Accretion Formation Research Articles

Hydrogen sulfide and metal-enriched atmosphere for a Jupiter-mass exoplanet.

As the closest transiting hot Jupiter to Earth, HD 189733b has been the benchmark planet for atmospheric characterization1-3. It has also been the anchor point for much of our theoretical understanding of exoplanet atmospheres from composition4, chemistry5,6, aerosols7 to atmospheric dynamics8, escape9 and modelling techniques10,11. Previous studies of HD 189733b have detected carbon and oxygen-bearing molecules H2O and CO (refs. 12,13) in the atmosphere. The presence of CO2 and CH4 has been claimed14,15 but later disputed12,16,17. The inferred metallicity based on these measurements, a key parameter in tracing planet formation locations18, varies from depletion19,20 to enhancement21,22, hindered by limited wavelength coverage and precision of the observations. Here we report detections of H2O (13.4σ), CO2 (11.2σ), CO (5σ) and H2S (4.5σ) in the transmission spectrum (2.4-5.0 μm) of HD 189733b. With an equilibrium temperature of about 1,200 K, H2O, CO and H2S are the main reservoirs for oxygen, carbon and sulfur. Based on the measured abundances of these three main volatile elements, we infer an atmospheric metallicity of three to five times stellar. The upper limit on the methane abundance at 5σ is 0.1 ppm, which indicates a low carbon-to-oxygen ratio (<0.2), suggesting formation through the accretion of water-rich icy planetesimals. The low oxygen-to-sulfur and carbon-to-sulfur ratios also support the planetesimal accretion formation pathway23.

Production increase of high-grade crude zinc oxide pellets at Shisaka Smelting Co., Ltd.

Shisaka Smelting Co., Ltd. has recovered crude zinc oxide pellets from an electric arc furnace dust (EAF dust) by the Waelz kiln process since 1977. The EAF dust processing line consists of a reduction roasting process, a Waelz oxide washing process, and a drying/calcination process. In late years, about 90,000 tons of EAF dust is processed annually at Shisaka. The recovered zinc is sold to zinc smelters as crude zinc oxide pellets, and the amount of production of the pellets is about 40,000 tons per year. Two types of zinc oxide pellets are produced, and the product for electro-refinery requires high quality, especially in fluorine reduction. Most of fluorine are distributed to the clinker in a reduction roasting process, and others are distributed to the Waelz oxide. Conventionally, high-grade crude zinc oxide pellets were produced by washing the Waelz oxide and by volatilizing and separating fluorine under high temperature operation in a drying rotary kiln. However, formation of accretion in the kiln and damage of the shell and refractories of the kiln often occurred under the influence of high temperature operation, and stable consecutive operation of the kiln was difficult.To improve this situation, the fluorine input was reduced by compounding management of EAF dust in the reduction roasting process, and the material residence time in the drying rotary kiln was extended by reducing rotary speed. These improvements resulted in stable consecutive operation under low temperature conditions and increased production of high-grade crude zinc oxide pellets. To improve this situation, the fluorine input was reduced by compounding management of EAF dust in the reduction roasting process, and the material residence time in the drying rotary kiln was extended by reducing rotary speed. These improvements resulted in stable consecutive operation under low temperature conditions and increased production of high-grade crude zinc oxide pellets.

Digital formation processes: A high-frequency, large-scale investigation

Large sources of digital trace data (i.e. “Big Data”) have become increasingly important in the study of material culture. However, akin to the offline material culture traditionally studied by archaeologists, digital trace data is rarely a passive reflection of human behavior – it is a complex palimpsest produced through a variety of erasure and accretion formation processes. To better understand how digital trace palimpsests are formed and how digital formation processes influence and inform our ability to interpret the offline material processes they index, we introduce a computational method – high-frequency archaeological survey – which allows us to observe digital formation processes at a high temporal resolution, as well as a large spatial scale. Using this method every hour for one month, we surveyed posts from across the United States in Craigslist's “Free Stuff” category (popularly called “Curb Alert”), a user-generated source of big digital trace data, indexing material things that have been placed on users' curbs for removal by scavengers or trash collectors. For each post, we observed its time-to-erasure and any edits that were made during the study period – finding that the posts that survive represent a biased sample of those that were posted over the course of the month, conditioned by how recently and on what day the post is posted, the material characteristics of things that are posted about, as well as regional variation. Far from only being evidence of biased end-of-month data, however, we show that further analysis of identified digital formation processes can be an important object of study in its own right – in this case, shedding new light on social scientific questions linking the exchange of “free stuff” with the process of social stratification and urban inequality in the United States. Overall, our findings suggest the importance of accounting for and explicitly analyzing digital formation processes in studies that utilize digital trace data.

