Migration of extrasolar planets to large orbital radii

Observations of structure in circumstellar debris discs provide circumstantial evidence for the presence of massive planets at large (several tens of au) orbital radii, where the timescale for planet formation via core accretion is prohibitively long. Here, we investigate whether a population of distant planets can be produced via outward migration subsequent to formation in the inner disc. Two possibilities for significant outward migration are identified. First, cores that form early at radii of around 10 au can be carried to larger radii via gravitational interaction with the gaseous disc. This process is efficient if there is strong mass loss from the disc - either within a cluster or due to photoevaporation from a star more massive than the Sun - but does not require the extremely destructive environment found, for example, in the core of the Orion Nebula. We find that, depending upon the disc model, gas disc migration can yield massive planets (several Jupiter masses) at radii of around 20-50 au. Second, interactions within multiple planet systems can drive the outer planet into a large, normally highly eccentric orbit. A series of scattering experiments suggests that this process is most efficient for lower mass planets within systems of unequal mass ratio. This mechanism is a good candidate for explaining the origin of relatively low mass giant planets in eccentric orbits at large radii.Comment: MNRAS, in pres

The formation of the solar system

The solar system started to form about 4.56 Gyr ago and despite the long intervening time span, there still exist several clues about its formation. The three major sources for this information are meteorites, the present solar system structure and the planet-forming systems around young stars. In this introduction we give an overview of the current understanding of the solar system formation from all these different research fields. This includes the question of the lifetime of the solar protoplanetary disc, the different stages of planet formation, their duration, and their relative importance. We consider whether meteorite evidence and observations of protoplanetary discs point in the same direction. This will tell us whether our solar system had a typical formation history or an exceptional one. There are also many indications that the solar system formed as part of a star cluster. Here we examine the types of cluster the Sun could have formed in, especially whether its stellar density was at any stage high enough to influence the properties of today's solar system. The likelihood of identifying siblings of the Sun is discussed. Finally, the possible dynamical evolution of the solar system since its formation and its future are considered.Comment: 36 pages, 7 figures, invited review in Physica Script

C and O Isotope Chemostratigraphy and Bulk Chemistry of Reef Limestones of the Tambaba Formation, Paraíba Basin, Northeastern Brazil

This work focuses on the behavior of the C and O isotopes and major and trace element chemistry of the carbonate rocks of the Tambaba Formation, Paraíba Basin, Northeastern Brazil. Thirteen carbonate samples collected from three vertical profiles located perpendicular to the bedding along the coast of the state of Paraíba were analyzed. The δ13C values ranged from 1.6 to 2.8‰ VPDB while the δ18O values ranged from -1.2 to 1.8‰ VPDB, thus suggest a restricted shallow-platform depositional environment. X-ray fluorescence analyses suggested diagenetic changes, such as the replacement of dolomite by calcite (Mn/Sr ratios from 0.6 to 28) and dolomitization, which was identified by high Mg/Ca ratios (0.5 to 0.6). The very low SiO2 and Al2O3 content attested to the low terrigenous material influx. The carbon isotope values suggest that the carbonate rocks were deposited after the Paleocene-Eocene Thermal Maximum (PETM) event

Horizontal spreading of planetary debris accreted by white dwarfs

White dwarfs with metal-polluted atmospheres have been studied widely in the context of the accretion of rocky debris from evolved planetary systems. One open question is the geometry of accretion and how material arrives and mixes in the white dwarf surface layers. Using the three-dimensional (3D) radiation hydrodynamics code CO5BOLD, we present the first transport coefficients in degenerate star atmospheres that describe the advection–diffusion of a passive scalar across the surface plane. We couple newly derived horizontal diffusion coefficients with previously published vertical diffusion coefficients to provide theoretical constraints on surface spreading of metals in white dwarfs. Our grid of 3D simulations probes the vast majority of the parameter space of convective white dwarfs, with pure-hydrogen atmospheres in the effective temperature range of 6000–18 000 K and pure-helium atmospheres in the range of 12 000–34 000 K. Our results suggest that warm hydrogen-rich atmospheres (DA; ≳13000 K) and helium-rich atmospheres (DB and DBA; ≳30000 K) are unable to efficiently spread the accreted metals across their surface, regardless of the time dependence of accretion. This result may be at odds with the current non-detection of surface abundance variations in white dwarfs with debris discs. For cooler hydrogen- and helium-rich atmospheres, we predict a largely homogeneous distribution of metals across the surface within a vertical diffusion time-scale. This is typically less than 0.1 per cent of disc lifetime estimates, a quantity that is revisited in this paper using the overshoot results. These results have relevance for studies of the bulk composition of evolved planetary systems and models of accretion disc physics

