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They found that Jupiter models (hat used EOSs consistent with the 6-Iold limiting deuterium compression data of Collinsetal.(1998). lead to core sizes of 0-10AZ... with total heavy element abundances (envelope plus core) of 10-25.	They found that Jupiter models that used EOSs consistent with the 6-fold limiting deuterium compression data of \citet{Collins98} lead to core sizes of 0-10, with total heavy element abundances (envelope plus core) of 10-25.
. Models computed using EOSs consistent with the harder 4.3-Fold limiting compression ol Ixnudsonetal.(2001.2004) ancl Boriskovetal.(2005). led to smaller cores sizes (0-3 )) but larger heavy elements abundances (25-35 )).	Models computed using EOSs consistent with the harder 4.3-fold limiting compression of \citet{Knudson01,Knudson04} and \citet{Boriskov05} led to smaller cores sizes (0-3 ) but larger heavy elements abundances (25-35 ).
Since other experiments have nol been able to replicate the soft Collinsetal.(1998) data. ancl (he data of Ixnudson et al.	Since other experiments have not been able to replicate the soft \citet{Collins98} data, and the data of Knudson et al.
and Doriskov οἱ al.	and Boriskov et al.
agree quite well while using different experimental setups. these harder EOS data sets are currently viewed by many as the most reliable. (For 2006).	agree quite well while using different experimental setups, these harder EOS data sets are currently viewed by many as the most reliable. \citep[For recent reviews, see][]{Nellis05,Nellis06}.
. Tests of the hvdrogen or deuterium EOS olf of the single-shock Hugoniot. perhaps at pressures of up to a lew Mbar. but temperatures below 107 IX. would be most valuable.	Tests of the hydrogen or deuterium EOS off of the single-shock Hugoniot, perhaps at pressures of up to a few Mbar, but temperatures below $^4$ K, would be most valuable.
For helium. our second most important constituent. new EOS data are sorely needed.	For helium, our second most important constituent, new EOS data are sorely needed.
No helium EOS data have been published since Nellisetal.(LO84).. and this data set only reached a maximum pressure of 560 kbar (56 Gpa).	No helium EOS data have been published since \citet{Nellis84}, and this data set only reached a maximum pressure of 560 kbar (56 Gpa).
In we show schematic interior structures of Jupiter and Saturn.	In we show schematic interior structures of Jupiter and Saturn.
We show pressures and (temperatures al (ree locations: the visible atmosphere (1 bar). near the molecular-to-metallic transition of hydrogen (2 Mbar). aud at the top of the heavy. element core of each planet.	We show pressures and temperatures at three locations: the visible atmosphere (1 bar), near the molecular-to-metallic transition of hydrogen (2 Mbar), and at the top of the heavy element core of each planet.
Atmospheric elemental abundances. as determined by the for Jupiter and by spectroscopy for Saturn. are shown within a grev box 2003)..	Atmospheric elemental abundances, as determined by the for Jupiter and by spectroscopy for Saturn, are shown within a grey box \citep{Atreya03}. .
These abundances should at least be representative of the entire molecular Ls reeion.	These abundances should at least be representative of the entire molecular $_2$ region.
If a PPT does not exist. these abundances should be representative of (he entire 11/16 envelope.	If a PPT does not exist, these abundances should be representative of the entire H/He envelope.
In both planets. (he molecular IH» region is depleted in helium relative to protosolar abundances (vonZahnetal.1993;Conrath&Gautier2000) indicating sedimentation of helium into metallie II Iavers.	In both planets, the molecular $_2$ region is depleted in helium relative to protosolar abundances \citep{vonzahn98,CG00} indicating sedimentation of helium into metallic H layers.
Recent evolutionary models for Saturn indicate this helium may rain through the metallic Hl region and form a laver on top of the core 2003).	Recent evolutionary models for Saturn indicate this helium may rain through the metallic H region and form a layer on top of the core \citep{FH03}.
. While the interior pressure-densitv. relation sets the structure of the planet. it is the pressure-Ltemperature relation that determines the thermal evolution.	While the interior pressure-density relation sets the structure of the planet, it is the pressure-temperature relation that determines the thermal evolution.
