Air mass (astronomy)

For air mass in meteorology, see air mass. For practical application, see air mass (solar energy).

In astronomy, air mass (or airmass) is the optical path length through Earth’s atmosphere for light from a celestial source. As it passes through the atmosphere, light is attenuated by scattering and absorption; the more atmosphere through which it passes, the greater the attenuation. Consequently, celestial bodies at the horizon appear less bright than when at the zenith. The attenuation, known as atmospheric extinction, is described quantitatively by the Beer–Lambert–Bouguer law.

“Air mass” normally indicates relative air mass, the path length relative to that at the zenith at sea level so, by definition, the sea-level air mass at the zenith is 1. Air mass increases as the angle between the source and the zenith increases, reaching a value of approximately 38 at the horizon. Air mass can be less than one at an elevation greater than sea level; however, most closed-form expressions for air mass do not include the effects of elevation, so adjustment must usually be accomplished by other means.

In some fields, such as solar energy and photovoltaics, air mass is indicated by the acronym AM; additionally, the value of the air mass is often given by appending its value to AM, so that AM1 indicates an air mass of 1, AM2 indicates an air mass of 2, and so on. The region above Earth’s atmosphere, where there is no atmospheric attenuation of solar radiation, is considered to have “air mass zero” (AM0).

Tables of air mass have been published by numerous authors, including Bemporad (1904), Allen (1976),^[1] and Kasten and Young (1989).

Calculating air mass

Plots of air mass using various formulas.

Zenith angle and altitude

Main article: Celestial coordinates

The angle of a celestial body with the zenith is the zenith angle (in astronomy, commonly referred to as the zenith distance). A body’s angular position can also be given in terms of altitude, the angle above the geometric horizon; the altitude $h$ and the zenith angle $z$ are thus related by

h=90^{\circ }-z\,.

Atmospheric Refraction

Atmospheric refraction causes light to follow an approximately circular path that is slightly longer than the geometric path, and the air mass must take into account the longer path (Young 1994). Additionally, refraction causes a celestial body to appear higher above the horizon than it actually is; at the horizon, the difference between the true zenith angle and the apparent zenith angle is approximately 34 minutes of arc. Most air mass formulas are based on the apparent zenith angle, but some are based on the true zenith angle, so it is important to ensure that the correct value is used, especially near the horizon.^[2]

Plane-parallel atmosphere

When the zenith angle is small to moderate, a good approximation is given by assuming a homogeneous plane-parallel atmosphere (i.e., one in which density is constant and Earth’s curvature is ignored). The air mass $X$ then is simply the secant of the zenith angle $z$ :

X=\sec \,z\,.

At a zenith angle of 60°, the air mass is approximately 2. The Earth is not flat, however, and, depending on accuracy requirements, this formula is usable for zenith angles up to about 60° to 75°. At greater zenith angles, the accuracy degrades rapidly, with $X=\sec \,z$ becoming infinite at the horizon; the horizon air mass in the more-realistic spherical atmosphere is usually less than 40.

Interpolative formulas

Many formulas have been developed to fit tabular values of air mass; one by Young and Irvine (1967) included a simple corrective term:

X=\sec \,z_{{\mathrm t}}\,\left[1-0.0012\,(\sec ^{2}z_{{\mathrm t}}-1)\right]\,,

where $z_{{\mathrm t}}$ is the true zenith angle. This gives usable results up to approximately 80°, but the accuracy degrades rapidly at greater zenith angles. The calculated air mass reaches a maximum of 11.13 at 86.6°, becomes zero at 88°, and approaches negative infinity at the horizon. The plot of this formula on the accompanying graph includes a correction for atmospheric refraction so that the calculated air mass is for apparent rather than true zenith angle.

Hardie (1962) introduced a polynomial in $\sec \,z-1$ :

X=\sec \,z\,-\,0.0018167\,(\sec \,z\,-\,1)\,-\,0.002875\,(\sec \,z\,-\,1)^{2}\,-\,0.0008083\,(\sec \,z\,-\,1)^{3}\,,

which gives usable results for zenith angles of up to perhaps 85°. As with the previous formula, the calculated air mass reaches a maximum, and then approaches negative infinity at the horizon.

