Where does Earth ’ s atmosphere get its energy ?

The Sun is Earth’s primary source of energy. In this paper, we compare the magnitude of the Sun to all other external (to the atmosphere) energy sources. These external sources were previously identified in Sellers (1965); here, we quantify and update them. These external sources provide a total energy to the Earth that is more than 3700 times smaller than that provided by the Sun, a vast majority of which is provided by heat from the Earth’s interior. After accounting for the fact that 71% of incident solar radiation is deposited into the earth system, the Sun provides a total energy to Earth that is still more than 2600 times larger than the sum of all other external sources.


Introduction
William D. Sellers book Physical Climatology, published in 1965, included a table on large-scale energy sources ''that act continuously or quasicontinuously in the atmosphere and at its boundaries'' (Table 2 in Sellers 1965).In a number of talks presented by the authors of this paper over the past decade, Sellers' (1965)  There are some noteworthy comments regarding the table.The caption to the table and its discussion in the text imply that the table is not intended to be considered complete.Some of the in situ energy sources in the original table, for example lightning discharges and fossil fuel combustion, appear to be arbitrary, accounting for a small number of important sources that could have been included.For example, convective and latent heat transfer and infrared emission were not in Sellers' list.A footnote to the table suggests that it was intended for comparative purposes: ''most of the data in this table and in Table 3 have been obtained from an unpublished series of notes by H.H. Lettau (Department of Meteorology, University of Wisconsin)''. 1n this paper, we attempted to maintain fidelity to the original intent of the table, giving primary attention to the same sources in Sellers (1965).The origins of most of the sources are external to the atmosphere and therefore, provide the intended context to the question, where does the atmosphere get its energy?That the list of internal sources is incomplete is of minor consequence.After all, in equilibrium these must balance the input from the Sun and other external sources since they are redistributions of those sources.A more complete accounting of internal sources can be found in other, widely referenced studies by Wild et al. (2013), Stephens et al. (2012), and Trenberth et al. (2009).Finally, it was not our intention to provide a complete literature review of the various sources of energy.The range of physical processes underlying the generation and dissipation of these energy sources requires an endeavor far beyond the scope of this paper.
The following Section 2 provides the background for the revisions to each of the terms in the original table.In Section 3, we provide a few external sources of energy that were not included in the original Sellers table.

Updates to Sellers' large-scale energy sources
Here we provide the basis for updates to the entries in Sellers' (1965) Table 2 (and shown in Table 2 in this paper).Each source is discussed in a subsection with the exception of lunar reflection and emission, which are combined in a single section.Note that the energy from these sources is deposited at depths varying from near the top-of-the-atmosphere (if there is such a thing) to the Earth's surface, necessitating a common reference depth to compare flux densities from different sources.Unless otherwise noted, flux densities are derived for a reference sphere of radius equal to Earth's mean radius; that is, the reference depth is at the surface.When measurement or model uncertainties were found in the published literature they were included in our updated values.In other cases, ranges of estimates are listed to provide either minimum to maximum power inputs for a given source or estimates from multiple references.In most (but not all) instances we resist explaining differences between our updated values and Sellers' original estimates because there is no way of determining how Sellers derived his values.Sellers and Lettau are deceased.

Solar irradiance
The Sun impacts the Earth and its atmosphere in a variety of ways and to differing degrees.The Sun's influence extends from the farthest reaches of Earth's magnetic field where charged particles from the Sun interact with Earth's magnetosphere, all the way down to Earth's surface.Here we present the Sun's dominant energy input to the Earth, solar irradiance, or radiant flux density.The most accurate measurement of the spectrally integrated solar irradiance, called Total Solar Irradiance (TSI), provided by Kopp & Lean (2011), is 1360.8W m À2 .Distributed uniformly over the Earth's surface (globally averaged) this amounts to 340.2 ± 0.12 W m À2 .This is the basis of reference for all of the other energy sources discussed in this section.Contrast this with Sellers' (1965) value of 348.9 W m À2 , more than a decade before the first measurements of TSI from space.Solar irradiance varies on timescales from minutes to eons (Willson & Hudson 1988;Hoyt & Schatten 1997;Usoskin et al. 2007;Solanki et al. 2013), due to the turbulent convection-induced dynamical motions and magnetic phenomena within the Sun (Charbonneau 2014) and the rotation of the Sun over a 27-day period (Fröhlich & Lean 2004).The top-of-the-atmosphere solar irradiance, or TSI, varies by approximately 0.1% over the 11-year solar cycle (Willson & Hudson 1991;Lean 1997;Fröhlich 2006;Kopp 2014).This energy is distributed across the entire spectrum from gamma rays (10 À10 m) to radiowaves (>10 2 m), although 97% of the total energy occurs between 200 and 2400 nm (Harder et al. 2009).Figure 1 shows the solar spectrum measured by the Spectral Irradiance Monitor (SIM) (Harder et al. 2005) onboard NASA's Solar Radiation and Climate Experiment (SORCE) satellite.Solar Spectral Irradiance (SSI) ranges from roughly 0.5 W m À2 nm À1 at 310 nm, to a maximum of around 2 W m À2 nm À1 at around 500 nm.SSI exhibits the greatest relative variability over the solar cycle at ultraviolet (UV) wavelengths; for example, the relative variability of irradiance in the extreme UV is over 100 times that of TSI, and there is very little variability in the infrared (Floyd et al. 2003;Ermolli et al. 2013 and references therein).
While TSI constrains the magnitude of solar variability, the Earth's climate response to the solar variability is wavelength dependent.Within Earth's atmosphere and its surface, the incoming solar energy is scattered and absorbed in unique, wavelength-dependent ways.The impact of solar variability on climate is thought to be a combination of several factors, many of which are beyond the scope of this paper.The reader is referred to Ermolli et al. (2013), Solanki et al. (2013), and Gray et al. (2010) for recent reviews of solar influences on climate.

