Pulsar timing irregularities and the imprint of magnetic field evolution

Context. The rotational evolution of isolated neutron stars is dominated by the magnetic field anchored to the solid crust of the star. Assuming that the core field evolves on much longer timescales, the crustal field evolves mainly though Ohmic dissipation and the Hall drift, and it may be subject to relatively rapid changes with remarkable effects on the observed timing properties. Aims. We investigate whether changes of the magnetic field structure and strength during the star evolution may have observable consequences in the braking index n. This is the most sensitive quantity to reflect small variations of the timing properties that are caused by magnetic field rearrangements. Methods. We performed axisymmetric, long-term simulations of the magneto-thermal evolution of neutron stars with state-of-the-art microphysical inputs to calculate the evolution of the braking index. Relatively rapid magnetic field modifications can be expected only in the crust of neutron stars, where we focus our study. Results. We find that the effect of the magnetic field evolution on the braking index can be divided into three qualitatively different stages depending on the age and the internal temperature: a first stage that may be different for standard pulsars (with n ~ 3) or low field neutron stars that accreted fallback matter during the supernova explosion (systematically n < 3); in a second stage, the evolution is governed by almost pure Ohmic field decay, and a braking index n > 3 is expected; in the third stage, at late times, when the interior temperature has dropped to very low values, Hall oscillatory modes in the neutron star crust result in braking indices of a high absolute value and both positive and negative signs. Conclusions. Current magneto-thermal evolution models predict a large contribution to the timing noise and, in particular, to the braking index, from temporal variations of the magnetic field. Models with strong (≳ 1014 G) multipolar or toroidal components, even with a weak (~1012 G) dipolar field are consistent with the observed trend of the timing properties.

A new code for the Hall-driven magnetic evolution of neutron stars

Over the past decade, the numerical modeling of the magnetic field evolution in astrophysical scenarios has become an increasingly important field. In the crystallized crust of neutron stars the evolution of the magnetic field is governed by the Hall induction equation. In this equation the relative contribution of the two terms (Hall term and Ohmic dissipation) varies depending on the local conditions of temperature and magnetic field strength. This results in the transition from the purely parabolic character of the equations to the hyperbolic regime as the magnetic Reynolds number increases, which presents severe numerical problems. Up to now, most attempts to study this problem were based on spectral methods, but they failed in representing the transition to large magnetic Reynolds numbers. We present a new code based on upwind finite differences techniques that can handle situations with arbitrary low magnetic diffusivity and it is suitable for studying the formation of sharp current sheets during the evolution. The code is thoroughly tested in different limits and used to illustrate the evolution of the crustal magnetic field in a neutron star in some representative cases. Our code, coupled to cooling codes, can be used to perform long-term simulations of the magneto-thermal evolution of neutron stars.

The imprint of the crustal magnetic field on the thermal spectra and pulse profiles of isolated neutron stars

Isolated neutron stars (NSs) show a bewildering variety of astrophysical manifestations, presumably shaped by the magnetic field strength and topology at birth. Here, using state-of-the-art calculations of the coupled magnetic and thermal evolution of NSs, we compute the thermal spectra and pulse profiles expected for a variety of initial magnetic field configurations. In particular, we contrast models with purely poloidal magnetic fields to models dominated by a strong internal toroidal component. We find that, while the former displays double-peaked profiles and very low pulsed fractions, in the latter, the anisotropy in the surface temperature produced by the toroidal field often results in a single pulse profile, with pulsed fractions that can exceed the 50–60 per cent level even for perfectly isotropic local emission. We further use our theoretical results to generate simulated ‘observed’ spectra, and show that blackbody (BB) fits result in inferred radii that can be significantly smaller than the actual NS radius, even as low as ∼1–2 km for old NSs with strong internal toroidal fields and a high absorption column density along their line of sight. We compute the size of the inferred BB radius for a few representative magnetic field configurations, NS ages and magnitudes of the column density. Our theoretical results are of direct relevance to the interpretation of X-ray observations of isolated NSs, as well as to the constraints on the equation of state of dense matter through radius measurements.