Flue Dust Reactions and Sticking Mechanisms in a Copper Flash Smelting Furnace Waste Heat Boiler: A Sampling Study

The formation of accretion layers within the waste heat boiler is a serious operational concern as it can potentially increase boiler downtime and, hence, limit continuous production. In previous Computational Fluid Dynamics studies, the accretion formation was predicted for an industrial-scale waste heat boiler, using a dust stickiness sub-routine of the model. In this study, a dust sampling campaign was used to validate this stickiness sub-routine. Furthermore, various sticking and reaction mechanisms of flue dust were investigated and compared to thermodynamic predictions. While the results suggest that the sub-routine is valid, the comparison of thermodynamics and species in the samples showed that the chemical reactions of the flue dust did not reach the thermodynamic equilibrium.Graphical

Условия формирования опасных отложений зернистой изморози на Полярном Урале

Synoptic conditions for the formation of high-intensity hard rime accretion on the territory of the Polar Urals are considered. A leading role of mesoscale processes primarily related to the terrain features in the formation of hard rime is revealed. Numerical experiments are implemented to reproduce the cases of hard rime formation on the territory of the Rai-Iz mountain range using the WRF-ARW mesoscale model. The simulation results and the methods used to interpret them made it possible to obtain detailed fields of meteorological parameters necessary for the correct assessment of the probability and intensity of the hard rime formation. It was also shown that it is reasonable to use model spatial steps of not more than 2 km for successful modeling of ice accretion in the form of hard rime. Keywords: severe weather events, ice accretion, icing, rime, hard rime, numerical weather prediction, WRF-ARW

A mesh-free formalism for ice accretion prediction due to large drop impingement

This paper presents a novel mesh-free framework, using the smoothed particle hydrodynamics method (SPH), for the analysis of large drop impingement and ice accretion prediction on land engineering structures. The SPH method is an efficient and effective approach for the analysis of dynamic fluid flow problems involving free-surface interfaces. In this paper, it has been extended to include the thermodynamics of the freezing process. This allows not only the prediction of drop impact, splashing, and retraction, but also drop freezing and the formation of ice accretion. This mesh-free approach solves a set of non-linear transient dynamic continuum equations. The code also employs an enthalpy-based energy evolution algorithm, coupled with a phase transition equation. Surface tension and adhesion are handled with an approach that is shown to provide an accurate prediction of impinging water drop behavior. Numerical results of drop impact and freezing have been validated against a combination of experimental data and simple ice accretion models. In addition, ice accretions resulting from multi-drop impingement and freezing have been predicted. It is also shown that the developed method can simulate the influence of surface wettability on ice accretion shapes. The presented mesh-free formalism provides a next-generation approach to ice accretion prediction.

NGTS-21b: an inflated Super-Jupiter orbiting a metal-poor K dwarf

ABSTRACT We report the discovery of NGTS-21b , a massive hot Jupiter orbiting a low-mass star as part of the Next Generation Transit Survey (NGTS). The planet has a mass and radius of 2.36 ± 0.21 MJ and 1.33 ± 0.03 RJ, and an orbital period of 1.543 d. The host is a K3V (Teff = 4660 ± 41 K) metal-poor ([Fe/H] = −0.26 ± 0.07 dex) dwarf star with a mass and radius of 0.72 ± 0.04 M⊙ and 0.86 ± 0.04R⊙. Its age and rotation period of $10.02^{+3.29}_{-7.30}$ Gyr and 17.88 ± 0.08 d, respectively, are in accordance with the observed moderately low-stellar activity level. When comparing NGTS-21b with currently known transiting hot Jupiters with similar equilibrium temperatures, it is found to have one of the largest measured radii despite its large mass. Inflation-free planetary structure models suggest the planet’s atmosphere is inflated by $\sim \! 21{{\ \rm per\ cent}}$, while inflationary models predict a radius consistent with observations, thus pointing to stellar irradiation as the probable origin of NGTS-21b’s radius inflation. Additionally, NGTS-21b’s bulk density (1.25 ± 0.15 g cm–3) is also amongst the largest within the population of metal-poor giant hosts ([Fe/H] &amp;lt; 0.0), helping to reveal a falling upper boundary in metallicity–planet density parameter space that is in concordance with core accretion formation models. The discovery of rare planetary systems such as NGTS-21 greatly contributes towards better constraints being placed on the formation and evolution mechanisms of massive planets orbiting low-mass stars.

