Low-temperature evolution of the Morondava rift basin shoulder in western Madagascar: An apatite fission track study

[1] The evolution of the rift shoulder and the sedimentary sequence of the Morondava basin in western Madagascar was mainly influenced by a Permo-Triassic continental failed rift (Karroo rift), and the early Jurassic separation of Madagascar from Africa. Karroo deposits are restricted to a narrow corridor along the basement-basin contact and parts of this contact feature a steep escarpment. Here, apatite fission track (AFT) analysis of a series of both basement and sediment samples across the escarpment reveals the low-temperature evolution of the exhuming Precambrian basement in the rift basin shoulder and the associated thermal evolution of the sedimentary succession. Seven basement and four Karroo sediment samples yield apparent AFT ages between ∼330 and ∼215 Ma and ∼260 and ∼95 Ma, respectively. Partially annealed fission tracks and thermal modeling indicate post-depositional thermal overprinting of both basement and Karroo sediment. Rocks presently exposed in the rift shoulder indicate temperatures of >60°C associated with this reheating whereby the westernmost sample in the sedimentary plain experienced almost complete resetting of the detrital apatite grains at temperatures of about ∼90–100°C. The younging of AFT ages westward indicates activity of faults, re-activating inherited Precambrian structures during Karroo sedimentation. Furthermore, our data suggest onset of final cooling/exhumation linked to (1) the end of Madagascar's drift southward relative to Africa during the Early Cretaceous, (2) activity of the Marion hot spot and associated Late Cretaceous break-up between Madagascar and India, and (3) the collision of India with Eurasia and subsequent re-organization of spreading systems in the Indian Ocean.

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.

Large igneous provinces and silicic large igneous provinces : progress in our understanding over the last 25 years

Large Igneous Provinces are exceptional intraplate igneous events throughout Earth’s history. Their significance and potential global impact is related to the total volume of magma intruded and released during these geologically brief events (peak eruptions are often within 1-5 Myrs duration) where millions to tens of millions of cubic kilometers of magma are produced. In some cases, at least 1% of the Earth’s surface has been directly covered in volcanic rock, being equivalent to the size of small continents with comparable crustal thicknesses. Large Igneous Provinces are thus important, albeit episodic episodes of new crust addition. However, most magmatism is basaltic so that contributions to crustal growth will not always be picked up in zircon geochronology studies that better trace major episodes of extension-related silicic magmatism and the silicic Large Igneous Provinces. Much headway has been made on our understanding of these anomalous igneous events over the last 25 years, driving many new ideas and models. This includes their: 1) global spatial and temporal distribution, with a long-term average of one event approximately every 20 Myrs, but a clear clustering of events at times of supercontinent break-up – Large Igneous Provinces are thus an integral part of the Wilson cycle and are becoming an increasingly important tool in reconnecting dispersed continental fragments; 2) compositional diversity that in part reflects their crustal setting of ocean basins, and continental interiors and margins where in the latter setting, LIP magmatism can be silicicdominant; 3) mineral and energy resources with major PGE and precious metal resources being hosted in these provinces, as well as magmatism impacting on the hydrocarbon potential of volcanic basins and rifted margins through enhancing source rock maturation, providing fluid migration pathways, and trap formation; 4) biospheric, hydrospheric and atmospheric impacts, with Large Igneous Provinces now widely regarded as a key trigger mechanism for mass extinctions, although the exact kill mechanism(s) are still being resolved; 5) role in mantle geodynamics and thermal evolution of the Earth, by potentially recording the transport of material from the lower mantle or core-mantle boundary to the Earth's surface and being a fundamental component in whole mantle convection models; and 6) recognition on the inner planets where the lack of plate tectonics and erosional processes and planetary antiquity means that the very earliest record of LIP events during planetary evolution may be better preserved than on Earth.