Population synthesis of isolated neutron stars with magneto-rotational evolution

We revisit the population synthesis of isolated radio-pulsars incorporating recent advances on the evolution of the magnetic field and the angle between the magnetic and rotational axes from new simulations of the magneto-thermal evolution and magnetosphere models, respectively. An interesting novelty in our approach is that we do not assume the existence of a death line. We discuss regions in parameter space that are more consistent with the observational data. In particular, we find that any broad distribution of birth spin periods with P0 ≲ 0.5 s can fit the data, and that if the alignment angle is allowed to vary consistently with the torque model, realistic magnetospheric models are favoured compared to models with classical magneto-dipolar radiation losses. Assuming that the initial magnetic field is given by a lognormal distribution, our optimal model has mean strength 〈log B0[G]〉 ≈ 13.0–13.2 with width σ(log B0) = 0.6–0.7. However, there are strong correlations between parameters. This degeneracy in the parameter space can be broken by an independent estimate of the pulsar birth rate or by future studies correlating this information with the population in other observational bands (X-rays and γ-rays).

Quiescent thermal emission from neutron stars in low-mass X-ray binaries

Context. We monitored the quiescent thermal emission from neutron stars in low-mass X-ray binaries after active periods of intense activity in X-rays (outbursts). Aims. The theoretical modeling of the thermal relaxation of the neutron star crust may be used to establish constraints on the crust composition and transport properties, depending on the astrophysical scenarios assumed. Methods. We numerically simulated the thermal evolution of the neutron star crust and compared them with inferred surface temperatures for five sources: MXB 1659−29, KS 1731−260, XTE J1701−462, EXO 0748−676  and IGR J17480−2446. Results. We find that the evolution of MXB 1659−29, KS 1731−260 and EXO 0748−676 can be well described within a deep crustal cooling scenario. Conversely, we find that the other two sources can only be explained with models beyond crustal cooling. For the peculiar emission of XTE J1701−462 we propose alternative scenarios such as residual accretion during quiescence, additional heat sources in the outer crust, and/or thermal isolation of the inner crust due to a buried magnetic field. We also explain the very recent reported temperature of IGR J17480−2446 with an additional heat deposition in the outer crust from shallow sources.

Population synthesis of isolated neutron stars with magneto-rotational evolution – II. From radio-pulsars to magnetars

Population synthesis studies constitute a powerful method to reconstruct the birth distribution of periods and magnetic fields of the pulsar population. When this method is applied to populations in different wavelengths, it can break the degeneracy in the inferred properties of initial distributions that arises from single-band studies. In this context, we extend previous works to include X-ray thermal emitting pulsars within the same evolutionary model as radio-pulsars. We find that the cumulative distribution of the number of X-ray pulsars can be well reproduced by several models that, simultaneously, reproduce the characteristics of the radio-pulsar distribution. However, even considering the most favourable magneto-thermal evolution models with fast field decay, lognormal distributions of the initial magnetic field overpredict the number of visible sources with periods longer than 12 s. We then show that the problem can be solved with different distributions of magnetic field, such as a truncated lognormal distribution, or a binormal distribution with two distinct populations. We use the observational lack of isolated neutron stars (NSs) with spin periods P > 12 s to establish an upper limit to the fraction of magnetars born with B > 1015 G (less than 1 per cent). As future detections keep increasing the magnetar and high-B pulsar statistics, our approach can be used to establish a severe constraint on the maximum magnetic field at birth of NSs.

The isolated neutron star candidate 2XMM J104608.7-594306

Over the last decade, X-ray observations have revealed the existence of several classes of isolated neutron stars (INSs) which are radio-quiet or exhibit radio emission with properties much at variance with those of ordinary radio pulsars. The identification of new sources is crucial in order to understand the relations among the different classes and to compare observational constraints with theoretical expectations. A recent analysis of the 2XMMp catalogue provided fewer than 30 new thermally emitting INS candidates. Among these, the source 2XMM J104608.7-594306 appears particularly interesting because of the softness of its X-ray spectrum, kT = 117 +/- 14 eV and N(H) = (3.5 +/- 1.1) x 10(21) cm(-2) (3 sigma), and of the present upper limits in the optical, m(B) greater than or similar to 26, m(V) greater than or similar to 25.5 and m(R) greater than or similar to 25 (98.76% confidence level), which imply a logarithmic X-ray-to-optical flux ratio log(F(X)/F(V)) greater than or similar to 3.1, corrected for absorption. We present the X-ray and optical properties of 2XMM J104608.7-594306 and discuss its nature in the light of two possible scenarios invoked to explain the X-ray thermal emission from INSs: the release of residual heat in a cooling neutron star, as in the seven radio-quiet ROSAT-discovered INSs, and accretion from the interstellar medium. We find that the present observational picture of 2XMM J104608.7-594306 is consistent with a distant cooling INS with properties in agreement with the most up-to-date expectations of population synthesis models: it is fainter, hotter and more absorbed than the seven ROSAT sources and possibly located in the Carina Nebula, a region likely to harbour unidentified cooling neutron stars. The accretion scenario, although not entirely ruled out by observations, would require a very slow (similar to 10 km s(-1)) INS accreting at the Bondi-Hoyle rate.