ABOUT THE SLAG-FREE SILICOCALCIUM AND SILICOBARIUM PRODUCTION METHOD

The state of production of silicocalcium and silicobarium by the carbon-thermal method from lumpy and briquetted charge is considered. It is shown that the use of lumpy charge leads to frequent adjustment of its composition, unstable technological and electrical melting conditions, gradual formation of carbide accretion in the furnace bath, which is an obstacle to the creation of continuous and low waste productions. The use of ore-coal briquettes makes it possible to optimize the chemistry of the reduction of elements with carbon, create favorable conditions for the occurrence of lowtemperature chemical reactions and reduce the energy intensity of the technological process. As a result of the use of orecoal briquettes, it becomes possible to mechanize the loading of the charge into the furnace, eliminate the labor-intensive operations to adjust the composition of the charge, utilize own production waste and organize the waste-free production. The examples of the use of the briquetted charge in a semi-industrial furnace with a capacity of 1.6 MVA are provided.

Transient CFD Calculation of Accretion Formation in a Copper Waste Heat Boiler

The operation of a copper Flash Smelting Furnace (FSF) is often limited by the availability of the downstream Waste Heat Boiler (WHB). Carry-over of concentrate into the boiler leads to accretion formation, which can cause boiler downtime. Hence, the minimization of flue dust and its accretions is an important operational goal. In this study, a Computational Fluid Dynamics (CFD) model is used to investigate how three different baffle plate designs influence accretion formation over a period of 24 hours. The predicted dust accretion patterns were compared for all baffle plate modifications, with differences found both in the resulting sedimentation and accretion of dust particles. While the dispersive design led to large, but evenly coated accretion risk zones, a streamlined design minimized their size but led to locally thick accretion layers. Based on these findings, design recommendations for the baffle plate were derived.

Severe hard rime accretion in the Far North of Russia: observations and modeling

Severe weather means any hazardous meteorological phenomena which can cause significant damage, serious social disruption, or loss of human life. Such weather phenomena include thunderstorms, hurricanes, tornados, ice storms, and many others. The main purpose of this research is a study of formation mechanisms of rime accretion and methods for their prediction. This is necessary to forecast these phenomena and minimize their economic and other losses. This work is dedicated to a detailed study of an extraordinary case of formation of rime accretion in the territory of the Yamalo-Nenets Autonomous Okrug, which occurred in early January 2016. Numerical experiments are used for an analysis of various methods for predicting areas of possible ice accretion formation. For the numerical experiments, the atmospheric model WRF-ARW has been chosen. For a theoretical assessment of icing intensity, the Makkonen formula is used. The results of this research are as follows: the main mechanisms of ice accretion formation have been identified for the territory of the Far North of Russia. Numerical experiments with the WRF-ARW model have been successful and reproduced the main signs of rime accretion. The results show that the model has successfully reproduced the icing start time and the icing intensity distribution throughout the entire numerical experiment. The quality of the model's assessment of the mass of rime accretion is difficult to estimate from data of only two meteorological stations; however, the values obtained are close to the observed ones.

The changing dynamics of the gas-dust flow in the flash smelter at Nadezhda metallurgical plant due to addition of a shield. Part 1. Model calculations

A poorer quality of the raw materials that go in the flash smelter operated by Nadezhda Metallurgical Plant, as well as the use of man-made deposits and fine ore concentrates with high concentrations of particles smaller than 10 &mu;m, leads to a higher amount of entrained dust. Dust entrained by the gas flow leads to the formation of accretion in the slag end, uptake shaft and waste heat boiler. A higher dust entrainment is associated with higher loads on the gas duct, higher material turnover, decreased performance and recovery of non-ferrous metals. Fitting the furnace crown with a shield avoiding any major changes to the furnace design or the smelting process helps change the dynamics of the gas flow and lower dust entrainment. This paper defines the optimum location and dimensions of such shield. Depending on the particle size and the density of the gas-dust flow, with the shield installed, the estimated reduction in the amount of dust getting in the dust treatment system may reach 20%.&nbsp;

