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PubMed2006

Carbon under extreme conditions: phase boundaries and electronic properties from first-principles theory.

At high pressure and temperature, the phase diagram of elemental carbon is poorly known. We present predictions of diamond and BC8 melting lines and their phase boundary in the solid phase, as obtained from first-principles calculations. Maxima are found in both melting lines, with a triple point located at approximately 850 GPa and approximately 7,400 K. Our results show that hot, compressed diamond is a semiconductor that undergoes metalization upon melting. In contrast, in the stability range of BC8, an insulator to metal transition is likely to occur in the solid phase. Close to the diamond/liquid and BC8/liquid boundaries, molten carbon is a low-coordinated metal retaining some covalent character in its bonding up to extreme pressures. Our results provide constraints on the carbon equation of state, which is of critical importance for devising models of Neptune, Uranus, and white dwarf stars, as well as of extrasolar carbon-rich planets.

Carbon↗

PubMed1990

Monodeuterated methane in the outer solar system. IV. Its detection and abundance on Neptune.

We have detected the 3 nu 2 band of CH3D in the spectrum of Neptune near 1.6 micrometers recorded at a spectral resolution of 4 cm-1 with the Cassegrain Fourier Transform Spectrometer at the 3.6 m Canada-France-Hawaii Telescope (CFHT) on Mauna Kea. Our analysis of this spectrum, using spectral synthesis techniques, yielded a CH3D/CH4 ratio of 6(+6)(-4) x 10(-4), which corresponds to a global D/H ratio for Neptune of 1.2(+1.2)(-0.8) x 10(-4), if CH3D is in isotopic fractionation equilibrium with HD. This value is about an order of magnitude larger than an earlier estimate by Orton et al. based on deconvolution measurements of unresolved molecular emission in the 8-10 micrometers region. Comparison of this new determination with previous studies of CH3D in the outer solar system shows that, as in the case of Uranus, the D/H on Neptune is strongly enhanced over that found on Jupiter and Saturn and is comparable to the D/H in methane on Titan and in terrestrial methane and water.

Astronomical Phenomena↗

PubMed1987

The interception and retention of 238Pu deposition by orange trees.

Radioisotope thermoelectric generators (RTG) transform the heat produced during the alpha decay of 238Pu into electrical energy for use by deep-space probes, such as the Voyager spacecraft, which have returned images and other data from Jupiter, Saturn and Uranus. Future missions involving RTGs may be launched aboard the space shuttle, and there is a remote possibility that an explosion of liquid-hydrogen and liquid-oxygen fuel could rupture the RTGs and disperse 238Pu into the atmosphere over central Florida. Research was performed to determine the potential transport to man of atmospherically dispersed Pu via contaminated orange fruits. The results indicate that the major contamination of oranges would result from the interception and retention of 238Pu deposition by fruits. The resulting surface contamination could enter human food chains through transfer to internal tissues during peeling or in the reconstituted juices and flavorings made from orange skins. The interception of 238Pu deposition by fruits is especially important because the results indicate no measurable loss of Pu from fruit surfaces through time or with washing. Approximately 1% of the 238Pu deposited onto an orange grove would be harvested in the year following deposition.

Aerospace Medicine↗

PubMed2006

H3+: the driver of giant planet atmospheres.

We present a review of recent developments in the use of H3+ molecular ion as a probe of physics and chemistry of the upper atmospheres of giant planets. This ion is shown to be a good tracer of energy inputs into Jupiter (J), Saturn (S) and Uranus (U). It also acts as a 'thermostat', offsetting increases in the energy inputs owing to particle precipitation via cooling to space (J and U). Computer models have established that H3+ is also the main contributor to ionospheric conductivity. The coupling of electric and magnetic fields in the auroral polar regions leads to ion winds, which, in turn, drive neutral circulation systems (J and S). These latter two effects, dependent on H3+, also result in very large heating terms, approximately 5 x 10(12) W for Saturn and greater than 10(14) W for Jupiter, planet-wide; these terms compare with approximately 2.5 x 10(11) W of solar extreme UV absorbed at Saturn and 10(12) W at Jupiter. Thus, H3+ is shown to play a major role in explaining why the temperatures of the giant planets are much greater (by hundreds of kelvin) at the top of the atmosphere than solar inputs alone can account for.

Journal Article↗

PubMed2001

Organic composition of C/1999 S4 (LINEAR): a comet formed near Jupiter?

In the current paradigm, Oort cloud comets formed in the giant planets' region of the solar nebula, where temperatures and other conditions varied greatly. The measured compositions of four such comets (Halley, Hyakutake, Hale-Bopp, and Lee) are consistent with formation from interstellar ices in the cold nebular region beyond Uranus. The composition of comet C/1999 S4 (LINEAR) differs greatly, which suggests that its ices condensed from processed nebular gas, probably in the Jupiter-Saturn region. Its unusual organic composition may require reevaluation of the prebiotic organic material delivered to the young Earth by comets.

