Measurements Of Solar UV Radiation Research Articles

Erythemal and vitamin D weighted solar UV dose-rates and doses estimated from measurements in mainland France and on Réunion Island.

Solar UV radiation causes beneficial and detrimental changes in human health. International and national Health agencies recommend avoiding sun exposure when the solar rays are strongest (typically 2h before and after solar noon). In this study we detail and refine such recommendations. We estimated biologically-effective radiation (inductive of erythema and pre-vitamin D) using spectral solar UV radiation measurements on a horizontal plane at three French sites equipped with spectroradiometers: Villeneuve d'Ascq (VDA) (North of France); Observatoire de Haute-Provence (OHP) (French Southern Alps); and Saint-Denis de La Réunion (SDR) on Réunion Island, in the Indian Ocean. These sites are very different: VDA is a semi-urban site in a flat region, OHP a rural mountainous site and SDR a coastal urban site on a small mountainous island. Biologically active radiation was analyzed by studying erythema induction and measuring pre-vitamin D synthesis. Dose-rates, doses and times for sunburn induction and vitamin D production were derived. Regarding the level of vitamin D dose considered here (1000IU), we found that at mainland sites time required for vitamin D synthesis was relatively long, even around solar noon, in winter months this could be 2-3h for phototype II individuals exposing their face and hands. In the tropics vitamin D could always be synthesized in a reasonable time (e.g. 20min in winter). By contrast, in summer, the required duration times (exposing face, hands, arms and legs) are very short, approximately 2-4min on the mainland and 1min in the tropics for phototype II individuals. In all skin phototypes the duration of sun exposure required to induce erythema was generally longer than that to produce vitamin D. These quantitative results, obtained using an instrument measuring on a horizontal plane and with an unobstructed view, do not represent realistic values for human exposure. To account for realistic human body exposure, received doses and times of exposure were adjusted. Our study shows that, mostly in summer, the time periods where limited solar exposure is recommended should be extended, especially at low latitude locations.

Solar UV radiation measurements in Marambio, Antarctica, during years 2017–2019

Abstract. In March 2017, measurements of downward global irradiance of ultraviolet (UV) radiation were started with a multichannel GUV-2511 radiometer in Marambio, Antarctica (64.23∘ S; 56.62∘ W), by the Finnish Meteorological Institute (FMI) in collaboration with the Servicio Meteorológico Nacional (SMN). These measurements were analysed and the results were compared to previous measurements performed at the same site with the radiometer of the Antarctic NILU-UV network during 2000–2008 and to data from five stations across Antarctica. In 2017/2018 the monthly-average erythemal daily doses from October to January were lower than those averaged over 2000–2008 with differences from 2.3 % to 25.5 %. In 2017/2018 the average daily erythemal dose from September to March was 1.88 kJ m−2, while in 2018/2019 it was 23 % larger (2.37 kJ m−2). Also at several other stations in Antarctica the UV radiation levels in 2017/2018 were below average. The maximum UV indices (UVI) in Marambio were 6.2 and 9.5 in 2017/2018 and 2018/2019, respectively, whereas during years 2000–2008 the maximum was 12. Cloud cover, the strength of the polar vortex and the stratospheric ozone depletion are the primary factors that influence the surface UV radiation levels in Marambio. The lower UV irradiance values in 2017/2018 are explained by the high ozone concentrations in November, February and for a large part of October. The role of cloud cover was clearly seen in December, and to a lesser extent in October and November, when cloud cover qualitatively explains changes which could not be ascribed to changes in total ozone column (TOC). In this study, the roles of aerosols and albedo are of minor influence because the variation of these factors in Marambio was small from one year to the other. The largest variations of UV irradiance occur during spring and early summer when noon solar zenith angle (SZA) is low and the stratospheric ozone concentration is at a minimum (the so-called ozone hole). In 2017/2018, coincident low total ozone column and low cloudiness near solar noon did not occur, and no extreme UV indices were measured.

