The Global Coupled 3 (GC3) configuration of the Met Office Unified Model is presented. Among other applications, GC3 is the basis of the United Kingdom's submission to the Coupled Model Intercomparison Project 6 (CMIP6). This paper documents the model components that make up the configuration (although the scientific descriptions of these components are in companion papers) and details the coupling between them. The performance of GC3 is assessed in terms of mean biases and variability in long climate simulations using present‐day forcing. The suitability of the configuration for predictability on shorter time scales (weather and seasonal forecasting) is also briefly discussed. The performance of GC3 is compared against GC2, the previous Met Office coupled model configuration, and against an older configuration (HadGEM2‐AO) which was the submission to CMIP5. In many respects, the performance of GC3 is comparable with GC2, however, there is a notable improvement in the Southern Ocean warm sea surface temperature bias which has been reduced by 75%, and there are improvements in cloud amount and some aspects of tropical variability. Relative to HadGEM2‐AO, many aspects of the present‐day climate are improved in GC3 including tropospheric and stratospheric temperature structure, most aspects of tropical and extratropical variability and top‐of‐atmosphere and surface fluxes. A number of outstanding errors are identified including a residual asymmetric sea surface temperature bias (cool northern hemisphere, warm Southern Ocean), an overly strong global hydrological cycle and insufficient European blocking.

Phototropic hypocotyl bending in response to blue light excitation is an important adaptive process that helps plants to optimize their exposure to light. In Arabidopsis thaliana, phototropic hypocotyl bending is initiated by the blue light receptors and protein kinases phototropin1 (phot1) and phot2. Phototropic responses also require auxin transport and were shown to be partially compromised in mutants of the PIN-FORMED (PIN) auxin efflux facilitators. We previously described the D6 PROTEIN KINASE (D6PK) subfamily of AGCVIII kinases, which we proposed to directly regulate PIN-mediated auxin transport. Here, we show that phototropic hypocotyl bending is strongly dependent on the activity of D6PKs and the PIN proteins PIN3, PIN4, and PIN7. While early blue light and phot-dependent signaling events are not affected by the loss of D6PKs, we detect a gradual loss of PIN3 phosphorylation in d6pk mutants of increasing complexity that is most severe in the d6pk d6pkl1 d6pkl2 d6pkl3 quadruple mutant. This is accompanied by a reduction of basipetal auxin transport in the hypocotyls of d6pk as well as in pin mutants. Based on our data, we propose that D6PK-dependent PIN regulation promotes auxin transport and that auxin transport in the hypocotyl is a prerequisite for phot1-dependent hypocotyl bending.

We attribute most of the development of extensive fractures in the Tharsis region to discrete tectonic provinces within the region, rather than to Tharsis as a single entity. One of these provinces is in Syria Planum. Faults and collapse structures in the Syria Planum tectonic province on Mars are grouped into 13 sets based on relative age, areal distribution, and morphology. According to superposition and fault crosscutting relations and crater counts we designate six distinct episodes of tectonic activity in the following chronologic order: stage I is an early to late Noachian deformation forming mostly east‐west structures (fault set IA); some large volcanoes also formed. Faults were produced possibly by flexural uplift. Also, arcuate, north trending grabens (set IB) indicate that faulting is transitional to the next stage. Stage II is late Noachian to early Hesperian radial faulting centered in Syria Planum, possibly due to isostatic uplift in late Noachian (set IIA) to early Hesperian (set IIB) time. Stage III is early to late Hesperian faulting tangential to Syria Planum that was related to local centers of uplift (sets III1‐III3) on the periphery of Syria Planum. Stage IV is a late Hesperian graben formation that was circumferential to Syria Planum (set IVA), caused either by collapse associated with eruption of magma or by flexure of the lithosphere due to volcanic loading. In association with volcanism, minor faulting occurred, producing an oval pattern of faults in southwest Syria Planum (set IVBl) and a radial pattern south of the planum (set IVB2) that apparently rejuvenated buried stage II faults. Stage V is a late Hesperian to early Amazonian development of grabens and troughs of Noctis Labyrinthus and western Valles Marineris (set V) that was probably instigated by local uplift; exposure of groundwater or ground ice zones may have produced further collapse and trough enlargement. Stage VI is early Amazonian northwest trending faulting in Noctis Fossae (set VIl), perhaps due to Tharsis Monies‐centered tectonism, and north northwest normal faulting along the eastern side of the Claritas rise (set VI2) that was due to tectonic subsidence. The duration of tectonic activity in the Syria Planum province was perhaps 2–3 b.y. Photoclinometric topographic profiles across 132 grabens and fault scarps show that Syria Planum grabens have widths (average of 2.5 km, and most range from 1 to 6 km) similar to lunar grabens, but the Martian grabens have slightly higher side walls (average about 132 m) and gentler wall slopes (average of 9° and range of 2°–25°) than lunar grabens (93 m high and 18° slopes). Scarp degradation on Mars has progressed through quakes, impact shaking, and dry slope processes; the lower slopes may be due to Mars’ higher gravity. Estimates of the amount of extension for individual grabens range from 20 to 350 m; most estimates of the thickness of the faulted layer range from 0.5 to 4.5 km (average is 1.5 km). This thickness range corresponds closely to the 0.8‐to 3.6‐km range in depth for p...

A set of Fe and Ti maps and regional values are obtained from the Apollo 15 and 16 orbital gamma ray data by energy band analysis. High‐Ti basalts predominate the early and late stages of mare volcanism with high‐Fe basaltic volcanism in the interim. The first evidence of a high‐Ti‐KREEP basalt association is found in the Aristarchus region. A N‐S asymmetry for Fe and Ti in the east limb and farside highlands complicates the E‐W asymmetry for Th but substantiates crustal inhomogeneity. The observed crustal inhomogeneity adds an additional objection to the primitive source model for crustal evolution. The high‐Ti‐KREEP basalt association and the general trend of decreasing mare basalt Ti with time lend support to the cumulate source model; however, this model cannot account for young, high‐Ti maria and the absence of KREEP in high‐Ti maria. The dynamic assimilation model better accounts for chemical variations observed on the moon.

We assess the impact of atmospheric horizontal resolution on the prediction skill and fidelity of seasonal forecasts. We show the response to an increase of atmospheric resolution from 0.8 to 0.3° horizontal grid spacing in parallel ensembles of forecasts. Changes in the prediction skill of major modes of tropical El Nino Southern Oscillation (ENSO) and extratropical North Atlantic Oscillation (NAO) variability are small and not detected and there is no discernible impact on the weak signal‐to‐noise ratio in seasonal predictions of the winter NAO at this range of resolutions. Although studies have shown improvements in the simulation of tropical cyclones as model resolution is increased, we find little impact on seasonal prediction skill of either their numbers or intensity. Over this range of resolutions it appears that the benefit of increasing atmospheric resolution to seasonal climate predictions is minimal. However, at yet finer scales there appears to be increased eddy feedback which could strengthen weak signals in predictions of the NAO. Until prediction systems can be run operationally at these scales, it may be better to use additional computing resources for other enhancements such as increased ensemble size, for which there is a clear benefit in extratropical seasonal prediction skill.