Rozenberg (1966) suggested

X=\left(\cos \,z+0.025e^{{-11\cos \,z}}\right)^{{-1}}\,,

which gives reasonable results for high zenith angles, with a horizon air mass of 40.

Kasten and Young (1989) developed^[3]

X={\frac {1}{\cos \,z+0.50572\,(6.07995^{\circ }+90-z)^{{-1.6364}}}}\,,

which gives reasonable results for zenith angles of up to 90°, with an air mass of approximately 38 at the horizon. Here the second $z$ term is in degrees.

Young (1994) developed

X={\frac {1.002432\,\cos ^{2}z_{{\mathrm t}}+0.148386\,\cos \,z_{{\mathrm t}}+0.0096467}{\cos ^{3}z_{{\mathrm t}}+0.149864\,\cos ^{2}z_{{\mathrm t}}+0.0102963\,\cos \,z_{{\mathrm t}}+0.000303978}}\,,

in terms of the true zenith angle $z_{{\mathrm t}}$ , for which he claimed a maximum error (at the horizon) of 0.0037 air mass.

Pickering (2002) developed

X={\frac {1}{\sin(h+{244}/(165+47h^{{1.1}}))}}\,,

where $h$ is apparent altitude $(90^{\circ }-z)$ in degrees. Pickering claimed his equation to have a tenth the error of Schaefer (1998) near the horizon.^[4]

Atmospheric models

Interpolative formulas attempt to provide a good fit to tabular values of air mass using minimal computational overhead. The tabular values, however, must be determined from measurements or atmospheric models that derive from geometrical and physical considerations of Earth and its atmosphere.

Nonrefracting radially symmetrical atmosphere

Atmospheric effects on optical transmission can be modelled as if the atmosphere is concentrated in approximately the lower 9 km.

If refraction is ignored, it can be shown from simple geometrical considerations (Schoenberg 1929, 173) that the path $s$ of a light ray at zenith angle $z$ through a radially symmetrical atmosphere of height $y_{{{\mathrm {atm}}}}$ is given by

s={\sqrt {R_{{\mathrm {E}}}^{2}\cos ^{2}z+2R_{{\mathrm {E}}}y_{{\mathrm {atm}}}+y_{{\mathrm {atm}}}^{2}}}-R_{{\mathrm {E}}}\cos \,z\,,

or alternatively,

s={\sqrt {\left(R_{{\mathrm {E}}}+y_{{\mathrm {atm}}}\right)^{2}-R_{{\mathrm {E}}}^{2}\sin ^{2}z}}-R_{{\mathrm {E}}}\cos \,z\,,

where $R_{{\mathrm E}}$ is the radius of the Earth.

Homogeneous atmosphere

If the atmosphere is homogeneous (i.e., density is constant), the path at zenith is simply the atmospheric height $y_{{{\mathrm {atm}}}}$ , and the relative air mass is

X={\frac s{y_{{\mathrm {atm}}}}}={\frac {R_{{\mathrm {E}}}}{y_{{\mathrm {atm}}}}}{\sqrt {\cos ^{2}z+2{\frac {y_{{\mathrm {atm}}}}{R_{{\mathrm {E}}}}}+\left({\frac {y_{{\mathrm {atm}}}}{R_{{\mathrm {E}}}}}\right)^{2}}}-{\frac {R_{{\mathrm {E}}}}{y_{{\mathrm {atm}}}}}\cos \,z\,.

If density is constant, hydrostatic considerations give the atmospheric height as

y_{{\mathrm {atm}}}={\frac {kT_{0}}{mg}}\,,

where $k$ is Boltzmann’s constant, $T_{0}$ is the sea-level temperature, $m$ is the molecular mass of air, and $g$ is the acceleration due to gravity. Although this is the same as the pressure scale height of an isothermal atmosphere, the implication is slightly different. In an isothermal atmosphere, 37% of the atmosphere is above the pressure scale height; in a homogeneous atmosphere, there is no atmosphere above the atmospheric height.

