The SOPHIE search for northern extrasolar planets: X. Detection and characterization of giant planets by the dozen

We present new radial velocity measurements of eight stars that were secured with the spectrograph SOPHIE at the 193 cm telescope of the Haute-Provence Observatory. The measurements allow detecting and characterizing new giant extrasolar planets. The host stars are dwarfs of spectral types between F5 and K0 and magnitudes of between 6.7 and 9.6; the planets have minimum masses Mp sin i of between 0.4 to 3.8 MJup and orbitalperiods of several days to several months. The data allow only single planets to be discovered around the first six stars (HD 143105, HIP 109600, HD 35759, HIP 109384, HD 220842, and HD 12484), but one of them shows the signature of an additional substellar companion in the system. The seventh star, HIP 65407, allows the discovery of two giant planets that orbit just outside the 12:5 resonance in weak mutual interaction. The last star, HD 141399, was already known to host a four-planet system; our additional data and analyses allow new constraints to be set on it. We present Keplerian orbits of all systems, together with dynamical analyses of the two multi-planet systems. HD 143105 is one of the brightest stars known to host a hot Jupiter, which could allow numerous follow-up studies to be conducted even though this is not a transiting system. The giant planets HIP 109600b, HIP 109384b, and HD 141399c are located in the habitable zone of their host star.

Close-in planets around giant stars: lack of hot-Jupiters and prevalence of multiplanetary systems

Extrasolar planets abound in almost any possible configuration. However, until five years ago, there was a lack of planets orbiting closer than 0.5 au to giant or subgiant stars. Since then, recent detections have started to populated this regime by confirming 13 planetary systems. We discuss the properties of these systems in terms of their formation and evolution off the main sequence. Interestingly, we find that 70.0 ± 6.6% of the planets in this regime are inner components of multiplanetary systems. This value is 4.2σ higher than for main-sequence hosts, which we find to be 42.4 ± 0.1%. The properties of the known planets seem to indicate that the closest-in planets (a< 0.06 au) to main-sequence stars are massive (i.e., hot Jupiters) and isolated and that they are subsequently engulfed by their host as it evolves to the red giant branch, leaving only the predominant population of multiplanetary systems in orbits 0.06

Biodiversity and molecular evolution of malacostraca

No actual cenário de perda acelerada de biodiversidade, o nosso conhecimento dos ecossistemas marinhos, apesar da sua extensão e complexidade, continua muito inferior ao dos ecossistemas terrestres. A classe Malacostraca (Arthropoda, Crustacea), um grupo dos mais representativos nos ecossistemas marinhos, apresenta um elevado nível de diversidade morfológica e ecológica, mas difícil sua identificação ao nível de espécie requer frequentemente a ajuda de especialistas em taxonomia. A utilização recente do “barcoding” (código de barras do ADN), revelou ser um método rápido e eficaz para a identificação de espécies em diversos grupos de metazoários, incluindo os Malacostraca. No âmbito desta tese foi construída uma base de dados de código de barras de ADN envolvendo 132 espécies de Malacostraca vários locais de amostragem no Atlântico Nordeste e Mediterrâneo. As sequências de ADN mitocondrial provenientes de 601 espécimes formaram, em 95% dos casos, grupos congruentes com as identificações baseadas em características morfológicas. No entanto, foi detectado polimorfismo em seis casos e a divergência intra-específica foi elevada em exemplares pertencentes a duas espécies morfológicas, sugerindo, neste caso, a ocorrência de especiação críptica. Este estudo confirma a utilidade do código de barras de ADN para a identificação de Malacostraca marinhos. Apesar do sucesso obtido, este método apresenta alguns problemas, como por exemplo a possível amplificação de pseudogenes. A ocorrência de pseudogenes e as possíveisabordagens para a detecção e resolução deste tipo de problemas são discutidas com base em casos de estudo: análises dos códigos de barras ADN na espécie Goneplax rhomboides (Crustacea, Decapoda). A análise dos códigos de barras ADN revelou ainda grupos prioritários de decápodes para estudos taxonómicos e sistemáticos, nomeadamente os decápodes dos géneros Plesionika e Pagurus. Neste âmbito são discutidas as relações filogenéticas entre espécies seleccionadas dos géneros Plesionika e Pagurus. Este trabalho aponta para várias questões no âmbito da biodiversidade e evolução molecular da classe Malacostraca que carecem de um maior esclarecimento, podendo ser considerado como a base para estudo futuros. Análises filogenéticas adicionais integrando dados morfológicos e moleculares de um maior número de espécies e de famílias deverão certamente conduzir a uma melhor avaliação da biodiversidade e da evolução dentro da classe.

An extreme planetary system around HD 219828: one long-period super Jupiter to a hot-Neptune host star

Context. With about 2000 extrasolar planets confirmed, the results show that planetary systems have a whole range of unexpected properties. This wide diversity provides fundamental clues to the processes of planet formation and evolution. Aims: We present a full investigation of the HD 219828 system, a bright metal-rich star for which a hot Neptune has previously been detected. Methods: We used a set of HARPS, SOPHIE, and ELODIE radial velocities to search for the existence of orbiting companions to HD 219828. The spectra were used to characterise the star and its chemical abundances, as well as to check for spurious, activity induced signals. A dynamical analysis is also performed to study the stability of the system and to constrain the orbital parameters and planet masses. Results: We announce the discovery of a long period (P = 13.1 yr) massive (m sini = 15.1 MJup) companion (HD 219828 c) in a very eccentric orbit (e = 0.81). The same data confirms the existence of a hot Neptune, HD 219828 b, with a minimum mass of 21 M⊕ and a period of 3.83 days. The dynamical analysis shows that the system is stable, and that the equilibrium eccentricity of planet b is close to zero. Conclusions: The HD 219828 system is extreme and unique in several aspects. First, ammong all known exoplanet systems it presents an unusually high mass ratio. We also show that systems like HD 219828, with a hot Neptune and a long-period massive companion are more frequent than similar systems with a hot Jupiter instead. This suggests that the formation of hot Neptunes follows a different path than the formation of their hot jovian counterparts. The high mass, long period, and eccentricity of HD 219828 c also make it a good target for Gaia astrometry as well as a potential target for atmospheric characterisation, using direct imaging or high-resolution spectroscopy. Astrometric observations will allow us to derive its real mass and orbital configuration. If a transit of HD 219828 b is detected, we will be able to fully characterise the system, including the relative orbital inclinations. With a clearly known mass, HD 219828 c may become a benchmark object for the range in between giant planets and brown dwarfs.

Secular and tidal evolution of circumbinary systems

We investigate the secular dynamics of three-body circumbinary systems under the effect of tides. We use the octupolar non-restricted approximation for the orbital interactions, general relativity corrections, the quadrupolar approximation for the spins, and the viscous linear model for tides. We derive the averaged equations of motion in a simplified vectorial formalism, which is suitable to model the long-term evolution of a wide variety of circumbinary systems in very eccentric and inclined orbits. In particular, this vectorial approach can be used to derive constraints for tidal migration, capture in Cassini states, and stellar spin–orbit misalignment. We show that circumbinary planets with initial arbitrary orbital inclination can become coplanar through a secular resonance between the precession of the orbit and the precession of the spin of one of the stars. We also show that circumbinary systems for which the pericenter of the inner orbit is initially in libration present chaotic motion for the spins and for the eccentricity of the outer orbit. Because our model is valid for the non-restricted problem, it can also be applied to any three-body hierarchical system such as star–planet–satellite systems and triple stellar systems.