Solar Value Research Articles

Variation of the low-mass end of the stellar initial mass function with redshift and metallicity

Abstract We report the stellar mass functions obtained from 20 radiation hydrodynamical simulations of star cluster formation in 500 M⊙ molecular clouds with metallicities of 3, 1, 1/10 and 1/100 of the solar value, with the clouds subjected to levels of the cosmic microwave background radiation that are appropriate for star formation at redshifts z = 0, 3, 5, 7, and 10. The calculations include a thermochemical model of the diffuse interstellar medium and treat dust and gas temperatures separately. We find that the stellar mass distributions obtained become increasingly bottom light as the redshift and/or metallicity are increased. Mass functions that are similar to a typical Galactic initial mass function are obtained for present-day star formation (z = 0) independent of metallicity, and also for the lowest-metallicity (1/100 solar) at all redshifts up to z = 10, but for higher metallicities there is a larger deficit of brown dwarfs and low-mass stars as the metallicity and redshift are increased. These effects are a result of metal-rich gas being unable to cool to as lower temperatures at higher redshift due to the warmer cosmic microwave background radiation. Based on the numerical results we provide a parameterisation that may be used to vary the stellar initial mass function with redshift and metallicity; this could be used in simulations of galaxy formation. For example, a bottom-light mass function reduces the mass-to-light ratio compared to a typical Galactic stellar initial mass function, which may reduce the estimated masses of high-redshift galaxies.

The ESO SupJup Survey V: exploring atmospheric variability and orbit of the super-Jupiter AB Pictoris b with CRIRES+

ABSTRACT A growing number of directly-imaged companions have been recently characterized, with robust constraints on carbon-to-oxygen ratios and even isotopic ratios. Many companions and isolated targets have also shown spectral variability. In this work, we observed the super-Jupiter AB Pictoris b across four consecutive nights using VLT/CRIRES+ as part of the ESO SupJup survey, exploring how the constraints on chemical composition and temperature profile change over time using spectral line shape variations between nights. We performed atmospheric retrievals of the high-resolution observations and found broadly consistent results across all four nights, but there were differences for some parameters. We clearly detect H$_2$O, $^{12}$CO, and $^{13}$CO in each night, but abundances varied by ${\sim} 2\sigma$, which was correlated to the deep atmosphere temperature profiles. We also found differences in the $^{12}$C$/^{13}$C ratios in each night by up to ${\sim} 3\sigma$, which seemed to be correlated with the cloud deck pressure. Our combined retrieval simultaneously analysing all nights together constrained broadly the average of each night individually, with the C/O$=0.59\pm 0.01$, consistent with solar composition, and $^{12}$C$/^{13}$C $= 102\pm 8$, slightly higher than the Interstellar Medium (ISM) and Solar System values. We also find a low projected rotational velocity, suggesting that AB Pictoris b is either intrinsically a slow rotator due to its young age or that the spin axis is observed pole-on with a ${\sim} 90^\circ$ misalignment with its orbit inclination. Future observations will be able to further explore the variability and orbit of AB Pictoris b as well as for other companions.

Comparative Analysis of Geospatial Tools for Solar Simulation

ABSTRACTThis paper performs, describes, and evaluates a comparison of seven software tools (ArcGIS Pro, GRASS GIS, SAGA GIS, CitySim, Ladybug, SimStadt, and UMEP) to calculate solar irradiation. The analysis focuses on data requirements, software usability, and accuracy simulation output. The use case for the comparison is solar irradiation on building surfaces, in particular on roofs. The research involves collecting and preparing spatial and weather data. Two test areas—the Santana district in São Paulo, Brazil, and the Henio rural area in Raalte, the Netherlands—were selected. In both cases, the study area encompasses the vicinity of a weather station. Therefore, the meteorological data from these stations serve as ground truth for the validation of the simulation results. We create several models (raster and vector) to meet the diverse input requirements. We present our findings and discuss the output from the software tools from both quantitative and qualitative points of view. Vector‐based simulation models offer better results than raster‐based ones. However, they have more complex data requirements. Future research will focus on evaluating the quality of the simulation results on vertical and tilted surfaces as well as the calculation of direct and diffuse solar irradiation values for vector‐based methods.

