bluuebunny/crossref_metadata_2025_split huggingface dataset:
Etude des inclusions fluides des minéralisations Ba,F(Zn,Pb) du district métallogénique sud de Belgique
Authors: Darimont Anne 
Published: November 2018

Vein-type mineralizations Ba,F(Zn-Pb) in Devonian (Frasnian, Givetian) carbonate host rocks from the metallogenetic district of South Belgium, are studied by fluid inclusions. The paragenetic sequence determined by petrographic studies at Beauraing is listed as follows : sphalerite-fluorite I, calcite-fluorite II, barite-galena.
First melting temperatures are lower than -50 °C. Filling temperatures Th and ice melting points Tm are : sphalerite (110 °C, -15 °C), fluorite I (75 °C, -23 °C), calcite (140 °C, -4 °C), fluorite II (125 °C, -2 °C) and barite (< 50 °C, —6 °C).
NaCl-CaCl2-H2O solutions represent fairly well the composition of the mineralizing brines ; in sphalerite, the molality in Cl- ions is around 4.4 ; and the salinity is comprised between 10 and 14 % NaCl with 10 and 6 % CaCl2.
The observation of fluorite II, characterized by Th= 125 °C and Tm = -2 °C, in the whole district attests to the regional distribution of the fluid responsible for this episode.
This study enables the reconstitution of thermobarometric evolution. The crystallization of sphalerite and fluorite I takes place around 1 000 bars and 180 °C, as shown by the intersection of their respective isochores in P-T diagram.
Deposition of calcite and fluorite II, characterized by the highest filling temperatures is suggested as a consequence of later reopening of veins, with subsequent decrease in pressure.
Barite and galena represent the low temperature final stage.
Caractéristiques physico-chimiques des fluides associés à la genèse du gisement de tungstène de Borralha (Nord Portugal)
Authors: Noronha Fernando 
Published: November 2018

The tungsten-ore deposit of Borralha is of the vein-type, with quartz being the gangue mineral. The ore deposit comprises, also, two collapse breccias cemented by quartz which are spatially related to the veins.
Schematically, the mineralized structures are characterized by an association of quartz, wolframite, scheelite and sulphides.
The temperature has not markedly changed from the tungstates up to the sulfides deposition : it lies between 330 °C and 290 °C.
During the main W-mineralization and breccia formation, the pressure ranged from 650 to 1 000 bars.
The hydrothermal fluids have an average salinity of 10 wt. % eq.NaCl. Initially, they contain up to 11 mole % CO2 and become purely aqueous. The fluids carrying W have compositions dominated by Na+, Cl-and HCO3- (Na > K) and are acidic. Their corrosive activity is weak : it only causes minor alteration of the wall-rock.
Fluid inclusions associated with the generation of pseudotachylyte and ultramylonite in the French Pyrénées
Authors: Passchier Cees W. 
Published: November 2018

Dans le Massif du Saint-Barthélémy, des rubans d'ultramylonite et de pseudotachylite se sont développés dans une zone de cisaillement importante à la fin d'une phase de mylonitisation à caractère rétromorphique. Certains rubans ultramylonitiques ont été partiellement formés par des mécanismes de recristallisation et de décroissance de la taille des grains, d'autres par une déformation ductile de la pseudotachylite. Des mesures microthermométriques indiquent que les inclusions fluides dans la zone de cisaillement contiennent du CO2 pur.
Le manque d'eau dans la phase fluide a probablement entraîné le durcissement de la roche pendant la déformation mylonitique. L'ultramylonite et la pseudotachylite ont été formées à 2-3,5 kbar et 450-550 °C. La température relativement élevée de la roche-hôte est probablement la cause principale de la déformation ductile de la pseudotachylite. Des recherches sur les inclusions fluides autour des rubans de pseudotachylite peuvent être importantes pour déterminer les conditions de formation de tels rubans.
Composition and significance of fluid inclusions in the Ilímaussaq peralkaline granite, South Greenland
Authors: Konnerup-Madsen Jens , Rose-Hansen John 
Published: November 2018