WASP-86b and WASP-102b: super-dense versus bloated planets

We report the discovery of two transiting planetary systems: a super dense, sub-Jupiter mass planet WASP-86b (Mpl = 0.82 ± 0.06 MJ; Rpl = 0.63 ± 0.01 RJ), and a bloated, Saturn-like planet WASP-102b (Mpl = 0.62 ± 0.04 MJ; Rpl = 1.27 ± 0.03 RJ). They orbit their host star every ∼5.03, and ∼2.71 days, respectively. The planet hosting WASP-86 is a F7 star (Teff = 6330±110 K, [Fe/H] = +0.23 ± 0.14 dex, and age ∼0.8–1 Gyr); WASP-102 is a G0 star (Teff = 5940±140 K, [Fe/H] = −0.09± 0.19 dex, and age ∼1 Gyr). These two systems highlight the diversity of planetary radii over similar masses for giant planets with masses between Saturn and Jupiter. WASP-102b shows a larger than model-predicted radius, indicating that the planet is receiving a strong incident flux which contributes to the inflation of its radius. On the other hand, with a density of ρpl = 3.24± 0.3 ρJ, WASP-86b is the densest gas giant planet among planets with masses in the range 0.05 Mpl J. With a stellar mass of 1.34 M⊙ and [Fe/H]= +0.23 dex, WASP-86 could host additional massive and dense planets given that its protoplanetary disc is expected to also have been enriched with heavy elements. In order to match WASP-86b’s density, an extrapolation of theoretical models predicts a planet composition of more than 80% in heavy elements (whether confined in a core or mixed in the envelope). This fraction corresponds to a core mass of approximately 210M⊕ for WASP-86b’s mass of Mpl∼260 M⊕. Only planets with masses larger than about 2 MJ have larger densities than that of WASP-86b, making it exceptional in its mass range

Stellar archaeology with Gaia: the Galactic white dwarf population

Gaia will identify several 1e5 white dwarfs, most of which will be in the solar neighborhood at distances of a few hundred parsecs. Ground-based optical follow-up spectroscopy of this sample of stellar remnants is essential to unlock the enormous scientific potential it holds for our understanding of stellar evolution, and the Galactic formation history of both stars and planets.Comment: Summary of a talk at the 'Multi-Object Spectroscopy in the Next Decade' conference in La Palma, March 2015, to be published in ASP Conference Series (editors Ian Skillen & Scott Trager

Fast spectrophotometry of WD 1145+017

WD 1145+017 is currently the only white dwarf known to exhibit periodic transits of planetary debris as well as absorption lines from circumstellar gas. We present the first simultaneous fast optical spectrophotometry and broad-band photometry of the system, obtained with the Gran Telescopio Canarias (GTC) and the Liverpool Telescope (LT), respectively. The observations spanned $5.5$ h, somewhat longer than the $4.5$-h orbital period of the debris. Dividing the GTC spectrophotometry into five wavelength bands reveals no significant colour differences, confirming grey transits in the optical. We argue that absorption by an optically thick structure is a plausible alternative explanation for the achromatic nature of the transits that can allow the presence of small-sized ($\sim\mu$m) particles. The longest ($87$ min) and deepest ($50$ per cent attenuation) transit recorded in our data exhibits a complex structure around minimum light that can be well modelled by multiple overlapping dust clouds. The strongest circumstellar absorption line, Fe II $\lambda$5169, significantly weakens during this transit, with its equivalent width reducing from a mean out-of-transit value of $2$ \AA\ to $1$ \AA\ in-transit, supporting spatial correlation between the circumstellar gas and dust. Finally, we made use of the Gaia Data Release 2 and archival photometry to determine the white dwarf parameters. Adopting a helium-dominated atmosphere containing traces of hydrogen and metals, and a reddening $E(B-V)=0.01$ we find $T_\mathrm{eff}=15\,020 \pm 520$ K, $\log g=8.07\pm0.07$, corresponding to M_\mathrm{WD}=0.63\pm0.05\ \mbox{\mathrm{M}_{\odot}} and a cooling age of $224\pm30$ Myr.Comment: 13 pages, 9 figures, accepted for publication in Monthly Notices of the Royal Astronomical Society (2018 Aug 22

