We have developed a Monte Carlo program that can account for Raman scattering in the ocean when polarization effects are not considered. The program is capable of coupling an inhomogeneous atmosphere to an inhomogeneous ocean through a dielectric interface. We have studied the filling in of both the 486-nm Hβ and the 518-nm Mg Fraunhofer lines caused by Raman scattering in the ocean. The amount of fill varies with solar zenith angle, angle of view, depth in the ocean, and magnitude of the cross sections. By monitoring the shapes of Fraunhofer lines we can learn a great deal about the relative importance of this inelastic process in oceanic optics.
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Absorption coefficient (see Ref. 12).
Raman scattering coefficient.
Hydrosol scattering coefficient (see Ref. 1).
Scattering coefficient for salt water (see Ref. 12).
Total extinction coefficient: c = a + br + bhyd + bsw.
Single-scattering albedo: ω0 = (br + bhyd + bsw)/c.
Table 4
Ratio of Core-to-Wing Irradiances(Ec/Ew) for the 486-nm Hβ Line as a Function of Depth for Both Upward and Downward Irradiancesa
Depth (m)
Upward
Downward
Upward
Downward
μ0 = −1.0
LRam
SRam
0.01
0.578
0.221
0.308
0.213
10
0.580
0.228
0.310
0.214
20
0.582
0.234
0.312
0.215
40
0.587
0.244
0.315
0.217
60
0.588
0.253
0.318
0.218
80
0.584
0.260
0.321
0.220
100
0.589
0.267
0.322
0.221
LRam + Hyd
SRam + Hyd
0.01
0.519
0.221
0.286
0.213
10
0.522
0.229
0.287
0.214
20
0.524
0.236
0.289
0.215
40
0.528
0.249
0.291
0.218
60
0.531
0.259
0.292
0.220
80
0.524
0.270
0.293
0.222
100
0.528
0.279
0.297
0.224
μ0 = −0.5
LRam+Hyd
SRam+Hyd
0.01
0.484
0.224
0.274
0.213
10
0.486
0.237
0.275
0.216
20
0.489
0.251
0.278
0.218
40
0.503
0.281
0.283
0.224
60
0.521
0.310
0.289
0.230
80
0.542
0.336
0.303
0.236
100
0.560
0.357
0.310
0.241
The results for two solar zenith angles are presented, i.e., θ0 = 0° (μ0 = −cos θ0 = −1.0) and θ0 = 60° (μ0 = −0.5).
Tables (4)
Table 1
Contributions of Various Input–Output Components to the Raman Differential Scattering Cross Sectiona
Absorption coefficient (see Ref. 12).
Raman scattering coefficient.
Hydrosol scattering coefficient (see Ref. 1).
Scattering coefficient for salt water (see Ref. 12).
Total extinction coefficient: c = a + br + bhyd + bsw.
Single-scattering albedo: ω0 = (br + bhyd + bsw)/c.
Table 4
Ratio of Core-to-Wing Irradiances(Ec/Ew) for the 486-nm Hβ Line as a Function of Depth for Both Upward and Downward Irradiancesa
Depth (m)
Upward
Downward
Upward
Downward
μ0 = −1.0
LRam
SRam
0.01
0.578
0.221
0.308
0.213
10
0.580
0.228
0.310
0.214
20
0.582
0.234
0.312
0.215
40
0.587
0.244
0.315
0.217
60
0.588
0.253
0.318
0.218
80
0.584
0.260
0.321
0.220
100
0.589
0.267
0.322
0.221
LRam + Hyd
SRam + Hyd
0.01
0.519
0.221
0.286
0.213
10
0.522
0.229
0.287
0.214
20
0.524
0.236
0.289
0.215
40
0.528
0.249
0.291
0.218
60
0.531
0.259
0.292
0.220
80
0.524
0.270
0.293
0.222
100
0.528
0.279
0.297
0.224
μ0 = −0.5
LRam+Hyd
SRam+Hyd
0.01
0.484
0.224
0.274
0.213
10
0.486
0.237
0.275
0.216
20
0.489
0.251
0.278
0.218
40
0.503
0.281
0.283
0.224
60
0.521
0.310
0.289
0.230
80
0.542
0.336
0.303
0.236
100
0.560
0.357
0.310
0.241
The results for two solar zenith angles are presented, i.e., θ0 = 0° (μ0 = −cos θ0 = −1.0) and θ0 = 60° (μ0 = −0.5).