On a étudié les inclusions fluides dans le quartz du granite péralcalin, des filons granitiques, et des filons de quartz dans l'intrusion essentiellement soussaturée en silice d'Ilímaussaq, Groenland du Sud. Contrairement aux fluides riches en hydrocarbures des syénites agpaïtiques de l'intrusion, les fluides dans le granite sont entièrement aqueux avec 2 à 64 % poids en équivalent NaCl et présentent des densités variables comprises entre 0,2 et 1,2. Les conditions de solidification du granite entre 650° et 700 °C et environ 1 kbar sont marquées par les inclusions fluides les plus précoces.
Les inclusions fluides des filons de quartz et des filons granitiques, formés par réaction entre la syénite à augite et les grès, contiennent du CO2 et du CH4 en plus des fluides aqueux. La différence marquée entre les fluides riches en hydrocarbures des filons granitiques et les fluides entièrement aqueux du granite indique que le granite alcalin d'Ilímaussaq, les syénites agpaïtiques à népheline et la syénite à augite ne sont pas liés par des processus d'assimilation des grès, mais que le liquide granitique représente un liquide acide étranger au liquide sous-saturé en silice d'Ilímaussaq.
Contribution to the theory of infiltration metasomatic zoning ; the formation of sharp fronts : a geometrical model
Authors: Guy Bernard 
Published: November 2018

We propose here a contribution to the simplest model accounting for the appearance of spatial concentration discontinuities during the formation of metasomatic rocks. It is based on the "infiltration" model of Korzhinskii (1970) which we have reconsidered because it seemed defective on that crucial point, beyond some particular aspects of simplification or exposition.
We show that there is a geometrical solution to the equation of Korzhinskii : it allows to visualize the evolution in time and space of the concentration profiles and the appearance and growth of discontinuity fronts. In the past the mere reasonning on the isotherm had made this evolution disappear and more or less implicitly led to particular initial and boundary conditions.
The main point is the possible appearance, within the framework of this model, of a triple solution : this expresses a qualitative change in the evolution of the system (bifurcation) and necessitates a choice that was not made clear by previous authors.
Dynamical Evolution and Merger Timescales of LISA Massive Black Hole Binaries in Disk Galaxy Mergers
Authors: Khan Fazeel M. , Capelo Pedro R. , Mayer Lucio , Berczik Peter 
Published: November 2018

Abstract
The Laser Interferometer Space Antenna (LISA) will detect gravitational-wave (GW) signals from merging supermassive black holes (BHs) with masses below 107 M
⊙. It is thus of paramount importance to understand the orbital dynamics of these relatively light central BHs, which typically reside in disk-dominated galaxies, in order to produce reliable forecasts of merger rates. To this aim, realistic simulations probing BH dynamics in unequal-mass disk galaxy mergers, into and beyond the binary hardening stage, are performed by combining smooth particle hydrodynamics and direct N-body codes. The structural properties and orbits of the galaxies are chosen to be consistent with the results of galaxy formation simulations. Stellar and dark matter distributions are triaxial down to the central 100 pc of the merger remnant. In all cases, a BH binary forms and hardens on timescales of at most 100 Myr, coalescing on another few-hundred-megayear timescale, depending on the characteristic density and orbital eccentricity. Overall, the sinking of the BH binary takes no more than ∼0.5 Gyr after the merger of the two galaxies is completed, but it can be much faster for very plunging orbits. Comparing with previous numerical simulations following the decay of BHs in massive early-type galaxies at z ∼ 3, we confirm that the characteristic density is the most crucial parameter determining the overall BH merging timescale, despite the structural diversity of the host galaxies. Our results lay down the basis for robust forecasts of LISA event rates in the case of merging BHs.
Electromagnetic Wave Emissions from a Turbulent Plasma with Density Fluctuations
Authors: Volokitin A. S. , Krafft C. 
Published: November 2018

Abstract
In the solar wind, Langmuir turbulence can generate electromagnetic waves at the fundamental plasma frequency ω

p
. This process can likely result from either linear wave transformations on the ambient random density inhomogeneities or resonant three-wave interactions involving Langmuir waves and ion acoustic oscillations. In the presence of sufficiently intense plasma density fluctuations of scales much larger than the Langmuir wavelengths, the first mechanism may be more efficient than the second one. A new approach to calculate the electromagnetic wave emissions by Langmuir wave turbulence in plasmas with background density fluctuations is developed. The evolution of the Langmuir turbulence is studied by numerically solving the Zakharov equations in such a two-dimensional plasma. The dynamics of the spatial distributions of the electric currents with frequencies close to ω

p
is calculated, as well as their emission into electromagnetic waves. The efficiency of this radiation is determined as a function of the level of the Langmuir turbulence, the characteristics of the density fluctuations, the background plasma temperature, the position of the satellite receiver, and the durations of the source’s emissions and spacecraft’s observations. The results obtained by the theoretical modeling and numerical simulations are successfully compared with space observations of electromagnetic waves radiated during Type III solar radio bursts.
KIC 2568888: To Be or Not to Be a Binary
Authors: Themessl N. , Hekker S. , Mints A. , García R. A. , Montellano A. García Saravia Ortiz de , Stetson P. B. , Ridder J. De 
Published: November 2018

