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The prevalence of dysfunction of the temporomandibular joint (TMJ), especially in people aged 18-65 years, reached 95-98% among all dental applications. The course of the pathology is usually hidden, with periodic recurrences, and has a long nature, which is accompanied by a decrease in overall quality of life. Treatment of this pathology of the TMJ is a set of complex therapeutic, orthopedic and psychological measures. The literature describes many ways to treat TMJ dysfunction, and one of the modern ones is the use of occlusal splints, which enables to change the position of the mandible, diagnose and eliminate musculoskeletal dysfunction of the TMJ. The aim of the study was to determine the effectiveness of treatment of musculoskeletal dysfunction of the TMJ with occlusal splints according to axiography. Material and methods. 274 patients aged 18 to 65 years were diagnosed with temporomandibular joint (TMJ) pain syndrome before and after treatment.Results. All patients with signs of TMJ dysfunction before treatment had a violation of the trajectory of the mandible (deviation – 68.7%, dyslexia – 31.3%). When opening and closing the mouth, asymmetrical shifts of the lower jaw to the sides of more than 2 mm (deviation from the midline – more than 2 mm) were observed. After treatment with occlusal splints there was an improvement in the trajectory of opening and closing the mouth: the number of patients with a violation of the trajectory decreased by 89.1%, and the displacement of the mandible during opening and closing the mouth in 92.4% of patients decreased on average to 0, 9 mm. When analyzing the movements of the mandible in the sagittal plane in 79 % of cases, deviations of the trajectory of the mandible were detected. After treatment with occlusive muscle relaxation splints, elimination of violations of the trajectory of the mandible in the transverse plane was noted in 93.4% of cases, reduction of displacement to 0.9 mm in 78.1% of patients. Сonclusions. The trajectory of the mandible in the sagittal plane improved in 80.1% of patients, normalization of the position of the mandible relative to the neuromuscular trajectory was achieved in 93.4% of clinical cases. According to the analysis of parameters, such treatment should be considered effective.

Population, man, human resources, human capital are the defining concepts in the consideration of issues related to the functioning of the national economy in modern economic conditions. It is generally recognized that labor activity is the main prerequisite that determines the material and spiritual wealth of man and society as a whole. Therefore, human resources at the present stage is one of the main components of the production potential of management in Ukraine, increasing the efficiency of use and reproduction of which are especially relevant. On the level of efficiency of human resources depends the level of welfare of the population, the development of productive forces, the scale of material production, etc. The development of intellectual productive forces and the strengthening of the influence of innovation and information factors contributes to the formation of a new socio-economic role of man in the modern economy and requires appropriate research. The article reveals the theoretical issues of trends in human capital development, a thorough analysis of the current state of human capital development and its importance in the modern economy. Based on the generalization of different views of scientists, the main stages of human capital formation in the agricultural sector of Ukraine's economy are identified and characterized. The problems of human capital use have been studied and proposals for its improvement have been worked out. It is revealed that the process of reproduction of human capital in agricultural enterprises and its effective use in the conditions of market transformations should be based on the principles of active policy aimed at reviving the economic situation in agriculture; scientific substantiation; development of measures in order to increase jobs and increase the labor needs of agricultural enterprises; improvement of the system of remuneration, social protection of agricultural workers; formation of the mechanism of social partnership, etc.

The prevalence of dysfunction of the temporomandibular joint, especially in people aged 18-60 years, reached 95-98 % among all dental applications. The course of the pathology is usually hidden, with periodic recurrences and has a long nature, which is accompanied by a decrease in overall quality of life. Treatment of this pathology of the temporomandibular joint is a set of complex therapeutic, orthopedic and psychological measures. The literature describes many ways to treat temporomandibular joint dysfunction, one of the modem ones is the use of occlusal splints, which allow to change the position of the mandible, diagnose and eliminate musculoskeletal dysfunction of the temporomandibular joint. The aim of the study was to determine the effectiveness of treatment of musculoskeletal dysfunction of the temporomandibular joint with occlusal splints according to axiography. 274 patients aged 18 to 65 years were diagnosed with temporomandibular joint pain syndrome before and after treatment. All patients with signs of temporomandibular joint dysfunction before treatment had a violation of the trajectory of the mandible (deviation is 68.7 %, dyslexia is 31.3 %). When opening and closing the mouth, asymmetrical shifts of the lower jaw to the sides of more than 2 mm (deviation from the midline is more than 2 mm) were observed. After treatment with occlusal splints there was an improvement in the trajectory of opening and closing the mouth: the number of patients with a violation of the trajectory decreased by 89.1 %, and the displacement of the mandible during opening and closing the mouth in 92.4 % of patients decreased on average to 0.9 mm. When analyzing the movements of the mandible in the sagittal plane in 79 % of cases, deviations of the trajectory of the mandible were detected. After treatment with occlusive muscle relaxation splints, elimination of violations of the trajectory of the mandible in the transverse plane was noted in 93.4 % of cases, reduction of displacement to 0.9 mm in 78.1 % of patients. The trajectory of the mandible in the sagittal plane improved in 80.1 % of patients, normalization of the position of the mandible relative to the neuromuscular trajectory was achieved in 93.4 % of clinical cases. According to the analysis of parameters, such treatment should be considered effective. Keywords: musculoskeletal dysfunction, temporomandibular joint, clinical dysfunction index, axiography, sagittal articular pathway angle, sagittal incisor pathway angle, Bennett’s angle (movement), duration.