Journal Article↗

PubMed2001

The spin temperature of NH3 in Comet C/1999S4 (LINEAR).

A high-dispersion spectrum of Comet C/1999S4 (LINEAR) was obtained in the optical region with the high-dispersion spectrograph on the Subaru telescope when the comet was 0.863 astronomical units from the Sun before its disintegration. We obtained high signal-to-noise ratio emission lines of the cometary NH2 bands from which an ortho-to-para ratio (OPR) of 3.33 +/- 0.07 was derived on the basis of a fluorescence excitation model. Assuming that cometary NH2 mainly originates from ammonia through photodissociation, the derived OPR of NH2 molecules should reflect that of ammonia, which provides information on the environment of molecular formation or condensation and of the thermal history of cometary ices. Assuming that the OPR of ammonia in comets was unchanged in the nucleus, the derived spin temperature of ammonia (28 +/- 2 kelvin) suggests that a formation region of the cometary ammonia ice was between the orbit of Saturn and that of Uranus in the solar nebula.

Ammonia↗

PubMed2004

Search for low-mass exoplanets by gravitational microlensing at high magnification.

Observations of the gravitational microlensing event MOA 2003-BLG-32/OGLE 2003-BLG-219 are presented, for which the peak magnification was over 500, the highest yet reported. Continuous observations around the peak enabled a sensitive search for planets orbiting the lens star. No planets were detected. Planets 1.3 times heavier than Earth were excluded from more than 50% of the projected annular region from approximately 2.3 to 3.6 astronomical units surrounding the lens star, Uranus-mass planets were excluded from 0.9 to 8.7 astronomical units, and planets 1.3 times heavier than Saturn were excluded from 0.2 to 60 astronomical units. These are the largest regions of sensitivity yet achieved in searches for extrasolar planets orbiting any star.

Journal Article↗

PubMed1996

The Morphogenesis of Bands and Zonal Winds in the Atmospheres on the Giant Outer Planets

The atmospheres of Jupiter, Saturn, Uranus, and Neptune were modeled as shallow layers of turbulent fluid overlying a smooth, spherical interior. With only the observed values of radius, rotation rate, average wind velocity, and mean layer thickness as model parameters, bands and jets spontaneously emerged from random initial conditions. The number, width, and amplitude of the jets, as well as the dominance of anticyclonic vortices, are in good agreement with observations for all four planets.

Journal Article↗

PubMed1997

Europa's magnetic signature: report from Galileo's pass on 19 December 1996.

On 19 December 1996 as Galileo passed close to Jupiter's moon, Europa, the magnetometer measured substantial departures from the slowly varying background field of Jupiter's magnetosphere. Currents coupling Europa to Jupiter's magnetospheric plasma could produce perturbations of the observed size. However, the trend of the field perturbations is here modeled as the signature of a Europa-centered dipole moment whose maximum surface magnitude is approximately 240 nanotesla, giving a rough upper limit to the internal field. The dipole orientation is oblique to Europa's spin axis. This orientation may not be probable for a field generated by a core dynamo, but higher order multipoles may be important as they are at Uranus and Neptune. Although the data can be modeled as contributions of an internal field of Europa, they do not confirm its existence. The dipole orientation is also oblique to the imposed field of Jupiter and thus not directly produced as a response to that field. Close to Europa, plasma currents appear to produce perturbations with scale sizes that are small compared with a Europa radius.

Extraterrestrial Environment↗

PubMed1999

Interiors of giant planets inside and outside the solar system.

An understanding of the structure and composition of the giant planets is rapidly evolving because of (i) high-pressure experiments with the ability to study metallic hydrogen and define the properties of its equation of state and (ii) spectroscopic and in situ measurements made by telescopes and satellites that allow an accurate determination of the chemical composition of the deep atmospheres of the giant planets. However, the total amount of heavy elements that Jupiter, Saturn, Uranus, and Neptune contain remains poorly constrained. The discovery of extrasolar giant planets with masses ranging from that of Saturn to a few times the mass of Jupiter opens up new possibilities for understanding planet composition and formation. Evolutionary models predict that gaseous extrasolar giant planets should have a variety of atmospheric temperatures and chemical compositions, but the radii are estimated to be close to that of Jupiter (between 0.9 and 1.7 Jupiter radii), provided that they contain mostly hydrogen and helium.

Astronomical Phenomena↗

PubMed1990

Androgyne becomes bisexual in sexological theory: Plato to Freud and neuroscience.