24% Efficient TOPCon-based back contacted polyZEBRA solar cells

This publication serves as an update on the progress of the back contacted polyZEBRA solar cell technology, which features Tunnel Oxide Passivating Contact (TOPCon) structures on both polarities. The solar cell efficiency mean values published by the end of last year have been improved by +1%abs to 24.0%. Following the key parameter changes, it is discussed how this improvement has been achieved. These changes are in particular the cell thickness and base resistivity, a dedicated wet-chemical cleaning step, the rear AlOx capping layer thickness and the pitch of the rear metallization pattern.

Determining the absolute chemical abundance of nitrogen and sulfur in the quasar outflow of 3C298

Context. Quasar outflows are key players in the feedback processes that influence the evolution of galaxies and the intergalactic medium. The chemical abundance of these outflows provides crucial insights into their origin and impact. Aims. We determine the absolute abundances of nitrogen and sulfur and the physical conditions of the outflow seen in quasar 3C298. Methods. We analyzed archival spectral data from the Hubble Space Telescope for 3C298. We measured the ionic column densities from the absorption troughs and compared the results to photoionization predictions made with the Cloudy code for three different spectral energy distributions (SEDs), including MF87, UV-soft, and HE0238 SEDs. We also calculated the ionic column densities of the excited and ground states of N III to estimate the electron number density and location of the outflow using the Chianti atomic database. Results. The MF87, UV-soft, and HE0238 SEDs yield nitrogen and sulfur abundances at supersolar, solar, and subsolar values, respectively, with a spread of 0.4–3 times solar. Additionally, we determined an electron number density of log(ne)≥3.3 cm−3, and the outflow might extend up to a maximum distance of 2.8 kpc. Conclusions. Our results indicate a solar metallicity within an uncertainty range of 60% that is driven by variations in the chosen SED and photoionization models. This study underscores the importance of the SED impact on determining chemical abundances in quasar outflows. These findings highlight the necessity of considering a wider range of possible abundances that span from subsolar to supersolar values.

A comparison between the ocean and offshore photovoltaic production system into microgrids: benefits and limits

The current work offers a detailed comparison of the advantages and disadvantages of microgrids concerning the developments of photovoltaic (PV) production installed near the shore and those installed offshore. As demand for renewable energy increases, integrating offshore and marine photovoltaic systems offers a promising approach to increase energy production while minimizing land use. This study explores the inherent advantages of offshore photovoltaic systems, including higher energy production due to the cooling effect of water, reduced reliance on land, and the ability to tap into sustained marine solar resources. On the other hand, this paper also addresses challenges associated with these systems, such as: B. Increased installation complexity, vulnerability to harsh ocean conditions, and potential impacts on marine ecosystems. The results in this paper show good performance for both offshore and floating PV systems, except that the offshore PV system excels over the other system by 3.13% in energy production. Moreover, the difference in the annual efficiency of the two PV systems reached 0.55%. These values are considered low because both systems are installed in water, given that both systems benefit from lower temperature and solar irradiation values. Nevertheless, these two systems equally present their own unique challenges including, but not limited to, operational and maintenance cost increase, effect on marine ecology and the technical hindrances on installation and grid interconnectivity. The aim of this review is to disentangle the achievements made regarding the current state of the art in floating photovoltaic technologies. When dealing with performance metrics, two solutions are examined in order to demonstrate the feasibility of providing the energy needs in an ecological way.