Earth's interior heat flux
The Earth is constantly emitting thermal energy (heat) from its interior and crust into the atmosphere and global oceans.Current estimates of the total heat flux from Earth's interior are 44.2 ± 1.0 • 10 12 W (Pollack et al. 1993;Gando et al. 2011) and 46 ± 3 • 10 12 W (Jaupart et al. 2015) with 32 ± 2 • 10 12 W lost through the ocean floor and 14 ± 1 • 10 12 W lost through continental areas (Jaupart et al. 2015).It is estimated that approximately half of this energy comes from radioactive decay of four primary elements: Uranium 238, Uranium 235, Thorium 232, and Potassium 40, and subsequent conduction and convection from the crust, mantle, and core (Fowler 1990;Stacey & Davis 2008); the remaining flux is likely due to primordial heat from gravitational energy during the formation of the Earth, which continues to cool since its formation (Fowler 1990;Gando et al. 2011).
There are estimates of the magnitude and spatial distribution (Fig. 2) of global heat loss.These estimates of global heat loss, summarized in Jaupart et al. (2015), span 41-47 • 10 12 W and are made using data sets of heat flux observations (Fig. 3) and, for the oceans, a combination of measurements with an improved theoretical thermal model validated against local measurements (Williams & Von Herzen 1974;Davies 1980aDavies , 1980b;;Sclater et al. 1980;Pollack et al. 1993;Davies & Davies, 2010;Jaupart et al. 2015).The thermal model is used to quantify the additional heat transfer by hydrothermal convective circulation (Stein & Stein, 1992) (i.e., in addition to the conductive ocean heat measured at heat flux observation sites), particularly in regions of young seafloors that are characterized by fractured crust and larger and more variable heat flows.Estimates of the energy released from Earth's interior made from observations alone are smaller, ranging from 29 to 34 • 10 12 W (Hofmeister & Criss 2005;Hamza et al. 2008).
Using the estimate from Jaupart et al. (2015) of 46 ± 3 • 10 12 W, we obtain an average surface flux density of 0.09 ± 0.006 W m À2 .We note the change from Sellers' (1965) estimate of 0.0612 W m À2 is likely attributable to the improvement in the number, location, and quality of measurements, improvements in hydrothermal circulation models, and improved understanding of uncertainties as identified in Jaupart et al. (2015) and references within.

Infrared and reflected radiation from the full Moon
It was difficult and in most cases, impossible, to determine the sources of differences between our updated estimates and those from Sellers' original table.Lunar emission and scattering of sunlight are two of the entries where we could reproduce exactly what Sellers estimated, making some common assumptions: the Moon emits as a blackbody and it is a perfect diffuser, scattering isotropically.In principle, neither assumption is true but they provide the basis for making a simple estimate.
Using these assumptions and simple energy balance, the emitted irradiance at the Moon's surface, F E , averaged over the sunlit side of the full Moon is: where a M is the lunar albedo and S 0 is the normally incident solar irradiance, or TSI.The reflected irradiance at the Moon's surface, F R , averaged over the sunlit hemisphere is: where the average cosine of solar zenith angle, " l, is 0.5.While the respective irradiances, F E and F R , contributing ) measured by the SIM instrument (Harder et al. 2005) between 300 and 2400 nm.
A.C. Kren et al.: Where does Earth's atmosphere get its energy? to Earth's energy budget would diminish by an amount proportional to the inverse of the square of the distance between Earth and Moon, the ratio of emitted to reflected irradiance is invariant with distance and is simply: Sellers' estimate of this ratio is exactly 3, indicating that he assumed a lunar albedo of 0.25, considerably higher than modern estimates closer to 0.1.For example, Matthews (2008) published a measured lunar albedo of 0.1362.Using this value, the ratio of emitted to reflected full Moon radiation is more than a factor of 6.To determine the value for both lunar irradiances requires TSI (S0) at the Moon, assumed to be the same as for Earth, 1360.8W m À2 (Kopp & Lean 2011).Using equations ( 1) and (2) we estimate a full Moon emitted irradiance of 588 W m À2 and reflected solar irradiance of 93 W m À2 .These simple estimates can be compared to measurements from the Clouds and the Earth's Radiant Energy System (CERES) Terra and Aqua satellite observations (Matthews 2008), which reported 977 W m À2 and 180 W m À2 for emitted and reflected irradiance, respectively, at 7°phase angle.To compare with the hemispherical-averaged values from our estimates, both measured irradiances are divided by 2, to arrive at 488.5 W m À2 for full Moon emission and 90 W m À2 for reflected solar irradiance.The latter is remarkably close to our simple estimate that used the same measured lunar albedo from Matthews (2008).There is a much larger difference, approximately 20%, between our simple estimate and measured lunar emission from CERES.This may be explained by measurements of lunar emissivity that differ significantly from unity over much of the infrared spectrum (Murcray 1965;Murcray et al. 1970).
Because in our simple model we assumed that the Moon scatters solar radiation isotropically and emits as a blackbody and therefore, also emits isotropically, scattered and emitted radiances are F R /p and F E /p, respectively.Furthermore,  because the solid angle that the Moon subtends at the Earth is much less than unity, we approximate the lunar irradiances incident on the Earth by the product of lunar radiance and the solid angle of the Moon, 6.5 • 10 À5 steradians.Using the CERES measurements of irradiances averaged over the full sunlit Moon we arrive at 0.010 W m À2 for full Moon emission and 0.0018 W m À2 for full Moon solar reflected irradiance incident on the Earth.Note that these values were derived for the mean of the Earth-Moon distance, which varies by approximately 13% over the orbit (Allen 1973), meaning that the full Moon emitted and reflected irradiance incident at Earth will vary by approximately 27%.

Combustion of coal, oil, and gas in the United States
The Sellers (1965) value of heat flux from combustion of coal, oil, and gas in the United States was 0.0024 W m À2 when globally distributed.To update, we used data for the consumption measurements of coal, oil, and gas over the continental United States for the year 2015 archived at the United States Energy Information Administration (EIA) (http://www.eia.gov).Since 1950, consumption of these resources in the U.S. has increased from 31 quadrillion British Thermal Units (BTUs) to approximately 79 quadrillion BTUs, leading to an updated flux density of 0.0052 W m À2 .For a global nonrenewable energy consumption estimate, including nuclear, we cite Flanner ( 2009) for the year 2005 to derive a flux density of 0.028 W m À2 .