Abstract
In cases where both components of a binary system show oscillations, asteroseismology has been proposed as a method to identify the system. For KIC 2568888, observed with Kepler, we detect oscillation modes for two red giants in a single power-density spectrum. Through an asteroseismic study we investigate if the stars have similar properties, which could be an indication that they are physically bound into a binary system. While one star lies on the red giant branch (RGB), the other, more evolved star, is either a RGB or asymptotic giant branch star. We found similar ages for the red giants and a mass ratio close to 1. Based on these asteroseismic results, we propose KIC 2568888 as a rare candidate binary system (∼0.1% chance). However, when combining the asteroseismic data with ground-based BVI photometry we estimated different distances for the stars, which we cross-checked with Gaia DR2. From Gaia we obtained for one object a distance between and broadly consistent with the distances from BVI photometry. For the other object we have a negative parallax with a not yet reliable Gaia distance solution. The derived distances challenge a binary interpretation and may either point to a triple system, which could explain the visible magnitudes, or, to a rare chance alignment (∼0.05% chance based on stellar magnitudes). This probability would even be smaller, if calculated for close pairs of stars with a mass ratio close to unity in addition to similar magnitudes, which may indeed indicate that a binary scenario is more favorable.
Dynamic Equilibrium Sets of the Atomic Content of Galaxies across Cosmic Time
Authors: Wang Liang , Obreschkow Danail , Lagos Claudia D. P. , Sweet Sarah M. , Fisher Deanne B. , Glazebrook Karl , Macciò Andrea V. , Dutton Aaron A. , Kang Xi 
Published: November 2018

Abstract
We analyze 88 independent, high-resolution, cosmological zoomed-in simulations of disk galaxies in the NIHAO simulations suite to explore the connection between the atomic gas fraction and angular momentum (AM) of baryons throughout cosmic time. The study is motivated by the analytical model of Obreschkow et al., which predicts a relation between the atomic gas fraction f
atm and the integrated atomic stability parameter

, where M and j are the mass and specific AM of the galaxy (stars+cold gas) and σ is the velocity dispersion of the atomic gas. We show that the simulated galaxies follow this relation from their formation (z ≃ 4) to the present within ∼0.5 dex. To explain this behavior, we explore the evolution of the local Toomre stability and find that 90%–100% of the atomic gas in all simulated galaxies is stable at any time. In other words, throughout the entire epoch of peak star formation until today, the timescale for accretion is longer than the timescale to reach equilibrium, thus resulting in a quasi-static equilibrium of atomic gas at any time. Hence, the evolution of f
atm depends on the complex hierarchical growth history primarily via the evolution of q. An exception is galaxies subject to strong environmental effects.
A Redshift-independent Efficiency Model: Star Formation and Stellar Masses in Dark Matter Halos at z ≳ 4
Authors: Tacchella Sandro , Bose Sownak , Conroy Charlie , Eisenstein Daniel J. , Johnson Benjamin D. 
Published: November 2018

Abstract
We explore the connection between the UV luminosity functions (LFs) of high-z galaxies and the distribution of stellar masses and star formation histories (SFHs) in their host dark matter halos. We provide a baseline for a redshift-independent star formation efficiency model to which observations and models can be compared. Our model assigns a star formation rate (SFR) to each dark matter halo based on the growth rate of the halo and a redshift-independent star formation efficiency. The dark matter halo accretion rate is obtained from a high-resolution N-body simulation in order to capture the stochasticity in accretion histories and to obtain spatial information for the distribution of galaxies. The halo mass dependence of the star formation efficiency is calibrated at z = 4 by requiring a match to the observed UV LF at this redshift. The model then correctly predicts the observed UV LF at z = 5–10. We present predictions for the UV luminosity and stellar mass functions, JWST number counts, and SFHs. In particular, we find a stellar-to-halo mass relation at z = 4–10 that scales with halo mass at M
h < 1011
M
⊙ as M
⋆ ∝ M
h
2, with a normalization that is higher than the relation inferred at z = 0. The average SFRs increase as a function of time to z = 4, although there is significant scatter around the average: about 6% of the z = 4 galaxies show no significant mass growth. Using these SFHs, we present redshift-dependent UV-to-SFR conversion factors, mass return fractions, and mass-to-light ratios for different initial mass functions and metallicities, finding that current estimates of the cosmic SFR density at z ∼ 10 may be overestimated by ∼0.1–0.2 dex.
A Role for Turbulence in Circumgalactic Precipitation
Authors: Voit G. Mark 
Published: November 2018