Accretion formation on the refractory lining during the melting of ferrosilicon

SYNOPSIS Accretions often form in furnaces when slag and charge materials attach to the refractory wall and build up over time. Accretion formation is usually unwanted because it reduces the working volume of the reactor and hinders material flow through the reactor. However, in some instances a thin, stable accretion layer may be desirable to protect the underlying refractory material. In order to prevent and/or manage accretion formation, it is important to understand the underlying principles of this phenomenon in the particular reactor. Excessive accretion formation hampered production at the Exxaro FerroAlloys ferrosilicon melting and atomization plant. This plant uses induction furnaces in which a 15% silicon-iron alloy is produced by batch smelting a mixture of ferrosilicon of 75%Si grade and low-carbon steel. The molten ferrosilicon alloy is then gas-atomized to a powdered product for use as a dense medium in mineral processing plants. The objective of this study was to investigate the effect of different impurity levels in the ferrosilicon feed material on the extent of accretion formation as well as the effect on the accretion properties, which influence the ease of accretion removal upon furnace shut-down. Refractory and accretion samples were collected after a furnace shut-down and characterized using X-ray diffraction and scanning electron microscopy-energy dispersive spectroscopy. It was concluded that the trace elements in the FeSi-75 feed material (Al, Ca, Mn) were mostly responsible for accretion formation, but that rust on the low-carbon steel and oxidation of the steel contributed to accretion attachment to the lining. The total contaminant content, calcium to aluminium ratio in the FeSi-75 feed material, and thereby the liquid to solids ratio in the accretion at temperature determine the strength of attachment as well as growth of the accretion. Keywords: Accretion, build-up, slag, refractory lining, ferrosilicon.

A Case Study on Accretion Formation in Rotary Kiln of DRI Process

In coal-based DRI process, accretion formation inside the rotary kiln is a genuine complex problem. Accretion formation in a rotary kiln of 100 tpd DRI plant has been investigated. The nature of accretion formation with respect to the charge burden and operational parameter have been discussed. High ash content in the coal and excess use of dolomite lead to accretion formation. Two different types of accretion are revealed; the major one is due to agglomeration of DRI by-products while another one is sintered product of DRI.

Flame analysis for prediction of thermocouple temperature and quality of sponge iron at TATA steel long products limited

The temperature profiles of the gas and charge in a coal-fired rotary sponge iron kiln affect both the iron ore reduction process and accretion formation. The temperature profile of charge is estimated from the eleven thermocouples (TC1-TC11) placed along the 80 m length of the kiln. The quality prediction models are heavily dependent upon the accuracy of the measurement of TC10. However, slowly, as the kiln’s campaign life increases TC10, and other thermocouples too, get corrupted due to deposition of material (accretions) on the thermocouples. At the beginning of the campaign, however, there is no accretion on TC10. In the present work, an attempt is made to directly correlate flame characteristics with TC10 and with quality of iron produced so that when TC10 is corrupted due to accretion or breakdown, we can still survive by using flame characteristics as a guide to control quality. The flame inside the rotary kiln has been analysed by using image analysis procedures for the first time in a sponge iron plant. The flame’s estimated average temperature and pixel intensity information are correlated with (a) the temperature measured by the thermocouple TC10 (which is installed at a distance of 20 m from the rotary kiln outlet hood) and (b) with quality of iron produced. It is found that use of average flame temperature for quality prediction has several advantages in terms of increased accuracy of prediction and quicker response time of flame to short-time changes in coal quality (particle size, moisture, ash content, etc) whereas TC10 thermocouple takes much longer to reflect these changes due to slow process of heat transfer to charge. In addition, the adverse effect of accretion formation on TC10 for quality prediction has been overcome.

Landscape evolution of Punta Arena sand spit (SE Baja California Peninsula, NW Mexico): Implications of ENSO on landscape erosion rates

