The atrial flow regulator is a new self-expandable double-disc fenestrated device providing a calibrated inter-atrial communication. Paediatric reports are scarce. We herein describe a case of complete atrioventricular block complicating the exemption use of an atrial flow regulator in a 5-kg infant with transposition of the great arteries, ventricular septal defect, and right ventricular outflow tract obstruction.

Pulmonary atresia with ventricular septal defect, non-confluent pulmonary arteries, and bilateral arterial duct is a rare and complex CHD. Physiologic ductal closure may lead to life-threatening hypoxia. We present a case of successful bilateral ductal stenting as a bridge to further lower-risk surgical repair.

Therapeutic options are limited for the management of extremely low-birth-weight infants with critical aortic coarctation despite high doses of prostaglandin infusion. We report successful hybrid, fluoroscopy-free, echocardiography-guided primary stenting of native aortic coarctation in a 920-grams premature infant.

Device-induced aortic obstruction is a known rare complication following transcatheter closure of patent ductus arteriosus in extremely low-birth-weight infants. Various mechanisms have been proposed. We report the first description of late aortic obstruction due to ductal vasoconstriction on pulmonic end causing device to be gradually pushed out of aortic end in a 980-gram premature infant.

We report the exceptional case of transcatheter treatment of a partial anomalous pulmonary venous drainage of the right lung to the innominate vein and dual drainage to the left atrium.

The long-term prospective multi-centre nationwide (French) observational study FRANCISCO will provide new information on perimembranous ventricular septal defect with left ventricular overload but no pulmonary hypertension in children older than 1 year. Outcomes will be compared according to treatment strategy (watchful waiting, surgical closure, or percutaneous closure) and anatomic features of the defect. The results are expected to provide additional guidance about the optimal treatment of this specific population, which is unclear at present.

For the shortest period exoplanets, star-planet tidal interactions are likely to have played a major role in the ultimate orbital evolution of the planets and on the spin evolution of the host stars. Although low-mass stars are magnetically active objects, the question of how the star’s magnetic field impacts the excitation, propagation and dissipation of tidal waves remains open. We have derived the magnetic contribution to the tidal interaction and estimated its amplitude throughout the structural and rotational evolution of low-mass stars (from K to F-type). We find that the star’s magnetic field has little influence on the excitation of tidal waves in nearly circular and coplanar Hot-Jupiter systems, but that it has a major impact on the way waves are dissipated.

The gravito-inertial waves propagating over a shellular baroclinic flow inside a rotating spherical shell are analysed using the Boussinesq approximation. The wave properties are examined by computing paths of characteristics in the non-dissipative limit, and by solving the full dissipative eigenvalue problem using a high-resolution spectral method. Gravito-inertial waves are found to obey a mixed-type second-order operator and to be often focused around short-period attractors of characteristics or trapped in a wedge formed by turning surfaces and boundaries. We also find eigenmodes that show a weak dependence with respect to viscosity and heat diffusion just like truly regular modes. Some axisymmetric modes are found unstable and likely destabilized by baroclinic instabilities. Similarly, some non-axisymmetric modes that meet a critical layer (or corotation resonance) can turn unstable at sufficiently low diffusivities. In all cases, the instability is driven by the differential rotation. For many modes of the spectrum, neat power laws are found for the dependence of the damping rates with diffusion coefficients, but the theoretical explanation for the exponent values remains elusive in general. The eigenvalue spectrum turns out to be very rich and complex, which lets us suppose an even richer and more complex spectrum for rotating stars or planets that own a differential rotation driven by baroclinicity.

Tetralogy of Fallot and coarctation of the aorta is an exceptional association. We report here four cases of infants referred for tetralogy of Fallot with or without pulmonary atresia associated with aortic coarctation from 1974 to 2013. All had a right aortic arch, and the coarctation was abnormally situated between the right common carotid and the right subclavian arteries. In all, two infants had an abnormal left subclavian artery and one child had DiGeorge syndrome. All underwent staged surgical repair of the left and right-sided obstructions. A review of the literature shows two types of coarctation in this context. In left aortic arch, coarctation is situated distal to the left subclavian artery. In right aortic arch, coarctation is distal to the right common carotid artery, mirror-image of interrupted left aortic arch type B, associated with anomalies of the branches of the aorta, and should be considered a complex anomaly of aortic arches in the setting of an outflow tract defect due to abnormal migration of cardiac neural crest cells. Screening for this unusual association is critical in the initial assessment of all patients with tetralogy of Fallot.