Abstract
The cooling time, t
cool, of the hot ambient medium pervading a massive galaxy does not drop much below 10 times the freefall time t
ff at any radius. Theoretical models have accounted for this finding by hypothesizing that cold clouds start to condense out of the ambient medium when t
cool/t
ff ≲ 10 and fuel a strong black hole feedback response, but they have not yet provided a simple explanation for the critical t
cool/t
ff ratio. This paper explores a heuristic model for condensation linking the critical ratio to turbulent driving of gravity wave oscillations. In the linear regime, internal gravity waves are thermally unstable in a thermally balanced medium. Buoyancy oscillations in a balanced medium with t
cool/t
ff ≫ 1 therefore grow until they saturate without condensing at an amplitude depending on t
cool/t
ff. However, in a medium with 10 ≲ t
cool/t
ff ≲ 20, turbulence with a velocity dispersion roughly half the galaxy’s stellar velocity dispersion can drive those oscillations into condensation. Intriguingly, this is indeed the gas-phase velocity dispersion observed among multiphase galaxy cluster cores. It is therefore possible that both the critical t
cool/t
ff ratio for condensation of ambient gas and the level of turbulence in that gas are determined by coupling between condensation, feedback, and turbulence. Such a system can converge to a well-regulated equilibrium state, if the fraction of feedback energy going into turbulence is subdominant.
ALMA Polarimetry of Sgr A*: Probing the Accretion Flow from the Event Horizon to the Bondi Radius
Authors: Bower Geoffrey C. , Broderick Avery , Dexter Jason , Doeleman Shepherd , Falcke Heino , Fish Vincent , Johnson Michael D. , Marrone Daniel P. , Moran James M. , Moscibrodzka Monika , Peck Alison , Plambeck Richard L. , Rao Ramprasad 
Published: November 2018

Abstract
Millimeter polarimetry of Sgr A* probes the linearly polarized emission region on a scale of ∼10 Schwarzschild radii (R

S
), as well as the dense, magnetized accretion flow on scales out to the Bondi radius (∼105
R

S
) through Faraday rotation. We present here multi-epoch ALMA Band 6 (230 GHz) polarimetry of Sgr A*. The results confirm a mean rotation measure,

, consistent with measurements over the past 20 yr, and support an interpretation of the RM as originating from a radiatively inefficient accretion flow with

. Variability is observed for the first time in the RM on timescales that range from hours to months. The long-term variations may be the result of changes in the line-of-sight properties in a turbulent accretion flow. Short-term variations in the apparent RM are not necessarily the result of Faraday rotation and may be the result of complex emission and propagatation effects close to the black hole, some of which have been predicted in numerical modeling. We also confirm the detection of circular polarization at a mean value of −1.1% ± 0.2%. It is variable in amplitude on timescales from hours to months, but the handedness remains unchanged from that observed in past centimeter- and millimeter-wavelength detections. These results provide critical constraints for the analysis and interpretation of Event Horizon Telescope data of Sgr A*, M87, and similar sources.
Three-dimensional Simulation of Double Detonations in the Double-degenerate Model for Type Ia Supernovae and Interaction of Ejecta with a Surviving White Dwarf Companion
Authors: Tanikawa Ataru , Nomoto Ken’ichi , Nakasato Naohito 
Published: November 2018

Abstract
We study the hydrodynamics and nucleosynthesis in the double-detonation model of Type Ia supernovae (SNe Ia) and the interaction between the ejecta and a surviving white dwarf (WD) companion in the double-degenerate scenario. We set up a binary star system with 1.0 and 0.6 M
⊙ carbon–oxygen (CO) WDs, where the primary WD consists of a CO core and helium (He) shell with 0.95 and 0.05 M
⊙, respectively. We follow the evolution of the binary star system from the initiation of an He detonation, ignition and propagation of a CO detonation, and the interaction of SN ejecta with the companion WD. The companion (or surviving) WD gets a flung-away velocity of ∼1700 km s−1 and captures 56Ni of ∼0.03 M
⊙ and He of