Crystal growth, transport and magnetic properties of rare-earth manganite Pr1-xPbxMnO3

Crystal growth, electrical and magnetic properties are reported for mixed valence manganite Pr1-xPbxMnO3 (x = 0.2, 0.23, and 0.3). The crystals with x = 0.2 and 0.23 are ferromagnetic and insulating, whereas that with x = 0.3 is ferromagnetic below 200 K and shows an insulator-metal transition at 235 K. This composition shows a magnetoresistance of 90% in a field of 5 T. In the paramagnetic region, the temperature dependence of magnetic susceptibility of the crystals follows a Curie-Weiss behavior. The thermal evolution of magnetization in the ferromagnetic phase varies as T-3/2, in accordance with Bloch's law. The spin-stiffness constant D obtained from the Bloch constant is found to increase linearly with x. The magnetization does not reach complete saturation upto a field of 5 T. A possible contribution of the Pr spins to the total magnetic moment is discussed.

Coexistence of para and ferromagnetic phases of Fe3+ in undoped CdZnTe (Zn similar to 4%) crystals

The signatures of the coexistence of para and ferromagnetic phases for the Fe3+ charge state of iron have been identified in the low temperature electron spin resonance (ESR) spectra in undoped CdZnTe (Zn similar to 4%) crystals and independently verified by superconducting quantum interference device (SQUID) and AC susceptibility measurements. In the paramagnetic phase the inverse of AC susceptibility follows the Curie-Weiss law. In the ferromagnetic phase the thermal evolution of magnetization follows the well-known Bloch T-3/2 law. This is further supported by the appearance of hysteresis in the SQUID measurements at 2 K below T-c which is expected to lie in between 2 and 2.5 K. (C) 2010 Elsevier Ltd. All rights reserved.

Synthesis and properties of willemite Zn2SiO4, and M2+: Zn2SiO4 (M = Co and Ni)

Fine particles of willemite, alpha -Zn2SiO4, were prepared by both solution combustion and sol-gel methods. Both processes yield single-phase, large-surface area (26- and 78-m(2)/g), sinteractive willemite powders. Thermal evolution of crystalline phases was studied using X-ray powder diffraction patterns. The combustion method favors low-temperature formation of willemite compared to the sol-gel method. The powders, when uniaxially pressed and sintered at 1300 degreesC, achieved 78-80% theoretical density. The microstructures of the sintered body show the presence of equiaxed 0.5- to 4-mum grains. Blue pigments of willemite doped with Co2+ and Ni2+ were also prepared by the combustion process.

DOES THE CHEMOTHERMAL INSTABILITY HAVE ANY ROLE IN THE FRAGMENTATION OF PRIMORDIAL GAS

The collapse of the primordial gas in the density regime similar to 10(8)-10(10) cm(-3) is controlled by the three-body H-2 formation process, in which the gas can cool faster than free-fall time-a condition proposed as the chemothermal instability. We investigate how the heating and cooling rates are affected during the rapid transformation of atomic to molecular hydrogen. With a detailed study of the heating and cooling balance in a 3D simulation of Pop III collapse, we follow the chemical and thermal evolution of the primordial gas in two dark matter minihalos. The inclusion of sink particles in modified Gadget-2 smoothed particle hydrodynamics code allows us to investigate the long-term evolution of the disk that fragments into several clumps. We find that the sum of all the cooling rates is less than the total heating rate after including the contribution from the compressional heating (pdV). The increasing cooling rate during the rapid increase of the molecular fraction is offset by the unavoidable heating due to gas contraction. We conclude that fragmentation occurs because H-2 cooling, the heating due to H-2 formation and compressional heating together set a density and temperature structure in the disk that favors fragmentation, not the chemothermal instability.

Mapeamento sísmico de intrusões ígneas na bacia do Amazonas e suas implicações para um modelo não-convencional de geração de hidrocarbonetos