Taking $T_{0}$ = 288.15 K, $m$ = 28.9644×1.6605×10⁻²⁷ kg, and $g$ = 9.80665 m/s² gives $y_{{\mathrm {atm}}}$ ≈ 8435 m. Using Earth’s mean radius of 6371 km, the sea-level air mass at the horizon is

X_{{\mathrm {horiz}}}={\sqrt {1+2{\frac {R_{{\mathrm {E}}}}{y_{{\mathrm {atm}}}}}}}\approx 38.87\,.

The homogeneous spherical model slightly underestimates the rate of increase in air mass near the horizon; a reasonable overall fit to values determined from more rigorous models can be had by setting the air mass to match a value at a zenith angle less than 90°. The air mass equation can be rearranged to give

{\frac {R_{{\mathrm {E}}}}{y_{{\mathrm {atm}}}}}={\frac {X^{2}-1}{2\left(1-X\cos z\right)}}\,;

matching Bemporad’s value of 19.787 at $z$ = 88° gives $R_{{\mathrm {E}}}/y_{{\mathrm {atm}}}$ ≈ 631.01 and $X_{{\mathrm {horiz}}}$ ≈ 35.54. With the same value for $R_{\mathrm {E} }$ as above, $y_{{\mathrm {atm}}}$ ≈ 10,096 m.

While a homogeneous atmosphere isn’t a physically realistic model, the approximation is reasonable as long as the scale height of the atmosphere is small compared to the radius of the planet. The model is usable (i.e., it does not diverge or go to zero) at all zenith angles, including those greater than 90° (see Homogeneous spherical atmosphere with elevated observer below). The model requires comparatively little computational overhead, and if high accuracy is not required, it gives reasonable results.^[5] However, for zenith angles less than 90°, a better fit to accepted values of air mass can be had with several of the interpolative formulas.

Variable-density atmosphere

In a real atmosphere, density decreases with elevation above mean sea level. The absolute air mass $\sigma$ then is

\sigma =\int \rho \,{\mathrm d}s\,.

For the geometrical light path discussed above, this becomes, for a sea-level observer,

\sigma =\int _{0}^{{y_{{\mathrm {atm}}}}}{\frac {\rho \,\left(R_{{\mathrm {E}}}+y\right){\mathrm d}y}{{\sqrt {R_{{\mathrm {E}}}^{2}\cos ^{2}z+2R_{{\mathrm {E}}}y+y^{2}}}}}\,.

The relative air mass then is

X={\frac \sigma {\sigma _{{\mathrm {zen}}}}}\,.

The absolute air mass at zenith $\sigma _{{\mathrm {zen}}}$ is also known as the column density.

Isothermal atmosphere

Several basic models for density variation with elevation are commonly used. The simplest, an isothermal atmosphere, gives

\rho =\rho _{0}e^{{-y/H}}\,,

where $\rho _{0}$ is the sea-level density and $H$ is the pressure scale height. When the limits of integration are zero and infinity, and some high-order terms are dropped, this model yields (Young 1974, 147),

X\approx {\sqrt {{\frac {\pi R}{2H}}}}\exp {\left({\frac {R\cos ^{2}z}{2H}}\right)}\,{\mathrm {erfc}}\left({\sqrt {{\frac {R\cos ^{2}z}{2H}}}}\right)\,.

An approximate correction for refraction can be made by taking (Young 1974, 147)

R=7/6\,R_{{\mathrm E}}\,,

where $R_{{\mathrm E}}$ is the physical radius of the Earth. At the horizon, the approximate equation becomes

X_{{\mathrm {horiz}}}\approx {\sqrt {{\frac {\pi R}{2H}}}}\,.

Using a scale height of 8435 m, Earth’s mean radius of 6371 km, and including the correction for refraction,

X_{{\mathrm {horiz}}}\approx 37.20\,.

Polytropic atmosphere

The assumption of constant temperature is simplistic; a more realistic model is the polytropic atmosphere, for which

T=T_{0}-\alpha y\,,

where $T_{0}$ is the sea-level temperature and $\alpha$ is the temperature lapse rate. The density as a function of elevation is

\rho =\rho _{0}\left(1-{\frac \alpha T}_{0}y\right)^{{1/(\kappa -1)}}\,,

where $\kappa$ is the polytropic exponent (or polytropic index). The air mass integral for the polytropic model does not lend itself to a closed-form solution except at the zenith, so the integration usually is performed numerically.