. Such He can be detected on the surface of surviving WDs. The SN ejecta contains a “companion-origin stream” and unburned materials stripped from the companion WD (

), although the stream compositions would depend on the He shell mass of the companion WD. The ejecta has also a velocity shift of ∼1000 km s−1 due to the binary motion of the exploding primary WD. These features would be prominent in nebular-phase spectra of oxygen emission lines from the unburned materials like SN 2010lp and iPTF14atg and of blue- or redshifted Fe-group emission lines from the velocity shift like a part of subluminous SNe Ia. We expect that SN Ia counterparts to the D6 model would leave these fingerprints for SN Ia observations.
Tidally Induced Bars in Gas-rich Dwarf Galaxies Orbiting the Milky Way
Authors: Gajda Grzegorz , Łokas Ewa L. , Athanassoula E. 
Published: November 2018

Abstract
Bars in galaxies may form not only through instability but also as a result of an interaction with another galaxy. In particular, they may appear in disky dwarf galaxies interacting with Milky Way–like galaxies. Here we report the results of Nbody/SPH simulations of such dwarfs orbiting in the static potential of a larger galaxy. We used several models of the dwarf galaxy, all of the same mass but covering a large range of gas fractions: 0%, 30%, and 70%. We also tested the impact of subgrid star formation processes. In all cases, bars of similar length formed in the stellar disk of the dwarfs at the first pericenter passage. However, unexpectedly, the gaseous component remained approximately axisymmetric and unaffected by the bar potential. The bar properties did not change significantly between two consecutive pericenters. The impact of the later encounters with the host depends strongly on the exact orientation of the bar at the pericenter. When the bar is spun up by the tidal force torque, it is also shortened. Conversely, if it is slowed down, it gets longer. In the models with a low gas fraction, the bars were more pronounced and survived until the end of the simulations, while in the dwarfs with a high gas fraction, the bars were destroyed after the second or third pericenter passage. In terms of the ratio of the corotation radius to the bar length, the bars are slow, and remain so independently of the encounters with the host.
An FMOS Survey of Moderate-luminosity, Broad-line AGNs in COSMOS, SXDS, and E-CDF-S
Authors: Schulze Andreas , Silverman John D. , Kashino Daichi , Akiyama Masayuki , Schramm Malte , Sanders Dave , Kartaltepe Jeyhan , Daddi Emanuele , Rodighiero Giulia , Renzini Alvio , Arimoto Nobuo , Nagao Tohru , Puglisi Annagrazia , Trakhtenbrot Benny , Civano Francesca , Suh Hyewon 
Published: November 2018

Abstract
We present near-IR spectroscopy in the J- and H-bands for a large sample of 243 X-ray-selected, moderate-luminosity Type 1 active galactic nuclei (AGNs) in the COSMOS, SXDS, and E-CDF-S survey fields using the multi-object spectrograph Subaru/FMOS. Our sample covers the redshift range 0.5 ≲ z ≲ 3.0 and X-ray luminosity range of 1043 ≲

≲ 1045 erg s−1. We provide emission-line properties and derived virial black hole mass estimates, bolometric luminosities, and Eddington ratios, based on Hα (211), Hβ (63), and Mg ii (4). We compare line widths, luminosities, and black hole mass estimates from Hα and Hβ, and augment these with commensurate measurements of Mg ii and C iv detected in optical spectra. We demonstrate the robustness of using Hα, Hβ, and Mg ii as reliable black hole mass estimators for high-z moderate-luminosity AGNs, while the use of C iv is prone to large uncertainties (≳0.4 dex). We extend a recently proposed correction based on the C iv blueshift to lower luminosities and black hole masses. While our sample shows an improvement in their C iv black hole mass estimates, the deficit of high blueshift sources reduces its overall importance for moderate-luminosity AGNs compared to the most luminous quasars. In addition, we revisit luminosity correlations between L
bol,

, L
[O iii], L
5100, and L
Hα
and find them to be consistent with a simple empirical model, based on a small number of well-established scaling relations. Finally, we highlight our highest redshift AGN, CID 781, at z = 4.6, which has the lowest black hole mass (∼108
M
⊙) among current near-IR samples at this redshift and is in a state of fast growth.