VLTI/GRAVITY Observations of AF Lep b: Preference for Circular Orbits, Cloudy Atmospheres, and a Moderately Enhanced Metallicity

Direct imaging observations are biased toward wide-separation, massive companions that have degenerate formation histories. Although the majority of exoplanets are expected to form via core accretion, most directly imaged exoplanets have not been convincingly demonstrated to follow this formation pathway. We obtained new interferometric observations of the directly imaged giant planet AF Lep b with the VLTI/GRAVITY instrument. We present three epochs of ∼50 μas relative astrometry and the K-band spectrum of the planet for the first time at a resolution of R = 500. Using only these measurements, spanning less than 2 months, and the Hipparcos-Gaia Catalogue of Accelerations, we are able to significantly constrain the planet’s orbit; this bodes well for interferometric observations of planets discovered by Gaia DR4. Including all available measurements of the planet, we infer an effectively circular orbit (e < 0.02, 0.07, and 0.13 at 1σ, 2σ, and 3σ, respectively) in spin–orbit alignment with the host and measure a dynamical mass of M p = 3.75M Jup ± 0.5M Jup. Models of the spectrum of the planet show that it is metal-rich ([M/H] = 0.75 ± 0.25), with a C/O abundance encompassing the solar value. This ensemble of results shows that the planet is consistent with core accretion formation.

A spectrophotometric analysis and dust properties of classical nova V5584 Sgr

ABSTRACT In this work, optical observations of the nova V5584 Sgr are presented. These observations cover different phases including pre-maximum, early decline, and nebular. The spectra are dominated by hydrogen Balmer, Fe ii, and O i lines with P-Cygni profiles in the early phase, which are subsequently observed in complete emission. The presence of numerous Fe ii lines and low ejecta velocity aligns with the Fe ii type nova classification. From optical and NIR colours, it is clear that this nova manifests dust formation in the ejecta. The dust temperature and mass were estimated from a spectral energy distribution (SED) fit to the JHK band magnitudes and the Wide field Infrared Survey Explorer data. Light-curve analysis shows t$_2$ and t$_3$ values of $\sim$ 26 and $\sim$ 48 d, classifying the nova as moderately fast. The physical and chemical properties during early decline and later phases were evaluated using the photoionization code CLOUDY. The best-fitting model parameters from two epochs of multiwavelength spectra are compatible with a hot white dwarf source with a roughly constant luminosity of $\sim$(2.08 $\pm$ 0.10) $\times$ 10$^{36}$ erg s$^{-1}$. We find an ejected mass of $\sim$(1.59 $\pm$ 0.04) $\times$ 10$^{-4}$ M$_{\odot }$. Abundance analysis indicates that the ejecta is significantly enriched relative to solar values, with O/H = 30.2, C/H = 10.8, He/H = 1.8, Mg/H = 1.68, Na/H = 1.55, and N/H = 45.5 in the early decline phase, and O/H = 4.5, Ne/H = 1.5, and N/H = 24.5 in the nebular phase.

Numerical Analysis of the Heat and Mass Transfer in a Ventilated Cavity for Turbulent Convective Flow With Extreme Hot and Humid Climate Conditions

ABSTRACTTo analyze the temperature and relative humidity (RH) in a room located in the Lacandona jungle in Chiapas, Mexico, a numerical heat and mass transfer study was performed. The study was carried out in a ventilated cavity, by introducing air flow into user‐occupied spaces. The study analyzed the combination of temperature and humidity percentage to create thermal comfort conditions. The finite volume method was used to solve the governing equations, while pressure–velocity coupling was done with the SIMPLEC algorithm. Turbulent airflow was considered, and modeled using the k–ε turbulence model, with Reynolds numbers (Re) in the range from 100 to 5000. Seven sets of weather conditions were considered for a warm April day with solar radiation values that ranged from 0 to 981 W/m², outdoor temperatures between 19.9°C and 35.3°C, as well as RH from 42% up to 100%. The study analyzed temperature, RH, distribution efficiencies, and heat fluxes. It was found that the average temperature closest to thermal comfort was 25.8°C. This corresponds to an Re = 5000, being the best hygrothermal conditions with an average RH of 50%. However, this level of RH is unattainable by many air conditioning systems.