Coastal bars are deltaic landforms resulting from sediment mobilization from source to sink. The formation, evolution and extinction of coastal bars is of broad interest for Quaternary studies because these are natural archives of former and present climatic conditions where complex ecological and biological relations take place. The Pacific coast of Mexico contains many coastal bars, like the strand-plain of Nayarit (~1400 km2) which is one of the largest around the world. We present the first ages of the largest sand spit (~8.5 km2) of the SE part of Baja California Peninsula, named Punta Arena. OSL ages indicate that the innermost bar is 0.26 ± 0.02 ka (1755 ± 20 AD). Using OSL ages and data obtained from Landsat images we estimate a mean sedimentation rate of ca. 7.7 m yr –1. Results from satellite images spanning for 32 years (1984 to 2016) confirms that sand spit is accreting at ca. 0.6 m yr –1 along the bar formation zone and to ca. 0.7 m yr –1 along the longshore drift zone, such rates however, are significantly lower compared other formation periods between 1755 and 1984 CE when sedimentation rates were ~ 8 to ~ 52 m yr –1. The progradation of the sand spit is consistent with the apparent development and density of vegetation which dramatically drops from inland towards the coast. The analysis of rainfall data spanning from 1950 to 2015 indicates that the largest periods of sedimentation along the sand spit are related with extended non-rainfall months occurring during ENSO conditions. Our data indicate that climate in SE Baja California Peninsula has remained more or less stable since the LIA and the periods of landscape erosion, leading to the formation of bars and sand spit accretion, mainly occur under the warm phase of ENSO (La Niña) which produces extended periods of landscape dryness and intense rainfalls during the winter.

Pengelolaan Lahan Akresi di Desa Pambang Pesisir, Pulau Bengkalis, Provinsi Riau

The breakwater construction to overcome abrasion at Pambang Pesisir has resulted in the formation of land accretion which expanded the coastal land and giving rises to issues in public management. This research was aimed to formulate the alternative management of land accretion. A field survey and light unmanned aerial vehicle (drone) data acquisition were used to observe the accretion formed. Furthermore, Analytical Hierarchy Process (AHP) was used to generate the alternative managements of land accretion. Accretion land was estimated around 80,359.4 m2and based on coastal area protection, living creature’s habitat, fisheries resources, tourism and business development benefit, social community supporting and sustainability of social interaction criteria’s, this area had great potential to be managed with use it for mangrove planting or rehabilitation sites in ecological land-based management.

Limonin: A triterpenoid exerts protective effect during lipopolysaccharide stimulated inflammation in BV2 microglial cells

Objectives: Neuroinflammation mediated by the reactive oxygen and nitrogen species (ROS and RNS, respectively) is responsible for the production of cytokines and chemokines in the central nervous system, which causes glial activation and associated pathology. Limonin is an oxygenated triterpenoid dilactone obtained from the families Rutaceae and Meliaceae. It exerts anticancer, antioxidant, antiviral, antinociceptive, and anti-inflammatory effects. In this study, we intended to analyze the anti-inflammatory and neuroprotective activities of limonin against neuroinflammation induced by lipopolysaccharide (LPS) in an in vitro model with BV2 immortalized murine microglial cells. Materials and Methods: Cytotoxicity of limonin was investigated via 3-(4,5-dimethylthiazolyl-2)-2,5-dipheniltetrazolium bromide tetrazol assay, and anti-inflammatory activity was assessed by analyzing the status of ROS, nitric oxide (NO), prostaglandin E2 (PGE2), interleukin (IL)-1β, IL-6, and tumor necrosis factor (TNF)-α using ELISA. The expression of inducible nitric oxide synthase (iNOS), TNF-α, IL-1β, and Cyclooxygenase (COX-2) was studied through immunoblot analysis. Results: Our results showed that pretreatment of LPS-induced microglial cells with limonin appreciably prevented the formation of ROS and prevented the accretion of NO, PGE2, IL-1β, IL-6, and TNF-α. Furthermore, limonin pretreatment significantly reduced the expressions of iNOS and COX-2. Conclusion: Our results indicate that limonin inhibits inflammatory response through repressing the formation of ROS, accretion and discharge of cytokines, and activation of inflammatory mediators. Limonin can be used as a neuro-protecting agent.

Accretion and star formation in ‘radio-quiet’ quasars

AbstractRadio observations allow us to identify a wide range of active galactic nuclei (AGN), which play a significant role in the evolution of galaxies. Amongst AGN at low radio-luminosities is the ‘radio-quiet’ quasar (RQQ) population, but how they contribute to the total radio emission is under debate, with previous studies arguing that it is predominantly through star formation. In this talk, SVW summarised the results of recent papers on RQQs, including the use of far-infrared data to disentangle the radio emission from the AGN and that from star formation. This provides evidence that black-hole accretion, instead, dominates the radio emission in RQQs. In addition, we find that this accretion-related emission is correlated with the optical luminosity of the quasar, whilst a weaker luminosity-dependence is evident for the radio emission connected with star formation. What remains unclear is the process by which this accretion-related emission is produced. Understanding this for RQQs will then allow us to investigate how this type of AGN influences its surroundings. Such studies have important implications for modelling AGN feedback, and for determining the accretion and star-formation histories of the Universe.