Metamorphism and kinetics in the Torres del Paine contact aureole

Contact aureoles provide an excellent geologic environment to study the mechanisms of metamorphic reactions in a natural system. The Torres del Paine (TP) intrusion is one of the most spectacular natural laboratories because of its excellent outcrop conditions. It formed in a period from 12.59 to 12.43 Ma and consists of three large granite and four smaller mafic batches. The oldest granite is on top, the youngest at the bottom of the granitic complex, and the granites overly the mafic laccolith. The TP intruded at a depth of 2-3 km into regional metamorphic anchizone to greenschist facies pelites, sandstones, and conglomerates of the Cerro Toro and Punta Barrosa formations. It formed a thin contact aureole of 150-400 m width. This thesis focuses on the reaction kinetics of the mineral cordierite in the contact aureole using quantitative textural analysis methods. First cordierite was formed from chlorite break¬down (zone I, ca. 480 °C, 750 bar). The second cordierite forming reaction was the muscovite break-down, which is accompanied by a modal decrease in biotite and the appearance of k- feldspar (zone II, 540-550 °C, 750 bar). Crystal sizes of the roundish, poikiloblastic cordierites were determined from microscope thin section images by manually marking each crystal. Images were then automatically processed with Matlab. The correction for the intersection probability of each crystal radius yields the crystal size distribution in the rock. Samples from zone I below the laccolith have the largest crystals (0.09 mm). Cordierites from zone II are smaller, with a maximum crystal radius of 0.057 mm. Rocks from zone II have a larger number of small cordierite crystals than rocks from zone I. A combination of these quantitative analysis with numerical modeling of nucleation and growth, is used to infer nucleation and growth parameters which are responsible for the observed mineral textures. For this, the temperature-time paths of the samples need to be known. The thermal history is complex because the main body of the intrusion was formed by several intrusive batches. The emplacement mechanism and duration of each batch can influence the thermal structure in the aureole. A possible subdivision of batches in smaller increments, so called pulses, will focus heat at the side of the intrusion. Focusing all pulses on one side increases the contact aureole size on that side, but decreases it on the other side. It forms a strongly asymmetric contact aureole. Detailed modeling shows that the relative thicknesses of the TP contact aureole above and below the intrusion (150 and 400 m) are best explained by a rapid emplacement of at least the oldest granite batch. Nevertheless, temperatures are significantly too low in all models, compared to observed mineral assemblages in the hornfelses. Hence, an other important thermal mechanisms needs to take place in the host rock. Clastic minerals in the immature sediments outside the contact aureole are hydrated due to small amounts of expelled fluids during contact metamorphism. This leads to a temperature increase of up to 50 °C. The origin of fluids can be traced by stable isotopes. Whole rock stable isotope data (6D and δ180) and chlorine concentrations in biotite document that the TP intrusion induced only very small amounts of fluid flow. Oxygen whole rock data show δ180 values between 9.0 and 10.0 %o within the first 5 m of the contact. Values increase to 13.0 - 15.0 %o further away from the intrusion. Whole rock 6D values display a more complex zoning. First, host rock values (-90 to -70 %o) smoothly decrease towards the contact by ca. 20 %o, up to a distance of ca. 150 m. This is followed by an increase of ca. 20 %o within the innermost 150 m of the aureole (-97.0 to -78 %o at the contact). The initial decrease in 6D values is interpreted to be due to Rayleigh fractionation accompanying the dehydration reactions forming cordierite, while the final increase reflects infiltration of water-rich fluids from the intrusion. An over-estimate on the quantity and the corresponding thermal effect yields a temperature increase of less than 30 °C. This suggests that fluid flow might have contributed only for a small amount to the thermal evolution of the system. A combination of the numerical growth model with the thermal model, including the hydration reaction enthalpies but neglecting fluid flow and incremental growth, can be used to numerically reproduce the observed cordierite textures in the contact aureole. This yields kinetic parameters which indicate fast cordierite crystallization before the thermal peak in the inner aureole, and continued reaction after the thermal peak in the outermost aureole. Only small temperature dependencies of the kinetic parameters seem to be needed to explain the obtained crystal size data. - Les auréoles de contact offrent un cadre géologique privilégié pour l'étude des mécanismes de réactions métamorphiques associés à la mise en place de magmas dans la croûte terrestre. Par ses conditions d'affleurements excellentes, l'intrusion de Torres del Paine représente un site exceptionnel pour améliorer nos connaissances de ces processus. La formation de cette intrusion composée de trois injections granitiques principales et de quatre injections mafiques de volume inférieur couvre une période allant de 12.50 à 12.43 Ma. Le plus vieux granite forme la partie sommitale de l'intrusion alors que l'injection la plus jeune s'observe à la base du complexe granitique; les granites recouvrent la partie mafique du laccolite. L'intrusion du Torres del Paine s'est mise en place a 2-3 km de profondeur dans un encaissant métamorphique. Cet encaissant est caractérisé par un métamorphisme régional de faciès anchizonal à schiste vert et est composé de pélites, de grès, et des conglomérats des formations du Cerro Toro et Punta Barrosa. La mise en place des différentes injections granitiques