Objectives. Study of ways to increase the efficiency of immediate prosthetic treatment of patients with asymmetric distally unlimited defects of dental rows by using clinical relining of partial removable dentures with elastic material to reduce the time of adaptation to dentures and normalize the functional activity of the masticatory muscles. Materials and methods. The efficiency of clinical relining of partial removable dentures using an elastic lining with Ufi Gel P from VOCO (Germany) was evaluated by electromyographic examination with BioEMG III electromyograph from BioRESEARCH Associates, Inc. (USA). The bioelectrical activity of the temporal and masseter muscles was evaluated during maximum voluntary clenching and mastication. The quantitative indicators of the amplitude of biopotentials (μV) and the qualitative characteristics of the chewing cycles were evaluated. Results. Our study has revealed that patients with asymmetric distally unlimited defects of dental rows had shown a significant decrease in the amplitude of biopotentials of the masticatory muscles compared to patients in the control group during maximum voluntary clenching and chewing, as well as a significant asymmetry of the bioelectric activity of the masticatory muscles on the right and left. During mastication there were significant differences in the size and duration of chewing cycles, a decrease in the duration of rest periods and the average number of chewing movements increased almost two times compared with intact dentition. A month after prosthetics, the indicators of bioelectrical activity of the masticatory muscles improved in both study groups of patients, but the most significant increase in amplitude was observed in the second group with a soft lining. There was also revealed a significant increase in the symmetry of bioelectric activity of the masticatory muscles, an improvement in the characteristics of the masticatory cycles and normalization of the activity and rest periods duration ratio in patients of the second group, while in patients of the 1st clinical group the indicators of symmetry did not change significantly. The average number of chewing movements required to chew the hazelnut kernel decreased to 38.7±16.2 and 29.3±10.7 respectively, in groups 1 and 2, which indicates an increase of masticatory efficiency. Conclusions. In the framework of this study, the high efficiency of elastic lining for the successful rehabilitation of patients with asymmetric distally unlimited defects in case of early prosthodontic interventions was proved. Our observations have shown that the use of the soft lining significantly increases the functional parameters of the masticatory system, shortens the period of adaptation to removable dentures and supports the formation of the alveolar processes relief without irregularities.

We report our search for methane in the atmosphere of Mars using high-spectral resolution heterodyne spectroscopy in the 7.8 μm wavelength region. Resolving power and frequency precision of >10 6 of the technique enable identification and full resolution of a targeted spectral line in the terrestrial-Mars spectrum observed from the ground. Observations were carried out on two occasions, in April 2010 and May 2012 at the McMath-Pierce Solar Telescope and the NASA Infrared Telescope Facility, respectively. A single line in the ν 4 band of methane at 1282.62448 cm −1 was targeted in both cases. No absorption due to methane was detected and only upper limits of ∼100 ppb for the martian atmospheric methane concentration were retrieved. Lack of observing time (due to weather) and telluric opacity greater than anticipated led to reduced signal-to-noise ratios (SNR). Based on current measurements and calculations, under proper viewing conditions, we estimate an achievable detection limit of ∼10 ppb using the infrared heterodyne technique – adequate for confirming reported detections of methane based on other techniques.

