man/man1/gendaylit.1

.\" RCSid "$Id: gendaylit.1,v 1.2 2009/06/06 20:22:49 greg Exp $"
.TH GENDAYLIT 1 4/12/94 "RADIANCE ISE/ADEME EXTENSIONS"
.SH NAME
gendaylit - generates a RADIANCE description of the daylight sources using Perez models for direct and diffuse components
.SH SYNOPSIS
.B "gendaylit month day hour [-P|-W|-L|-G|-E] input_value(s) "
[
.B options
]
.br
.B "gendaylit -ang altitude azimuth [-P|-W|-L|-G|-E] input_value(s) "
[
.B options
]
.SH DESCRIPTION
.I Gendaylit
produces a RADIANCE scene description based on an angular distribution of the
daylight sources (direct+diffuse) for the given atmospheric conditions 
(direct and diffuse component of the solar radiation), date and
local standard time. The default output is the radiance of the sun (direct) and the sky (diffuse)
integrated over the visible spectral range (380-780 nm). We have used the
calculation of the sun's position and the ground brightness models which
were programmed in
.I gensky.                                              

The diffuse angular distribution is calculated using the Perez et al.
sky luminance distribution model (see Solar Energy Vol. 50, No. 3, pp. 235-245, 1993) which, quoting Perez,
describes "the mean instantaneous sky luminance angular distribution patterns for all sky
conditions from overcast to clear, through partly cloudy, skies". The correctness of the 
resulting sky radiance/luminance values in this simulation is ensured through the normalization of the modelled 
sky diffuse to the measured sky diffuse irradiances/illuminances.

As described below, the radiation can be defined with the pairs direct-normal and diffuse-horizontal irradiance
(-W option), direct-horizontal and diffuse-horizontal irradiance (-G option), direct-normal and diffuse-horizontal
illuminance (-L option) or global-horizontal irradiation alone (-E option). The direct-normal radiation
is understood here as the radiant flux coming from the sun and an area of approximately 3 degrees around the sun
(World Meteorological Organisation specifications for measuring the direct radiation.
The aperture angle of a pyrheliometer is approximately 6 degrees). 
To simplify the calculations for the direct radiation, the sun is represented as a disk and no   
circumsolar radiation is modelled in the 3 degrees around the sun. This means that
all the measured/evaluated direct radiation is added to the 0.5 degree sun source. 

The direct and diffuse solar irradiances/illuminances are the inputs needed for the calculation.
These quantities are the commonly accessible data from radiometric measurement centres or from the
Test Reference Year. The use of such data is the recommended method for achieving the most accurate
simulation results.

The atmospheric conditions are modelled with the Perez et al. parametrization  
(see Solar Energy Vol. 44, No 5, pp. 271-289, 1990), which is dependent on the values for
the direct-normal and the diffuse-horizontal irradiances. The three parameters
are epsilon, delta and the solar zenith angle. "Epsilon variations express the transition from 
a totally overcast sky (epsilon=1) to a low turbidity clear sky (epsilon>6); delta 
variations reflect the opacity/thickness of the clouds". Delta can vary from 0.05
representing a dark sky to 0.5 for a very bright sky. Not every combination of
epsilon, delta and solar zenith angle is possible. For a clear day, if 
epsilon and the solar zenith angle are known, then delta can be determined. For intermediate or overcast
days, the sky can be dark or bright, giving a range of possible values for delta
when epsilon and the solar zenith are fixed. The relation between epsilon and delta
is represented in a figure on page 393 in Solar Energy Vol.42, No 5, 1989. Note that the 
epsilon parameter is a function of the solar zenith angle. It means that a clear day 
will not be defined by fixed values of epsilon and delta. Consequently the input
parameters, epsilon, delta and the solar zenith angle, have to be determined on a graph.
It might be easier to work with the measured direct and diffuse components (direct normal irradiance/illuminance
and diffuse horizontal irradiance/illuminance) than with the epsilon and delta parameters.

The conversion of irradiance into illuminance for the direct and the diffuse
components is determined by the luminous efficacy models of Perez et al. (see 
Solar Energy Vol. 44, No 5, pp. 271-289, 1990). To convert the luminance values
into radiance integrated over the visible range of the spectrum, 
we devide the luminance by the white light efficacy factor of  
179 lm/W. This is consistent with the RADIANCE calculation because the luminance
will be recalculated from the radiance integrated over the visible range by:

luminance = radiance_integrated_over_visible_range * 179   or
luminance = (RED*.263 + GREEN*.655 + BLUE*.082) * 179    with the capability
to model colour (where radiance_integrated_over_visible_range == (RED + GREEN + BLUE)/3).