Magnetic storm dissipation
Geomagnetic storms are caused by high-speed streams of the solar wind that increase the flux of energetic particles entering the magnetosphere, creating an enhanced ring current formed by ions and electrons that circle the Earth (Gonzalez et al. 1994) and causing a change in Earth's magnetic field (Akasofu 1978;Gonzalez et al. 1994;Kamide et al. 1998;Eddy 2009;Lopez et al. 2009).Coronal Mass Ejections (CMEs) and to a lesser extent, coronal holes, are primarily responsible for geomagnetic storms (Gosling et al. 1991;Kamide et al. 1998).CMEs, which are most prevalent during solar maximum (Kamide et al. 1998), are intense bursts of the solar wind that can reach speeds of 2000 km s À1 (Gosling & Forsyth 2001) and rise above the solar corona.Coronal holes, more prevalent during solar minimum, are regions of anomalously low density and temperature in the solar corona that emit plasma at speeds of 750-800 km s À1 (Zirker 1977;Kamide et al. 1998).Magnetic storms are principal drivers of major disturbances on Earth, such as power system blackouts and phone system outages (Boteler et al. 1998;Pulkkinen 2007).However, we also have magnetic storms to thank for the creation of beautiful aurorae in the night sky.
There are different pathways for the dissipation of energy from geomagnetic storms (Weiss et al. 1992;Slinker et al. 1995;Silbergleit et al. 1997;Lu et al. 1998;Slavin et al. 1998).The partitioning of the magnetic storm dissipation energy can be estimated using multiple techniques including ground and satellite-based observations of energy fluxes, empirical formulas (e.g., Pulkkinen et al. 2002;Li et al. 2012), model simulations (Palmroth et al. 2004;Tanskanen et al. 2005;Ngwira et al. 2013), and assimilation techniques (Lu et al. 1998).In empirical methods, for example, estimates of the solar wind input energy, a function of solar wind speed and solar magnetic field orientation and strength (Silbergleit et al. 1997) is used to determine the energy input into the magnetosphere (Gonzalez et al. 1994;Pulkkinen et al. 2002).In-situ measurements of the precipitation of auroral particles (Pulkkinen et al. 2002) can be used in combination with auroral models to estimate magnetic storm energy.Assimilation techniques such as the Assimilative Mapping of Ionospheric Electrodynamics (AMIE) method can also be used to study magnetic storm energy and dissipation; in one particular case it was shown that 400 GW (1 GW = 1.0 • 10 9 W) of energy was deposited during a magnetic storm and partitioned such that 190 GW went into Joule heating, 120 GW into ring current injection, and 90 GW into auroral precipitation (Lu et al. 1998).
The average magnetic storm flux density dissipation that spans substorm through intense geomagnetic activity is 0.00399 W m À2 when distributed over the Earth's surface.Auroral emission is included in this estimate.Since Sellers (1965) treated auroral emission separately from geomagnetic storm dissipation, we remove the average auroral flux density equal to 3.7 • 10 À4 W m À2 (see Sect. 2.8 for details) from the average magnetic storm flux density.The resulting global average flux density for magnetic storm dissipation, excluding the auroral component, is 0.00362 W m À2 and the range in values spans ~10 À5 W m À2 to ~10 À3 W m À2 .The Sellers (1965) estimate of 6.8 • 10 À5 W m À2 falls within this range.

Solar atmospheric tides
The Sun imparts a tidal force on Earth's atmosphere through radiative heating of the atmosphere and surface and latent heat release via global scale convection (Zhang et al. 2010a(Zhang et al. , 2010b)).Additional sources of tidal forcing come from nonlinear interactions between planetary waves (McLandress 2002), interactions between gravity waves and tides (McLandress & Ward 1994), and to a lesser extent, by the gravitational force of the Sun on the Earth (Hagan & Forbes 2002).Each of these components modifies the dynamical motion of the upper atmosphere through temperature and wind perturbations.The solar tides are one of the dominant features present in the mesosphere and lower thermosphere (Chapman & Lindzen 1970;Oberheide et al. 2002).
Radiative and latent heating components due to the Sun produce tidal oscillations and amplitudes that can be found at both diurnal and semi-diurnal timescales, with additional components often ignored due to their smaller contributions (Chapman & Lindzen 1970).This heating, the vast majority of which originates in the troposphere, generates vertically propagating internal gravity waves that arise from density fluctuations (Holton 2004).These waves propagate vertically into the upper atmosphere, where their growth and amplitudes increase exponentially, influencing the large-scale global circulation patterns through temperature, pressure, and wind modulation (Oberheide et al. 2002;Zhang et al. 2010a).These waves dissipate and reach maximum amplitude in the mesosphere and lower thermosphere at altitudes between 80 and 120 km (Zhang et al. 2010a).
At the surface, heating from sensible and latent heat fluxes over land and ocean can induce pressure amplitudes of approximately 1.3 hPa (Dai & Wang 1999).In the mesosphere and lower thermosphere, satellite observations of radiative flux and temperature, as well as tidal and general circulation models, indicate amplitudes of the solar atmospheric tide on zonal mean temperature and winds ranging from 10 to 40 K and 20 to 60 ms À1 , respectively (Forbes 1982b;Angelats & Forbes 2002;Hagan & Forbes 2002;Forbes et al. 2006Forbes et al. , 2008;;Hagan et al. 2009;Zhang et al. 2010aZhang et al. , 2010b)).Groves & Forbes (1984) estimated the energy dissipated within the atmosphere by the diurnal and semi-diurnal solar tidal forces.First, they calculated the time averaged and subsequent global mean vertical energy flux deposited in the upper atmosphere using a numerical tidal model from the surface to 400 km, which included temperature, pressure, wind, and vertical velocity fields derived by Forbes (1982a).This tidal model incorporated background wind and temperature fields, atmospheric composition, eddy and molecular diffusion, and tidal forcing through realistic water vapor and ozone heating rates in the upper atmosphere (Forbes 1982a).Globally averaged, the solar diurnal and equinox semi-diurnal components of the vertical energy flux are 1.64 • 10 À3 W m À2 and 0.044 • 10 À3 W m À2 , together yielding a global average at Earth's surface of 1.68 • 10 À3 W m À2 (Groves & Forbes 1984), roughly 50% smaller than the estimate from Sellers (1965) of 3.4 • 10 À3 W m À2 .

