A discussion of the spectral distribution and intensity of the radiation fluxes from various sources contributing to the radiation environment of interplanetary space is presented. The radiation from both the quiet and disturbed sun is described in some detail and current estimates of radiation from other sources are given.
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The flux in the extreme ultraviolet and x-ray regions below 100 A and in the radio region at wavelengths longer than 1 cm shows great enhancements when the sun is disturbed. The flux in some regions may increase by a factor of 102 to 105 or even more above the flux from the quiet sun. Such outbursts rarely last more than a few hours.
H. Friedman, Physics of the Upper Atmosphere (ed. J. A. Ratcliffe, Academic Press, 1960) (for 0–100 A).
H. E. Hinteregger, J. Geophys. Research 66, 2367 (1961).
C. R. Detwiler, D. L. Garrett, J. D. Purcell, and R. Tousey, Ann. géophys. 17, 9, 263 (1961) (for 1000–3000 A).
F. S. Johnson, J. Meteorol. 11, 431 (1954).
Table III
Spectral Brightness Temperatures of the Quiet Sun from Measurements of the Continuum
H. Friedman, Physics of the Upper Atmosphere (ed. J. A. Ratcliffe, Academic Press, 1960).
C. R. Detwiler, J. D. Purcell, and R. Tousey, Astron. J. 66, 281 (1961).
C. W. Allen, Astrophysical Quantities (Univ. London, 1955), p. 141.
R. Peyturaux, Ann. astrophys. 15, 302 (1952).
A. K. Pierce, Astrophys J. 119, 312 (1954).
C. B. Farmer and S. J. Todd, Report No. DP 927, EMI Electronics Ltd., London, 1961.
F. Saiedy and R. M. Goody, Monthly Notices Roy. Astron. Soc. 119, 213 (1959).
R. J. Coates, Astrophys. J. 128, 83 (1958).
R. N. Whitehurst, J. Copland, and F. H. Mitchell, J. Appl. Phys. 28, 295 (1957).
S. N. Vernov, A. E. Chudakov, E. V. Gorchakov, J. I. Lozachev, and P. V. Vakulov, paper presented at Fifth CSAGI Assembly, Moscow (1958).
J. E. Kupperian, Jr. and H. Friedman, paper presented at Fifth CSAGI Assembly, Moscow (1958).
These values converted from equivalent number of tenth magnitude visual stars per square degree (S) to units of 10−12 times the solar disc brightness H by the formula (Roach et al., Astrophys J. 119, 253 (1954)) log H = log S − 3.480.
M. F. Ingham, Monthly Notices Roy. Astron. Soc. 122, 157 (1961).
C. W. Allen, Astrophysical Quantities (Univ. London, 1955), p. 171.
D. E. Blackwell and M. F. Ingham, Monthly Notices Roy. Astron. Soc. 122, 113, 129, 143 (1961).
Table VI
Spectral Distribution of Radiation Density in Interstellar Spacea
Wavelength (microns)
0.05
0.1
0.2
0.3
0.4
0.5
0.6
0.8
1.0
Radiation density (10−14ergs cm−3μ−1)
3
11
26
34
45
62
82
121
162
C. W. Allen, Astrophysical Quantities (Univ. London, 1955), p. 228.
The flux in the extreme ultraviolet and x-ray regions below 100 A and in the radio region at wavelengths longer than 1 cm shows great enhancements when the sun is disturbed. The flux in some regions may increase by a factor of 102 to 105 or even more above the flux from the quiet sun. Such outbursts rarely last more than a few hours.
H. Friedman, Physics of the Upper Atmosphere (ed. J. A. Ratcliffe, Academic Press, 1960) (for 0–100 A).
H. E. Hinteregger, J. Geophys. Research 66, 2367 (1961).
C. R. Detwiler, D. L. Garrett, J. D. Purcell, and R. Tousey, Ann. géophys. 17, 9, 263 (1961) (for 1000–3000 A).
F. S. Johnson, J. Meteorol. 11, 431 (1954).
Table III
Spectral Brightness Temperatures of the Quiet Sun from Measurements of the Continuum
H. Friedman, Physics of the Upper Atmosphere (ed. J. A. Ratcliffe, Academic Press, 1960).
C. R. Detwiler, J. D. Purcell, and R. Tousey, Astron. J. 66, 281 (1961).
C. W. Allen, Astrophysical Quantities (Univ. London, 1955), p. 141.
R. Peyturaux, Ann. astrophys. 15, 302 (1952).
A. K. Pierce, Astrophys J. 119, 312 (1954).
C. B. Farmer and S. J. Todd, Report No. DP 927, EMI Electronics Ltd., London, 1961.
F. Saiedy and R. M. Goody, Monthly Notices Roy. Astron. Soc. 119, 213 (1959).
R. J. Coates, Astrophys. J. 128, 83 (1958).
R. N. Whitehurst, J. Copland, and F. H. Mitchell, J. Appl. Phys. 28, 295 (1957).
S. N. Vernov, A. E. Chudakov, E. V. Gorchakov, J. I. Lozachev, and P. V. Vakulov, paper presented at Fifth CSAGI Assembly, Moscow (1958).
J. E. Kupperian, Jr. and H. Friedman, paper presented at Fifth CSAGI Assembly, Moscow (1958).
These values converted from equivalent number of tenth magnitude visual stars per square degree (S) to units of 10−12 times the solar disc brightness H by the formula (Roach et al., Astrophys J. 119, 253 (1954)) log H = log S − 3.480.
M. F. Ingham, Monthly Notices Roy. Astron. Soc. 122, 157 (1961).
C. W. Allen, Astrophysical Quantities (Univ. London, 1955), p. 171.
D. E. Blackwell and M. F. Ingham, Monthly Notices Roy. Astron. Soc. 122, 113, 129, 143 (1961).
Table VI
Spectral Distribution of Radiation Density in Interstellar Spacea
Wavelength (microns)
0.05
0.1
0.2
0.3
0.4
0.5
0.6
0.8
1.0
Radiation density (10−14ergs cm−3μ−1)
3
11
26
34
45
62
82
121
162
C. W. Allen, Astrophysical Quantities (Univ. London, 1955), p. 228.
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