From 
.I gensky, if the hour is preceded by a plus sign ('+'), then it is interpreted as local solar time instead of standard time.
The second form gives the solar angles explicitly. The altitude is measured in degrees above the horizon, and the
azimuth is measured in degrees west of South. The x axis points east, the y axis points north, and the z axis
corresponds to the zenith. The actual material and surface(s) used for the sky is left up to the user.
In addition to the specification of a sky distribution function,
.I gendaylit
suggests an ambient value in a comment at the beginning of the description to use with the
.I \-av
option of the RADIANCE rendering programs. (See rview(1) and rpict(1).) This value is the cosine-weighted
radiance of the sky in W/sr/m^2.
.PP
.I Gendaylit
can be used with the following input parameters. They offer three possibilities
to run it: with the Perez parametrization, with irradiance values and with illuminance values.
.TP 10n
.BR \-P 
.I epsilon 
.I delta  
(these are the Perez parameters)
.TP
.BR \-W 
.I direct-normal-irradiance
(W/m^2), 
.I diffuse-horizontal-irradiance
(W/m^2)
.TP
.BR \-G 
.I direct-horizontal-irradiance
(W/m^2), 
.I diffuse-horizontal-irradiance
(W/m^2)
.TP
.BR \-L 
.I direct-normal-illuminance
(lm/m^2), 
.I diffuse-horizontal-illuminance
(lm/m^2)
.TP
.BR \-E 
.I global-horizontal-irradiance
(W/m^2)
.PP
The -E option calculates the diffuse irradiance fraction with the model of Erbs, Klein and Duffie (Solar Energy 28/4, 1982), 
being followed by the calculation of the -G option. Due to the high uncertainty of the model, the results have to be handled 
with care. A second irradiance value, if available, is definitely recommended.
.PP
The output can be set to either the radiance of the visible radiation, the solar radiance (full spectrum) or the luminance.
.TP 10n
.BR \-O [0|1|2]  
(0=output in W/m^2/sr visible radiation (default), 1=output in W/m^2/sr solar radiation, 2=output in lm/m^2/sr luminance).
.PP
.I Gendaylit
supports the following options.
.TP 10n
.BR \-s
The source description of the sun is not generated.
.TP
.BR \-w
Suppress warning messages
.TP
.BI -g \ rfl
Average ground reflectance is
.I rfl.
This value is used to compute
.I skyfunc
when Dz is negative.
.PP
The following options do not apply when the solar
altitude and azimuth are given explicitly.
.TP
.BI -a \ lat
The site latitude is
.I lat
degrees north.
(Use negative angle for south latitude.)
This is used in the calculation of sun angle.
.TP
.BI -o \ lon
The site longitude is
.I lon
degrees west.
(Use negative angle for east longitude.)
This is used in the calculation of solar time and sun angle.
Be sure to give the corresponding standard meridian also!
If solar time is given directly, then this option has no effect.
.TP
.BI -m \ mer
The site standard meridian is
.I mer
degrees west of Greenwich.
(Use negative angle for east.)
This is used in the calculation of solar time.
Be sure to give the correct longitude also!
If solar time is given directly, then this option has no effect.
.TP
.BI -i \ time_interval [min]
If gendaylit is used with weather files, the specified instantaneous points of time may be incorrect. This error occurs
due to the fact that measurement results are frequently defined for time intervals, not for specific points of time.
Although gendaylit is working correctly, this may lead to wrong outputs especially at low sun altitudes.
The -i option allows to specify the time interval of the measurements in minutes, causing the solar position to be corrected for low sun
altitudes. A warning message is returned if a correction has been performed.