Lightning discharge energy
Global sensible and latent heat fluxes transport heat and moisture vertically into the atmosphere, providing energy to fuel thunderstorms.The majority of lightning is associated with these convective thunderstorms (Uman 1987;MacGorman & Rust 1998;Rakov & Uman 2003).The original source of these energy fluxes is, of course, the Sun.
The first estimate of global lightning frequency was performed by Brooks (1925).This estimate was derived by compiling a climatological survey of thunderstorm frequency over the globe, obtained from meteorological stations and ocean ship logs.Data was primarily available over central Europe and eastern North America.Using a flash rate measured from a single storm in England in June 1908, Brooks (1925) applied his thunderstorm climatology to infer global lightning flash rate as a function of season, latitude, ocean, and land (Orville & Spencer 1979).He obtained an average global frequency of 100 flashes s À1 .This value was well accepted until the satellite observations commenced in the 1960s (Orville & Spencer 1979).Estimates of lightning frequency from satellites using photometers, photographs, and lightning detectors (e.g., Sparrow & Ney 1968, 1971;Orville & Spencer 1979;Kotaki & Katoh 1983;Mackerras et al. 1998) showed a wide range in frequency, from 14 to 400 flashes s À1 (Orville & Spencer 1979;Mackerras et al. 1998;Schumann & Huntrieser 2007).Most of these estimates were hampered by a limited observational period, taken primarily at night, over selected regions, and exhibited low detection efficiency (Christian et al. 2003).This led to uncertainties in the frequency of lightning over diurnal, seasonal, and annual time periods.
More recent space-borne measurements of lightning frequency establish global lightning flash rates of 44 ± 5 flashes s À1 based on a 5-year climatology using day and night intra- Figure 4 shows the annually averaged global distribution of total lightning activity (flashes km À2 yr À1 ) from 1995 to 2013 (Cecil et al. 2014, with data updated through 2013).The majority of lightning flashes occur in the tropics and over land, where the storm updrafts are most intense to produce electrification (Zipser 1994).Approximately 1.46 billion flashes occur annually over the Earth (Cecil et al. 2014).We derived the global power per unit area dissipated by lightning discharges by multiplying the average amount of energy per single lightning flash by the global lightning frequency.Using the Cecil et al. (2014) estimate of 46 flashes s À1 and the dissipative range of energy per flash of 10 9 -10 10 J (Price et al. 1997), the total power dissipated globally by lightning per year is 4.6 • 10 10 to 4.6 • 10 11 W.This corresponds to a global power per unit area between 9 • 10 À5 and 9 • 10 À4 W m À2 , with an average of 4.95 • 10 À4 W m À2 .Sellers' (1965) estimate of 2.0 • 10 À4 W m À2 is within this range.