Compound atmosphere

Earth’s atmosphere consists of multiple layers with different temperature and density characteristics; common atmospheric models include the International Standard Atmosphere and the US Standard Atmosphere. A good approximation for many purposes is a polytropic troposphere of 11 km height with a lapse rate of 6.5 K/km and an isothermal stratosphere of infinite height (Garfinkel 1967), which corresponds very closely to the first two layers of the International Standard Atmosphere. More layers can be used if greater accuracy is required.^[6]

Refracting radially symmetrical atmosphere

When atmospheric refraction is considered, the absolute air mass integral becomes^[7]

\sigma =\int _{{r_{{\mathrm {obs}}}}}^{{r_{{\mathrm {atm}}}}}{\frac {\rho \,{\mathrm d}r}{{\sqrt {1-\left({\frac {n_{{\mathrm {obs}}}}n}{\frac {r_{{\mathrm {obs}}}}r}\right)^{2}\sin ^{2}z}}}}\,,

where $n_{{\mathrm {obs}}}$ is the index of refraction of air at the observer’s elevation $y_{{\mathrm {obs}}}$ above sea level, $n$ is the index of refraction at elevation $y$ above sea level, $r_{{\mathrm {obs}}}=R_{{\mathrm {E}}}+y_{{\mathrm {obs}}}$ , $r=R_{{\mathrm {E}}}+y$ is the distance from the center of the Earth to a point at elevation $y$ , and $r_{{\mathrm {atm}}}=R_{{\mathrm {E}}}+y_{{\mathrm {atm}}}$ is distance to the upper limit of the atmosphere at elevation $y_{{\mathrm {atm}}}$ . The index of refraction in terms of density is usually given to sufficient accuracy (Garfinkel 1967) by the Gladstone–Dale relation

{\frac {n-1}{n_{{\mathrm {obs}}}-1}}={\frac {\rho }{\rho _{{\mathrm {obs}}}}}\,.

Rearrangement and substitution into the absolute air mass integral gives

\sigma =\int _{{r_{{\mathrm {obs}}}}}^{{r_{{\mathrm {atm}}}}}{\frac {\rho \,{\mathrm d}r}{{\sqrt {1-\left({\frac {n_{{\mathrm {obs}}}}{1+(n_{{\mathrm {obs}}}-1)\rho /\rho _{{\mathrm {obs}}}}}\right)^{2}\left({\frac {r_{{\mathrm {obs}}}}r}\right)^{2}\sin ^{2}z}}}}\,.

The quantity $n_{{\mathrm {obs}}}-1$ is quite small; expanding the first term in parentheses, rearranging several times, and ignoring terms in $(n_{{\mathrm {obs}}}-1)^{2}$ after each rearrangement, gives (Kasten and Young 1989)

\sigma =\int _{{r_{{\mathrm {obs}}}}}^{{r_{{\mathrm {atm}}}}}{\frac {\rho \,{\mathrm d}r}{{\sqrt {1-\left[1+2(n_{{\mathrm {obs}}}-1)(1-{\frac \rho {\rho _{{\mathrm {obs}}}}})\right]\left({\frac {r_{{\mathrm {obs}}}}r}\right)^{2}\sin ^{2}z}}}}\,.

Homogeneous spherical atmosphere with elevated observer

Air mass for elevated observer in homogeneous spherical atmosphere

In the figure at right, an observer at O is at an elevation $y_{{\mathrm {obs}}}$ above sea level in a uniform radially symmetrical atmosphere of height $y_{{\mathrm {atm}}}$ . The path length of a light ray at zenith angle $z$ is $s$ ; $R_{\mathrm {E} }$ is the radius of the Earth. Applying the law of cosines to triangle OAC,

