Planetary population synthesis

In stellar astrophysics, the technique of population synthesis has been successfully used for several decades. For planets, it is in contrast still a young method which only became important in recent years because of the rapid increase of the number of known extrasolar planets, and the associated growth of statistical observational constraints. With planetary population synthesis, the theory of planet formation and evolution can be put to the test against these constraints. In this review of planetary population synthesis, we first briefly list key observational constraints. Then, the work flow in the method and its two main components are presented, namely global end-to-end models that predict planetary system properties directly from protoplanetary disk properties and probability distributions for these initial conditions. An overview of various population synthesis models in the literature is given. The sub-models for the physical processes considered in global models are described: the evolution of the protoplanetary disk, the planets' accretion of solids and gas, orbital migration, and N-body interactions among concurrently growing protoplanets. Next, typical population synthesis results are illustrated in the form of new syntheses obtained with the latest generation of the Bern model. Planetary formation tracks, the distribution of planets in the mass-distance and radius-distance plane, the planetary mass function, and the distributions of planetary radii, semimajor axes, and luminosities are shown, linked to underlying physical processes, and compared with their observational counterparts. We finish by highlighting the most important predictions made by population synthesis models and discuss the lessons learned from these predictions - both those later observationally confirmed and those rejected.Comment: 47 pages, 12 figures. Invited review accepted for publication in the 'Handbook of Exoplanets', planet formation section, section editor: Ralph Pudritz, Springer reference works, Juan Antonio Belmonte and Hans Deeg, Ed

A new population pharmacokinetic model for recombinant factor IX‐Fc fusion concentrate including young children with haemophilia B

Aims: Recombinant factor IX Fc fusion protein (rFIX‐Fc) is an extended half‐life factor concentrate administered to haemophilia B patients. So far, a population pharmacokinetic (PK) model has only been published for patients aged ≥12 years. The aim was to externally evaluate the predictive performance of the published rFIX‐Fc population PK model for patients of all ages and develop a model that describes rFIX‐Fc PK using real‐world data. Methods: We collected prospective and retrospective data from patients with haemophilia B treated with rFIX‐Fc and included in the OPTI‐CLOT TARGET study (NTR7523) or United Kindom (UK)‐EHL Outcomes Registry (NCT02938156). Predictive performance was assessed by comparing predicted with observed FIX activity levels. A new population PK model was constructed using nonlinear mixed‐effects modelling. Results: Real‐world data were obtained from 37 patients (median age: 16 years, range 2–71) of whom 14 were aged <12 years. Observed FIX activity levels were significantly higher than levels predicted using the published model, with a median prediction error of −48.8%. The new model showed a lower median prediction error (3.4%) and better described rFIX‐Fc PK, especially for children aged <12 years. In the new model, an increase in age was correlated with a decrease in clearance (P < .01). Conclusions: The published population PK model significantly underpredicted FIX activity levels. The new model better describes rFIX‐Fc PK, especially for children aged <12 years. This study underlines the necessity to strive for representative population PK models, thereby avoiding extrapolation outside the studied population

Spin-resolved neutron spectroscopy from the heavy Fermion compound CeCu 6

Neutron time-of-flight spectroscopy with neutron polarisation analysis permits the in situ separation of magnetic and lattice vibrational energy spectra. Preliminary experiments on the heavy Fermion compound, CeCu 6, in which the Ce magnetic moment is suppressed by the Kondo effect, allow an indicative separation of a broadened crystal field transition and features due to lattice vibrations. An inelastic spin-flip feature at -12 meV is due to the crystal field while an inelastic non-spin-flip feature at -6 meV is predominantly due to phonon scattering

Measurement of σ(ppˉ→Z)⋅\bm{\sigma (p \bar p \to Z) \cdot}Br(Z→ττ)\bm{(Z \to \tau \tau)} at s=\bm{\sqrt{s}=}1.96 TeV

D0We present a measurement of the cross section for $Z$ production times the branching fraction to $\tau$ leptons, $\sigma \cdot$Br$(Z\to \tau^+ \tau^-)$, in $p \bar p$ collisions at $\sqrt{s}=$1.96 TeV in the channel in which one $\tau$ decays into $\mu \nu_{\mu} \nu_{\tau}$, and the other into $\rm {hadrons} + \nu_{\tau}$ or $e \nu_e \nu_{\tau}$. The data sample corresponds to an integrated luminosity of 226 pb$^{-1}$ collected with the D{\O}detector at the Fermilab Tevatron collider. The final sample contains 2008 candidate events with an estimated background of 55%. From this we obtain $\sigma \cdot$Br$(Z \to \tau^+ \tau^-)=237 \pm 15$(stat)$\pm 18$(sys)$\pm 15$(lum) pb, in agreement with the standard model prediction