The temperature of the deep interior sets the heat content of the planet.	The temperature of the deep interior sets the heat content of the planet.
The hieher the temperatures in the planet's interior. the longer it will take to cool to agiven luminosity.	The higher the temperatures in the planet's interior, the longer it will take to cool to agiven luminosity.
This has been investigated recently by Sammon&Guillot(2004) for Jupiter.	This has been investigated recently by \citet{Saumon04} for Jupiter.
Thev computed. evolution models of	They computed evolution models of
The concatenated spectra of 5 such classes reveal several clusters of ir lunes. listed in Sec.	The concatenated spectra of 5 such classes reveal several clusters of ir lines, listed in Sec.
3.H which are characterized by their vibrational mode. ic. the atomic elements or functional eroups involved iu the motion. or the type of coherent motion of the atoms.	3, which are characterized by their vibrational mode, i.e. the atomic elements or functional groups involved in the motion, or the type of coherent motion of the atoms.
Each cluster is found to coincide reasonably well with one or the other of the tabulated UIBs.	Each cluster is found to coincide reasonably well with one or the other of the tabulated UIBs.
But the «enusitv of lines in cach cluster is still iusufficieut for the svuthesized spectruni to approach observed spectra.	But the density of lines in each cluster is still insufficient for the synthesized spectrum to approach observed spectra.
Section \| therefore discusses the effects of inking together two or more of the selected elementary structures to GIVE so-caled composite structures.	Section 4 therefore discusses the effects of linking together two or more of the selected elementary structures to give so-called composite structures.
This. too. “deusifies” the lue clusters. aud so helps 1nulding up the spectral bands.	This, too, “densifies" the line clusters, and so helps building up the spectral bands.
It also gives rise to new "elobal. or bulk. 1oes, farther aud farther in the red. which coutribute to the uuderlvius contiuuuni.	It also gives rise to new “global", or bulk, modes, farther and farther in the red, which contribute to the underlying continuum.
It turus out that at least a few thousand atoms are required for the svuthesized spectruui ο compare with observed spectra;	It turns out that at least a few thousand atoms are required for the synthesized spectrum to compare with observed spectra.
Other cousideratious (scatteriue cross-secticn. resilieuce. ete.)	Other considerations (scattering cross-section, resilience, etc.)
also poiut to much larger dust erain sizes (~O lina).	also point to much larger dust grain sizes $\sim0.1 \mu$ m).
Based on the above. Sec.	Based on the above, Sec.
5 displavs the concatenated spectruuu of a large family of clementary and composite structures. iu adequate relative numbers so as to best fit a typical UID spectruu.	5 displays the concatenated spectrum of a large family of elementary and composite structures, in adequate relative numbers so as to best fit a typical UIB spectrum.
The corresponudiug dust conrposition and strucures are eiveu iu Sec.	The corresponding dust composition and structures are given in Sec.
6.	6.
Finally. excitation aud subsequenut ir ο]ΙΟn are discussed in Sec.	Finally, excitation and subsequent ir emission are discussed in Sec.
7.	7.
This section describes the clemeutary structures that were used to build up a colpcucdinu whose ir spectru looks like a generic UID. spectra.	This section describes the elementary structures that were used to build up a compendium whose ir spectrum looks like a generic UIB spectrum.
They were selected for their atomic composition to be compatible with cosmic albmucdauc‘os GQuainly hydrocarbons). for their siuicity aud for their spectra to clisplas OL or more lines within oue or more UID. but noue outside.	They were selected for their atomic composition to be compatible with cosmic abundances (mainly hydrocarbons), for their simplicity and for their spectrum to display one or more lines within one or more UIB, but none outside.
Clues were also found in the sketches of ποιο kerogoe restructures (see Behar aud Vandenbroucke (1986).. aud coal structures (see Speight (1991))).	Clues were also found in the sketches of “young" kerogen structures (see Behar and Vandenbroucke \cite{beh}, and coal structures (see Speight \cite{spe}) ).
The latter include not ouly small PAITs. but :so colcaterated G- and 5- membered rings.	The latter include not only small PAH's, but also concatenated 6- and 5- membered rings.