Auroral emission
The aurora is a luminous emission that takes place in the upper part of the atmosphere (Liu et al. 2008).It is driven by the interaction between Earth's magnetic field and solar energetic particles carried by the solar wind (Vazquez & Vaquero 2010).When the solar energetic particles interact with atomic and molecular nitrogen and oxygen at altitudes between 90 and 150 km, the excited nitrogen and oxygen atoms and molecules emit excess energy and drop into a lower energy state, producing the auroral light (Bone 2007).These energetic particles also produce upper atmospheric warming, ionization, dissociation, and recombination, as well as increased horizontal wind velocity and the generation of vertical winds (Christensen et al. 1997;Hecht et al. 2006;Oyama et al. 2010).These energetic particles therefore play a significant role in the chemistry of the upper stratosphere to the lower mesosphere (Seppälä et al. 2006;Pulkkinen 2007;Jackman et al. 2009).The predominant particles responsible for the auroral precipitation are charged electrons in the 1-30 keV range (Bone 2007), with charged protons contributing ~10-15% of the total (Hardy et al. 1989;Emery et al. 2008).The aurora occurs in both the northern (aurora borealis) and southern (aurora australis) polar regions.
Since the 1970s, measurements of the auroral emission and energy fluxes have been available from global satellite observations (e.g., Hardy et al. 1985;Fuller-Rowell & Evans 1987;Torr et al. 1995;Germany et al. 1997;Frey et al. 2001;Christensen et al. 2003;Emery et al. 2008;Hecht et al. 2008;Liou 2010).The global auroral power can be calculated directly by the in-situ energy flux measurements, indirectly by incorporating the observed emissions into auroral models, or through empirical relationships between the auroral brightness and energy flux (e.g., Newell et al. 2001Newell et al. , 2009;;Emery et al. 2008).
We obtain a direct estimate of the auroral emission, over the 275-815 nm spectral range by using observations from the Optical Spectrograph and InfraRed Imager System (OSIRIS) spectrograph on the Odin spacecraft (Gattinger et al. 2009(Gattinger et al. , 2010)).OSIRIS measures the limb brightness of the aurora at 1 nm resolution at a tangent altitude of 105 km (Gattinger et al. 2009).We spectrally integrate OSIRIS aurora spectra at a single latitude and longitude from 2003 (Gattinger et al. 2009; Fig. 1) and 2005 (Gattinger et al. 2010; Fig. 1) and obtain 0.044 W m À2 and 0.060 W m À2 , respectively.To convert these values to a global auroral emission, we make the following assumptions.First, the width of the auroral oval is 6.5°e xtending from 60.5°to 67°N (Akasofu 1966;Rostoker & Skone 1993); we compute the surface area bounded by these latitude and longitudes at an altitude of 105 km above Earth to be equal to 1.27 • 10 13 m 2 .Second, the aurora does not vary in time or space so the point values of auroral emission obtained using the Gattinger et al (2009;2010) data are representative of all latitudes and longitudes within the defined auroral oval.Therefore, the conversion from hemispheric to global auroral power is a factor of 2. Using these assumptions, the global auroral power derived from the OSIRIS point values is 1.12 • 10 12 W and 1.52 • 10 12 W, respectively.By taking the average of these values and then another average over Earth's surface area, we derive an average global auroral flux density of 2.6 • 10 À3 W m À2 .
Using the same set of assumptions given above, we use a point value of auroral emission of 0.018 W m À2 (Chamberlain 1961; Table 5.5) to compute an average global average auroral flux density of 8.96 • 10 À4 W m À2 .Similarly, measurements of three intense geomagnetic storms in October and November 2003 were shown to provide an average global auroral power dissipation of 613 GW (Alex et al. 2006); we used this value to derive a global average auroral flux density of 1.2 • 10 À3 W m À2 .
The range in auroral flux densities varies with the time rate of change of magnetic activity acting on the magnetosphere.The planetary index, K p , is representative of the time rate of change of magnetic activity where large values of K p indicate intense magnetic and auroral activity (Dessler & Fejer 1963).Hubert et al. (2002) derived hemispheric auroral power for four magnetic storm events in 2000 and related these to K p level by matching the observed in-situ energy flux measurements to climatological energy flux maps (based on K p levels 0-5+; Fuller-Rowell & Evans 1987).The hemispheric power ranges from ~20 GW for K p of 3 to as high as 115 GW for K p of 6 (Hubert et al. 2002).Luan et al. (2010) found a similar range in hemispheric auroral power as a function of K p level from ~5 years of satellite measurements (~30 GW for K p 3 to ~92 GW for K p 6).Again, using the same set of assumptions listed above, we converted the Hubert et al. (2002) auroral power values to energy flux densities as a function of K p index to obtain a range in globally averaged auroral flux densities from 7.8 • 10 À5 W m À2 for K p of 3 to 4.5 • 10 À4 W m À2 for K p of 6.
Our ranges in auroral flux densities were derived using assumptions that affect the accuracy of our estimations.We assumed the aurora is hemispherically symmetrical, which it is not (Laundal & Østgaard 2009;Luan et al. 2010).We also assumed that the auroral emission at one latitude and longitude is representative of all locations within the auroral oval, but there is spatial and seasonal variability (Miyashita et al. 2005;Coumans et al. 2004;Luan et al 2010).Given these caveats, we provide an estimate of the ranges in globally averaged auroral flux density equal to ~10 À5 W m À2 to 10 À4 W m À2 (for K p levels of 3 to 6) to ~10 À3 W m À2 (for intense geomagnetic activity).An average, over all geomagnetic activity levels, is 3.7 • 10 À4 W m À2 .The Sellers (1965) estimate of 4.8 • 10 À5 W m À2 falls within this range.

Zodiacal irradiance
The zodiacal irradiance (or light) is sunlight scattered from the zodiacal cloud, which is composed of micron to millimeter sized particles of interplanetary dust distributed between the Sun and the orbit of the asteroid belt and orbiting the Sun in a disk along the ecliptic (Edberg & Levy 1994;Fixsen & Dwek 2002;Ishiguro et al. 2013).It is visible to the naked eye as a bright column of light above the horizon and can be seen in the evening after sunset and in the morning before sunrise (Leinert 1975;Grün & Dikarev 2009).
The greatest density of dust particles is found closest to the Sun; at 2.5 AU the zodiacal light brightness is <3% of that observed at 1 AU (Tsumura et al. 2010): contributions beyond 3.3 AU are negligible (Hanner et al. 1974).The particles are lost by gravitational entrainment by the Sun (the Poynting-Robertson drag effect), collisions with other dust particles, planetary perturbations, and momentum exchange with the solar wind (Fixsen & Dwek 2002;Yang & Ishiguro 2015).These loss mechanisms are compensated by dust produced through impacts or ice sublimation (Yang & Ishiguro 2015).
The emission and scattering of radiation by the zodiacal dust cloud is wavelength dependent.Peak scattering occurs at 0.5 lm (Leinert et al. 1998).At 3.6 lm, the scattering and emission contributions are roughly equal (Krick et al. 2012).Emission dominates in the mid to far infrared reaching peak values between 10 and 12 lm.The spectral distribution of zodiacal light follows closely the solar spectrum in the visible, but is slightly shifted to longer wavelengths (Tsumura et al. 2010).In the infrared, the emission approximates that of a blackbody with a temperature between 280 and 286 K (Kelsall et al. 1998;Wright 1998).A comparison of observations (Reach et al. 2003) to zodiacal light models shows qualitative agreement to within 10%.
Here we calculate the zodiacal radiation by using measurements of the zodiacal radiance in the visible (0.55 lm) and infrared (12 lm) from Grün & Dikarev (2009) at various ecliptic latitudes and longitudes.The solar spectrum from 0.25 lm to 10 lm is used to scale the scattered radiance in the shortwave and a blackbody curve from 0.35 lm to 100 lm with peak emission at 12 lm to scale the emitted radiance.Although the measurements from Grün & Dikarev (2009) were made over one-quarter of the celestial sphere, the zodiacal cloud is approximately symmetric with respect to the ecliptic plane (Leinert et al. 1998).Integrating the normal component of the broadband shortwave and longwave radiances, L (h, /), over the solid angle of one-quarter of the celestial sphere, and multiplying by a factor of 4 (to account for the full celestial sphere) gives a total irradiance, F: We compute a range in the infrared zodiacal radiation bounded by dust temperatures of 280 K and 286 K and report the total irradiance as the sum of scattered and emitted contributions.We find an average total zodiacal irradiance of 5.67 • 10 À5 W m À2 , ranging from 5.65 • 10 À5 W m À2 to 5.68 • 10 À5 W m À2 .This value was obtained from the sum of the total emission component of 4.715 • 10 À5 W m À2 , which is an average total infrared emission from a zodiacal dust cloud with temperatures spanning 280 to 286 K (4.73 • 10 À5 W m À2 to 4.7 • 10 À5 W m À2 , respectively), and a scattered light component of 9.54 • 10 À6 W m À2 .
Our computed value is an order of magnitude larger than Sellers' (1965) estimate of 3.4 • 10 À6 W m

À2
. It is plausible that the Sellers (1965) estimate did not consider the component of infrared emission from the dust grains due to a lack of emission measurements until the 1970s (Leinert et al. 2002).However, we note that our method of scaling the scattered and emitted components based on measurements at two wavelengths could result in a larger integrated energy value.