a généré une auréole de contact de 150-400 m d'épaisseur autour de l'intrusion. Cette thèse se concentre sur la cinétique de réaction associée à la formation de la cordiérite dans les auréoles de contact en utilisant des méthodes quantitatives d'analyses de texture. On observe plusieurs générations de cordiérite dans l'auréole de contact. La première cordiérite est formée par la décomposition de la chlorite (zone I, environ 480 °C, 750 bar), alors qu'une seconde génération de cordiérite est associée à la décomposition de la muscovite, laquelle est accompagnée par une diminution modale de la teneur en biotite et l'apparition de feldspath potassique (zone II, 540-550 °C, 750 bar). Les tailles des cristaux de cordiérites arrondies et blastic ont été déterminées en utilisant des images digitalisées des lames minces et en marquant individuellement chaque cristal. Les images sont ensuite traitées automatiquement à l'aide du programme Matlab. La correction de la probabilité d'intersection en fonction du rayon des cristaux permet de déterminer la distribution de la taille des cristaux dans la roche. Les échantillons de la zone I, en dessous du lacolite, sont caractérisés par de relativement grands cristaux (0.09 mm). Les cristaux de cordiérite de la zone II sont plus petits, avec un rayon maximal de 0.057 mm. Les roches de la zone II présentent un plus grand nombre de petits cristaux de cordiérite que les roches de la zone I. Une combinaison de ces analyses quantitatives avec un modèle numérique de nucléation et croissance a été utilisée pour déduire les paramètres de nucléation et croissance contrôlant les différentes textures minérales observées. Pour développer le modèle de nucléation et de croissance, il est nécessaire de connaître le chemin température - temps des échantillons. L'histoire thermique est complexe parce que l'intrusion est produite par plusieurs injections successives. En effet, le mécanisme d'emplace¬ment et la durée de chaque injection peuvent influencer la structure thermique dans l'auréole. Une subdivision des injections en plus petits incréments, appelés puises, permet de concentrer la chaleur dans les bords de l'intrusion. Une mise en place préférentielle de ces puises sur un côté de l'intrusion modifie l'apport thermique et influence la taille de l'auréole de contact produite, auréole qui devient asymétrique. Dans le cas de la première injection de granite, une modélisation détaillée montre que l'épaisseur relative de l'auréole de contact de Torres del Paine au-dessus et en dessous de l'intrusion (150 et 400 m) est mieux expliquée par un emplacement rapide du granite. Néanmoins, les températures calculées dans l'auréole de con¬tact sont trop basses pour que les modèles thermiques soient cohérants par rapport à la taille de cette auréole. Ainsi, un autre mecanisme exothermique est nécessaire pour permettre à la roche encais¬sante de produire les assemblages observés. L'observation des roches encaissantes entourant les granites montre que les minéraux clastiques dans les sédiments immatures au-dehors de l'auréole sont hydratés suite à la petite quantité de fluide expulsée durant le métamorphisme de contact et/ou la mise en place des granites. Les réactions d'hydratation peuvent permettre une augmentation de la température jusqu'à 50 °C. Afin de déterminer l'origine des fluides, une étude isotopique de roches de l'auréole de contact a été entreprise. Les isotopes stables d'oxygène et d'hydrogène sur la roche totale ainsi que la concentration en chlore dans la biotite indiquent que la mise en place des granites du Torres del Paine n'induit qu'une circulation de fluide limitée. Les données d'oxygène sur roche totale montrent des valeurs δ180 entre 9.0 et 10.0%o au sein des cinq premiers mètres du contact. Les valeurs augmentent jusqu'à 13.0 - 15.0 plus on s'éloigne de l'intrusion. Les valeurs 5D sur roche totale montrent une zonation plus complexe. Les valeurs de la roche encaissante (-90 à -70%o) diminuent progressivement d'environ 20%o depuis l'extérieur de l'auréole jusqu'à une distance d'environ 150 m du granite. Cette diminution est suivie par une augmentation d'environ 20%o au sein des 150 mètres les plus proches du contact (-97.0 à -78%o au contact). La diminution initiale des valeurs de 6D est interprétée comme la conséquence du fractionnement de Rayleigh qui accompagne les réactions de déshydratation formant la cordiérite, alors que l'augmentation finale reflète l'infiltration de fluide riche en eau venant de l'intrusion. A partir de ces résultats, le volume du fluide issu du granite ainsi que son effet thermique a pu être estimé. Ces résultats montrent que l'augmentation de température associée à ces fluides est limitée à un maximum de 30 °C. La contribution de ces fluides dans le bilan thermique est donc faible. Ces différents résultats nous ont permis de créer un modèle thermique associé à la for¬mation de l'auréole de contact qui intègre la mise en place rapide du granite et les réactions d'hydratation lors du métamorphisme. L'intégration de ce modèle thermique dans le modèle numérique de croissance minérale nous permet de calculer les textures des cordiérites. Cepen¬dant, ce modèle est dépendant de la vitesse de croissance et de nucléation de ces cordiérites. Nous avons obtenu ces paramètres en comparant les textures prédites par le modèle et les textures observées dans les roches de l'auréole de contact du Torres del Paine. Les paramètres cinétiques extraits du modèle optimisé indiquent une cristallisation rapide de la cordiérite avant le pic thermique dans la partie interne de l'auréole, et une réaction continue après le pic thermique dans la partie la plus externe de l'auréole. Seules de petites dépendances de température des paramètres de cinétique semblent être nécessaires pour expliquer les don¬nées obtenues sur la distribution des tailles de cristaux. Ces résultats apportent un éclairage nouveau sur la cinétique qui contrôle les réactions métamorphiques.