General Models for Monthly Average Daily Global Solar Irradiation

With the world’s growing demand for electricity and the crucial need to reduce greenhouse gas emissions, it’s more important than ever to develop renewable energies, particularly solar power. The study carried out in this document is in line with the same principle, i.e. to improve the exploitation of solar energy. Its aim is to develop a mathematical model for mean monthly daily global solar irradiation that is independent of measurement data and suitable for all sites worldwide. For this study, we used daily global solar irradiation data for a horizontal surface. These data are from 60 sites worldwide and cover the period from 2000 to 2023. To examine the quality of the models established in the document, we carried out an investigation into performance tools. We have presented two, including MAPE (Mean Absolute Percentage Error) and Pearson’s correlation coefficient. Based on the daily global solar irradiance data from the 60 sites, the empirical model of extraterrestrial daily solar irradiance, and computational tools, we have formulated mathematical expressions of solar irradiance. It has the particularity of being independent of measurement data such as the duration of the day and temperature of the sites. It requires only the latitudes of the locations to estimate the solar potential values of the sites. A study of the performance of the established model showed that the model of monthly mean daily global solar irradiation values has fairly acceptable accuracy and fairly good correlation.

Chemical enrichment in LINERs from MaNGA. I. Tracing the nuclear abundances of oxygen and nitrogen in LINERs with varied ionizing sources

The chemical enrichment in low-ionization nuclear emission-line regions (LINERs) is still an issue with spatial resolution spectroscopic data because we lack studies and because the nature of their ionizing source is uncertain, although they are the most abundant type of active galaxies in the nearby Universe. Considering different scenarios for the ionizing source (hot old stellar populations, active galactic nuclei, or inefficient accretion disks), we analyze the implications of these assumptions to constrain the chemical content of the gas-phase interstellar medium. We used a sample of 105 galaxies from the survey called Mapping Nearby Galaxies at Apache Point Observatory (MaNGA), whose nuclear central spaxels show LINER-like emission. For each scenario we considered, we built a grid of photoionization models (4928 models for each considered ionizing source) that were later used in the open-source code HII-CHI-Mistry . This allowed us to estimate chemical abundance ratios such as 12+log(O/H) or log(N/O) and to constrain the ionization parameters that characterize the ionized interstellar medium in these galaxies. The oxygen abundances in the nuclear region of LINER-like galaxies are spread over a wide range 8.08 $&lt;$ 12+log(O/H) $&lt;$ 8.89, with a median solar value (in agreement with previous studies) when models for active galactic nuclei are considered. Nevertheless, the nitrogen-to-oxygen ratio we derived is much less affected by the assumptions on the ionizing source and indicates suprasolar values (log(N/O) = -0.69). By comparing the different scenarios, we show that if hot old stellar populations caused the ionization of the interstellar medium, a complex picture (e.g., outflows and/or inflows that scale with the galaxy chemical abundance) would be needed to explain the chemical enrichment history, whereas the assumption of active galactic nucleus activity is compatible with the standard scenario that is found in most galaxies.

Composição química de revestimentos frios e a influência na refletância solar e emitância térmica

Abstract Cool materials have higher values of solar reflectance and lower values of thermal emittance, although still high when compared to conventional coatings, thus, their surfaces are less heated. In this regard, the goal was to identify the chemical elements present on cool surfaces that influence solar reflectance and thermal emittance. To this end, the spectral reflectance and the thermal emittance were measured with methods and equipment standardized by the Cool Roof Rating Council (CRRC) of 23 elastomeric cool coatings commercialized in the Brazilian market, and the chemical composition of the surfaces with EDS (Energy-dispersive X-ray detector) coupled to the field emission scanning electron microscope (FE-SEM) was analyzed. The presence of the metallic chemical element (titanium) in greater quantities on the surfaces was not decisive for lower thermal emittance values. The surfaces of materials with lower carbon and higher oxygen content have higher near infrared and solar reflectance. Therefore, surfaces with a matte finish have higher solar reflectance values because of the higher ratio of pigments in relation to resin than those with a glossy finish, which are mistakenly associated with higher reflectance due to its high surface gloss.

