A candidate super-Earth planet orbiting near the snow line of Barnard's star.

Barnard's star is a red dwarf, and has the largest proper motion (apparent motion across the sky) of all known stars. At a distance of 1.8 parsecs1, it is the closest single star to the Sun; only the three stars in the α Centauri system are closer. Barnard's star is also among the least magnetically active red dwarfs known2,3 and has an estimated age older than the Solar System. Its properties make it a prime target for planetary searches; various techniques with different sensitivity limits have been used previously, including radial-velocity imaging4-6, astrometry7,8 and direct imaging9, but all ultimately led to negative or null results. Here we combine numerous measurements from high-precision radial-velocity instruments, revealing the presence of a low-amplitude periodic signal with a period of 233 days. Independent photometric and spectroscopic monitoring, as well as an analysis of instrumental systematic effects, suggest that this signal is best explained as arising from a planetary companion. The candidate planet around Barnard's star is a cold super-Earth, with a minimum mass of 3.2 times that of Earth, orbiting near its snow line (the minimum distance from the star at which volatile compounds could condense). The combination of all radial-velocity datasets spanning 20 years of measurements additionally reveals a long-term modulation that could arise from a stellar magnetic-activity cycle or from a more distant planetary object. Because of its proximity to the Sun, the candidate planet has a maximum angular separation of 220 milliarcseconds from Barnard's star, making it an excellent target for direct imaging and astrometric observations in the future.

A giant exoplanet orbiting a very-low-mass star challenges planet formation models.

Surveys have shown that super-Earth and Neptune-mass exoplanets are more frequent than gas giants around low-mass stars, as predicted by the core accretion theory of planet formation. We report the discovery of a giant planet around the very-low-mass star GJ 3512, as determined by optical and near-infrared radial-velocity observations. The planet has a minimum mass of 0.46 Jupiter masses, very high for such a small host star, and an eccentric 204-day orbit. Dynamical models show that the high eccentricity is most likely due to planet-planet interactions. We use simulations to demonstrate that the GJ 3512 planetary system challenges generally accepted formation theories, and that it puts constraints on the planet accretion and migration rates. Disk instabilities may be more efficient in forming planets than previously thought.

The development of links between stereocilia in hair cells of the chick basilar papilla.

Auditory papillae of chicks (embryonic age 6-21 days) were examined by scanning and transmission electron microscopy, in order to trace the development of the tip links between the stereocilia, and in order to trace the development of the spatial organisation of the tip links. In the most immature bundles, stereocilia were not graded in height, while strands of tenuous material interconnected adjacent stereocilia, this material being concentrated in a band near the tips of the stereocilia. The material joined the stereocilia in all directions, with no preferential direction for the interconnecting material being visible. Similarly, no columnar organisation of the stereocilia was visible. As soon as a gradation in height of the stereocilia began to appear, material could be seen running upwards from the shorter stereocilia to the adjacent lengthening stereocilia. There was a continuum in appearance between (i) the material running laterally between short immature stereocilia, (ii) the material running upwards between stereocilia which were developing a gradation in height, and (iii) the tip links seen in more mature bundles. It is suggested that tip links are a specialisation of the links which join immature stereocilia laterally near their tips. It is also suggested that the orientation of tip links, parallel to the hair cell axis of bilateral symmetry, is produced by the gradient in growth of the stereocilia.

Morphological correlates of mechanotransduction in acousticolateral hair cells.

The development of ideas on mechanotransduction in acousticolateral hair cells is described, leading to the current idea that transduction depends on deflection of the bundle of stereocilia by a force parallel to the plane of the sensory epithelium. Electrophysiological experiments are summarised, suggesting that transduction depends on a shear between the different rows of stereocilia, and that the transducer channels are situated towards the tips of the stereocilia. Analysis of the ways that shear between the rows of stereocilia could be detected suggests that tip links are the structures which are most likely to transmit the stimulus-induced forces to the transducer channels on the membrane. The directional selectivity of mechanotransduction is associated with the position of the kinocilium and gradation in heights of the stereocilia; evidence is presented suggesting that in the lateral line these are partly determined by the mitosis giving rise to the hair cell. Tip links differentiate out of links which initially join the stereocilia in all directions, with their final spatial organisation, which sets the directional selectivity of mechanotransduction, probably being determined by the gradient in growth of the stereocilia.