Using the maternal immune stimulation model of schizophrenia to investigate the therapeutic efficacy of neuromodulation techniques

The present work used a neurodevelopmental rodent model of schizophrenia, namely the maternal immune stimulation (MIS) model, to study the potency of electrical neuromodulation techniques to ameliorate and even prevent schizophrenia-relevant behavioral and neurobiological abnormalities. Acute and focal deep brain stimulation (DBS) to the medial prefrontal cortex (mPFC) was found to be therapeutically relevant as it successfully normalized deficits in sensorimotor gating and attention selectivity apparent in the adult MIS animals. Using a longitudinal approach the development of sensorimotor gating deficits in the MIS model was traced and was found to exhibit a maturational delay, in accordance with the clinical situation. Further, this approach revealed aberrant neurochemistry profile in the mPFC during the pre-symptomatic period of adolescence, prior to the outbreak of the behavioral deficits. Thus, chronic DBS to the mPFC of adolescent MIS animals was tested and revealed that this approach could prevent the development of deficits in sensorimotor gating, attentional selectivity and reversal learning. Along with these effects, DBS was able to prevent increased lateral ventricles volume and neurochemical alterations as well as the prevention of altered microglia in this model. Finally, a non-invasive neuromodulation technique in the form of transcranial direct current stimulation (tDCS) was chronically applied during adolescence to the prefrontal cortex and revealed that tDCS prevented behavioral deficits belonging to the positive-symptomatology of schizophrenia, along with abnormal lateral ventricles volume. Taken together, this pre-clinical, translational-directed work points to the plausible efficacy of early, non-invasive, neuromodulation approach as a preventive measure for the development of schizophrenia

Interior Models of Saturn: Including the Uncertainties in Shape and Rotation

The accurate determination of Saturn's gravitational coefficients by Cassini could provide tighter constrains on Saturn's internal structure. Also, occultation measurements provide important information on the planetary shape which is often not considered in structure models. In this paper we explore how wind velocities and internal rotation affect the planetary shape and the constraints on Saturn's interior. We show that within the geodetic approach (Lindal et al., 1985, ApJ, 90, 1136) the derived physical shape is insensitive to the assumed deep rotation. Saturn's re-derived equatorial and polar radii at 100 mbar are found to be 54,445 $\pm$10 km and 60,365$\pm$10 km, respectively. To determine Saturn's interior we use {\it 1 D} three-layer hydrostatic structure models, and present two approaches to include the constraints on the shape. These approaches, however, result in only small differences in Saturn's derived composition. The uncertainty in Saturn's rotation period is more significant: with Voyager's 10h39mns period, the derived mass of heavy elements in the envelope is 0-7 M$_{\oplus}$. With a rotation period of 10h32mns, this value becomes $<4$ $M_{\oplus}$, below the minimum mass inferred from spectroscopic measurements. Saturn's core mass is found to depend strongly on the pressure at which helium phase separation occurs, and is estimated to be 5-20 M$_{\oplus}$. Lower core masses are possible if the separation occurs deeper than 4 Mbars. We suggest that the analysis of Cassini's radio occultation measurements is crucial to test shape models and could lead to constraints on Saturn's rotation profile and departures from hydrostatic equilibrium.Comment: Accepted for publication in Ap

The Effects of Metallicity, and Grain Growth and Settling on the Early Evolution of Gaseous Protoplanets

Giant protoplanets formed by gravitational instability in the outer regions of circumstellar disks go through an early phase of quasi-static contraction during which radii are large and internal temperatures are low. The main source of opacity in these objects is dust grains. We investigate two problems involving the effect of opacity on the evolution of planets of 3, 5, and 7 M_J. First, we pick three different overall metallicities for the planet and simply scale the opacity accordingly. We show that higher metallicity results in slower contraction as a result of higher opacity. It is found that the pre-collapse time scale is proportional to the metallicity. In this scenario, survival of giant planets formed by gravitational instability is predicted to be more likely around low-metallicity stars, since they evolve to the point of collapse to small size on shorter time scales. But metal-rich planets, as a result of longer contraction times, have the best opportunity to capture planetesimals and form heavy-element cores. Second, we investigate the effects of opacity reduction as a result of grain growth and settling, for the same three planetary masses and for three different values of overall metallicity. When these processes are included, the pre-collapse time scale is found to be of order 1000 years for the three masses, significantly shorter than the time scale calculated without these effects. In this case the time scale is found to be relatively insensitive to planetary mass and composition. However, the effects of planetary rotation and accretion of gas and dust, which could increase the timescale, are not included in the calculation. The short time scale we find would preclude metal enrichment by planetesimal capture, as well as heavy-element core formation, over a large range of planetary masses and metallicities.Comment: 22 pages, accepted to Icaru

The formation of mini-Neptunes

Mini-Neptunes seem to be common planets. In this work we investigate the possible formation histories and predicted occurrence rates of mini-Neptunes assuming the planets form beyond the iceline. We consider pebble and planetesimal accretion accounting for envelope enrichment and two different opacity conditions. We find that the formation of mini-Neptunes is a relatively frequent output when envelope enrichment by volatiles is included, and that there is a "sweet spot" for mini-Neptune formation with a relatively low solid accretion rate of ~10^{-6} Earth masses per year. This rate is typical for low/intermediate-mass protoplanetary disks and/or disks with low metallicities. With pebble accretion, envelope enrichment and high opacity favor the formation of mini-Neptunes, with more efficient formation at large semi-major axes (~30 AU) and low disk viscosity. For planetesimal accretion, such planets can form also without enrichment, with the opacity being a key aspect in the growth history and favorable formation location. Finally, we show that the formation of Neptune-like planets remains a challenge for planet formation theories.Comment: Accepted for publication in Ap