.SH EXAMPLES
A clear non-turbid sky for a solar altitude of 60 degrees and an azimut of 0 degree might be defined by:
.IP "" .2i
gendaylit -ang 60 0 -P 6.3 0.12 or gendaylit -ang 60 0 -W 840 135
This sky description corresponds to the clear sky standard of the CIE.
.PP
The corresponding sky with a high turbidity is:
.IP "" .2i
gendaylit -ang 60 0 -P 3.2 0.24 or gendaylit -ang 60 0 -W 720 280 
.PP
The dark overcast sky (corresponding to the CIE overcast standard, see CIE draft standard,
Pub. No. CIE DS 003, 1st Edition, 1994) is obtained by:
.IP "" .2i
gendaylit -ang 60 0 -P 1 0.08
.PP
A bright overcast sky is modelled with a larger value of delta, for example:
.IP "" .2i
gendaylit -ang 60 0 -P 1 0.35 
.PP
To generate the same bright overcast sky for March 2th at 3:15pm standard time at a site
latitude of 42 degrees, 108 degrees west longitude, and a 110 degrees standard meridian:
.IP "" .2i
gendaylit 3 2 15.25 -a 42 -o 108 -m 110 -P 1 0.35
.PP 
.SH FILES
/usr/local/lib/ray/perezlum.cal
.SH AUTHOR
Jean-Jacques Delaunay, Jan Wienold, Wendelin Sprenger, Fraunhofer ISE (Freiburg i.B., Germany) ([email protected])
.SH ACKNOWLEDGEMENTS
The first work on this program was supported by the German Federal Ministry for Research
and Technology (BMFT) under contract No. 0329294A, and a scholarship from 
the French Environment and Energy Agency (ADEME) which was co-funded by Bouygues. 
Many thanks to Peter Apian-Bennewitz, Arndt Berger, Christian Reetz, Ann Kovach, R. Perez, C. Gueymard and G. Ward for their help.
.SH "SEE ALSO"
gensky(1), rpict(1), rview(1), xform(1)
Revision:	1.4
Committed:	Fri Aug 9 16:44:19 2013 UTC (11 years, 8 months ago) by greg
Branch:	MAIN
CVS Tags:	rad5R2, rad4R2P2, rad5R0, rad5R1, rad4R2, rad4R2P1
Changes since 1.3:	+20 -15 lines
Log Message:	Bug fixes and new -E and -i options (from Wendelin Sprenger and Jan Wienold)
#	User	Rev	Content
1	greg	1.3	.\" RCSid "$Id: gendaylit.1,v 1.2 2009/06/06 20:22:49 greg Exp $"
2	greg	1.2	.TH GENDAYLIT 1 4/12/94 "RADIANCE ISE/ADEME EXTENSIONS"
3	greg	1.1	.SH NAME
4	greg	1.4	gendaylit - generates a RADIANCE description of the daylight sources using Perez models for direct and diffuse components
5	greg	1.1	.SH SYNOPSIS
6	greg	1.4	.B "gendaylit month day hour [-P\|-W\|-L\|-G\|-E] input_value(s) "
7	greg	1.1	[
8			.B options
9			]
10			.br
11	greg	1.4	.B "gendaylit -ang altitude azimuth [-P\|-W\|-L\|-G\|-E] input_value(s) "
12	greg	1.1	[
13			.B options
14			]
15			.SH DESCRIPTION
16			.I Gendaylit
17			produces a RADIANCE scene description based on an angular distribution of the
18			daylight sources (direct+diffuse) for the given atmospheric conditions
19			(direct and diffuse component of the solar radiation), date and
20	greg	1.3	local standard time. The default output is the radiance of the sun (direct) and the sky (diffuse)
21	greg	1.1	integrated over the visible spectral range (380-780 nm). We have used the
22			calculation of the sun's position and the ground brightness models which
23			were programmed in
24			.I gensky.
25
26			The diffuse angular distribution is calculated using the Perez et al.
27			sky luminance distribution model (see Solar Energy Vol. 50, No. 3, pp. 235-245, 1993) which, quoting Perez,
28			describes "the mean instantaneous sky luminance angular distribution patterns for all sky
29			conditions from overcast to clear, through partly cloudy, skies". The correctness of the
30			resulting sky radiance/luminance values in this simulation is ensured through the normalization of the modelled
31			sky diffuse to the measured sky diffuse irradiances/illuminances.
32
33	greg	1.3	As described below, the radiation can be defined with the pairs direct-normal and diffuse-horizontal irradiance
34	greg	1.4	(-W option), direct-horizontal and diffuse-horizontal irradiance (-G option), direct-normal and diffuse-horizontal
35			illuminance (-L option) or global-horizontal irradiation alone (-E option). The direct-normal radiation
36			is understood here as the radiant flux coming from the sun and an area of approximately 3 degrees around the sun
37			(World Meteorological Organisation specifications for measuring the direct radiation.
38			The aperture angle of a pyrheliometer is approximately 6 degrees).
39	greg	1.1	To simplify the calculations for the direct radiation, the sun is represented as a disk and no
40			circumsolar radiation is modelled in the 3 degrees around the sun. This means that
41			all the measured/evaluated direct radiation is added to the 0.5 degree sun source.
