Reconciling the centimeter- and millimeter-wavelength ammonia absorption spectra under jovian conditions: Extensive millimeter-wavelength measurements and a consistent model

Devaraj, Kiruthika; Steffes, Paul G.; Karpowicz, Bryan M.

doi:10.1016/j.icarus.2010.12.010

Cited by 11 publications

(18 citation statements)

References 41 publications

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“…Measurements from the Cassini-Huygens probe confirm that Saturn's top cloud deck is composed of ammonia clouds [1] with a brightness temperature between 140 and 190 K. Below Jupiter's tropopause are ammonia clouds, with temperatures between 200 and 800 K and pressures between 0.6 and 0.9 bar, as well as NH 4 SH and H 2 O clouds at lower altitudes and pressures between 1 and 7 bar.…”

Section: Introductionmentioning

confidence: 91%

“…Ammonia is subject to molecular inversion by tunnelling of the hydrogen atoms, leading to a perturbation in the vibrational spectrum, a doubling of each line. The inversion leads to an absorption at and slightly below 23.79 GHz, which makes ammonia readily observable at microwave frequencies [4]. Ammonia has a high specific heat capacity for a molecular substance, which is inconsistent with the simplicity of the isolated molecular structure.…”

Section: Ammonia Properties Hugoniots and Eos Surfacesmentioning

confidence: 99%

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Equation of state of ammonia

Mulford

Swift

Hamel

2014

J. Phys.: Conf. Ser.

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Abstract. Ammonia and water are critical components of extraterrestrial bodies, determining the density and physical properties of the Outer Planets, their moons, and of extrasolar planets. Ammonia is unusual in having a high heat capacity relative to other molecular species. Equations of state (EOS) are presented for ammonia and for mixtures of ammonia and water. Their properties are discussed in terms of chemical compositions that evolve as pressure and temperature are varied. The NH 4 OH hydrate of ammonia is known to exist as a separate molecular species at pressures above about 5 GPa, and an effort was made to include reaction between NH 3 and H 2 O in the mixture EOS. The EOS are suitable for calculating structures of icy planets and exoplanets, and of impacts. mass-radius relations which bound the possible interpretations of composition and structure for extraterrestrial bodies of unknown composition, such as exoplanets.

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Section: Introductionmentioning

confidence: 91%

Section: Ammonia Properties Hugoniots and Eos Surfacesmentioning

confidence: 99%

Equation of state of ammonia

Mulford

Swift

Hamel

2014

J. Phys.: Conf. Ser.

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“…Thatχ (Z,T c (t)) in Eq. (38) has no term linear in t seems plausible in that the decoherence mechanism in our model has been chosen specifically to carry X information into the environment. The uppermost curves in Figs. 3(a) and 3(b) represent…”

Section: Information Flowsmentioning

confidence: 99%

“…where the first equality comes from Theorem 3 of [12], and the second from (38); the correction must be negative in view of the bound in Eq. (29).…”

Section: Information Flowsmentioning

confidence: 99%

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Consistent histories for tunneling molecules subject to collisional decoherence

2012

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The decoherence of a two-state tunneling molecule, such as a chiral molecule or ammonia, due to collisions with a buffer gas is analyzed in terms of a succession of quantum states of the molecule satisfying the conditions for a consistent family of histories. Withhω the separation in energy of the levels in the isolated molecule and γ a decoherence rate proportional to the rate of collisions, we find for γ ω (strong decoherence) a consistent family in which the molecule flips randomly back and forth between the left-and right-handed chiral states in a stationary Markov process. For γ < ω there is a family in which the molecule oscillates continuously between the different chiral states, but with occasional random changes of phase, at a frequency that goes to zero at a phase transition γ = ω. This transition is similar to the behavior of the inversion frequency of ammonia with increasing pressure, but will be difficult to observe in chiral molecules such as D 2 S 2 . There are additional consistent families both for γ > ω and for γ < ω. In addition, we relate the speed with which chiral information is transferred to the environment to the rate of decrease of complementary types of information (e.g., parity information) remaining in the molecule itself.

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