Lunar tides
The Moon produces oscillations in the atmosphere due to the gravitational interaction of the Earth and Moon (Chapman & Lindzen 1970).These atmospheric tides are considerably smaller in amplitude than the dominant, atmospheric thermal tide of the Sun (Chapman & Lindzen 1970;Vial & Forbes 1994;Sandford et al. 2006).The dominant component of the lunar atmospheric tide is the M 2 tide with a period of 12.42 h (Chapman & Lindzen 1970;Sandford et al. 2006;Forbes et al. 2013).According to Chapman & Lindzen (1970), there are as many as 30 components comprising the lunar tide, most of which are much smaller in amplitude and, therefore, are often ignored due to the limited ability of measurements to detect their small signal (Sandford et al. 2006).Platzman (1991) performed an energy balance study of the lunar atmospheric tide by incorporating the three factors of the ocean, body, and load tides, characterized by barometric pressure data from Haurwitz & Cowley (1969) and satellite altimeter data of sea-tide dissipation and sea-tide elevation from NASA's Geodetic Satellite (Geosat) (Cartwright & Ray, 1990).The energy dissipated in the atmosphere due to the lunar atmospheric tide was determined as the sum of excitation energy from the Moon's gravitational effect on the body and load tides and by the vertical flux of tidal energy the atmosphere receives from the ocean (Platzman 1991).Annually averaged results showed that the lunar atmospheric tidal dissipation was on the order of 10 GW and maintained almost entirely by the ocean tide (Platzman 1991).This value corresponds to 1.96 • 10 À5 W m À2 when averaged at Earth's surface.This value is roughly 50% larger than that of Sellers (1965).

Total radiation from stars
Radiation from stars originates from beyond the heliosphere within the Milky Way galaxy.It is estimated that the Milky Way galaxy contains about 10 11 stars, with a total mass of 2 • 10 41 kg (Gonzalo 2008).Measuring the radiation from stars is difficult due to foreground sources from airglow and zodiacal light (e.g., Brandt & Draine 2012;Arai et al. 2015).
The energy density of starlight spans the ultraviolet through the infrared.Models of stellar emission between 0.09 and 0.245 lm use a power-law approximation and between 0.245 and 8 lm, a sum of three dilute blackbodies with dilution factor ''W'', and temperature ''T'' (Mathis et al. 1983;Draine 2011;Brandt & Draine 2012).The dilution factor is the ratio of energy density ''u'', to the energy density of the undiluted blackbody radiation temperature.The different blackbody temperatures reflect the emission from stars at different stages in their life cycle and the dilution factor, typically (1, reflects the dilution of the radiation over great distances (Mathis et al. 1983;Draine 2011).The relationship between stellar radiation energy density and temperature for a dilute blackbody is: where the astrophysical radiation constant, a, is equal to 4r/c (7.565767 ), and c is the speed of light.
Various studies have reported values for the stellar radiation density.In Table 3, we summarize the radiation energy density values for a selection of these studies (see references listed in table) and convert them to a flux density.
Relevant comments necessary to interpret our derivations are noted in the rightmost column.
We report an average flux density of Milky Way starlight of 6.78 • 10 À6 W m À2 derived from an average of stellar flux densities computed using the blackbody temperatures and dilution factors reported in Draine (2011) and Mathis et al. (1983) (see first and second rows of Table 3).This estimate corresponds to an effective blackbody temperature for the Milky Way starlight of 3.31 K.The range of stellar flux densities in Table 3 spans 5.62 • 10 À6 W m À2 to 7.94 • 10 À6 W m À2 .Our average stellar flux density estimate is approximately 50% smaller than the Sellers (1965) estimate of 1.4 • 10 À5 W m À2 , which would correspond to an effective blackbody temperature of 3.96 K.