42
43	greg	1.3	The direct and diffuse solar irradiances/illuminances are the inputs needed for the calculation.
44			These quantities are the commonly accessible data from radiometric measurement centres or from the
45			Test Reference Year. The use of such data is the recommended method for achieving the most accurate
46			simulation results.
47	greg	1.1
48			The atmospheric conditions are modelled with the Perez et al. parametrization
49			(see Solar Energy Vol. 44, No 5, pp. 271-289, 1990), which is dependent on the values for
50	greg	1.3	the direct-normal and the diffuse-horizontal irradiances. The three parameters
51	greg	1.1	are epsilon, delta and the solar zenith angle. "Epsilon variations express the transition from
52			a totally overcast sky (epsilon=1) to a low turbidity clear sky (epsilon>6); delta
53			variations reflect the opacity/thickness of the clouds". Delta can vary from 0.05
54			representing a dark sky to 0.5 for a very bright sky. Not every combination of
55			epsilon, delta and solar zenith angle is possible. For a clear day, if
56			epsilon and the solar zenith angle are known, then delta can be determined. For intermediate or overcast
57			days, the sky can be dark or bright, giving a range of possible values for delta
58			when epsilon and the solar zenith are fixed. The relation between epsilon and delta
59	greg	1.3	is represented in a figure on page 393 in Solar Energy Vol.42, No 5, 1989. Note that the
60	greg	1.1	epsilon parameter is a function of the solar zenith angle. It means that a clear day
61			will not be defined by fixed values of epsilon and delta. Consequently the input
62			parameters, epsilon, delta and the solar zenith angle, have to be determined on a graph.
63			It might be easier to work with the measured direct and diffuse components (direct normal irradiance/illuminance
64			and diffuse horizontal irradiance/illuminance) than with the epsilon and delta parameters.
65
66			The conversion of irradiance into illuminance for the direct and the diffuse
67			components is determined by the luminous efficacy models of Perez et al. (see
68			Solar Energy Vol. 44, No 5, pp. 271-289, 1990). To convert the luminance values
69			into radiance integrated over the visible range of the spectrum,
70			we devide the luminance by the white light efficacy factor of
71			179 lm/W. This is consistent with the RADIANCE calculation because the luminance
72	greg	1.3	will be recalculated from the radiance integrated over the visible range by:
73	greg	1.1
74			luminance = radiance_integrated_over_visible_range * 179 or
75			luminance = (RED.263 + GREEN.655 + BLUE.082) 179 with the capability
76			to model colour (where radiance_integrated_over_visible_range == (RED + GREEN + BLUE)/3).
77
78			From
79	greg	1.4	.I gensky, if the hour is preceded by a plus sign ('+'), then it is interpreted as local solar time instead of standard time.
80	greg	1.3	The second form gives the solar angles explicitly. The altitude is measured in degrees above the horizon, and the
81			azimuth is measured in degrees west of South. The x axis points east, the y axis points north, and the z axis
82			corresponds to the zenith. The actual material and surface(s) used for the sky is left up to the user.
83			In addition to the specification of a sky distribution function,
84	greg	1.1	.I gendaylit
85	greg	1.3	suggests an ambient value in a comment at the beginning of the description to use with the
86	greg	1.1	.I \-av
87	greg	1.3	option of the RADIANCE rendering programs. (See rview(1) and rpict(1).) This value is the cosine-weighted
88			radiance of the sky in W/sr/m^2.
89	greg	1.1	.PP
90			.I Gendaylit
91			can be used with the following input parameters. They offer three possibilities
92	greg	1.3	to run it: with the Perez parametrization, with irradiance values and with illuminance values.
93	greg	1.1	.TP 10n
94			.BR \-P
95			.I epsilon
96			.I delta
97			(these are the Perez parameters)
98			.TP
99			.BR \-W
100			.I direct-normal-irradiance
101			(W/m^2),
102			.I diffuse-horizontal-irradiance
103			(W/m^2)
104			.TP
105	greg	1.3	.BR \-G
106			.I direct-horizontal-irradiance
107			(W/m^2),
108			.I diffuse-horizontal-irradiance
109			(W/m^2)
110			.TP
111	greg	1.1	.BR \-L
112			.I direct-normal-illuminance
113			(lm/m^2),
114			.I diffuse-horizontal-illuminance
115			(lm/m^2)
116	greg	1.4	.TP
117			.BR \-E
118			.I global-horizontal-irradiance
119			(W/m^2)
120			.PP
