THE SOLAR RESOURCE: PART I MINES ParisTech Center Observation, Impacts, Energy (Tel.: +33 (0) )

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1 MASTER REST Solar Resource Part I THE SOLAR RESOURCE: PART I MINES ParisTech Center Observation, Impacts, Energy philippe.blanc@mines-paristech.fr (Tel.: +33 (0) ) MASTER REST Solar Resource Introduction 2 Center Observation, Impacts, Energy Department Energy and Process of MINES ParisTech Scientific object: Development and application of methods for estimating and representing geophysical parameters and other information, for energy (i.e., solar, wind, hydro, biomass, ) Based on: Remote sensing and digital geography Applied Mathematics Information technologies Physics (metrology, meteorology, wave-matter interactions ) MINES ParisTech 1

2 MASTER REST Solar Resource Part I 3 Introduction Main research topics related to energy Meteorology for energy Evaluation of energy resources: solar, offshore wind Construction of databases of geophysical and meteorological parameters for solar and wind energy Mapping of geophysical and meteorological parameters Metrology for experimentation Life Cycle Analysis, Environmental Impacts Dissemination of information through the web ( project.mesor.net) 4 Summary and goals of the course Fundamentals for Solar Radiation Energy Analysis of the solar radiation variations Why the solar radiation is not uniform over the Planets What is its temporal evolution (short, medium and long terms) Modeling of surface solar radiation The basis for the characterization of downwelling surface solar radiation (ground- and satellite- based) Different uses for PV and CSP applications Bankable datasets TMY Solar resource forecasting MINES ParisTech 2

3 MASTER REST Solar Resource Part I 5 - SOLAR RADIATION - FUNDAMENTALS Introduction 6 Solar Energy Huge quantity of energy from the Sun ( GW) for, at least, 4 or 5 billion years Required surfaces of PV plants for the energetic need (rough order of magnitude) France World MINES ParisTech 3

4 MASTER REST Solar Resource Part I Some relevant units 7 Irradiance: incident power flux Power per area (W/m 2 ) Irradiation: incident energy flux received energy per area (J/m 2, Wh/m 2 ) (Sum of irradiance during an integration time) Note : 1 Wh/m 2 = 3600 J/m 2 These quantities can be: Spectral : spectral distribution (ex. W/m 2 /µm) Broadband or total : amount of radiation integrated over the whole spectrum Spectral distribution of the solar radiation 8 Spectral distribution of a blackbody at 5520 K IR : 0,8 < l < 10 µm Visible : 0,4 < l < 0,8 µm UV : 0,12 < l < 0,4 µm Extreme UV : 0,01 < l < 0,12 µm X-ray: 10-4 < l < 0,01 µm Gamma-ray l < 10-4 µm Energetic distribution of the TOA solar rad. 98% between 0,3 and 4 µm 8% in the UV domain 48% in the visible domain 42% in IR domain MINES ParisTech 4

5 MASTER REST Solar Resource Part I Variability of the solar radiation 9 The maximum of irradiance at the sea level is around 1000 W/m 2 and depends on: The hour of the day The day of year (Sun-Earth distance, seasons, ) The geographic localization (latitude effects, local meteorology, orography, ) The atmospherics conditions (aerosols, water vapor, cloud conditions, etc.) The orientation of the solar collectors (panels, mirrors, ) Sun-Earth astronomy 10 Distance, declination, Earth s rotation AU 1 AU 149,6 M.km (AU: Astronomical Unit) AU Source : Wikipedia MINES ParisTech 5

6 MASTER REST Solar Resource Part I Déclinaison ( ) Solar constant 11 Solar Constant : Annual mean of the broadband normal irradiance at the Top of Atmosphere (TOA) E sc = 1367 W/m 2 ± 0.1 % TOA normal Irradiance for the day of the year ddd E TOA-NI (ddd) = E sc (1 + (ddd)) 1320 W/m 2 < E TOA-NI (ddd) < 1415 W/m 2 Solar Declination 12 Solar Declination : The angle composed by the direction to the sun and the equatorial plane d Jan Feb Mar Apr May Jun Jul Aug Sep Oct Nov Dec Jan Mois MINES ParisTech 6

7 MASTER REST Solar Resource Part I Hour angle 13 = (p / 12) (TST 12) [rad] TST = 12 (1 + /p) [h] 14 S : S : S : Angular position of the Sun for a local observer solar zenith angle (SZA) solar elevation (complementary angle of the SZA) solar azimuth ( existence of different conventions) - Norm ISO19115 : from North, Eastward - 0 : towards equator, from East to West S MINES ParisTech 7