Detecção do vírus da Artrite Encefalite Caprina por nested PCR e nested RT-PCR em ovócitos e fluido uterino.

Resumo: A Artrite Encefalite Caprina (CAE) é uma enfermidade infectocontagiosa causada por um vírus pertencente ao gênero lentivírus, denominado de vírus da Artrite Encefalite Caprina (CAEV). O CAEV é encontrado em vários tecidos, como o nervoso, o pulmonar, o da glândula mamária e do trato genital masculino e feminino. Desta forma, objetivou-se com este trabalho identificar a presença do CAEV, pelas técnicas de diagnóstico moleculares, em ovócitos e fluido uterino, visando avaliar a possibilidade de transmissão do CAEV pela reprodução. Foram selecionadas 13 cabras comprovadamente infectadas, as quais foram submetidas à eutanásia para coleta do aparelho reprodutor, aspiração do fluido uterino e dissecção dos ovários para coleta de ovócitos. Para identificação do CAEV nas amostras coletadas, na forma de provírus e na forma livre, foram realizadas as técnicas de PCRn e RT-PCRn, respectivamente. Observaram-se que 53,8% dos ovócitos foram positivos à técnica de RT-PCRn, enquanto apenas 9,1% foram positivos à PCRn. A técnica de RT-PCRn também identificou o vírus no fluido uterino de 46,1% das fêmeas testadas. Embora as 13 cabras em experimento fossem portadoras do CAEV, 30,8% apresentaram resultados negativos na PCRn e RT-PCRn em todas as amostras analisadas (ovócito e fluido uterino). Conclui-se que a PCRn e a RT-PCRn podem ser utilizadas no diagnóstico da CAE tendo os ovócitos e o fluido uterino como materiais de análise, e que a presença do CAEV nestes materiais aponta para o risco da transmissão do CAEV através das tecnologias reprodutivas aplicadas às fêmeas. [Caprine Arthritis Encephalitis virus is detected in oocytes and uterine fluid by nested PCR and nested RT-PCR]. Abstract: Caprine arthritis-encephalitis (CAE) is an infectious disease caused by the caprine arthritis-encephalitis virus (CAEV), belonging to the lentivirus genus. The presence of the virus has been observed in the nervous system, respiratory tract and mammary gland, and also in the male and female genital tract. The objective of this study is to identify the virus in oocyte and uterine fluid of infected goats by molecular diagnostic techniques, in order to assess the possibility of CAEV transmission with reproduction. Thirteen infected goats were selected and submitted to euthanasia for the collection of the reproductive system, aspiration of the uterine fluid and dissection of ovaries for oocyte collection. In order to identify the CAEV in the collected material, in the protovirus and free forms, it was submitted to the nRT-PCR and nPCR techniques, respectively. As a result, it was observed that 53.8% of oocytes were positive to nRT-PCR, while only 9.1% were positive to nPCR. The nRT-PCR also identified the virus in the uterine fluid of 46.1% of the tested females. Even though the 13 goats had CAEV, 30.8% presented negative results in nPCR and nRTPCR in all of the analyzed samples (oocyte and uterine fluid). This work concludes that nRT-PCR and nPCR can be used in the diagnosis of CAE for the analysis with oocytes and uterine fluid, and that the presence of CAEV in these materials points out to the risk of CAEV transmission through reproductive technologies used in females