Structure et évolution thermique de la croûte supérieure des chaînes de subduction : approches thermologique et modélisation numérique, dans les North Cascades (U.S.A) et de la zone de faille Motagua (Guatemala)

Cette thèse cible l'étude de la structure thermique de la croûte supérieure (<10km) dans les arcs magmatiques continentaux, et son influence sur l'enregistrement thermochronologique de leur exhumation et de leur évolution topographique. Nous portons notre regard sur deux chaînes de montagne appartenant aux Cordillères Américaines : Les Cascades Nord (USA) et la zone de faille Motagua (Guatemala). L'approche utilisée est axée sur la thermochronologie (U-Th-Sm)/He sur apatite et zircon, couplée avec la modélisation numérique de la structure thermique de la croûte. Nous mettons en évidence la variabilité à la fois spatiale et temporelle du gradient géothermique, et attirons l'attention du lecteur sur l'importance de prendre en compte la multitude des processus géologiques perturbant la structure thermique dans les chaînes de type cordillère, c'est à dire formées lors de la subduction océanique sous un continent.Une nouvelle approche est ainsi développée pour étudier et contraindre la perturbation thermique autour des chambres magmatiques. Deux profiles âge-elevation (U-Th-Sm)/He sur apatite et zircon, ont été collectées 7 km au sud du batholithe de Chilliwack, Cascades Nord. Les résultats montrent une variabilité spatiale et temporelle du gradient géothermique lors de l'emplacement magmatique qui peut être contrainte et séparé de l'exhumation. Durant l'emplacement de l'intrusion, la perturbation thermique y atteint un état d'équilibre (-80-100 °C/km) qui est fonction du flux de magma et de ia distance à la source du magma, puis rejoint 40 °C/km à la fin du processus d'emplacement magmatique.Quelques nouvelles données (U-Th)/He, replacées dans une compilation des données existantes dans les Cascades Nord, indiquent une vitesse d'exhumation constante (-100 m/Ma) dans le temps et l'espace entre 35 Ma et 2 Ma, associée à un soulèvement uniforme de la chaîne contrôlé par l'emplacement de magma dans la croûte durant toute l'activité de l'arc. Par contre, après ~2 Ma, le versant humide de la chaîne est affecté par une accélération des taux d'exhumation, jusqu'à 3 km de croûte y sont érodés. Les glaciations ont un triple effet sur l'érosion de cette chaîne: (1) augmentation des vitesses d'érosion, d'exhumation et de soulèvement la où les précipitations sont suffisantes, (2) limitation de l'altitude contrôlé par la position de Γ Ε LA, (3) élargissement du versant humide et contraction du versant aride de la chaîne.Les modifications des réseaux de drainage sont des processus de surface souvent sous-estimés au profil d'événements climatiques ou tectoniques. Nous proposons une nouvelle approche couplant une analyse géomorphologique, des données thermochronologiques de basse température ((U-Th-Sm)/He sur apatite et zircon), et l'utilisation de modélisation numérique thermo-cinématique pour les mettre en évidence et les dater; nous testons cette approche sur la gorge de la Skagit river dans les North Cascades.De nouvelles données (U-Th)/He sur zircons, complétant les données existantes, montrent que le déplacement horizontal le long de la faille transformante continentale Motagua, la limite des plaques Caraïbe/Amérique du Nord, a juxtaposé un bloc froid, le bloc Maya (s.s.), contre un bloque chaud, le bloc Chortis (s.s.) originellement en position d'arc. En plus de donner des gammes d'âges thermochronologiques très différents des deux côtés de la faille, le déplacement horizontal rapide (~2 cm/a) a produit un fort échange thermique latéral, résultant en un réchauffement du côté froid et un refroidissement du côté chaud de la zone de faille de Motagua.Enfin des données (U-Th-Sm)/He sur apatite témoignent d'un refroidissement Oligocène enregistré uniquement dans la croûte supérieure de la bordure nord de la zone de faille Motagua. Nous tenterons ultérieurement de reproduire ce découplage vertical de la structure thermique par la modélisation de la