G.A.S.

Context. Star formation in galaxies is inefficient, and understanding how star formation is regulated in galaxies is one of the most fundamental challenges of contemporary astrophysics. Radiative cooling, feedback from supernovae and active galactic nuclei (AGN), and large-scale dynamics and dissipation of turbulent energy act over various time and spatial scales and all regulate star formation in a complex gas cycle. Aims. This paper presents the physics implemented in a new semi-analytical model of galaxy formation and evolution called the Galaxy Assembler from dark-matter Simulation (G.A.S.). Methods. The fundamental underpinning of our new model is the development of a multiphase interstellar medium (ISM) in which energy produced by supernovae and AGN maintains an equilibrium between a diffuse, hot, and stable gas and a cooler, clumpy, and low-volume filling factor gas. The hot gas is susceptible to thermal and dynamical instabilities. We include a description of how turbulence leads to the formation of giant molecular clouds through an inertial turbulent energy cascade, assuming a constant kinetic energy transfer per unit volume. We explicitly modelled the evolution of the velocity dispersion at different scales of the cascade and accounted for thermal instabilities in the hot halo gas. Thermal instabilities effectively reduce the impact of radiative cooling and moderates accretion rates onto galaxies, and in particular, for those residing in massive haloes. Results. We show that rapid and multiple exchanges between diffuse and unstable gas phases strongly regulates star formation rates in galaxies because only a small fraction of the unstable gas is forming stars. We checked that the characteristic timescales describing the gas cycle, gas depletion timescale, and star-forming laws at different scales are in good agreement with observations. For high-mass haloes and galaxies, cooling is naturally regulated by the growth of thermal instabilities, so we do not need to implement strong AGN feedback in this model. Our results are also in good agreement with the observed stellar mass function from z ≃ 6.0 to z ≃ 0.5. Conclusion. Our model offers the flexibility to test the impact of various physical processes on the regulation of star formation on a representative population of galaxies across cosmic times. Thermal instabilities and the cascade of turbulent energy in the dense gas phase introduce a delay between gas accretion and star formation, which keeps galaxy growth inefficient in the early Universe. The main results presented in this paper, such as stellar mass functions, are available in the GALAKSIENN library.

Evolutionary models of cold and low-mass planets: cooling curves, magnitudes, and detectability

Context.Future instruments like the Near Infrared Camera (NIRCam) and the Mid Infrared Instrument (MIRI) on theJames WebbSpace Telescope (JWST) or the Mid-Infrared E-ELT Imager and Spectrograph (METIS) at the European Extremely Large Telescope (E-ELT) will be able to image exoplanets that are too faint (because they have a low mass, and hence a small size or low effective temperature) for current direct imaging instruments. On the theoretical side, core accretion formation models predict a significant population of low-mass and/or cool planets at orbital distances of ~10–100 au.Aims.Evolutionary models predicting the planetary intrinsic luminosity as a function of time have traditionally concentrated on gas-dominated giant planets. We extend these cooling curves to Saturnian and Neptunian planets.Methods.We simulated the cooling of isolated core-dominated and gas giant planets with masses of 5M⊕–2M♃. The planets consist of a core made of iron, silicates, and ices surrounded by a H/He envelope, similar to the ice giants in the solar system. The luminosity includes the contribution from the cooling and contraction of the core and of the H/He envelope, as well as radiogenic decay. For the atmosphere we used grey,AMES-Cond,petitCODE, andHELIOSmodels. We considered solar and non-solar metallicities as well as cloud-free and cloudy atmospheres. The most important initial conditions, namely the core-to-envelope-mass ratio and the initial (i.e. post formation) luminosity are taken from planet formation simulations based on the core accretion paradigm.Results.We first compare our cooling curves for Uranus, Neptune, Jupiter, Saturn, GJ 436b, and a 5M⊕planet with a 1% H/He envelope with other evolutionary models. We then present the temporal evolution of planets with masses between 5M⊕and 2M♃in terms of their luminosity, effective temperature, radius, and entropy. We discuss the impact of different post formation entropies. For the different atmosphere types and initial conditions, magnitudes in various filter bands between 0.9 and 30 micrometer wavelength are provided.Conclusions.Using blackbody fluxes and non-grey spectra, we estimate the detectability of such planets with JWST. We found that a 20 (100)M⊕planet can be detected with JWST in the background limit up to an age of about 10 (100) Myr with NIRCam and MIRI, respectively.