{\begin{aligned}\left(R_{{E}}+y_{{atm}}\right)^{{2}}&=s^{{2}}+\left(R_{{E}}+y_{{obs}}\right)^{{2}}-2\left(R_{{E}}+y_{{obs}}\right)s\cos \left(180^{{\circ }}-z\right)\\&=s^{{2}}+\left(R_{{E}}+y_{{obs}}\right)^{{2}}+2\left(R_{{E}}+y_{{obs}}\right)s\cos z\end{aligned}}

expanding the left- and right-hand sides, eliminating the common terms, and rearranging gives

{{s}^{{2}}}+2\left({{R}_{{{\text{E}}}}}+{{y}_{{{\text{obs}}}}}\right)s\cos z-2{{R}_{{{\text{E}}}}}{{y}_{{{\text{atm}}}}}-y_{{{\text{atm}}}}^{{2}}+2{{R}_{{{\text{E}}}}}{{y}_{{{\text{obs}}}}}+y_{{{\text{obs}}}}^{{2}}=0\,.

Solving the quadratic for the path length s, factoring, and rearranging,

s=\pm {\sqrt {{{\left({{R}_{{{\text{E}}}}}+{{y}_{{{\text{obs}}}}}\right)}^{{2}}}{{\cos }^{{2}}}z+2{{R}_{{{\text{E}}}}}\left({{y}_{{{\text{atm }}}}}-{{y}_{{{\text{obs}}}}}\right)+y_{{{\text{atm}}}}^{{2}}-y_{{{\text{obs}}}}^{{2}}}}-({{R}_{{{\text{E}}}}}+{{y}_{{{\text{obs}}}}})\cos z\,.

The negative sign of the radical gives a negative result, which is not physically meaningful. Using the positive sign, dividing by $y_{{\mathrm {atm}}}$ , and cancelling common terms and rearranging gives the relative air mass:

X={\sqrt {{{\left({\frac {{{R}_{{{\text{E}}}}}+{{y}_{{{\text{obs}}}}}}{{{y}_{{{\text{atm}}}}}}}\right)}^{{2}}}{{\cos }^{{2}}}z+{\frac {2{{R}_{{{\text{E}}}}}}{y_{{{\text{atm}}}}^{{2}}}}\left({{y}_{{{\text{atm}}}}}-{{y}_{{{\text{obs}}}}}\right)-{{\left({\frac {{{y}_{{{\text{obs}}}}}}{{{y}_{{{\text{atm}}}}}}}\right)}^{{2}}}+1}}-{\frac {{{R}_{{{\text{E}}}}}+{{y}_{{{\text{obs}}}}}}{{{y}_{{{\text{atm}}}}}}}\cos z\,.

With the substitutions ${\hat {r}}=R_{{\mathrm {E}}}/y_{{\mathrm {atm}}}$ and ${\hat {y}}=y_{{\mathrm {obs}}}/y_{{\mathrm {atm}}}$ , this can be given as

X={\sqrt {{{({\hat {r}}+{\hat {y}})}^{{2}}}{{\cos }^{{2}}}z+2{\hat {r}}(1-{\hat {y}})-{\hat {y}}^{2}+1}}\;-\;({\hat {r}}+{\hat {y}})\cos z\,.

When the observer’s elevation is zero, the air mass equation simplifies to

X={\sqrt {{{\left({\frac {{{R}_{{{\text{E}}}}}}{{{y}_{{{\text{atm}}}}}}}\right)}^{{2}}}{{\cos }^{{2}}}z+{\frac {2{{R}_{{{\text{E}}}}}}{{{y}_{{{\text{atm}}}}}}}+1}}-{\frac {{{R}_{{{\text{E}}}}}}{{{y}_{{{\text{atm}}}}}}}\cos z\,.

Maximum zenith angle

Maximum zenith angle for elevated observer in homogeneous spherical atmosphere

When the observer is at an elevation greater than that of the horizon, the zenith angle can be greater than 90°. The maximum possible zenith angle occurs when the ray is tangent to Earth’s surface; from triangle OCG in the figure at right,

\cos \gamma ={\frac {{{R}_{{{\text{E}}}}}+{{y}_{{{\text{obs}}}}}-h}{{{R}_{{{\text{E}}}}}+{{y}_{{{\text{obs}}}}}}}\,,

where $h$ is the observer’s height above the horizon. The geometrical dip of the horizon $\gamma$ is related to $z_{{\mathrm {max}}}$ by

\gamma ={{z}_{{{\text{max}}}}}-90{}^{\circ }\,,

so that

\cos \gamma =\cos \left({{z}_{{{\text{max}}}}}-90{}^{\circ }\right)=\sin {{z}_{{{\text{max}}}}}\,.