formation d'un bassin transtensif et de circulation de fluides le long de la faille de Motagua. - This thesis focuses on the influence of the dynamic thermal structure of the upper crust (<10km) on the thermochronologic record of the exhumational and topographic history of magmatic continental arcs. Two mountain belts from the American Cordillera are studied: the North Cascades (USA) and the Motagua fault zone (Guatemala). I use a combined approach coupling apatite and zircon (U-Th-Sm}/He thermochronology and thermo- kinematic numerical modelling. This study highlights the temporal and spatial variability of the geothermal gradient and the importance to take into account the different geological processes that perturb the thermal structure of Cordilleran-type mountain belts (i.e. mountain belts related to oceanic subduction underneath a continent}.We integrate apatite and zircon (U-Th)/He data with numerical thermo-kinematic models to study the relative effects of magmatic and surface processes on the thermal evolution of the crust and cooling patterns in the Cenozoic North Cascades arc (Washington State, USA). Two age-elevation profiles that are located 7 km south of the well-studied Chiliiwack intrusions shows that spatial and temporal variability in geothermal gradients linked to magma emplacement can be contrained and separated from exhumation processes. During Chiliiwack batholith emplacement at -35-20 Ma, the geothermal gradient of the country rocks increased to a very high steady-state value (80-100°C/km), which is likely a function of magma flux and the distance from the magma source area. Including temporally varying geothermal gradients in the analysis allows quantifying the thermal perturbation around magmatic intrusions and retrieving a relatively simple denudation history from the data.The synthesis of new and previously published (U-Th)/He data reveals that denudation of the Northern Cascades is spatially and temporally constant at -100 m/Ma between ~32 and ~2 Ma, which likely reflects uplift due to magmatic crustal thickening since the initiation of the Cenozoic stage of the continental magmatic arc. In contrast, the humid flank of the North Cascades is affected by a ten-fold acceleration in exhumation rate at ~2 Ma, which we interpret as forced by the initiation of glaciations; around 3 km of crust have been eroded since that time. Glaciations have three distinct effects on the dynamics of this mountain range: (1) they increase erosion, exhumation and uplift rates where precipitation rates are sufficient to drive efficient glacial erosion; (2) they efficiently limit the elevation of the range; (3) they lead to widening of the humid flank and contraction of the arid flank of the belt.Drainage reorganizations constitute an important agent of landscape evolution that is often underestimated to the benefit of tectonic or climatic events. We propose a new method that integrates geomorphology, low-temperature thermochronometry (apatite and zircon {U-Th-Sm)/He), and 3D numerical thermal-kinematic modelling to detect and date drainage instability producing recent gorge incision, and apply this approach to the Skagit River Gorge, North Cascades.Two zircon (U-Th)/He age-elevation profiles sampled on both sides of the Motagua Fault Zone (MFZ), the boundary between the North American and the Caribbean plates, combined with published thermochronological data show that strike-slip displacement has juxtaposed the cold Maya block (s.s.) against the hot, arc derived, Chortis block (s.s ), producing different age patterns on both sides of the fault and short-wavelength lateral thermal exchange, resulting in recent heating of the cool side and cooling of the hot side of the MFZ.Finally, an apatite (U-Th-Sm)/He age-elevation profile records rapid cooling at -35 Ma localized only in the upper crust along the northern side of the Motagua fault zone. We will try to reproduce these data by modeling the thermal perturbation resulting from the formation of a transtensional basin and of fluid flow activity along a crustal- scale strike-slip fault.

