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PubMed1993

Screening and psychological debriefing of adolescent survivors of life-threatening events.

There is a perceived need for schools and casualty departments to receive appropriate information and guidelines in order to minimise the effect of PTSD. A recommended screening battery for PTSD was administered at the start of a two-session debriefing group and again three months later to a group of seven young survivors of a minibus accident. No studies using this screen other than those of shipping disasters have been reported to date. Screen scores were compared with those of survivors of the cruise ship Jupiter. No significant differences were found between minibus survivors when assessed at six months (before intervention), and Jupiter survivors, who when assessed at five months had already undergone debriefing. Post-debriefing assessment of minibus survivors demonstrated significant reductions on all measures.

Adaptation, Psychological↗
PubMed2003

[Extrasolar terrestrial planets and possibility of extraterrestrial life].

Recent development of research on extrasolar planets are reviewed. About 120 extrasolar Jupiter-mass planets have been discovered through the observation of Doppler shift in the light of their host stars that is caused by acceleration due to planet orbital motions. Although the extrasolar planets so far observed may be limited to gas giant planets and their orbits differ from those of giant planets in our Solar system (Jupiter and Saturn), the theoretically predicted probability of existence of extrasolar terrestrial planets that can have liquid water ocean on their surface is comparable to that of detectable gas giant planets. Based on the number of extrasolar gas giants detected so far, about 100 life-sustainable planets may exist within a range of 200 light years. Indirect observation of extrasolar terrestrial planets would be done with space telescopes within several years and direct one may be done within 20 years. The latter can detect biomarkers on these planets as well.

Astronomical Phenomena↗
PubMed2000

The long-term psychological effects of a disaster experienced in adolescence: I: The incidence and course of PTSD.

Previous studies have shown that children and adolescents exposed to traumatic experience in a disaster can suffer from high levels of post-traumatic stress. The present paper is the first a series reporting on the long-term follow-up of a group of young adults who as teenagers had survived a shipping disaster-the sinking of the "Jupiter" in Greek waters-between 5 and 8 years previously. The general methodology of the follow-up study as a whole is described, and the incidence and long-term course of Post-Traumatic Stress Disorder (PTSD). It is the first study of its kind on a relatively large, representative sample of survivors, using a standardised diagnostic interview, and comparing survivors with a community control group. Survivors of the Jupiter disaster (N = 217), and 87 young people as controls, were interviewed using the Clinician Administered PTSD Scale (CAPS). Of the 217 survivors, 111 (51.7%) had developed PTSD at some time during the follow-up period, compared with an incidence in the control group of 3.4 % (N = 87). In the large majority of cases of PTSD in the survivors for whom time of onset was recorded, 90 % (N = 110), onset was not delayed, being within 6 months of the disaster. About a third of those survivors who developed PTSD (30%, N = 111) recovered within a year of onset, through another third (34 %, N = 111) were still suffering from the disorder at the time of follow-up, between 5 and 8 years after the disaster. Issues relating to the generalisability of these findings are discussed.

Adolescent↗
PubMed1995

[Memorandum on the origin of Rx, the signal be employed to the heading in the prescription].

The symbol variously written Rp. Rx. or R. is still employed by physicians to head their prescriptions. In our country, we have learned and believe that the origin of the symbol is an abbreviation of the Latin word for "recipe." In Europe, another suggestion of the origin of the symbol appears to represent the astronomical sign of the planet Jupiter. There is, however, no evidence to support this suggestion. As regards the Jupiter symbol it is probably that printer may have used the sign as the nearest approach he had in type to the abbreviated sign for recipe. It is believed that the confusion between the two symbols is due to a mere typographical coincidence. A careful examination of the various styles of writing the symbol, clearly shows that the sign was originally adopted as an abbreviation of the word "recipe." Recently, it has been suggested that the symbol originates in "the eye of Horus," but, as regards the eye of Horus symbol, much more still remains to be examined. Thus, I will suspend judgement until the facts of the matter become clear, and expect further researches in future.

History of Pharmacy↗
PubMed2002

[Long-term functional results of adult intra-articular distal humeral fractures treated by open reduction and plate osteosynthesis].

