxidized Iron ◽  
Tectonic Settings ◽  
Major Factors ◽  
X Ray Absorption

Mantle oxygen fugacity exerts a primary control on mass exchange between Earth’s surface and interior at subduction zones, but the major factors controlling mantle oxygen fugacity (such as volatiles and phase assemblages) and how tectonic cycles drive its secular evolution are still debated. We present integrated measurements of redox-sensitive ratios of oxidized iron to total iron (Fe3+/ΣFe), determined with Fe K-edge micro–x-ray absorption near-edge structure spectroscopy, and pre-eruptive magmatic H2O contents of a global sampling of primitive undegassed basaltic glasses and melt inclusions covering a range of plate tectonic settings. Magmatic Fe3+/ΣFe ratios increase toward subduction zones (at ridges, 0.13 to 0.17; at back arcs, 0.15 to 0.19; and at arcs, 0.18 to 0.32) and correlate linearly with H2O content and element tracers of slab-derived fluids. These observations indicate a direct link between mass transfer from the subducted plate and oxidation of the mantle wedge.

scholarly journals Searching for a kinematic signature of the moderately metal-poor stars in the Milky Way bulge using N-body simulations

2018 ◽  
Vol 615 ◽  
pp. A100 ◽  
Author(s):  
A. Gómez ◽  
P. Di Matteo ◽  
M. Schultheis ◽  
F. Fragkoudi ◽  
M. Haywood ◽  
...  
Keyword(s):  
Milky Way ◽  
Thin Disk ◽  
Secular Evolution ◽  
Thick Disc ◽  
Thin Disc ◽  
The Mean ◽  
The Difference ◽  
Different Origins ◽  
Argos Data ◽  
Internal Evolution

Although there is consensus that metal-rich stars in the Milky Way bulge are formed via secular evolution of the thin disc, the origin of their metal-poor counterparts is still under debate. Two different origins have been invoked for metal-poor stars: they might be classical bulge stars or stars formed via internal evolution of a massive thick disc. We use N-body simulations to calculate the kinematic signature given by the difference in the mean Galactocentric radial velocity (ΔVGC) between metal-rich stars ([Fe/H] ≥ 0) and moderately metal-poor stars (–1.0 ≤ [Fe/H] < 0) in two models, one containing a thin disc and a small classical bulge (B/D = 0.1), and the other containing a thin disc and a massive centrally concentrated thick disc. We reasonably assume that thin-disk stars in each model may be considered as a proxy of metal-rich stars. Similarly, bulge stars and thick-disc stars may be considered as a proxy of metal-poor stars. We calculate ΔVGC at different latitudes (b = 0°, − 2°, − 4°, − 6°, − 8° and − 10°) and longitudes (l = 0°, ± 5°, ± 10° and ± 15°) and show that the ΔVGC trends predicted by the two models are different. We compare the predicted results with ARGOS data and APOGEE DR13 data and show that moderately metal-poor stars are well reproduced with the co-spatial stellar discs model, which has a massive thick disc. Our results give more evidence against the scenario that most of the metal-poor stars are classical bulge stars. If classical bulge stars exists, most of them probably have metallicities [Fe/H] < –1 dex, and their contribution to the mass of the bulge should be a small percentage of the total bulge mass.

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