Then

\sin {{z}_{{{\text{max}}}}}={\frac {{{R}_{{{\text{E}}}}}+{{y}_{{{\text{obs}}}}}-h}{{{R}_{{{\text{E}}}}}+{{y}_{{{\text{obs}}}}}}}\,.

For a non-negative height $h$ , the angle $z_{{\mathrm {max}}}$ is always ≥ 90°; however, the inverse sine functions provided by most calculators and programming languages return values in the range ±90°. The value can be placed in the proper quadrant by

{{z}_{{{\text{max}}}}}=180{}^{\circ }-{{\sin }^{{-1}}}{\frac {{{R}_{{{\text{E}}}}}+{{y}_{{{\text{obs}}}}}-h}{{{R}_{{{\text{E}}}}}+{{y}_{{{\text{obs}}}}}}}\,.

If the horizon is at sea level, $y_{{\mathrm {obs}}}=h$ , and this simplifies to

{{z}_{{{\text{max}}}}}=180{}^{\circ }-{{\sin }^{{-1}}}{\frac {{{R}_{{{\text{E}}}}}}{{{R}_{{{\text{E}}}}}+h}}\,.

Nonuniform distribution of attenuating species

Atmospheric models that derive from hydrostatic considerations assume an atmosphere of constant composition and a single mechanism of extinction, which isn’t quite correct. There are three main sources of attenuation (Hayes and Latham 1975): Rayleigh scattering by air molecules, Mie scattering by aerosols, and molecular absorption (primarily by ozone). The relative contribution of each source varies with elevation above sea level, and the concentrations of aerosols and ozone cannot be derived simply from hydrostatic considerations.

Rigorously, when the extinction coefficient depends on elevation, it must be determined as part of the air mass integral, as described by Thomason, Herman, and Reagan (1983). A compromise approach often is possible, however. Methods for separately calculating the extinction from each species using closed-form expressions are described in Schaefer (1993) and Schaefer (1998). The latter reference includes source code for a BASIC program to perform the calculations. Reasonably accurate calculation of extinction can sometimes be done by using one of the simple air mass formulas and separately determining extinction coefficients for each of the attenuating species (Green 1992, Pickering 2002).

Air mass and astronomy

Atmospheric transmittance across the electromagnetic spectrum.

In optical astronomy the air mass provides an indication of the deterioration of the observed image, not only as regards direct effects of spectral absorption, scattering and reduced brightness, but also an aggregation of visual aberrations, e.g. resulting from atmospheric turbulence, collectively referred to as the quality of the seeing.^[8] On bigger telescopes, such as the WHT (Wynne and Warsick 1988) and VLT (Avila, Rupprecht, and Becker 1997), the atmospheric dispersion can be so severe that it affects the pointing of the telescope to the target. In such cases an atmospheric dispersion compensator is used, which usually consists of two The Greenwood frequency and Fried parameter, both relevant for adaptive optics depend on the air mass above them (or more specifically, on the zenith angle).

In radio astronomy the air mass (which influences the optical path length) is not relevant. The lower layers of the atmosphere, modeled by the air mass, do not significantly impede radio waves, which are of much lower frequency than optical waves. Instead, some radio waves are affected by the ionosphere in the upper atmosphere. Newer aperture synthesis radio telescopes are especially affected by this as they “see” a much larger portion of the sky and thus the ionosphere. In fact, LOFAR needs to explicitly calibrate for these distorting effects (van der Tol and van der Veen 2007; de Vos, Gunst, and Nijboer 2009), but on the other hand can also study the ionosphere by instead measuring these distortions (Thidé 2007).