A novel efficient broadband model to derive daily surface solar Ultraviolet radiation (0.280–0.400 μm)

The climatic characteristics of solar Ultraviolet radiation (UV) are of vital important for the climate change and photochemical reactions. High-quality records of solar UV radiation are the premise for solar UV researches and applications, but solar UV radiation observations are sparse around the world. Among all wavelength of UV radiations, only UVA (0.315–0.400 nm) and UVB (0.280–0.315 nm) could reach the earth surface. This study attempted to develop a novel efficient physically broadband parameterization (hereafter, FASTUV) for estimating surface solar UV radiation (0.280–0.400 μm) in all-sky conditions based on Leckner's spectral model for calculating shortwave solar radiation, using MERRA_2 reanalysis data. The Quadratic polynomial formula and artificial neural networks were used to calculate the cloud transmittance for UV, using sunshine durations measurements at 2474 CMA stations. The surface solar UV radiation measurements at 29 CERN (The Chinese Ecosystem Research Network) stations were used for validating the estimated UV values. The result showed the FASTUV model could be used for estimating UV values with high accuracy, strong robustness and fast speed. Then, the spatial and temporal variation of surface solar UV radiation in China were revealed. The result indicated that the Qinghai Tibetan Plateau and the Palmier Plateau has always been the areas with highest UV values, while the Northeastern China is the area with the lowest UV values. Meanwhile, the FASTUV model have been packaged into a software namely ‘FASTUV_V1.0’. We provide the executable file of FASTUV model in publicly available repository: https://doi.org/10.6084/m9.figshare.11409666.

Comparative measurements of solar UV irradiation at the high-mountain stations of BEO-Moussala (BG) and NAO-Rozhen (BG)

Damaging UV radiation is an important object of investigation related to its impact on biological species. Data acquired at high-altitude stations reveal dangerous events of incident UV radiation reaching the Earth surface. Continuous multi-UV spectral measurements by open-source equipment could further deepen the knowledge of solar light propagation and the events of radiation transfer and atmospheric absorption processes. This report describes recent results on high-resolution UVA, UVB, UVC measurements of solar UV radiation at the mountain stations in Bulgaria.

Seasonal Deposition and Lifting of Dust on Mars as Observed by the Curiosity Rover

In situ measurements by the Curiosity rover provide a unique opportunity for studying the effects of dust on assets placed at the surface of Mars. Here we use in situ measurements of solar UV radiation to quantify the seasonal and interannual variability of dust accumulation on the sensor on the rover deck. We show that the amount of dust accumulated on the sensor follows a seasonal cycle, with net dust removal during the perihelion season until Ls ~ 300°, and net dust deposition until the end of the aphelion season (Ls ~ 300°–180°). We use independent in situ measurements of atmospheric opacity and pressure perturbations in combination with numerical modeling, showing that daytime convective vortices and nighttime winds are likely responsible for the seasonal dust cleaning, with the role of nighttime wind being more important in Martian Year (MY) 32 than in MY 33 and that of daytime convective vortices being more important in MY 33 than in MY 32. The fact that the UV sensor is cleaner in MY 33 than in MY 32 indicates that natural cleaning events make solar energy an excellent candidate to power extended (multiannual) Mars missions at similar latitudes as the Curiosity rover.

Агаар мандлын тунгалагжилтын коэффициентыг тооцоолох нь

The ability of the atmosphere to pass electromagnetic wave depends on the mass of air, traced rays, as well as water vapor and dust in the air. Transparency of the atmosphere varies for different wavelengths of radiation and the greater the smaller the absorption and scattering in the atmosphere. Transparency of the atmosphere can be characterized by a transmission coefficient equal to the percentage of radiation that passes through the atmosphere at the steep fall-rays, or so-called turbidity factor, which shows the extent to which the transparency of the real atmosphere in these conditions is different from a perfectly clean and dry (perfect) air. The atmospheric transparency at various points of the globe is not the same. The most transparent air into the pole regions because there it contains the smallest amount of dust and moisture. Changes in humidity and dust content of air in this paragraph for the year determines the annual variation of atmospheric transparency at this point. In this paper we define the atmospheric transmission coefficient from measurements of solar UV radiation in different parts of Mongolia.