White luminescence from Si+ and C+ ion-implanted SiO2 films

The microstructural and optical analysis of SiO2 layers emitting white luminescence is reported. These structures have been synthesized by sequential Si+ and C+ ion implantation and high-temperature annealing. Their white emission results from the presence of up to three bands in the photoluminescence (PL) spectra, covering the whole visible spectral range. The microstructural characterization reveals the presence of a complex multilayer structure: Si nanocrystals are only observed outside the main C-implanted peak region, with a lower density closer to the surface, being also smaller in size. This lack of uniformity in their density has been related to the inhibiting role of C in their growth dynamics. These nanocrystals are responsible for the band appearing in the red region of the PL spectrum. The analysis of the thermal evolution of the red PL band and its behavior after hydrogenation shows that carbon implantation also prevents the formation of well passivated Si/SiO2 interfaces. On the other hand, the PL bands appearing at higher energies show the existence of two different characteristics as a function of the implanted dose. For excess atomic concentrations below or equal to 10%, the spectra show a PL band in the blue region. At higher doses, two bands dominate the green¿blue spectral region. The evolution of these bands with the implanted dose and annealing time suggests that they are related to the formation of carbon-rich precipitates in the implanted region. Moreover, PL versus depth measurements provide a direct correlation of the green band with the carbon-implanted profile. These PL bands have been assigned to two distinct amorphous phases, with a composition close to elemental graphitic carbon or stoichiometric SiC.

Trace element chemistry and U-Pb dating of zircons from oceanic gabbros and their relationship with whole rock composition (Lanzo, Italian Alps)

The U-Pb ages and the trace element content of zircon U-Pb along with major and trace element whole rock data on gabbroic dikes from the Lanzo lherzolitic massif, N-Italy, have been determined to constrain crustal accretion in ocean-continent transition zones. Three Fe-Ti gabbros were dated from the central and the southern part of the massif providing middle Jurassic ages of 161 +/- 2, 158 +/- 2 and 163 +/- 1 Ma, which argue for magmatic activity over few millions of years. Zircon crystals are characterized by high but variable Th/U ratios, rare earth element patterns enriched in heavy rare earths, pronounced positive Ce and negative Eu-anomalies consistent with crystallization after substantial plagioclase fractionation. The zircon trace element composition coupled with whole rock chemistry was used to reconstruct the crystallization history of the gabbros. A number of gabbros crystallized in situ, and zircon precipitated from trapped, intercumulus liquid, while other gabbros represent residual liquids that were extracted from a cumulus pile and crystallized along syn-magmatic shear zones. We propose a model in which the emplacement mechanism of gabbroic rocks in ocean-continent transition zones evolves from in situ crystallization to stratified crystallization with efficient extraction of residual liquid along syn-magmatic shear zones. Such an evolution of the crystallization history is probably related to the thermal evolution of the underlying mantle lithosphere.

Caracterización y clasificación geoquímica de asfaltitas cubanas

Traditional biomarker parameters and aromatic compounds were applied to characterize and classify ten Cuban asphaltites (asphaltene-rich petroleum occurring as seeps or filling veins, joints, cavities and fissures). Genetic molecular parameters were compared in order to establish oil-oil correlations between samples. Thermal evolution was investigated using saturated biomarker and aromatic maturity parameters. All samples seem to represent petroleum in the early catagenetic stage. Statistical procedures used as auxiliary techniques show that they represent oils of Family II (marine anoxic carbonate sourced oils), except for 2 samples interpreted as belonging to Family III oils (normal marine siliciclastic suboxic sourced oils).