Air mass and solar energy

Solar irradiance spectrum above atmosphere and at surface

Main article: Air mass (solar energy)

Atmospheric attenuation of solar radiation is not the same for all wavelengths; consequently, passage through the atmosphere not only reduces intensity but also alters the spectral irradiance. Photovoltaic modules are commonly rated using spectral irradiance for an air mass of 1.5 (AM1.5); tables of these standard spectra are given in ASTM G 173-03. The extraterrestrial spectral irradiance (i.e., that for AM0) is given in ASTM E 490-00a.^[9]

For many solar energy applications when high accuracy near the horizon is not required, air mass is commonly determined using the simple secant formula described in the section Plane-parallel atmosphere.

Notes

↑ Allen’s air mass table was an abbreviated compilation of values from earlier sources, primarily Bemporad (1904).
↑ At very high zenith angles, air mass is strongly dependent on local atmospheric conditions, including temperature, pressure, and especially the temperature gradient near the ground. In addition low-altitude extinction is strongly affected by the aerosol concentration and its vertical distribution. Many authors have cautioned that accurate calculation of air mass near the horizon is all but impossible.
↑ The Kasten and Young formula was originally given in terms of altitude $\gamma$ as
$X={\frac {1}{\sin \,\gamma +0.50572\,(\gamma +6.07995^{\circ })^{{-1.6364}}}}\;;$
in this article, it is given in terms of zenith angle for consistency with the other formulas.
↑ Pickering (2002) uses Garfinkel (1967) as the reference for accuracy.
↑ Although acknowledging that an isothermal or polytropic atmosphere would have been more realistic, Janiczek and DeYoung (1987) used the homogeneous spherical model in calculating illumination from the Sun and Moon, with the implication that the slightly reduced accuracy was more than offset by the considerable reduction in computational overhead.
↑ The notes for Reed Meyer’s air mass calculator describe an atmospheric model using eight layers and using polynomials rather than simple linear relations for temperature lapse rates.
↑ See Thomason, Herman, and Reagan (1983) for a derivation of the integral for a refracting atmosphere.
↑ Observing tips: air mass and differential refraction retrieved 15 May 2011.
↑ ASTM E 490-00a was reapproved without change in 2006.