Plato conceptualized primordial humans as androgynes, the children of the moon. The primordial hermaphroditism of the mammalian embryo became known 2 1/2 millennia later in the mid-19th century. By 1864 Ulrichs had transposed the new knowledge from embryology to sexology to explain those to whom he gave the name Urnings (after Uranus who gave womanless birth to Venus from sea spume) as having "a woman's mind trapped in a man's body" (anima muliebris corpore virili inclusa). Urning became displaced by sexual inversion, and eventually by homosexual, a term coined together with heterosexual by Kertbeny as recently as 1869. The embryological principle of primordial hermaphroditism became linked to evolutionary Darwinism by way of Haeckel's principle of recapitulation, epitomized as "ontogeny recapitulates phylogeny." The recapitulation principle became linked, in turn, to the principle of intrapsychic primordial bisexuality, which became a cornerstone of Freud's psychoanalytic theory. Genetics influences the outcome of bipotentiality not directly but by way of hormonal programming of the brain, prenatally or neonatally, rather than pubertally and in maturity. Bipotentiality within the brain has been investigated chiefly in the hypothalamus where male/female dimorphism has been recognized, but its determinants and stages of differentiation, both prenatal and postnatal, remain to be fully ascertained. Neuroanatomical research on the outcome of male/female bipotentiality as gay, straight, or in between is politically and morally opposed by those who postulate a bipotential preference or voluntary choice. In stimulus-response associationism, to which behavior-modification theory belongs, bisexuality is equipotential, and either alternative may be evoked, ostensibly, dependent on the stimulus situation. In ethological theory, the effectiveness of stimulus-response bonding is confined chronologically to a critical period of development and is restricted phylogenetically by an innate recognition mechanism and an innate releasing mechanism. These limits are compatible, however, with some degree of both individual and ethnic variation.

Bisexuality↗

PubMed1989

The carbon budget in the outer solar nebula.

Detailed models of the internal structures of Pluto and Charon, assuming rock and water ice as the only constituents, indicate that the mean silicate mass fraction of this two-body system is on the order of 0.7; thus the Pluto/Charon system is significantly "rockier" than the satellites of the giant planets (silicate mass fraction approximately 0.55). This compositional contrast reflects different formation mechanisms: it is likely that Pluto and Charon formed directly from the solar nebula, while the circumplanetary nebulae that produced the giant planet satellites were derived from envelopes that surrounded the forming giant planets (envelopes in which icy planetesimals dissolved more readily than rocky planetesimals). Simple cosmic abundance calculations, and the assumption that the Pluto/Charon system formed directly from solar nebula condensates, strongly suggest that the majority of the carbon in the outer solar nebula was in the form of carbon monoxide; these results are consistent with (1) inheritance from the dense molecular clouds in the interstellar medium (where CH4/CO < 10(-2) in the gas phase) and/or (2) of the Lewis and Prinn kinetic inhibition model of solar nebula chemistry. Theoretical predictions of the C/H enhancements in the atmospheres of the giant planets, when compared to the actual observed enhancements, suggest that 10%, or slightly more, of the carbon in the outer solar nebula was in the form of condensed materials (although the amount of condensed C may have dropped slightly with increasing heliocentric distance). Strict compositional limits computed for the Pluto/Charon system using the densities of CH4 and CO ices indicate that these pure ices are at best minor components in the interiors of these bodies, and imply that CH4 and CO ices were not the dominant C-bearing solids in the outer nebula. Clathrate-hydrates could not have appropriated enough CH4 or CO to be the major form of condensed carbon, although such clathrates may be necessary to explain the presence of methane on Pluto after its formation from a CO-rich nebula. Laboratory studies of carbonaceous chondrites, and spacecraft observations of Comet Halley, strongly suggest that of the remaining possibilities, organic material, rather than elemental carbon, is the most likely candidate for the dominant C-bearing solid in the outer solar nebula. We conclude that the majority of the carbon in the outer solar nebula was in gaseous CO; 10% to a few tens of percent of the C was in condensed organic materials; and at least a trace amount of carbon was in methane gas.

Carbon↗

PubMed1990

Deuterium enrichment in the primitive ices of the protosolar nebula.

We have estimated the D/H ratio that may have been present in the primitive ices in the protosolar nebula. Using observations of the CH3D/CH4 ratio in the outer planets, we developed two simple but limiting models which constrain the amount of dilution that deuterated volatiles which were contributed to the planetary atmospheres by evaporated primordial ices may have undergone by mixing with the original hydrogen envelopes. The models suggest that the D/H ratio in these ices was probably somewhere between a few times 10(-4) and 10(-3). These planetary-atmosphere-derived results are compared with other solar system bodies thought to contain primitive material and with D/H ratios observed in interstellar polyatomic molecules.

Atmosphere↗

PubMed1984

Chemical evolution on the giant planets and Titan.

We summarize the current status of atmospheric chemistry in the atmospheres of the outer solar system with special emphasis on the question of HCN formation on Jupiter, differences between polar and equatorial compositions on Jupiter, the coloration of the Great Red Spot, and the unique environment of Titan.