Cosmic microwave background radiation
The spectral distribution of energy within the Milky Way galaxy and beyond (extragalactic) covers gamma rays through radio waves (e.g., Draine 2011;Cooray 2016).However, theoretical calculations (discussed below) provide evidence that the Cosmic Microwave Background (CMB) was the sole contributor to cosmic radiation considered by Sellers (1965).
The CMB is of extragalactic origin (Cooray 2016).Recent precision measurements (de Bernardis 2015 and references therein) support the theory that the CMB is the remnant of the big bang (Noterdaeme et al. 2011), ''of a time when the universe was very hot, which has now cooled down by its expansion'' (Stanev 2004).It is universal and radiates almost entirely isotropically (Draine 2011;Bucher 2015), with peak energy in the microwave region (500 lm-5 cm; Fixsen et al. 1996).
Radiation in equilibrium with its surroundings, blackbody radiation, is described by the Planck distribution, the spectral integral of which is the Stefan-Boltzmann law, relating temperature ''T'', to the radiative energy density ''u'': or equivalently, temperature to irradiance, F: r is the Stefan-Boltzmann constant (5.67 • 10 À8 W m À2 K À4 ), and the astrophysical radiation constant Table 3. Stellar radiation energy densities derived from four different literature sources derived using equation ( 5) using the published blackbody temperatures and dilution factors (listed in the table) and converted to flux density using the Stefan-Boltzmann law.Note that various studies adopt different numbering for the blackbody temperatures; here, we adopt a numbering scheme that increases with increasing stellar temperature.For a 5th literature source, we derived the stellar flux density from a reported value of stellar mean radiation intensity (see table comments).
We modeled the UV radiation as a blackbody.
T 1 = 3000 We modeled the UV radiation as a blackbody. (Y)  Draine (2011) increased this dilution factor relative to Mathis et al. (1983) to better agree with Cosmic Background Explorer (COBE) Diffuse Infrared Background Experiment (DIRBE) photometry. (b) Our derived value differs from Draine (2011) (Table 12.1).Mean radiation intensity (for 0.09 < k < 8 lm) = 1.69 • 10 À2 erg s À1 cm À2 (a) u = 5.63 • 10 À14 F total = 5.87 • 10 À6 Mezger (1990) (a) We converted to J m À2 s À1 and divided by the speed of light to convert to a radiation energy density.We treated the radiation as blackbody.T 1 = 4000 T 2 = 7500 T 3 = 14,500 ''a'' is equal to 4r/c (7.565767 • 10 À16 J m À3 K À4 ), c is the speed of light.Measurements from space (Fixsen et al. 1996;Fixsen 2009) yield a CMB temperature of 2.72548 ± 0.00057 K (Fixsen 2009).From equations ( 6) and ( 7), the total energy density of CMB radiation is 4.17 • 10 À14 J m À3 and the flux density at the top-of-the-atmosphere is 3.13 • 10 À6 W m À2 , with an uncertainty of ±2.62 This is an order of magnitude smaller than the Sellers (1965) estimate of 3.1 • 10 À5 W m À2 , which would arise from a CMB temperature of 4.8 K, in close agreement with the theoretical estimate of the CMB temperature of 5 K by Alpher & Herman (1948).The first measurement of the CMB temperature, 3.5 ± 1.0 K, by Penzias & Wilson (1965) likely came too late to be included in Sellers' table.
The review by Plane (2012) and references therein of estimates of the global mass influx of Interplanetary Dust Particles (IDP) into Earth's atmosphere show variations in the measurements by more than a factor of 50, ranging from 5 • 10 3 kg day À1 to 2.7 • 10 5 kg day À1 .These come from a variety of measurements, ranging from space-borne dust detectors, radar and lidar, aircraft, satellites, as well as accumulation of meteoric dust on deep sea sediments and ice cores (Grün et al. 1983;Brownlee 1985;Wasson & Kyte 1987;Love & Brownlee 1993;Ceplecha et al. 1998;Mathews et al. 2001;Brown et al. 2002;Janches et al. 2006;Maurette 2006;Plane 2012).In addition to the broad range of global mass influx, the entry velocity of IDPs is found to exhibit a bimodal nature, ranging between a slow (~15 km s À1 ) and fast (~55 km s À1 ) component (Janches et al. 2006 and references within).Plane (2012) suggests three ranges in the mass influx and entry velocity of IDP based on various measurements and modeling.First, a low range of meteoroid mass influx between 5 • 10 3 kg day À1 and 1 • 10 4 kg day À1 with an entry velocity less than 15 km s À1 .Second, a medium range in mass influx between ~2 • 10 4 kg day À1 and 5 • 10 4 kg day À1 with an average micrometeorite entry velocity of greater than 20 km s À1 .Third, an upper range in mass influx between 1 • 10 5 kg day À1 and 3 • 10 5 kg day À1 .
To compute the mechanical energy dissipated by the passage of micrometeorites through Earth's atmosphere, we assume the kinetic energy of their passage is equivalent to their mechanical energy.We use representative mass influx values, m, for low, medium, and high influx conditions as defined by the average of the respective mass influx ranges defined in Plane (2012).We use typical entry velocities, v, of 15 km s À1 , 55 km s À1 , and ~30 km s À1 representative of the low, medium, and high categories from Janches et al. (2006).Our calculations, presented as daily average power estimates, give values of 9.8 • 10 6 W, 6.1 • 10 8 W, and 1.0 • 10 9 W for the low, medium, and high categories, respectively.When the power is globally averaged at Earth's surface, the flux of dissipated mechanical energy is 1.9 • 10 À8 W m À2 , 1.2 • 10 À6 W m À2 , and 2.0 • 10 À6 W m À2 for low, medium, and high categories, respectively.The average of these flux values is 1.1 • 10 À6 W m À2 , an order of magnitude smaller than the Sellers (1965) estimate.The wide range in daily global mass influx (10 3 -10 5 kg day À1 ) and entry velocities (15-55 km s À1 ) of these micrometeoroids is one possible reason for the discrepancies in these two values.Also, earlier estimates for the influx rates of meteoroid material were larger (~10 6 kg day À1 ; Hawkins 1956;Hawkins & Upton 1958).These earlier estimates were deduced from radio echo and photographic observations, producing an energy dissipation in line with the Sellers (1965) value.