References

Allen, C. W. 1976. Astrophysical Quantities, 3rd ed. 1973, reprinted with corrections, 1976. London: Athlone, 125. ISBN 0-485-11150-0.
ASTM E 490-00a (R2006). 2000. Standard Solar Constant and Zero Air Mass Solar Spectral Irradiance Tables. West Conshohocken, PA: ASTM. Available for purchase from ASTM.Optical Telescopes of Today and Tomorrow
ASTM G 173-03. 2003. Standard Tables for Reference Solar Spectral Irradiances: Direct Normal and Hemispherical on 37° Tilted Surface. West Conshohocken, PA: ASTM. Available for purchase from ASTM.
Avila, Gerardo; Rupprecht, Gero; Beckers, J. M. (1997). Arne L. Ardeberg, ed. "Atmospheric dispersion correction for the FORS Focal Reducers at the ESO VLT". Proceedings of SPIE. 2871 Optical Telescopes of Today and Tomorrow. SPIE: 1135–1143. Bibcode:1997SPIE.2871.1135A. doi:10.1117/12.269000.
Bemporad, A. 1904. Zur Theorie der Extinktion des Lichtes in der Erdatmosphäre. Mitteilungen der Grossh. Sternwarte zu Heidelberg Nr. 4, 1–78.
Garfinkel, B. 1967. Astronomical Refraction in a Polytropic Atmosphere. Astronomical Journal 72:235–254. doi: 10.1086/110225. Bibcode 1967AJ.....72..235G.
Green, Daniel W. E. 1992. Magnitude Corrections for Atmospheric Extinction. International Comet Quarterly 14, July 1992, 55–59.
Hardie, R. H. 1962. In Astronomical Techniques. Hiltner, W. A., ed. Chicago: University of Chicago Press, 184–. LCCN 62009113. Bibcode 1962aste.book.....H.
Hayes, D. S., and D. W. Latham. 1975. A Rediscussion of the Atmospheric Extinction and the Absolute Spectral-Energy Distribution of Vega. Astrophysical Journal 197:593–601. doi: 10.1086/153548. Bibcode 1975ApJ...197..593H.
Janiczek, P. M., and J. A. DeYoung. 1987. Computer Programs for Sun and Moon Illuminance with Contingent Tables and Diagrams, United States Naval Observatory Circular No. 171. Washington, D.C.: United States Naval Observatory. Bibcode 1987USNOC.171.....J.
Kasten, F.; Young, A. T. (1989). "Revised optical air mass tables and approximation formula". Applied Optics. 28: 4735–4738. Bibcode:1989ApOpt..28.4735K. doi:10.1364/AO.28.004735.
Pickering, K. A. (2002). "The Southern Limits of the Ancient Star Catalog" (PDF). DIO. 12 (1): 20–39.
Rozenberg, G. V. 1966. Twilight: A Study in Atmospheric Optics. New York: Plenum Press, 160. Translated from the Russian by R. B. Rodman. LCCN 65011345.
Schaefer, B. E. 1993. Astronomy and the Limits of Vision. Vistas in Astronomy 36:311–361. doi: 10.1016/0083-6656(93)90113-X. Bibcode 1993VA.....36..311S.
Schaefer, B. E. 1998. To the Visual Limits: How deep can you see?. Sky & Telescope, May 1998, 57–60.
Schoenberg, E. 1929. Theoretische Photometrie, Über die Extinktion des Lichtes in der Erdatmosphäre. In Handbuch der Astrophysik. Band II, erste Hälfte. Berlin: Springer.
Thidé, Bo. 2007. Nonlinear physics of the ionosphere and LOIS/LOFAR Plasma Physics and Controlled Fusion. 49(12B, December): B103–B107. doi: 10.1088/0741-3335/49/12B/S09. Bibcode 2007PPCF...49..103T.
Thomason, L. W., B. M. Herman, and J. A. Reagan. 1983. The effect of atmospheric attenuators with structured vertical distributions on air mass determination and Langley plot analyses. Journal of the Atmospheric Sciences 40:1851–1854. doi: 10.1175/1520-0469(1983)040<1851:TEOAAW>2.0.CO;2. Bibcode 1983JAtS...40.1851T.
van der Tol, S., and A. J. van der Veen. 2007 Ionospheric Calibration for the LOFAR Radio Telescope. International Symposium on Signals, Circuits and Systems, July, 2007. doi: 10.1109/ISSCS.2007.4292761. Available as PDF.
de Vos, M., A. W. Gunst, and R. Nijboer. 2009. The LOFAR Telescope: System Architecture and Signal Processing. Proceedings of the IEEE. 97(8): 1431–1437. doi: 10.1109/JPROC.2009.2020509. Bibcode 2009IEEEP..97.1431D. Available as PDF from www.astro.rug.nl.
Wynne, C. G., and S. P. Worswick. 1988. Atmospheric dispersion at prime focus. Royal Astronomical Society, Monthly Notices 230:457–471 (February 1988). Bibcode 1988MNRAS.230..457W.
Young, A. T. 1974. Atmospheric Extinction. Ch. 3.1 in Methods of Experimental Physics, Vol. 12 Astrophysics, Part A: Optical and Infrared. ed. N. Carleton. New York: Academic Press. ISBN 0-12-474912-1.
Young, A. T. 1994. Air mass and refraction. Applied Optics. 33:1108–1110. doi: 10.1364/AO.33.001108. Bibcode 1994ApOpt..33.1108Y. (payment required)
Young, A. T., and W. M. Irvine. 1967. Multicolor photoelectric photometry of the brighter planets. I. Program and procedure. Astronomical Journal 72:945–950. doi: 10.1086/110366. Bibcode 1967AJ.....72..945Y.

External links

Reed Meyer’s downloadable airmass calculator, written in C (notes in the source code describe the theory in detail)
NASA Astrophysics Data System A source for electronic copies of some of the references.

This article is issued from Wikipedia - version of the 1/27/2016. The text is available under the Creative Commons Attribution/Share Alike but additional terms may apply for the media files.