Ammonia↗

PubMed1986

Search for organic molecules in the outer solar system.

Recent developments of millimeter astronomy have led to the discovery of more and more complex molecules in the interstellar medium. In a similar way, attempts have been made to detect complex molecules in the atmospheres of the most primitive bodies of the Solar System, i.e. outer planets and comets, as well as in Titan's atmosphere. An important progress has been achieved thanks to the continuous development of infrared astronomy, from the ground and from space vehicles. In particular, an important contribution has come from the IRIS-Voyager infrared spectrometer with the detection of prebiotic molecules on Titan, and some complex organic molecules on Jupiter and Saturn. Another important result has been the observation of carbonaceous material in the immediate surroundings of Comet Halley's nucleus. In the near future, the search for organic molecules in the outer Solar System should benefit from the developments of large millimeter antennae, and in the next decade, from the operation of infrared Earth-orbiting spacecrafts (ISO, SIRTF).

Astronomy↗

PubMed2005

Effect of rosuvastatin or atorvastatin on urinary albumin excretion and renal function in type 2 diabetic patients.

The effect of rosuvastatin or atorvastatin on urinary albumin excretion (UAE) was determined in type 2 diabetic patients. A randomized, double-blind, parallel-group, response-based design compared rosuvastatin 10mg (titrated to 40 mg) with atorvastatin 10mg (titrated to 80 mg) in type 2 diabetic patients with dyslipidemia, with dose titration to an LDL-C target of <3.0 mmol/L. Overnight timed urine collections were obtained at baseline, 8 and 16 weeks to UAE. Glomerular filtration rate (GFR) was determined using the Modification of Diet in Renal Disease formula. Patients with paired, UAE collections of at least 8h duration were analyzed (n=344). No significant change from baseline in UAE was observed for either treatment group or between-treatment groups at 16 weeks, and median UAE for both treatment groups remained within normal limits (rosuvastatin 4.5 microg/min, atorvastatin 5.0 microg/min). A similar absence of change from baseline was observed for 51 patients with UAE above the normal range at study entry (>20 microg/min). No significant change in GFR from baseline after 16 weeks was observed for either treatment group. These data provide reassurance that type 2 diabetic patients can be treated with higher efficacy statins without clinically meaningful effects on urinary albumin excretion.

Aged↗

PubMed1997

Ion irradiation: its relevance to the evolution of complex organics in the outer solar system.

Ion irradiation of carbon containing ices produces several effects among which the formation of complex molecules and even refractory organic materials whose spectral color and molecular complexity both depend on the amount of deposited energy. Here results from laboratory experiments are summarized. Their relevance for the formation and evolution of simple molecules and complex organic materials on planetary bodies in the external Solar System is outlined.

Carbon↗

PubMed1987

Light hydrocarbons from plasma discharge in H2-He-CH4: first results and Uranian auroral chemistry.

Voyager 2 found that the Uranian magnetosphere has a substantial flux of energetic charged particles, which becomes rich in higher energies at low magnetospheric L near the orbit of Miranda. The electrons precipitate to produce aurorae, which have been observed in the ultraviolet. The more energetic component of the precipitating electrons can initiate radiation chemistry in the methane-poor stratosphere, near 0.1 mbar where the CH4 mole fraction XCH4 approximately equal to 10(-5). We present laboratory results for cold plasma (glow) discharge in continuous flow H2-He-CH4 atmospheres with mol fractions XCH4 = 10(-2) to 10(-3) and total pressure p = 60 to 0.6 mbar. The yields of simple hydrocarbons in these experiments and an estimate of precipitating electron flux consistent with the Voyager ultraviolet spectroscopy results indicate the globally averaged auroral processing rate of CH4 to higher hydrocarbons approximately equal to 3 x 10(6) C cm-2 s-1, comparable to the globally averaged photochemical production rate. The local rate approximately 2 x 10(8) C cm-2 s-1 in the auroral zones (approximately 20 degrees in diameter) at 15 degrees S and 45 degrees N latitude greatly exceeds the photochemical rate. Even at very low XCH4 approximately equal to 10(-3) the yield (summed over all products) G > approximately 10(-2) C/100 eV and the average slope alpha = > approximately -0.4, where the summation is over all product molecules of a given carbon number eta and the square brackets denote abundance. The yield therefore decreases slowly with molecular complexity: hydrocarbons through C7Hx should be present in auroral zones at abundances > approximately 10(-2) of the simplest C2 hydrocarbons. Saturated hydrocarbons (C2H6, C3H8, C4H10, etc.) are mostly shielded from photodissociation by C2H2 and will therefore persist at the sunlit, as well as the currently dark, magnetic polar regions.

Atmosphere↗