A maioria das bacias paleozóicas brasileiras apresenta matéria orgânica termicamente pouco evoluída nos intervalos correspondentes ao Devoniano. O modelo mais adequado para se entender a geração, migração e acumulação de HC estaria relacionado às fases de intrusão de diabásio. No caso da Bacia do Amazonas, embora tenha havido condições de soterramento suficientes para a geração de hidrocarbonetos, não se deve descartar o modelo não convencional de geração como uma das formas possíveis de dar origem as acumulações comerciais de óleo e gás. Acredita-se que o intervalo mais apropriado para a geração de hidrocarbonetos (HC) inclua apenas as rochas depositadas no intervalo Frasniano, embora as rochas associadas ao intervalo Llandoveriano, também, devam ser observadas com atenção. Com o intuito de compreender melhor o papel da atividade magmática na evolução da Bacia do Amazonas, foi realizado o mapeamento sísmico de soleiras de diabásio e análise de dados geoquímicos de pirólise Rock-Eval e COT. Assim, foi possível avaliar a geração/migração de hidrocarbonetos e a variação dos parâmetros geotérmicos na Bacia do Amazonas, causados pela intrusão das soleiras de diabásio. A análise sismoestratigráfica baseou-se na interpretação de 20 linhas sísmicas 2D pós-stack, na qual foram reconhecidos e mapeados horizontes sísmicos (topos de formações e corpos ígneos intrusivos), utilizando dados de poços e dados da literatura para correlação. As intrusões de soleiras estão presentes nas sucessões de folhelhos/siltitos e anidritas das formações Andirá e Nova Olinda, respectivamente. Observou-se que as soleiras de diabásio podem estar intimamente relacionadas a diques sistematicamente orientados, tendo estes diques a função de alimentadores das soleiras. Extensas soleiras planares com segmentos transgressivos ocorrem nos níveis estratigráficos mais rasos da Bacia do Amazonas, e em maiores volumes nas formações Andirá e Nova Olinda. Em algumas regiões as soleiras desenvolvem morfologias marcantes em forma de pires. Esses corpos possuem espessuras que podem chegar a 500m. Comumente, a geometria em lençol denotada pelo paralelismo dos refletores está presente em toda extensão do mapeamento da bacia. Também foram observadas estruturas em domo. O efeito térmico imposto pelas intrusões dos corpos ígneos, diques e soleiras foi de grande importância, pois sem ele não haveria calor para a transformação da matéria orgânica. Através da análise de pirólise Rock-Eval e teor de carbono orgânico, foi possível avaliar e correlacionar os parâmetros como S2 (potencial de geração), IH (índice de hidrogênio), S1 (hidrocarbonetos livres) e Tmax (evolução térmica) com a profundidade. Foram utilizados dados de 04 poços na qual dois deles foram compilados a partir de artigos e teses publicados. As rochas potencialmente geradoras de petróleo são aquelas que apresentam COT igual ou superior a 1%. Dos quatro poços analisados, dois deles apresentam COT > 1% para a Formação Barreirinhas, mostrando que as rochas sedimentares são potencialmente geradoras de HC. Altos valores Tmax podem ser justificados pelo efeito térmico causado por intrusões de diabásio. Os resultados de índice de hidrogênio (IH) apresentaram valores abaixo de 200mgHC/g COT, indicando o potencial gerador desta bacia para gás.

Geoquímica orgânica das Formações Ererê, Barreirinha e Curiri (meso e neo devoniano) em dois poços na porção oeste da bacia do Amazonas