Some other external sources
There are a few omissions in Sellers' original table that warrant discussion: airglow, galactic cosmic rays, and Earthshine.
Airglow is emission from Earth's upper atmosphere between altitudes of 80 and 300 km induced by absorption of solar radiation by various atmospheric constituents (Chamberlain 1961;Leinert et al. 1998;Khomich et al. 2008).The subsequent excitation, dissociation, recombination, and ionization of these species produce emissions of light known as airglow (Meinel 1951;Meier 1991;Khomich et al. 2008).Airglow emission over the 0.1-0.9lm range was estimated using spectra of the dayglow (Broadfoot et al. 1997) and nightglow from the Arizona Airglow Experiment (GLO) flown on the space shuttles STS-53 (December 1992) and STS-74 (November 1995;Broadfoot & Bellaire 1999).We determined the airglow emission by spectrally integrating the dayglow (0.1-0.9 lm) and nightglow (0.24-0.9 lm) brightness curves that were provided by Lyle Broadfoot (personal communication).We assumed that the airglow does not vary spatially (not always true; see Gao et al., 2016) and emission is isotropic.We calculate for the dayglow and nightglow values of 4.82 • 10 À3 W m À2 and 2.37 • 10 À3 W m À2 , respectively; an average of these values, 3.6 • 10 À3 W m À2 , is similar in magnitude to that reported by Khomich et al. (2008).Pertsev & Perminov (2008) using ground-based observation data at Moscow, Russia from 2000 to 2006, report solar cycle variations of 30-40% in hydroxyl (OH) and molecular oxygen; seasonal variations were also found.Gao et al. (2016Gao et al. ( ) analyzed 13 years (2002Gao et al. ( -2015) ) of globally averaged nightglow emissions at selected wavelength bands in the infrared from nitrogen oxide (NO) at 5.3 lm, OH at 1.6 and 2.0 lm, and oxygen (O 2 ) at 1.27 lm using data from the Sounding of the Atmosphere using Broadband Emission Radiometry (SABER) and Solar Extreme Ultraviolet Experiments (SEE) on the Thermosphere-Ionosphere-Mesosphere Energetics and Dynamics (TIMED) satellite (Mlynczak 1997); these measurements show variability over the 11-year solar cycle of ~12% in OH, ~22% in O 2 , and ~176% in NO.
Galactic Cosmic Rays (GCRs) are charged particles, predominantly protons, that originate outside the solar system, most likely from supernova explosions (Blasi 2013).They continually bombard the Earth's atmosphere with energies sufficiently high (approximately 10 7 eV to 10 21 eV) to influence various altitude-dependent atmospheric phenomena based on the magnitude of the GCR energies (Mironova et al. 2015).These influences can be primary or secondary in nature.A primary effect is when ionization energy is released when a GCR particle is absorbed within the atmosphere.Secondary effects occur when collisions between GCR particles and atmospheric gases produce elementary charged particles, such as electrons, gamma-rays, and mesons that cascade down to lower altitudes (Bazilevskaya 2000).The influx of GCRs into the solar system and Earth's atmosphere is affected predominantly by the Sun's magnetic cycle; the GCR flux is out of phase with this magnetic cycle (Mironova et al. 2015).Shorter term, episodic, modulation in GCRs can also occur from releases of energy from the Sun's photosphere (i.e.solar flares) or from the Sun's corona (i.e.coronal mass ejections) that cause disturbances that ''sweep away'' the GCRs (Bazilevskaya 2000).Earth's magnetic field may also act as a shield, deflecting cosmic rays toward the poles along field lines due to their partially charged nature (NRC 1994;Bazilevskaya et al. 2008).
Earthshine, also known as ashen light, is ''the glow of the 'dark' part of the lunar disk that is visible to a nighttime observer'' (Goode et al. 2001).It is the amount of sunlight that is reflected by the Earth onto the Moon and then reflected from the Moon back onto the Earth.It is of interest here not because it is a significant energy source but because it can be used to estimate Earth's albedo (Goode et al. 2001).Bohren & Clothiaux (2006) give the ratio of full Moon to new Moon to be 9300.From this, and assuming that the ratio of full and new Moon spectral reflectance scale the same as it does in the visible, we estimate the magnitude of Earthshine to be full Moon reflected irradiance 0.0018 W m À2 (from Sect.2.3) divided by 9300, or 1.93 • 10 À7 W m À2 .

Summary
We provide updates to Sellers' (1965) Table 1 of large-scale energy sources that act continuously or quasicontinuously in the atmosphere and at its boundaries.The original intent of our referencing this table was to compare the sum of all external (to the atmosphere) energy sources to the Sun.If we exclude lightning discharges and fossil fuel combustion, we see that the rate of energy provided by the Sun is over 3000 times greater than all other sources.Going one step further, eliminating all sources that represent transformations of solar energy (lunar emission and reflection, magnetic storms, airglow, solar tides, and zodiacal light), the ratio of solar to non-solar sources is almost 3800.Even after recognizing that only a fraction, 0.71 (e.g.Wild et al. 2013), of solar energy is deposited into (absorbed by) the Earth system, that amount still exceeds the energy from all other external sources by a factor of approximately 2700.In the absence of the Sun, the radiative equilibrium temperature of the Earth (assumed to be a blackbody) would be approximately 36 K.

Fig. 2 .
Fig. 2. Contributions of total global heat flux over land and ocean in mW m À2 based on observations and a thermal model, which is used to determine the cooling of the oceanic lithosphere.Figure reprinted from Jaupart et al. (2015), with permission from Elsevier, license number 3984240052236.

Fig. 3 .
Fig. 3.The global observing network of observing sites for measuring the heat flow from Earth's interior.Red dots denote the Davies & Davies (2010) study with 55% more observing sites than the Pollack et al. (1993) study.From Davies & Davies (2010).Reproduced with permission from J. H. Davies.
cloud and cloud-to-ground flash observations from NASA's Optical Transient Detector (OTD) on board the Microlab-1 satellite (OV-1) (Christian et al. 2003).Cecil et al. (2014) updated the global lightning flash climatology to 46 flashes s À1 , varying seasonally from 35 flashes s À1 in February, to 60 flashes s À1 in August, by merging data from the OTD sensor (1995-2000) with the Lightning Imaging Sensor (LIS) on the Tropical Rainfall Measuring Mission (TRMM) satellite from 1998 to 2010.

Fig. 4 .
Fig. 4. The annualized distribution of total lightning activity derived from the Optical Transient Detector (OTD) and Lightning Imaging Sensor (LIS) in units of flashes km À2 yr À1 .Figure updated from Cecil et al. (2014) and provided by Daniel Cecil to include data through 2013.

Table 2 (
Table 1 in this paper) has been reproduced to emphasize the overwhelming dominance that solar radiation contributes to Earth's energy budget.On the basis of viewer responses to those presentations, an update to Sellers' table is presented herein (see Table 2) to bring several of the table entries up to date.

Table 2 .
Revised energy sources from current study.Flux density and relative input values are defined the same as in Table1.Values are global averages, and where applicable, are mean values over the solar cycle.The solar irradiance value is globally averaged at 1 AU.The third column from left is the estimated uncertainty, if known; in some cases, a range is reported from the literature.See text for further discussion.The fifth column lists the section number of each energy source.

Table 1 .
Sellers (1965) fromSellers (1965)and relative to that of the Sun (final column).Relative input calculated with respect to the flux density values (middle column).Values are global averages.