OBJECTIVES: We assessed the long-term functional results of surgical treatment of distal intra-articular humeral fractures, together with the factors having influence on the outcome. METHODS: Thirty-four patients (25 males, 9 females; mean age 38 years; range 20 to 78 years) who were treated by open reduction and plate osteosynthesis were retrospectively evaluated. All fractures were type C according to the AO classification. Five patients had open fractures. Thirty-three patients had surgery within the first two days after trauma. Posterior (n=19), lateral (n=13), and lateral and medial (n=2) incisions were used. Intra-articular olecranon osteotomy was performed in 11 patients in whom a posterior incision was used. The mean follow-up period was 81.5 months (range 24 to 141 months). Functional evaluation was made according to the criteria described by Jupiter et al. RESULTS: Postoperative complications included infection in four patients, nerve lesion in four patients, nonunion of the olecranon in one patient, and fixation failure in one patient. The mean elbow flexion was 115.1 degrees, and the mean extension loss was 26.3 degrees. Four patients had severe pain and deformities. According to the criteria by Jupiter et al., the results were excellent in six (17.7%), good in 15 (44.1%), fair in nine (26.4%), and poor in four (11.8%) patients. The rate of excellent and good results were higher in closed fractures, in males, in patients at 20 to 40 years of age, in those undergoing posterior incisions and intra-articular olecranon osteotomy, and in patients in whom double-plate osteosynthesis was used. CONCLUSION: Our results suggest that age, gender, infection, preservation of neural function, successful rigid fixation, an anatomic restoration of the joint surface, and early rehabilitation are effective factors on the functional outcome.

Adult↗
PubMed2005

[Treatment of AO type C2-C3 fractures of the distal end of the radius with external fixation].

OBJECTIVES: We evaluated the results of combined treatment with closed reduction, grafting, K-wires, and external fixation in patients with fractures of the distal end of the radius. METHODS: Of 24 patients (15 males, 9 females; mean age 34 years; range 21-73), 16 patients had C2, eight patients had C3 fractures according to the AO classification. Three patients had open fractures, and four patients had signs of median nerve compression. Treatment included closed reduction, autologous grafting (16 cases) followed by fixation with 2 to 5 K-wires, and an external fixator. Clinical and radiographic results were assessed according to the Gartland-Werley's and Stewart's criteria, respectively, and degenerative changes to the Knirk-Jupiter's criteria. The mean follow-up was 35 months (range 25 to 52 months). RESULTS: All of the 19 patients who were employed returned to preinjury working conditions in a mean of 3.5 months. Radial length was preserved to a great extent. The mean amount of collapse of the joint surface was 1.4 mm. The mean loss was 6.7% in radial inclination, and 17.6% in the volar tilt. According to the Stewart's criteria, the results were good, moderate, and poor in 12, nine, and three patients, respectively. Flexion-extension (75%), supination-pronation (70%), and radial-ulnar deviation (75%) were preserved to a great extent. Grip force amounted to 70% of the healthy side. According to the Gartland-Werley criteria, three patients had excellent, eight patients had good, 10 patients had moderate, and three patients had poor results. According to the Knirk-Jupiter's criteria, degenerative changes were slight in 11 patients, moderate in six patients, and severe in one patient. Six patients had no signs of degeneration. Complications included pin track infections (n=4), early transient reflex sympathetic dystrophy (n=2), and hypoesthesia along the superficial branch of the radial nerve (n=2). CONCLUSION: Treatment of the distal end fractures of the radius (AO type C2-C3) with a combination of external fixation, grafting, and percutaneous K-wires provides almost normal radiologic and clinical parameters.

Adult↗
PubMed1993

The condensation and vaporization behavior of ices containing SO2, H2S, and CO2: implications for Io.

In an extension of previously reported work on ices containing CO, CO2, H2O, CH3OH, NH3, and H2, measurements of the physical and infrared spectral properties of ices containing molecules relevant to Jupiter's moon Io are presented. These include studies on ice systems containing SO2, H2S, and CO2. The condensation and sublimation behaviors of each ice system and surface binding energies of their components are discussed. The surface binding energies can be used to calculate the residence times of the molecules on a surface as a function of temperature and thus represent important parameters for any calculation that attempts to model the transport of these molecules on Io's surface. The derived values indicate that SO2 frosts on Io are likely to anneal rapidly, resulting in less fluffy, "glassy" ices and that H2S can be trapped in the SO2 ices of Io during night-time hours provided that SO2 deposition rates are on the order of 5 micrometers/hr or larger.

Carbon Dioxide↗
PubMed1995

Comets, impacts, and atmospheres.

We are proposing a model for the delivery of volatiles to the inner planets by icy planetesimals (comets). Laboratory studies of the trapping of gases in ice forming at low temperatures simulate the formation of comet nuclei at various distances from the Sun in the solar nebula. The total gas content as well as the relative proportions of gases trapped in the ice are strong functions of temperature. As they trap N2 inefficiently, all planetesimals formed interior to Neptune are deficient in nitrogen, acquiring values of C/N resembling those found in the inner planet volatile inventories. A mixture of three basic types of comets appears capable of accounting for the observed volatile inventories on Venus, Earth, and Mars, with the caveat that impact erosion is necessary to explain the present condition of the martian atmosphere. The model includes the possibility of several epochs of clement conditions on early Mars. Some tests of these ideas are suggested, including measurements in Jupiter's atmosphere by the Galileo probe.

