Mid-infrared spectrum of the zodiacal light observed   with 
 ISOPHOT

Leinert, Ch.; Ábrahám, P.; Acosta–Pulido, J. A.; Lemke, D.; Siebenmorgen, R.

doi:10.1051/0004-6361:20021029

Cited by 27 publications

(20 citation statements)

References 16 publications

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“…It also agrees with infrared observations showing silicates emission features (see e.g. Reach et al 1996;Leinert et al 2002), with the analysis of the IDPs collected in the stratosphere of the Earth and micrometeorites collected in ices (for a review, see Jessberger et al 2001) and with recent analyses of Stardust samples (see e.g. Zolensky et al 2006;Sandford et al 2006).…”

Section: Discussionsupporting

confidence: 90%

Inferring the interplanetary dust properties

Lasue¹,

Levasseur-Regourd²,

Fray

et al. 2007

A&A

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Context. Since in situ studies and interplanetary dust collections only provide a spatially limited amount of information about the interplanetary dust properties, it is of major importance to complete these studies with properties inferred from remote observations of scattered and emitted light, with interpretation through simulations. Aims. Physical properties of the interplanetary dust in the near-ecliptic symmetry surface, such as the local polarization, temperature, and composition, together with their heliocentric variations, may be derived from scattered and emitted light observations, giving clues to the respective contribution of the particle sources. Methods. A model of light scattering by a cloud of solid particles constituted by spheroidal grains and aggregates thereof is used to interpret the local light-scattering data. Equilibrium temperature of the same particles allows us to interpret the temperature heliocentric variations. Results. A good fit of the local polarization phase curve, P α , near 1.5 AU from the Sun is obtained for a mixture of silicates and more absorbing organic material (≈40% in mass) and for a realistic size distribution typical of the interplanetary dust in the 0.2 µm to 200 µm size range. The contribution of dust particles of cometary origin is at least 20% in mass. The same size distribution of particles gives a dependence of the temperature with the solar distance, R, in R −0.45 that is different than the typical black body behavior. The heliocentric dependence of P α=90 • is interpreted as a progressive disappearance of solid organic (such as HCN polymers or amorphous carbon) towards the Sun. Conclusions.

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Section: Discussionsupporting

confidence: 90%

Inferring the interplanetary dust properties

Lasue¹,

Levasseur-Regourd²,

Fray

et al. 2007

A&A

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“…But we do not. Leinert et al (2002) found that the ZE spectra at various ecliptic latitudes observed by ISOPHOT are not significantly deviated from blackbody SEDs in the wavelength range from 6 to 12 μm. They concluded that the IPDs are well mixed over the IPD cloud.…”

Section: Discussionmentioning

confidence: 81%

“…In the mid-IR wavelength range, the background brightness is dominated by the ZE (Leinert et al 1998). The spectral energy distribution (SED) of ZE is described by that of a blackbody (Ootsubo et al 1998;Leinert et al 2002;Reach et al 2003). Hence, the background brightness is assumed to follow the blackbody-type SED…”

Section: The Irc All-sky Surveymentioning

confidence: 99%

Brightness map of the zodiacal emission from the AKARI IRC All-Sky Survey

Pyo

Ueno

Kwon

et al. 2010

A&A

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The first Japanese infrared space mission AKARI successfully scanned the whole sky with its two main instruments, the Infrared Camera (IRC) and the Far-Infrared Surveyor (FIS). The AKARI All-Sky Survey provides us with an invaluable opportunity to examine the zodiacal emission (ZE) over the entire sky in the leading as well as the trailing direction of the Earth's motion. We describe our efforts to reduce the ZE brightness map from the AKARI's survey in the 9 μm waveband. Compared with the interplanetary dust cloud model of Kelsall et al. (1998), the map requires an increase of the contribution of the resonance ring component to the ZE brightness by about 20%. We paid special attention to the north and south ecliptic pole brightnesses. The symmetry plane's inclination and longitude of ascending node need to be modified from those in Kelsall et al. (1998) to reach a best fit to the observed pole brightness difference.

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“…We find an average total zodiacal irradiance of 5. . 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.…”

Section: Zodiacal Irradiancementioning

confidence: 91%

Where does Earth’s atmosphere get its energy?

Kren

Pilewskie

Coddington

2017

J. Space Weather Space Clim.

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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.

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Mid-infrared spectrum of the zodiacal light observed with ISOPHOT

Cited by 27 publications

References 16 publications

Inferring the interplanetary dust properties

Inferring the interplanetary dust properties

Brightness map of the zodiacal emission from the AKARI IRC All-Sky Survey

Where does Earth’s atmosphere get its energy?

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