Metal-strong Inflows at the Outer-galactic-scale of a Quasar

We present an analysis of the absorption-line system in the Very Large Telescope/Ultraviolet and Visual Echelle Spectrograph spectrum at a redshift of z a = 3.1448 associated with the quasar SDSS J122040.23+092326.96, whose systematic redshift is z e = 3.1380 ± 0.0007, measured from the Hβ+[O iii] emission lines in our newly acquired NIR P200/TripleSpec data. This absorbing system, detected in numerous absorption lines, including the N v, N iii, C iv, C iii, Si iv, Si iii, and H i Lyman series, can be resolved into seven kinematic components with redshifted velocities ranging from 200 to 900 km s−1. The high-ionization N v doublet detected and the rather narrow Lyman series measured (b ≈ 14 km s−1) suggest that the absorption gas is photoionized, possibly by the quasar. A low density is inferred by the fact that N iii λ989.80 is significantly detected while N iii*λ991.57 ( lognc=3.3cm−3 ) is undetectably weak. A firm lower limit of a solar value to the abundance of the gas can be set based on the measurements of Si iv and H i column densities, as first proposed by F. Hamann. Detailed photoionization simulations indicate that T1, and possibly the absorber as a whole, has metallicities of Z ∼ 1.5 − 6.0 Z ☉, and is located at ∼15 kpc from the quasar nucleus. The metal-strong absorption inflows at the outskirt of the quasar host galaxy most likely originated in situ and were driven by stellar processes, such as stellar winds and/or supernova explosions. Such a relatively rare system may hold important clues to understanding the baryonic cycling of galaxies, and more cases could be picked out using relatively strong Si iv and weak Lyman absorption lines.

The Hubble Constant Anchor Galaxy NGC 4258: Metallicity and Distance from Blue Supergiants

A quantitative spectroscopic study of blue supergiant stars in the Hubble constant anchor galaxy NGC 4258 is presented. The non-LTE analysis of Keck I telescope LRIS spectra yields a central logarithmic metallicity (in units of the solar value) of [Z] = −0.05 ± 0.05 and a very shallow gradient of −(0.09 ± 0.11) r/r 25 with respect to galactocentric distance in units of the isophotal radius. Good agreement with the mass–metallicity relationship of star-forming galaxies based on stellar absorption line studies is found. A comparison with H ii region oxygen abundances obtained from the analysis of strong emission lines shows reasonable agreement when the M. Pettini & B. E. J. Pagel calibration is used, while the D. Zaritsky et al. calibration yields values that are 0.2–0.3 dex larger. These results allow us to put the metallicity calibration of the Cepheid period–luminosity relation in this anchor galaxy on a purely stellar basis. Interstellar reddening and extinction are determined using Hubble Space Telescope and JWST photometry. Based on extinction-corrected magnitudes, combined with the stellar effective temperatures and gravities we determine, we use the flux-weighted gravity–luminosity relationship to estimate an independent spectroscopic distance. We obtain a distance modulus m − M = 29.38 ± 0.12 mag, in agreement with the geometrical distance derived from the analysis of the water maser orbits in the galaxy’s central circumnuclear disk.

Solar-optical and thermal behavior of photochromic glazing: Small-scale testing under real sky conditions

The poor performance of conventional building glazing, which is usually responsible for large climatization needs and glare problems, has been promoting the development of innovative smart glazing technologies with an improved performance. Photochromic glazing, a type of smart glazing, exhibits a dynamic behavior by darkening/bleaching in reaction to the presence/absence of solar radiation. The aim of this study is to evaluate the thermal and solar-optical behavior of a photochromic filmed clear glazing, against the same glazing without film, through experimental tests. The transmittance and reflectance spectra of the glazing solutions were initially measured with a spectrophotometer. Then two small-scale models were used to assess the behavior of the glazing solutions under real sky conditions (clear and overcast). The thermal behavior was assessed through air and surface temperature measurements. The solar-optical behavior was investigated through solar radiation and illuminance measurements, which were also used to compute the solar and visible transmittance of the glazing systems, respectively. The dynamic behavior of the photochromic film resulted on a reduction of 14 % of the interior temperature. Interior illuminance and irradiance levels were significantly reduced with the film, corresponding to 10–50 % and 15–35 % visible and solar transmittance values of the photochromic glazing, respectively.