O estudo geoquímico detalhado em dois poços (A e B) na porção oeste da Bacia do Amazonas visou o entendimento da quantidade, fonte e evolução térmica da matéria orgânica presente nas Formações Ererê, Barreirinha e Curiri. Foram efetuadas análises de Carbono Orgânico Total (COT), pirólise Rock-Eval e biomarcadores. Os teores de carbono orgânico total da Formação Barreirinha (Membro Abacaxis) que variam de 1,43% a 8,39%, indicaram que este intervalo possui quantidade de matéria orgânica necessária para ser considerado potencialmente gerador de óleo e gás. As outras unidades litoestratigráficas apresentaram teores de COT pouco significativos. Com base nos dados de pirólise, identificou-se que o intervalo com o melhor potencial gerador corresponde ao Membro Abacaxis. Esta seção no poço A possui índice de hidrogênio (IH) ligeiramente superior a 200 mg HC/gCOT e um potencial gerador (S2)variando de 4 a 17,76 mg de HC/g de rocha, indicando um bom à excelente potencial adequado à geração de gás e condensado. Já no poço B, em decorrência do aumento da evolução térmica, os valores de S2 e IH são mais baixos(variando de 5 a 10 mgHC/g de rocha e com valores entre 50 e 150 mg HC/gCOT, respectivamente), apenas indicando um bom potencial à geração de gás. Segundo diagrama tipo Van Krevlen, a matéria orgânica deste intervalo é heterogênea e se comporta como querogênio tipo II e III no poço A e do tipo III e IV no poço B. As características dos biomarcadores encontrados no Membro Abacaxis indicam uma origem algal e ambiente marinho. O Membro Urariá e a Formação Curiri apresentam indicadores sugestivos de aporte de matéria orgânica de origem terrestre, sendo que o Membro Urariá ainda mostra algumas assinaturas semelhantes com o Membro Abacaxis. Devido a baixa concentração dos biomarcadores cíclicos nas amostras do Poço B, não foi possível realizar uma caracterização da fonte da matéria orgânica da Formação Ererê. A avaliação dos parâmetros utilizados para a interpretação da evolução térmica, como Tmax, taxa de transformação (TT), índice de produção (IP), reflectância da vitrinita calculada (Roc) e razões entre alcanos lineares e ramificados (P/nC17 e F/nC18), indicaram que no intervalo gerador do Poço A houve geração de hidrocarbonetos, mas ainda não correu a migração. No caso do Poço B, os dados mostram que neste intervalo já houve geração e migração de hidrocarbonetos.

Análise da evolução termomecânica da Bacia do Amazonas

Os dados geológicos e geofísicos escolhidos para o tema de estudo pertencem a Bacia do Amazonas, na região centro-norte do Brasil. A Bacia do Amazonas é uma bacia intracratônica com cerca de 500.000 km. A mesma está limitada ao norte pelo Escudo das Guianas e ao sul pelo Escudo Brasileiro. O limite oeste com a Bacia do Solimões é marcado pelo Arco de Purus, ao passo que o Arco de Gurupá constitui seu limite leste. Possui características inerentes a uma bacia intracratônica paleozóica, com uma longa história evolutiva, marcada por discordâncias expressivas e com uma cunha sedimentar relativamente rasa se comparada às bacias cretáceas brasileiras, o que levanta controvérsia a respeito da suficiência do soterramento para a eficiência de geração de hidrocarboneto. Podem ser reconhecidas nos 5000 m do preenchimento sedimentar da Bacia do Amazonas, duas seqüências de primeira ordem: uma paleozóica, intrudida por diques e soleiras de diabásio, na passagem do Triássico para o Jurássico, e uma mesozóica-cenozóica que representam um aspecto importante na evolução térmica da matéria orgânica que ocorre na primeira seqüência. Com relação à exploração de petróleo, apesar do fomento exploratório ocorrido nos últimos anos, a bacia ainda é considerada pouco explorada sendo sua maior reserva a da província de Urucu. Um dos fatores que dificultam bastante a exploração desta bacia assim como a bacia do Solimões a oeste é o acesso restrito, pois estão situadas em áreas remotas e florestadas, de difícil acesso, com muitas reservas indígenas e florestais, o que causa restrições logísticas, operacionais e legais. O efeito térmico das intrusões ígneas é considerado como o responsável pelo acréscimo de calor necessário à maturação da matéria orgânica e conseqüente geração de hidrocarbonetos. Este trabalho contribui com a reconstrução da história térmica desta bacia a partir da modelagem das variáveis termais e da história de soterramento. Para isso, foram utilizados modelos consagrados na literatura, que permitem, de forma simples, a estimativa do fluxo térmico através do embasamento e da seqüência sedimentar. Na análise da influência de intrusões ígneas na estrutura térmica da bacia, o modelo bidimensional desenvolvido pelo método de diferenças finitas se mostrou apropriado. Utilizou-se o fluxo térmico basal calculado nas condições de contorno da modelagem da influência térmica das ígneas. Como resultado obteve-se a estruturação térmica da bacia e a historia maturação de suas rochas geradoras