Validation of satellite-based noontime UVI with NDACC ground-based instruments: influence of topography, environment and satellite overpass time

Abstract. Spectral solar UV radiation measurements are performed in France using three spectroradiometers located at very different sites. One is installed in Villeneuve d'Ascq, in the north of France (VDA). It is an urban site in a topographically flat region. Another instrument is installed in Observatoire de Haute-Provence, located in the southern French Alps (OHP). It is a rural mountainous site. The third instrument is installed in Saint-Denis, Réunion Island (SDR). It is a coastal urban site on a small mountainous island in the southern tropics. The three instruments are affiliated with the Network for the Detection of Atmospheric Composition Change (NDACC) and carry out routine measurements to monitor the spectral solar UV radiation and enable derivation of UV index (UVI). The ground-based UVI values observed at solar noon are compared to similar quantities derived from the Ozone Monitoring Instrument (OMI, onboard the Aura satellite) and the second Global Ozone Monitoring Experiment (GOME-2, onboard the Metop-A satellite) measurements for validation of these satellite-based products. The present study concerns the period 2009–September 2012, date of the implementation of a new OMI processing tool. The new version (v1.3) introduces a correction for absorbing aerosols that were not considered in the old version (v1.2). Both versions of the OMI UVI products were available before September 2012 and are used to assess the improvement of the new processing tool. On average, estimates from satellite instruments always overestimate surface UVI at solar noon. Under cloudless conditions, the satellite-derived estimates of UVI compare satisfactorily with ground-based data: the median relative bias is less than 8 % at VDA and 4 % at SDR for both OMI v1.3 and GOME-2, and about 6 % for OMI v1.3 and 2 % for GOME-2 at OHP. The correlation between satellite-based and ground-based data is better at VDA and OHP (about 0.99) than at SDR (0.96) for both space-borne instruments. For all sky conditions, the median relative biases are much larger, with large dispersion for both instruments at all sites (VDA: about 12 %; OHP: 9 %; SDR: 11 %). Correlation between satellite-based and ground-based data is still better at VDA and OHP (about 0.95) than at SDR (about 0.73) for both satellite instruments. These results are explained considering the time of overpass of the two satellites, which is far from solar noon, preventing a good estimation of the cloud cover necessary for a good modelling of the UVI. Site topography and environment are shown to have a non-significant influence. At VDA and OHP, OMI v1.3 shows a significant improvement with respect to v1.2, which did not account for absorbing aerosols.

Comparison of ground-based measurements of solar UV radiation at four sites on the Tibetan Plateau

We compare results for the UV index (UVI), the total ozone column (TOC), and the radiation modification factor (RMF, being 1 in the absence of clouds and aerosols) at four sites on the Tibetan Plateau. The results were obtained by analyzing ground measurements by multichannel moderate-bandwidth filter instruments for the period July 2008-September 2010, and radiative transfer modeling was used to aid the interpretation of the results. The highest UVI of 20.6 was measured in Tingri (28.7°N; 4335m). For July, monthly mean UVI values were 14.5 and 12.9 in Tingri and Lhasa (29.7°N; 3683m), respectively. Generally, the UVI levels in Tingri and Lhasa were higher than in Nagchu (31.5°N; 4510m) and Linzhi (29.7°N; 2995m), due to less cloud cover at the former two sites. In 2009, the annual mean UVI and RMF values were 6.8 and 0.7 for Linzhi, 8.8 and 0.92 for Lhasa, 10.5 and 0.92 for Tingri, and 6.7 and 0.7 for Nagchu. Radiative transfer simulations indicate that the latitude difference would correspond to an increase in the UVI of about 0.3 from Nagchu to Tingri; whereas, the altitude difference would correspond to a reduction of about 1.5%, implying that the observed difference is due to the difference in cloud cover. The annual mean TOC values were found to be 260-264 Dobson units (DU) in Lhasa, Linzhi, and Nagchu, and 252 DU in Tingri. TOC values in Lhasa were found to agree within 3% with those derived from Ozone Monitoring Instrument (OMI) measurements.