Multi-criteria decision-making optimization of a two-staged solar power plant for low radiation zone through the social decision units

The effective use of renewable energy has been the most common problem of the last few years. The optimal designs of renewable energy systems are the most crucial issue among these problems. However, the optimal points can differ according to the perspectives. In this study, the effects of the different social aspects were investigated on the optimal design of the two-staged solar power plant operating under low solar radiation. In this regard, three social perspectives were handled to optimize the design parameters, including investor, engineering and consumer sights. Thus, different system designs were formed considering different thermodynamical parameters, solar radiation values, and working fluids. The formed designs were then thermodynamically analyzed through energy and exergy methods and economically analyzed through the net present value (NPV) method to obtain the input and output values to determine the optimal points. Finally, the efficiency analysis technique with output satisficing (EATWOS) analysis was handled for three different social aspects to make a decision on the optimal system. The social aspects were included in the optimization through the analytical hierarchic process (AHP) for inputs and outputs. The results show that the social perspectives have essential effects on the optimal designs of the energy systems. As a result, the system’s energy and exergy efficiency for the investor basis were determined as 20.88 % and 22.42 %, respectively. This system can produce 93.55 MW of power generation with a profit of 103 million US$ at the end of 20 years. The system’s energy and exergy efficiency for the engineering basis were determined as 20.56 % and 22.08 %, respectively. This system can produce 71.17 MW of power generation with a profit of 80 million US$. The system’s energy and exergy efficiency for the consumer basis were determined as 19.65 % and 21.09 %, respectively. This system can produce 88.03 MW of power generation with a profit of 92 million US$.

Production Performance and Cost Analysis of 60 Kwp Grid-Connected Photovoltaic System in Ayaş

The Ankara University Ayaş Horticulture Research and Application Station was chosen as the study area for this investigation. It is situated in the Uğurçayırı neighborhood of Ayaş district, in the center of the districts of Ayaş, Güdül, Beypazarı, and Polatlı. Saplings, vegetables, fruits, clover, medicinal, and spice plants are all produced on the 406-hectare land. The analysis employed a variety of solar energy potential sources, including Ayaş, GEPA (2023), MGM HELİOSAT (2021), PVGIS (2021), IRENA (2021), Solar Med Atlas (2021), NASA SSE (2021), SOLARGIS (2019), Global Solar Atlas, and NREL data. In addition, the design cost of a 60 kW photovoltaic system connected to the grid in Ayaş and the daily average/annual total production values according to months were calculated, taking into account the installed solar energy capacity and production values of the Ministry of Energy in the area. Ayaş's annual solar radiation is 1628 kWh/m2. The average daily electricity production is 252 kWh, and the total annual production is 91980 kWh. A 60 kW PV system's installation cost is 50150 USD. The system has a six-year repayment period. Furthermore, the PV system will mitigate 59.7 kilograms of CO2 emissions annually.

Photovoltaic Integrated Shading Devices in the Retrofitting of Existing Buildings on Chinese Campuses Within a Regional Context

