man/man1/gendaylit.1

.\" RCSid "$Id: gendaylit.1,v 1.1 2009/06/06 20:20:04 greg Exp $"
.TH GENDAYLIT 1 4/12/94 "RADIANCE ISE/ADEME EXTENSIONS"
.SH NAME
gendaylit - generates a RADIANCE description of the daylit sources using Perez models for diffuse and direct components
.SH SYNOPSIS
.B "gendaylit month day hour [-P|-W|-L] direct_value diffuse_value "
[
.B options
]
.br
.B "gendaylit -ang altitude azimuth [-P|-W|-L] direct_value diffuse_value "
[
.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 (diffus)
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.

The direct 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. 

.I The direct and diffuse 
.I solar irradiances/illuminances 
.I are the inputs needed 
.I for the calculation.
These quantities are the commonly accessible data from radiometric measurement centres, conversion models 
(e.g. global irradiance to direct irradiance), 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 and the diffuse 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,
or can be obtained from the author of this RADIANCE extension upon request. 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.
.PP
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.
.PP
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 the irradiance values
and with the 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 \-L 
.I direct-normal-illuminance
(lm/m^2), 
.I diffuse-horizontal-illuminance
(lm/m^2)
.PP
The output can be set to either the radiance of the visible radiation (default), the solar radiance (full spectrum) or the luminance.
.TP 10n
.BR \-O [0|1|2]  
(0=output in W/m^2/sr visible radiation, 0=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
.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.
.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, FhG-ISE Freiburg, ([email protected])
.SH ACKNOWLEDGEMENTS
The 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, Ann Kovach, R. Perez, C. Gueymard and G. Ward for their help.
.SH "SEE ALSO"
gensky(1), rpict(1), rview(1), xform(1)
Revision:	1.2
Committed:	Sat Jun 6 20:22:49 2009 UTC (16 years ago) by greg
Branch:	MAIN
CVS Tags:	rad4R1, rad4R0
Changes since 1.1:	+2 -1 lines
Log Message:	Fixed problem with man page
#	Content
1	.\" RCSid "$Id: gendaylit.1,v 1.1 2009/06/06 20:20:04 greg Exp $"
2	.TH GENDAYLIT 1 4/12/94 "RADIANCE ISE/ADEME EXTENSIONS"
3	.SH NAME
4	gendaylit - generates a RADIANCE description of the daylit sources using Perez models for diffuse and direct components
5	.SH SYNOPSIS
6	.B "gendaylit month day hour [-P\|-W\|-L] direct_value diffuse_value "
7	[
8	.B options
9	]
10	.br
11	.B "gendaylit -ang altitude azimuth [-P\|-W\|-L] direct_value diffuse_value "
12	[
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	local standard time. The default output is the radiance of the sun (direct) and the sky (diffus)
21	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	The direct radiation is understood here as the radiant flux coming from the sun
34	and an area of approximately 3 degrees around the sun (World Meteorological Organisation specifications
35	for measuring the direct radiation. The aperture angle of a pyrheliometer is approximately 6 degrees).
36	To simplify the calculations for the direct radiation, the sun is represented as a disk and no
37	circumsolar radiation is modelled in the 3 degrees around the sun. This means that
38	all the measured/evaluated direct radiation is added to the 0.5 degree sun source.
39
40	.I The direct and diffuse
41	.I solar irradiances/illuminances
42	.I are the inputs needed
43	.I for the calculation.
44	These quantities are the commonly accessible data from radiometric measurement centres, conversion models
45	(e.g. global irradiance to direct irradiance), or from the Test Reference Year. The use of such
46	data is the recommended method for achieving the most accurate simulation results.
47
48
49	The atmospheric conditions are modelled with the Perez et al. parametrization
50	(see Solar Energy Vol. 44, No 5, pp. 271-289, 1990), which is dependent on the values for
51	the direct and the diffuse irradiances. The three parameters
52	are epsilon, delta and the solar zenith angle. "Epsilon variations express the transition from
53	a totally overcast sky (epsilon=1) to a low turbidity clear sky (epsilon>6); delta
54	variations reflect the opacity/thickness of the clouds". Delta can vary from 0.05
55	representing a dark sky to 0.5 for a very bright sky. Not every combination of
56	epsilon, delta and solar zenith angle is possible. For a clear day, if
57	epsilon and the solar zenith angle are known, then delta can be determined. For intermediate or overcast
58	days, the sky can be dark or bright, giving a range of possible values for delta
59	when epsilon and the solar zenith are fixed. The relation between epsilon and delta
60	is represented in a figure on page 393 in Solar Energy Vol.42, No 5, 1989,