Atmosphere↗
PubMed1985

The Jovian stratosphere in the ultraviolet.

The center-of-disk reflectivity of Jupiter in the wavelength range from 1450 to 3150 angstroms has been computed from 30 low-dispersion IUE spectra taken during solar maximum in 1978-1980. A vertically inhomogeneous radiative transfer program is used to compute model reflectivities of various stratospheric compositions for comparison. Ammonia and acetylene are well determined because they show narrow absorption bands in the ultraviolet. Above 1800 angstroms, these two gases provide a good fit to the data, but not below. At shorter wavelengths the fit would be much improved by a small amount (0.5-1.5 ppb) of propadiene/allene (C3H4). Voyager IRIS spectra show that the IR bands of allene are not strong enough to be detected in such a small amount. Additional absorption around 1600 angstroms can be reproduced best with the presence of cyclopropane (C3H6, <15 ppb), although other absorbers (e.g., hydrocarbon molecules with more than three carbon atoms, oxygen- or nitrogen-containing molecules, or a high-altitude haze) could also explain the spectrum in this region. The data are too noisy to detect possible CO Cameron band absorption near 2000 angstroms.

Acetylene↗
PubMed1988

Estimation of the reaction rate for the formation of CH3O from H + H2CO: implications for chemistry in the Solar System.

It is argued that the formation of the methoxy radical (CH3O) from H + H2CO may play an essential role in the reduction of CO to CH4. The rate coefficient for this reaction has been estimated using the approximate theory of J. Troe (1977a, J. Chem. Phys. 66, 4745) and transition state theory. We briefly discuss the implications of this reaction for the chemistry of CO on Jupiter, in the solar nebula, for interpreting the laboratory experiments of A. Bar-Nun and A. Shaviv (1975, Icarus 24, 197) and A. Bar-Nun and S. Chang (1983, J. Geophys. Res. 88, 6662) and for organic synthesis in the prebiotic terrestrial atmosphere.

Atmosphere↗
PubMed1991

Troposphere-stratosphere interactions in a one-dimensional model of Jovian photochemistry.

A simple one-dimensional model of the Jovian atmosphere including the coupling between a rapidly mixed troposphere and a stagnant stratosphere is presented. We treat analytically the case of a chemically unreactive species flowing downward through the stratosphere and troposphere with a constant flux. The calculated concentration profile has a maximum value approximately one atmospheric scale height above the tropopause. The corresponding mixing ratio rapidly decreases in the lower stratosphere. The contrast between the peak stratosphere and tropopause concentrations reflects the variation between the lower stratosphere and upper troposphere eddy diffusion coefficients. Numerical simulations of unreactive CO and C2H6, considering high-altitude photochemical sources (yielding downward fluxes to the troposphere) and deep troposphere thermochemical sources, demonstrate that upper troposphere abundances may have a large photochemical contribution. Recent observations of CO near 5 bar can be reproduced by a model using any one of three different tropospheric eddy diffusion profiles: a constant value of approximately 10(8) cm2 sec-1, a constant value of < or approximately 10(4) cm2 sec-1, or a two-layer model with a rapidly mixed (10(8) cm2 sec-1) layer below 20 bar and a slower mixing layer (10(4) cm2 sec-1) between 100 mbar and 20 bar. In the latter two scenarios, the photochemical source is an important and/or dominant source of upper tropospheric CO. However, the upper tropospheric C2H6 abundances are distinctly different among the three cases. These calculations suggest objectives for higher spectral resolution observations, critical vertical scales for planning experiments on future missions to Jupiter, and predictions that can be tested with the Galileo probe mass spectrometer.

Atmosphere↗
PubMed1992

Radiation chemistry in the Jovian stratosphere: laboratory simulations.

Low-pressure continuous-flow laboratory simulations of plasma induced chemistry in H2/He/CH4/NH3 atmospheres show radiation yields of hydrocarbons and nitrogen-containing organic compounds that increase with decreasing pressure in the range 2-200 mbar. Major products of these experiments that have been observed in the Jovian atmosphere are acetylene (C2H2), ethylene (C2H4), ethane (C2H6), hydrogen cyanide (HCN), propane (C3H8), and propyne (C3H4). Major products that have not yet been observed on Jupiter include acetonitrile (CH3CN), methylamine (CH3NH2), propene (C3H6), butane (C4H10), and butene (C4H8). Various other saturated and unsaturated hydrocarbons, as well as other amines and nitriles, are present in these experiments as minor products. We place upper limits of 10(6)-10(9) molecules cm-2 sec-1 on production rates of the major species from auroral chemistry in the Jovian stratosphere, and calculate stratospheric mole fraction contributions. This work shows that auroral processes may account for 10-100% of the total abundances of most observed organic species in the polar regions. Our experiments are consistent with models of Jovian polar stratospheric aerosol haze formation from polymerization of acetylene by secondary ultraviolet processing.