Retrofitting existing buildings to be more energy-efficient is a tremendous contribution to the sustainability of society. The application of photovoltaic integrated shading devices (PVSDs) accords with this ambition by blocking out unwanted radiant heat gain and generating clean electricity. The deployment of PVSDs needs sensible design strategies to optimize the production of renewable energy while retaining the aesthetic quality of the built-up environment, especially in historic campuses. The concept was tested in a case study of buildings in South China University of Technology (SCUT) using Ladybug 1.4.0 and PVsyst 7.2, utilizing the existing “Xia’s shading” design method in historical environments and optimizing the design from the perspective of photovoltaic performance. Firstly, the photovoltaic (PV) panels were integrated as architectural components, and the parameters were incorporated into a mathematical equation based on “Xia’s shading” design method. This was followed by the assessment of the solar energy harvesting potential based on simulated annual solar irradiation values. Lastly, the PV panels’ solar irradiation potential under these different parameters was shown in figures to identify the optimum parameters combination for PVSD applications. The proposed methodology could evolve as a design tool and thus further assist in promoting the large-scale adoption of PVSDs in retrofit projects.

Development of New Models Using Empirical Modeling of Global Solar Radiation and Its Application in Usak City, Turkey

With this study, 12 empirical models in the literature, 2 new models developed within the scope of this study, SARAH and CMSAF satellite-based models, COSMO and ERA5 re-analysis solar radiation data sets in the PVGIS database were compared in order to detect the monthly average global solar radiation coming to the horizontal plane of Usak province. New models developed within the scope of the study; it uses the region's temperature, cloudiness coefficient and sunset hour angle. In comparison of the datas within the scope of the study; coefficient of determination (R²), mean percent error (MPE), deviation error (MBE), root mean square error (RMSE), absolute relative error (ARE) parameters were used. As a result of the evaluations, the method that most successfully predicts the global solar radiation values of Usak province was tried to be determined. According to the monthly evaluation of the models; It was determined that 14 models and satellite-based systems have absolute relative error values below 5% in March-April-May-June, September-October and December. The most accurate estimates were realized for May in 16 of 18 different estimation methods used in the study. The coefficient of determination of empirical models and PVGIS data sets was above 0.97. When the success of the models was evaluated according to the RMSE values, It was determined that the logarithmic based Model 14 (0.90058 RMSE, 0.98327 R2, -1.079894 MPE, -0.05033 MBE, 0.185628 t) which was obtained by using the sunset hour angle and the max-min temperature difference developed within the scope of this study, made the most accurate estimations. COSMO data from spatial data (1.053134 RMSE, 0.979036 R2, -1.196348 MPE, -0.25105 MBE, 0.8141 t) made successful estimations, but the accuracy of the COSMO data was lower than the data estimated by Model 14. It was concluded that used the models and satellite-based systems were generally successful. As a result, In the studies to be carried out for the global solar radiation forecast of Usak province. It has been concluded that Model 14 developed within the scope of the study can be used in precise calculations and COSMO data from PVGIS datas can be used in more superficial or pre-feasibility studies.

Evidence for Type Ib/c Origin of the Supernova Remnant G292.0+1.8

Circumstellar material (CSM) produced by mass loss from massive stars (≳10 M ⊙) through strong stellar winds or binary stripping provides rich information for understanding progenitors of core-collapse supernova remnants. In this paper we present a grating spectroscopy of a Galactic SNR G292.0+1.8, which is claimed to be a Type Ib/c remnant in a binary system according to recent studies. If G292.0+1.8 had experienced a strong mass-loss via binary interactions before its explosion, an oxygen-rich material produced in the He-burning layer is expected to be observed in the central belt-like structure formed by shock-heated CSM. Using the Reflection Grating Spectrometer onboard XMM-Newton, we detect N vii Lyα line (0.50 keV) for the first time in G292.0+1.8 and find that the abundance ratio of nitrogen to oxygen is significantly lower (N/O = 0.5 ± 0.1) than the solar value. This low N/O suggests that the progenitor of G292.0+1.8 experienced strong mass-loss and ended up as a Wolf–Rayet star exposing the He-burning layer at the presupernova. Comparing our result and the evolution models of single stars and binaries, we conclude that the progenitor of G292.0+1.8 experienced strong enough mass-loss to occur a Type Ib/c supernova. Our finding is another crucial piece of evidence for a stripped-envelope supernova such as Type Ib/c as the origin of G292.0+1.8.