8 MASTER REST Solar Resource Part I Apparent sun position during the day 15 At latitude = 45 June 22 March 21 / September 23 December 22 Apparent sun position during the day 16 At latitude = 0 June 22 March 21 / September 23 December 22 MINES ParisTech 8

9 MASTER REST Solar Resource Part I Apparent sun position during the day 17 At latitude = 65 June 22 March 21 / September 23 December 22 Astronomical Daylength 18 MINES ParisTech 9

10 MASTER REST Solar Resource Part I Local Daylength 19 Local orographic effects (shadow effect of the local surrounding relief) 20 Time references True Solar Time (TST), Mean Solar Time (MST) True Solar Time (TST) or apparent solar time Definition: for a local observer on the Earth, the Sun is at its zenith solar noon (and crosses its local meridian) at 12 h TST. Apparent solar day (time between the crossing of the local meridian) is variable (Earth heliocentric eccentricity, declination) Mean Solar Time (MST) based (on an imaginary mean Sun) The mean solar day is 24 h For a local observer, the Sun is at its zenith at, in annual mean, 12 H MST MINES ParisTech 10

11 MASTER REST Solar Resource Part I 21 At latitude = 45 Time references Mean Solar Time (MST) Solar Azimuth / Elevation at 12:00 MST during one year 22 Time references Universal Time Legal Time The MST depends on the localization (longitude) Universal Time (common notations: UT, GMT or Z) MST at the Greenwich longitude (long. 0 ) UT1 UTC The Legal Time is defined for a country UTC + Time Zone (TZ) + Daylight Saving Time (DST) MINES ParisTech 11

12 MASTER REST Solar Resource Part I 23 Time references Universal Time Legal Time Source : Wikipedia DST observed in blue 24 Time references Determination of Mean Solar Time Earth rotation in 24 h Longitude between 0 à h corresponds to 360 / 24 = 15 1 of longitude is equivalent to 4 min (60 min / 15 ) MST(lon) = UT + lon(deg)/15 (in decimal hour) Example: à 4:30 h UT MST in Beijing (long = ) = ( ) = 12.2 h = 12:12 h MST in Santiago, Chile (long = ) = ( )=-0.2 h = 23:48 of the previous day MINES ParisTech 12

13 MASTER REST Solar Resource Part I 25 Time references True Solar Time (TST) and Mean Solar Time (MST) The Earth heliocentric orbit is approx. an ellipse Earth s angular speed not constant The Sun is not at its zenith at 12 h MST but only as a mean Note: The time difference is less than 17 min For a local observer, the difference between MST and TST is different, approx. day by day: This difference is the Equation of Time TST(j) MST(j) sin(j-2.8π/180) sin(2j+ 19.7π/180) j = 2π(ddd/ ) (day angle, radian) Time references Equation of Time 26 MINES ParisTech 13

14 MASTER REST Solar Resource Part I Angles for tilted plans 27 cos i = cosb cos S + sin b sin S cos( S - ) i β : slope or tilt of the plan (0: horizontal, p/2: vertical) α : azimuth of the plan ( same convention as S ) i : Incident angle of the Sun rays b = 0 i = S =p/2- S 28 Example: TOA Irradiance for different locations and different tilted plans MINES ParisTech 14

15 MASTER REST Solar Resource Part I 29 Example: TOA Irradiance for different locations and different tilted plans June 21 Slope 0 December 21 Slope 0 30 Example: TOA Irradiance for different locations and different tilted plans June 21 Slope 45 December 21 Slope 45 MINES ParisTech 15

16 MASTER REST Solar Resource Part I 31 Example : effects of sun-tracking on TOA irradiation Continuous tracking of sun: Two axis: normal irradiation (cos i = 1) One axis: Slope constant, sun-tracking in azimuth Azimuth constant, sun-tracking in slope Axis North-South (alpha = 90 ) Axis East-West (alpha = 180 or 0, depending on the hemisphere) 32 Example: TOA Irradiance for different locations and different tilted plans June 21 DNI December 21 DNI MINES ParisTech 16

17 MASTER REST Solar Resource Part I 33 Example: TOA Irradiance for different locations and different tilted plans June 21 Trck-azimuth (slope 45 ) December 21 Trck-azimuth (slope 45 ) 34 Example: TOA Irradiance for different locations and different tilted plans June 21 Trck-slope N-S December 21 Trck-slope N-S MINES ParisTech 17

18 MASTER REST Solar Resource Part I 35 Example: TOA Irradiance for different locations and different tilted plans June 21 Trck-slope E-W December 21 Trck-slope E-W 36 At latitude = 45 Example : effects of sun-tracking on TOA irradiation MINES ParisTech 18