The influence of viscous and latent heating on crystal-rich magma flow in a conduit

The flow dynamics of crystal-rich high-viscosity magma is likely to be strongly influenced by viscous and latent heat release. Viscous heating is observed to play an important role in the dynamics of fluids with temperature-dependent viscosities. The growth of microlite crystals and the accompanying release of latent heat should play a similar role in raising fluid temperatures. Earlier models of viscous heating in magmas have shown the potential for unstable (thermal runaway) flow as described by a Gruntfest number, using an Arrhenius temperature dependence for the viscosity, but have not considered crystal growth or latent heating. We present a theoretical model for magma flow in an axisymmetric conduit and consider both heating effects using Finite Element Method techniques. We consider a constant mass flux in a 1-D infinitesimal conduit segment with isothermal and adiabatic boundary conditions and Newtonian and non-Newtonian magma flow properties. We find that the growth of crystals acts to stabilize the flow field and make the magma less likely to experience a thermal runaway. The additional heating influences crystal growth and can counteract supercooling from degassing-induced crystallization and drive the residual melt composition back towards the liquidus temperature. We illustrate the models with results generated using parameters appropriate for the andesite lava dome-forming eruption at Soufriere Hills Volcano, Montserrat. These results emphasize the radial variability of the magma. Both viscous and latent heating effects are shown to be capable of playing a significant role in the eruption dynamics of Soufriere Hills Volcano. Latent heating is a factor in the top two kilometres of the conduit and may be responsible for relatively short-term (days) transients. Viscous heating is less restricted spatially, but because thermal runaway requires periods of hundreds of days to be achieved, the process is likely to be interrupted. Our models show that thermal evolution of the conduit walls could lead to an increase in the effective diameter of flow and an increase in flux at constant magma pressure.

The long-term stability of a possible aqueous ammonium sulfate ocean inside Titan

We model the thermal evolution of a subsurface ocean of aqueous ammonium sulfate inside Titan using a parameterized convection scheme. The cooling and crystallization of such an ocean depends on its heat flux balance, and is governed by the pressure-dependent melting temperatures at the top and bottom of the ocean. Using recent observations and previous experimental data, we present a nominal model which predicts the thickness of the ocean throughout the evolution of Titan; after 4.5 Ga we expect an aqueous ammonium sulfate ocean 56 km thick, overlain by a thick (176 km) heterogeneous crust of methane clathrate, ice I and ammonium sulfate. Underplating of the crust by ice I will give rise to compositional diapirs that are capable of rising through the crust and providing a mechanism for cryovolcanism at the surface. We have conducted a parameter space survey to account for possible variations in the nominal model, and find that for a wide range of plausible conditions, an ocean of aqueous ammonium sulfate can survive to the present day, which is consistent with the recent observations of Titan's spin state from Cassini radar data [Lorenz, R.D., Stiles, B.W., Kirk, R.L., Allison, M.D., del Marmo, P.P., Iess, L., Lunine, J.I., Ostro, S.J., Hensley, S., 2008. Science 319, 1649–1651].

Emulation of chiral hydrogenation catalysts by adsorbtion of small molecules onto Ni surfaces

Adsorption of small molecules on the Ni{111} and NiO{111} surfaces is investigated under UHV and elevated pressures (~10-1 mbar) of hydrogen and water. The molecules considered are chosen for their relevance to understanding the mechanism of enantioselective hydrogenation on Raney Nickel modified by chiral molecules. Adsorption of water onto, and its subsequent reaction with, oxygen-covered Ni{111} is dependent on the initial atomic oxygen coverage. An OH species (O1s binding energy 531.5eV), oriented perpendicular to the surface, forms at atomic oxygen coverages <0.25ML. The reaction does not consume all the adsorbed oxygen for coverages ≥0.12ML. The p(2×2) atomic oxygen uperstructure is unreactive, while an OH species is formed on the p(√3×√3) superstructure at binding energy 530.9eV. L-alanine is adsorbed on Ni{111} as a model chiral modifier molecule. At low coverages, alanine forms a presumed tridentate alaninate species for coverages ≥0.11ML at 250K. A minority, bidentate zwitterionic species forms at coverages >0.11ML, but was not observed at 300K. Saturation occurs at 0.25ML. At high alanine coverages (≥0.19ML) and H2 pressure (≥1×10-2 mbar), the tridentate L-alaninate converts to bidentate zwitterionic L-alanine at 300K. Thermal evolution of L-alanine on Ni{111} under varying hydrogen pressures is examined. Adsorption of L-alanine onto hydroxylated NiO{111} at 300K in UHV, mimicking a catalyst surface under aqueous conditions, yields the tridentate alaninate which is immune to the effects of elevated hydrogen pressure. Exposing the L-alanine/Ni{111} adsorption system to water (≤10-1 mbar) oxidises the surface and recreates the L-alanine/hydroxylated NiO{111} system. Pyruvic acid on Ni{111} is examined as a model for hydrogenation substrate adsorption. Behaviour is coverage dependent and several conformations are possible at low coverages (≤0.1ML). Annealing at coverages <0.2ML causes a condensation reaction, releasing water onto the surface. High coverages do not condense and a saturation coverage of ~0.35ML is found.