61	or can be obtained from the author of this RADIANCE extension upon request. Note that the
62	epsilon parameter is a function of the solar zenith angle. It means that a clear day
63	will not be defined by fixed values of epsilon and delta. Consequently the input
64	parameters, epsilon, delta and the solar zenith angle, have to be determined on a graph.
65	It might be easier to work with the measured direct and diffuse components (direct normal irradiance/illuminance
66	and diffuse horizontal irradiance/illuminance) than with the epsilon and delta parameters.
67
68
69	The conversion of irradiance into illuminance for the direct and the diffuse
70	components is determined by the luminous efficacy models of Perez et al. (see
71	Solar Energy Vol. 44, No 5, pp. 271-289, 1990). To convert the luminance values
72	into radiance integrated over the visible range of the spectrum,
73	we devide the luminance by the white light efficacy factor of
74	179 lm/W. This is consistent with the RADIANCE calculation because the luminance
75	will be recalculated from the radiance integrated over the visible range by :
76
77	luminance = radiance_integrated_over_visible_range * 179 or
78
79	luminance = (RED.263 + GREEN.655 + BLUE.082) 179 with the capability
80	to model colour (where radiance_integrated_over_visible_range == (RED + GREEN + BLUE)/3).
81
82	From
83	.I gensky
84	, if the hour is preceded by a plus sign ('+'), then it is interpreted
85	as local solar time instead of standard time.
86	The second form gives the solar angles explicitly.
87	The altitude is measured in degrees above the horizon, and the
88	azimuth is measured in degrees west of South.
89	.PP
90	The x axis points east,
91	the y axis points north, and the z axis corresponds to the zenith.
92	The actual material and surface(s) used for the sky is left
93	up to the user.
94	.PP
95	In addition to the specification of
96	a sky distribution function,
97	.I gendaylit
98	suggests an ambient value in a comment at the beginning of the
99	description to use with the
100	.I \-av
101	option of the RADIANCE rendering programs.
102	(See rview(1) and rpict(1).)
103	This value is the cosine-weighted radiance of the sky in
104	W/sr/m^2.
105	.PP
106	.I Gendaylit
107	can be used with the following input parameters. They offer three possibilities
108	to run it: with the Perez parametrization, with the irradiance values
109	and with the illuminance values.
110	.TP 10n
111	.BR \-P
112	.I epsilon
113	.I delta
114	(these are the Perez parameters)
115	.TP
116	.BR \-W
117	.I direct-normal-irradiance
118	(W/m^2),
119	.I diffuse-horizontal-irradiance
120	(W/m^2)
121	.TP
122	.BR \-L
123	.I direct-normal-illuminance
124	(lm/m^2),
125	.I diffuse-horizontal-illuminance
126	(lm/m^2)
127	.PP
128	The output can be set to either the radiance of the visible radiation (default), the solar radiance (full spectrum) or the luminance.
129	.TP 10n
130	.BR \-O [0\|1\|2]
131	(0=output in W/m^2/sr visible radiation, 0=output in W/m^2/sr solar radiation, 2=output in lm/m^2/sr luminance)
132	.PP
133	.I Gendaylit
134	supports the following options.
135	.TP 10n
136	.BR \-s
137	The source description of the sun is not generated.
138	.TP
139	.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	.SH EXAMPLES
174	A clear non-turbid sky for a solar altitude of 60 degrees and an azimut of 0 degree might be defined by:
175	.IP "" .2i
176	gendaylit -ang 60 0 -P 6.3 0.12 or gendaylit -ang 60 0 -W 840 135
177	This sky description corresponds to the clear sky standard of the CIE.
178	.PP
179	The corresponding sky with a high turbidity is:
180	.IP "" .2i
181	gendaylit -ang 60 0 -P 3.2 0.24 or gendaylit -ang 60 0 -W 720 280
182	.PP
183	The dark overcast sky (corresponding to the CIE overcast standard, see CIE draft standard,
184	Pub. No. CIE DS 003, 1st Edition, 1994) is obtained by:
185	.IP "" .2i
186	gendaylit -ang 60 0 -P 1 0.08
187	.PP
188	A bright overcast sky is modelled with a larger value of delta, for example:
189	.IP "" .2i
190	gendaylit -ang 60 0 -P 1 0.35
191	.PP
192	To generate the same bright overcast sky for March 2th at 3:15pm standard time at a site
193	latitude of 42 degrees, 108 degrees west longitude, and a 110 degrees standard meridian:
194	.IP "" .2i
195	gendaylit 3 2 15.25 -a 42 -o 108 -m 110 -P 1 0.35
196	.PP
197	.SH FILES
198	/usr/local/lib/ray/perezlum.cal
199	.SH AUTHOR
200	Jean-Jacques Delaunay, FhG-ISE Freiburg, ([email protected])
201	.SH ACKNOWLEDGEMENTS
202	The work on this program was supported by the German Federal Ministry for Research
203	and Technology (BMFT) under contract No. 0329294A, and a scholarship from
204	the French Environment and Energy Agency (ADEME) which was co-funded by Bouygues.
205	Many thanks to Peter Apian-Bennewitz, Arndt Berger, Ann Kovach, R. Perez, C. Gueymard and G. Ward for their help.
206	.SH "SEE ALSO"
207	gensky(1), rpict(1), rview(1), xform(1)