UV solar radiation on a tilted and horizontal plane: Analysis and comparison of 4years of measurements

In the global wavelength range (300–3000 nm), it is known that a plane with a slope equal to the latitude of the location, receives more annual energy than the horizontal plane, mainly due to the increase in direct irradiation on the interest plane. The UV (280–400 nm) spectra at the earth surface, has a larger component of diffuse and a minor component of direct solar radiation compared to the global wavelength range, therefore the increase in annual energy due to plane inclination should also be different. This work, analyzes 4 years of solar UV radiation measurements performed on tilted and horizontal planes located at the Plataforma Solar de Almería, Spain. The monthly mean ratio of tilted/horizontal solar UV irradiation varies with the time of the year, reaching values of 1.25 and 0.95 for winter and summer, respectively. The same ratio in the solar global spectra rises up to 1.70 and 0.85 for the same months. The annual UV solar energy increase on a plane tilted 37° and oriented towards the equator is around 3–4%, whereas is around 10% in the global spectra. In this way UV annual energy increase due to inclination and orientation of the plane is much lower than that for global radiation. Determination of a unique method to assess all possible inclinations and orientations, require simultaneous measurement of diffuse and direct UV radiation performed with radiometers of identical spectral response. Given the worldwide scarcity of these type of data, an empirical correlation that relates horizontal UV irradiation to that on a 37° inclined plane was determined. Monthly and annual tendencies of solar UV irradiation have been analyzed and compared with the solar global irradiation.

UV measurements in the 3000–5000 m altitude region in Tibet

We present measurements of solar UV radiation performed with multichannel moderate‐bandwidth NILU‐UV filter instruments during winter and summer in 2003 in the altitude region from 3000 m to 5000 m at 29°N in the Lhasa region in Tibet. During summer the UV index was found frequently to exceed 15 on clear days and occasionally to exceed 20 on partially cloudy days. High altitudes, low ozone column amounts, clean atmospheres, and relatively low latitudes are factors that contribute to the high UV levels on the Tibetan plateau. UV index values of 12 were measured in late winter for a solar zenith angle of 40° at a snow‐covered 5000 m altitude site. This is a 35% increase compared to a corresponding snow‐free surface. Our measurements show that the solar UV radiation increases with altitude. For clear‐sky and snow‐free conditions the altitude increase is 7–8% per km for erythemal UV dose rates and 3% per km at a wavelength of 340 nm. Results from clear‐sky calculations using a multiple‐scattering radiative transfer model were found to agree within 5% with clear‐sky UV measurements. Radiative transfer calculations combined with measurements were used to estimate the influence of clouds on the UV radiation at the surface. On the average the variable cloud cover in Lhasa reduced the daily integrated erythemal UV dose by 25%. The NILU‐UV instruments also provide total ozone column amounts. The mean difference between daily total ozone column amounts derived from NILU‐UV measurements and from Earth Probe TOMS data was −1.4% ± 3.2% (1σ).

Diurnal discrepancies in spectral solar UV radiation measurements

Unexpected diurnal discrepancies between high-quality spectroradiometers were observed during the 2000 Nordic Ozone Group Intercomparison campaign. The spectral ratios of the irradiances showed a diurnal variation of approximately 2-9%. This cannot be explained by the nonideal angular response of the instruments' input optics in one plane (cosine effect). Instead, by using a radiative transfer model, we show that differences in the angular response in four azimuth planes have the potential to bias the measured data by up to 4.4% (azimuth effect). Other relevant factors are also discussed and quantified and are shown to be significant when diurnal changes in radiation are explained by environmental factors, or when measured data are compared with model or satellite data. Again, intercomparison campaigns have the potential to reveal errors that would otherwise remain undetected.