121			The -E option calculates the diffuse irradiance fraction with the model of Erbs, Klein and Duffie (Solar Energy 28/4, 1982),
122			being followed by the calculation of the -G option. Due to the high uncertainty of the model, the results have to be handled
123			with care. A second irradiance value, if available, is definitely recommended.
124	greg	1.1	.PP
125	greg	1.3	The output can be set to either the radiance of the visible radiation, the solar radiance (full spectrum) or the luminance.
126	greg	1.1	.TP 10n
127			.BR \-O [0\|1\|2]
128	greg	1.3	(0=output in W/m^2/sr visible radiation (default), 1=output in W/m^2/sr solar radiation, 2=output in lm/m^2/sr luminance).
129	greg	1.1	.PP
130			.I Gendaylit
131			supports the following options.
132			.TP 10n
133			.BR \-s
134			The source description of the sun is not generated.
135			.TP
136	greg	1.3	.BR \-w
137			Suppress warning messages
138			.TP
139	greg	1.1	.BI -g \ rfl
140			Average ground reflectance is
141			.I rfl.
142			This value is used to compute
143			.I skyfunc
144			when Dz is negative.
145			.PP
146			The following options do not apply when the solar
147			altitude and azimuth are given explicitly.
148			.TP
149			.BI -a \ lat
150			The site latitude is
151			.I lat
152			degrees north.
153			(Use negative angle for south latitude.)
154			This is used in the calculation of sun angle.
155			.TP
156			.BI -o \ lon
157			The site longitude is
158			.I lon
159			degrees west.
160			(Use negative angle for east longitude.)
161			This is used in the calculation of solar time and sun angle.
162			Be sure to give the corresponding standard meridian also!
163			If solar time is given directly, then this option has no effect.
164			.TP
165			.BI -m \ mer
166			The site standard meridian is
167			.I mer
168			degrees west of Greenwich.
169			(Use negative angle for east.)
170			This is used in the calculation of solar time.
171			Be sure to give the correct longitude also!
172			If solar time is given directly, then this option has no effect.
173	greg	1.3	.TP
174	greg	1.4	.BI -i \ time_interval [min]
175	greg	1.3	If gendaylit is used with weather files, the specified instantaneous points of time may be incorrect. This error occurs
176			due to the fact that measurement results are frequently defined for time intervals, not for specific points of time.
177			Although gendaylit is working correctly, this may lead to wrong outputs especially at low sun altitudes.
178	greg	1.4	The -i option allows to specify the time interval of the measurements in minutes, causing the solar position to be corrected for low sun
179			altitudes. A warning message is returned if a correction has been performed.
180	greg	1.3
181	greg	1.1	.SH EXAMPLES
182			A clear non-turbid sky for a solar altitude of 60 degrees and an azimut of 0 degree might be defined by:
183			.IP "" .2i
184			gendaylit -ang 60 0 -P 6.3 0.12 or gendaylit -ang 60 0 -W 840 135
185			This sky description corresponds to the clear sky standard of the CIE.
186			.PP
187			The corresponding sky with a high turbidity is:
188			.IP "" .2i
189	greg	1.3	gendaylit -ang 60 0 -P 3.2 0.24 or gendaylit -ang 60 0 -W 720 280
190	greg	1.1	.PP
191			The dark overcast sky (corresponding to the CIE overcast standard, see CIE draft standard,
192			Pub. No. CIE DS 003, 1st Edition, 1994) is obtained by:
193			.IP "" .2i
194	greg	1.3	gendaylit -ang 60 0 -P 1 0.08
195	greg	1.1	.PP
196			A bright overcast sky is modelled with a larger value of delta, for example:
197			.IP "" .2i
198			gendaylit -ang 60 0 -P 1 0.35
199			.PP
200			To generate the same bright overcast sky for March 2th at 3:15pm standard time at a site
201			latitude of 42 degrees, 108 degrees west longitude, and a 110 degrees standard meridian:
202			.IP "" .2i
203			gendaylit 3 2 15.25 -a 42 -o 108 -m 110 -P 1 0.35
204			.PP
205			.SH FILES
206			/usr/local/lib/ray/perezlum.cal
207			.SH AUTHOR
208	greg	1.3	Jean-Jacques Delaunay, Jan Wienold, Wendelin Sprenger, Fraunhofer ISE (Freiburg i.B., Germany) ([email protected])
209	greg	1.1	.SH ACKNOWLEDGEMENTS
210	greg	1.3	The first work on this program was supported by the German Federal Ministry for Research
211	greg	1.1	and Technology (BMFT) under contract No. 0329294A, and a scholarship from
212			the French Environment and Energy Agency (ADEME) which was co-funded by Bouygues.
213	greg	1.3	Many thanks to Peter Apian-Bennewitz, Arndt Berger, Christian Reetz, Ann Kovach, R. Perez, C. Gueymard and G. Ward for their help.
214	greg	1.1	.SH "SEE ALSO"
215			gensky(1), rpict(1), rview(1), xform(1)