We investigate the properties of small-amplitude inertial waves propagating in a differentially rotating incompressible fluid contained in a spherical shell. For cylindrical and shellular rotation profiles and in the inviscid limit, inertial waves obey a second-order partial differential equation of mixed type. Two kinds of inertial modes therefore exist, depending on whether the hyperbolic domain where characteristics propagate covers the whole shell or not. The occurrence of these two kinds of inertial modes is examined, and we show that the range of frequencies at which inertial waves may propagate is broader than with solid-body rotation. Using high-resolution calculations based on a spectral method, we show that, as with solid-body rotation, singular modes with thin shear layers following short-period attractors still exist with differential rotation. They exist even in the case of a full sphere. In the limit of vanishing viscosities, the width of the shear layers seems to weakly depend on the global background shear, showing a scaling in ${E}^{1/ 3} $ with the Ekman number $E$, as in the solid-body rotation case. There also exist modes with thin detached layers of width scaling with ${E}^{1/ 2} $ as Ekman boundary layers. The behaviour of inertial waves with a corotation resonance within the shell is also considered. For cylindrical rotation, waves get dramatically absorbed at corotation. In contrast, for shellular rotation, waves may cross a critical layer without visible absorption, and such modes can be unstable for small enough Ekman numbers.

Compte tenu de la radiosensibilité accrue des enfants aux rayonnements ionisants, notre objectif est d’évaluer les risques de cancers solides et de leucémies à long terme associés aux expositions médicales reçues pendant l’enfance. Deux études de cohorte sont réalisées par le Laboratoire d’épidémiologie de l’Institut de radioprotection et de sûreté nucléaire (IRSN). L’une, la « Cohorte Enfant Scanner » porte sur les enfants nés après le 01/01/1995 et exposés aux rayonnements ionisants lors de scanners réalisés entre 2000 et 2013. L’autre porte sur les enfants exposés lors de procédures de cardiologie interventionnelle avant l’âge de 10 ans entre 2000 et 2013. Pour chacune des cohortes, une évaluation rétrospective individuelle de l’exposition sera réalisée par l’Unité d’expertise en radioprotection médicale de l’IRSN. Un suivi passif en termes de cancers solides et de leucémies sera réalisé grâce aux données des registres de cancers pédiatriques et aux données de mortalité. La « Cohorte Enfant Scanner » est constituée de plus 80 000 enfants et s’inscrit dans le projet européen EPI-CT, qui regroupe 9 cohortes nationales. À terme, la cohorte des enfants en cardiologie interventionnelle regroupera plus de 8 000 enfants. Ces études de cohortes, avec un suivi prolongé, permettront d’étudier l’impact sur la santé des expositions radiologiques reçues pendant l’enfance.

Planet migration plays a crucial role in shaping planetary systems, and has therefore received a lot of attention in recent years in an effort to compare the statistical properties of observed exoplanets with the predictions of planet formation and migration theories. By modifying the propagation properties of the waves induced by the planet in the disk, the presence of a strong magnetic field can dramatically influence planet migration, in some cases reversing its direction. The more realistic case of a weaker magnetic field is less clear, although turbulent MHD simulations by Baruteau et al. (2011) suggest an effect on the corotation torque. Here, we present a study of the corotation torque in 2D laminar disks containing a toroidal magnetic field. We performed MHD simulations of the interaction between the magnetic field and the horseshoe motion of the gas, and found that this results in an additional corotation torque. This additional torque can be strong enough to reverse migration even for a field which pressure is only one percent of the thermal pressure. We speculate that this could lead to long range outward migration in the outer part of protoplanetary disks and may explain the observations by direct imaging of planets at several tens of AU from their star like the 4 planets system HR 8799.

We investigate the impact of the disk self-gravity on type I migration. We first show that considering a planet migrating in a disk without self-gravity can lead to a significant overestimate of the migration rate. Unbiased drift rates can be obtained only if the planet and the disk feel the same gravitational potential. We then confirm that the disk gravity slightly accelerates type I migration.

We investigate type I migration in a two-dimensional adiabatic disk. We find entropy perturbations that are advected in the planet's coorbital region. These entropy perturbations yield an excess of corotation torque that scales with the unperturbed entropy gradient at corotation. This torque excess can be large enough to slow down migration significantly, or even stop it.