Comparative measurements of solar UV radiation with spore dosimetry at three European and two Japanese sites

Spore dosimetry of solar UV radiation has been employed in several field intercomparison campaigns carried out in summer months in Japan and Europe. The dose-rate profiles, total daily doses and personal daily exposures have been determined and compared at five sites based on the spore inactivation dose (SID). The maximum dose rate (0.83 SID/min) and the maximum daily dose (197 SID) observed at subtropical Naha (26.2°N) are about three times those observed at subarctic Abisko (68.4°N). The amounts of personal exposure during three European campaigns are moderate and show a tendency of inverse relationships with the daily doses.

New Entrance Optics for Solar Spectral UV Measurements

ABSTRACTThe investigation of the impact of solar UV radiation on the biosphere requires spectral measurements of solar UV radiation of high accuracy. However, the accuracy of current measurements is limited, and this can partly be attributed to the entrance optics of the instruments used for these examinations. The angular response of spectro‐radiometers measuring spectral global UV irradiance should be given by the cosine of the incidence angle. In‐tercomparison campaigns have shown that deviations from this ideal cosine response lead to uncertainties in solar measurements of more than 10%. Here we present recently developed entrance optics that reduce these uncertainties to ±4% in the UV. The new entrance optics have been characterized with respect to their angular response, transmission, weather durability, fluorescence and dependence of the angular response on wavelength and polarization. Solar spectroradiometric measurements carried out with the new optics were compared with simultaneously performed measurements of a second spectroradiometer that was equipped with a conventional diffuser. The deviations of up to 12% between both systems are quantitatively explained to within 3%.

Detailed analysis of solar ultraviolet radiation: a preliminary investigation on data collected at Rome (‘La Sapienza’ University)

The importance of solar ultraviolet radiation and its impact on human health is well known by the scientific community. Variations of the ozone layer can influence the UV radiation reaching the Earth's surface, especially at short wavelengths. Thus, it is important to study any possible ozone fluctuations. At the Physics Department, University of Rome, a Brewer spectrophotometer MKIV is located and is used to measure total ozone and UV flux in the 290–325 nm region with a resolution of 0.5 nm. Measurements of damaging ultraviolet radiation (DUV), defined as the incident radiation weighted against an action spectrum which relates the sensitivity of the human body to UV radiation, are also processed. This work is a preliminary investigation on the spectral solar UV radiation measurements performed at Rome during the years 1992/1993.

Spectral measurements of solar UVB radiation and its relations to total ozone, SO2, and clouds

Spectral solar UV radiation measurements performed at Thessaloniki, Greece (40°N), are presented, and the influence of various atmospheric constituents such as total ozone, cloud cover, and columnar SO2 on these measurements is examined. By comparing UV radiation measurements at days with different total ozone amounts the magnification factor was calculated. Its values range from 1 to 20, depending on the wavelength and the total ozone. A relationship between the UV radiation and the cloud cover was established, being representative only for measurements at 50° solar zenith angle. In addition, the influence of columnar SO2 variations on UV irradiances was also studied. Finally, an attempt was made to compare the relative influence of these parameters on UV radiation, which proved that total ozone is the major factor controlling the solar UVB radiation received at the ground.

Solar UV radiation measurements at potsdam (52°22′N, 13°5′E)

The UV instruments described in part I of this paper have been applied for measurements of solar global UV radiation in three different wavelength regions (310–320 nm, 315–391 nm, and 296–388 nm). UV radiation values obtained since 1985 are analyzed. Different types of regression equations were compared as to how much information on UV radiation is contained in total global radiation measurements (400–2800 nm). Applying those regression equations allows us to estimate UV radiation from measurements of total global radiation, which are readily available.

Solar UV irradiance and some biological consequences: Bombay, India

Measurements of solar UV radiation (UVR) at Bombay, India, lattitude 18.5 North and longitude 72.5 East were recorded using Eppley UV radiometer for a 2-year period. The UV irradiance is calculated and presented. The annual and diurual trends in the quantitation of UVR are examined. The consequences of solar UVR and its projected increase are discussed with special reference to its biological effects and results of UVR on experimental animal systems vis a vis and epidemiological data in the Indian context.

Solar radiation in the extreme ultraviolet and its variation with solar rotation

Solar UV radiation measurements by OSO-3, obtaining flux variation over solar rotation period