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↗
PubMed1987

Europa, tidally heated oceans, and habitable zones around giant planets.

Tidal dissipation in the satellites of a giant planet may provide sufficient heating to maintain an environment favorable to life on the satellite surface or just below a thin ice layer. In our own solar system, Europa, one of the Galilean satellites of Jupiter, could have a liquid ocean which may occasionally receive sunlight through cracks in the overlying ice shell. In such case, sufficient solar energy could reach liquid water that organisms similar to those found under Antarctic ice could grow. In other solar systems, larger satellites with more significant heat flow could represent environments that are stable over an order of Aeons and in which life could perhaps evolve. We define a zone around a giant planet in which such satellites could exist as a tidally-heated habitable zone. This zone can be compared to the habitable zone which results from heating due to the radiation of a central star. In our solar system, this radiatively-heated habitable zone contains the Earth.

Biomass↗
PubMed1994

Ulysses charged particle measurements between 1 and 5 AU from the sun.

Proton fluxes obtained by two instruments carried on the ESA/NASA Ulysses spacecraft are reported for the period from launch in October 1990 till Jupiter encounter in February 1992. Proton energy ranges are 24-59, 71-99, 130-320, 320-2100 and > 2100 MeV. The Sun was very active during this period, the events of March 1991 being some of the largest of the solar cycle. The relationship between events on the Sun and the observed proton flux is discussed.

Electrons↗
PubMed1995

Photolysis of phosphine in the presence of acetylene and propyne, gas mixtures of planetary interest.

Phosphine (PH3) 1 has been observed in the atmospheres of Jupiter and Saturn. We have studied the photochemical reactions of this compound with acetylene (C2H2), an alkyne also detected in these atmospheres. The volatile products formed in these reactions were characterized by H, 31P and 13C NMR. The ethenylphosphine 2 is the first product formed in the photolysis of PH3 in the presence Of C2H2. Photolysis of PH3 in the presence of propyne (C3H4) led to the formation of the Z- and E-prop-1-enylphosphines and traces of 1-methylethenylphosphine. A reaction pathway is proposed. The initial step is the dissociation of PH3 to hydrogen and PH2 radicals. Addition of the phosphinyl radical on alkyne occurs as the next step. Vinylphosphines are then formed by radical combination. This proposed reaction pathway takes into account the nature of the products and studies devoted to the photolysis of germane (GeH4) or hydrogen sulfide (H2S) in the presence of alkyne. Attempts to detect the methylidynephosphine HC triple bond P (the isoelectronic compound of HC triple bond N), in the photolysis products of PH3-C2H2 mixtures were unsuccessful. The application of these findings to Jovian and Saturn atmospheric chemistry is discussed.

Acetylene↗
PubMed2002

Circular polarization of light by planet Mercury and enantiomorphism of its surface minerals.

Different mechanisms for the generation of circular polarization by the surface of planets and satellites are described. The observed values for Venus, the Moon, Mars, and Jupiter obtained by photo-polarimetric measurements with Earth based telescopes, showed accordance with theory. However, for planet Mercury asymmetric parameters in the circular polarization were measured that do not fit with calculations. For BepiColombo, the ESA cornerstone mission 5 to Mercury, we propose to investigate this phenomenon using a concept which includes two instruments. The first instrument is a high-resolution optical polarimeter, capable to determine and map the circular polarization by remote scanning of Mercury's surface from the Mercury Planetary Orbiter MPO. The second instrument is an in situ sensor for the detection of the enantiomorphism of surface crystals and minerals, proposed to be included in the Mercury Lander MSE.

Astronomy↗
PubMed1998

Evidence for a subsurface ocean on Europa.

Ground-based spectroscopy of Jupiter's moon Europa, combined with gravity data, suggests that the satellite has an icy crust roughly 150 km thick and a rocky interior. In addition, images obtained by the Voyager spacecraft revealed that Europa's surface is crossed by numerous intersecting ridges and dark bands (called lineae) and is sparsely cratered, indicating that the terrain is probably significantly younger than that of Ganymede and Callisto. It has been suggested that Europa's thin outer ice shell might be separated from the moon's silicate interior by a liquid water layer, delayed or prevented from freezing by tidal heating; in this model, the lineae could be explained by repetitive tidal deformation of the outer ice shell. However, observational confirmation of a subsurface ocean was largely frustrated by the low resolution (>2 km per pixel) of the Voyager images. Here we present high-resolution (54 m per pixel) Galileo spacecraft images of Europa, in which we find evidence for mobile 'icebergs'. The detailed morphology of the terrain strongly supports the presence of liquid water at shallow depths below the surface, either today or at some time in the past. Moreover, lower-resolution observations of much larger regions suggest that the phenomena reported here are widespread.

Extraterrestrial Environment↗