19 h h h MASTER REST Solar Resource Part I Annual sum of TOA irradiation (kwh/m 2 ) jour jour kwh/m² 3000 kwh/m² kwh/m² 2000 kwh/m² 1500 kwh/m² 1000 kwh/m² 500 kwh/m² jour Summary for the astronomical parameters relevant for the TOA irradiances 38 Important astronomical parameters : Day length Solar Zenith Angle (and Incident angle for tilted plans) Earth s heliocentric position Zonal irradiation with respect to latitude MINES ParisTech 19

20 MASTER REST Solar Resource Part I Annual sum of TOA irradiation (kwh/m 2 ) 39 Yearly sum of TOA Somme global annuelle horizontal d'irradiation irradiation globale (kwh/m hors atmosphère 2 ) (kwh/ m 2 ) kwh/m² 3000 kwh/m² 2500 kwh/m² 2000 kwh/m² 1500 kwh/m² 1000 kwh/m² 500 kwh/m² Annual sum of ground irradiation (kwh/m 2 ) Spatial variability due to atmosphere conditions 3500 kwh/m² 3000 kwh/m² 2500 kwh/m² 2000 kwh/m² 1500 kwh/m² 1000 kwh/m² 500 kwh/m² MINES ParisTech 20

21 MASTER REST Solar Resource Part I 41 Absorption: mainly Atmospheric effects on downwelling solar radiation Ozone for the UV domain (upper layers of the atm.) Water vapor: Wide and various absorption lines from 0.65 µm High absorption after 4 µm Scattering: particles that reradiates of energy of incident waves in all the direction (scattering pattern) Gas molecules (and particles of size << ): Rayleigh s law -4 Aerosol: Ångstrøm s law defining the Aerosol Optical Depth (AOD) d a = b(/ 0 ) -a ( 0 =1 µm) Clouds: water drops and ice crystals implies strong depletion Depletion modeled by the Cloud Optical Depth (COD) Source : INES ( 42 Atmospheric effects on downwelling solar radiation The resulting depletion due to absorption and scattering is called extinction MINES ParisTech 21

22 MASTER REST Solar Resource Part I 43 Atmospheric effects on solar radiation Air Mass The length of the optical path is called the Air Mass (AM) Solar Elevation Angle S AM 1/sin S At the sea level with standard atmospheric conditions The larger the AM, the stronger the extinction phenomena 44 Two scalars that synthesizes the description of radiation under clear-sky conditions (cloud free) Linke Turbidity factor (TL) Typical TL in Europe: 3 4 Cloud free Condition Linke turbidity - visibility Visibility (V) Horizontal visibility distance Very clear sky : km. Very turbid sky : < 30 km 1 V 328 sin TL S MINES ParisTech 22

23 MASTER REST Solar Resource Part I 45 Spectral irradiance under clear-sky conditions Simulation with a radiative transfer model (libradtran) TOA, SZA=32 cos(60 )/cos(32 ) 0.59 VIS = 50 km, SZA=32 TOA, SZA=60 VIS = 10 km, SZA=60 VIS = 10 km, SZA=32 Solar radiation decreases with SZA Solar radiation increases with Visibility < 0.55 µm : ozone absorption and air molecules scattering < 0.95 µm : absorption of water vapor Cloud extinction 46 Mainly scattering, including retro-scattering Isotropic Scattering Global depletion up to % Wavelength dependent Extinction depends on the Cloud Optical Depth (COD) (unitless) : 0 : no depletion 3-4 : hard to see the sun clearly through the cloud (i.e. strong depletion of the direct component) MINES ParisTech 23

24 MASTER REST Solar Resource Part I COD: 15 SZA: 32 Cloud extinction 47 Radiation components at the ground levels 48 Beam or direct component (B): Radiation coming from the Sun position. Diffuse component (D): Radiation coming from the sky, due to scattering Reflected component (R): Diffuse components from the ground (ground albedo) Global radiation G(b, ) = B (b, ) + D (b, ) + R (b, ) Note: for horizontal surface R = 0 MINES ParisTech 24

25 MASTER REST Solar Resource Part I 49 Example of direct / diffuse irradiances under clear sky conditions K d =D/G Turbidity : depletion of global and a transfer to diffuse (increase of diffuse component with turbidity) Decrease of K d with wavelength High visibility: strong decrease and B > D for short wavelength (0.35 µm) Low visibility: Kd tends to be flat, B >D for higher wavelength (0.65 µm) 50 Different solar radiation components Different systems of Solar energy conversion MINES ParisTech 25

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