Remote sensing observations meet some limitations when used to study the bulk atmospheric composition of the giant planets of our solar system. A remarkable example of the superiority of in situ probe measurements is illustrated by the exploration of Jupiter, where key measurements such as the determination of the noble gases abundances and the precise measurement of the helium mixing ratio have only been made available through in situ measurements by the Galileo probe. This paper describes the main scientific goals to be addressed by the future in situ exploration of Saturn placing the Galileo probe exploration of Jupiter in a broader context and before the future probe exploration of the more remote ice giants. In situ exploration of Saturn's atmosphere addresses two broad themes that are discussed throughout this paper: first, the formation history of our solar system and second, the processes at play in planetary atmospheres. In this context, we detail the reasons why measurements of Saturn's bulk elemental and isotopic composition would place important constraints on the volatile reservoirs in the protosolar nebula. We also show that the in situ measurement of CO (or any other disequilibrium species that is depleted by reaction with water) in Saturn's upper troposphere would constrain its bulk O/H ratio. We highlight the key measurements required to distinguish competing theories to shed light on giant planet formation as a common process in planetary systems with potential applications to most extrasolar systems. In situ measurements of Saturn's stratospheric and tropospheric dynamics, chemistry and cloud-forming processes will provide access to phenomena unreachable to remote sensing studies. Different mission architectures are envisaged, which would benefit from strong international collaborations., Comment: Submitted to Planetary and Space Science

著者人数：156名, Accepted: 2008-05-27, 資料番号: SA1000998000

We report observations of temperatures in the Venus upper mesosphere/lower thermosphere. Data were acquired between 22 and 24 October 2007 at the NASA Infrared Telescope Facility on Mauna Kea, Hawaii using the NASA Goddard Space Flight Center Heterodyne Instrument for Planetary Wind and Composition (HIPWAC). Fully resolved non-thermal emission (non-LTE) lines in the 10.6 μ m band of CO2 from various rotational levels were used to study rotational and kinetic temperatures on the Venus dayside. From models the emission is assumed to originate in the range of ∼ 100 –120 km altitude. Rotational temperatures were derived from the intensity distribution of the CO2 lines measured at the equator/45° east, mid-latitudes (45° north and south)/45° east, and 70° south/30° east. Retrieved values (171–236 K) disagree with the observed kinetic temperatures in all but one point (45° north/45° east). In addition, the measured intensities show a large dispersion originating most likely in the Venus atmosphere. Information on kinetic temperatures was extracted from the widths of the emission lines. Temperature values range from 224 to 236 K and were retrieved at the equator/45° east, mid-latitudes (45° north and south)/45° east, and 70° south/30° east, and along the equator at various longitudes with an accuracy of up to 2 K. These values are higher than the Venus International Reference Atmosphere model predicts. The longitudinal scan shows kinetic temperatures of ∼ 230 –250 K from the subsolar point to 40° offset from the terminator followed by a decrease to ∼ 120 K close to the terminator.

We report observations of Venus atmospheric wind near 110 km altitude by means of high-resolution mid-infrared spectroscopy. Data were acquired May 28–June 4, 2007 at the McMath-Pierce Solar Telescope (Kitt Peak, Arizona, USA), during a coordinated ground-based observing campaign in support of Venus Express. The Cologne Tuneable Heterodyne Infrared Spectrometer (THIS) was used to measure the Doppler shift of fully resolved non-LTE emission lines of CO2 at 959.3917 cm - 1 ( 10.423 μ m ) to determine wind velocity. Spatial resolution was ∼ 1.7 arcsec on Venus’ apparent diameter of 20–22 arcsec. Zonal wind velocities were retrieved at six different latitudes close to the west limb. Retrieved zonal velocities—parallel to Venus’ retrograde solid body rotation—range 3 ± 7 m / s ( 1 σ ) at the equator to a maximum of 32 ± 4 m / s ( 1 σ ) at southern mid-latitude ( 45 ∘ S ) , decreasing at higher latitudes and thus suggesting a retrograde double jet structure for the zonal component. The subsolar-to-antisolar circulation component was measured at one position, 45 ∘ towards the sunlit limb from the central meridian, on the equator. The retrieved subsolar-to-antisolar component at this position implies a cross-terminator velocity of 52 ± 18 m / s ( 1 σ ) . Retrieved velocities are lower than previous results, suggesting spatial and/or temporal variability of dynamics in the mesosphere/thermosphere of Venus.

Spectroscopic data obtained by the Infrared Interferometer Spectrometer (IRIS) aboard Voyager 1 and 2 have been re-visited. Using the spectroscopic data and footprints of the IRIS aperture on the planet, we constructed images of the stratosphere of Jupiter at the emission bands of hydrocarbons including , and . Thermal emission from the hydrocarbons on Jupiter originates from a broad region of the stratosphere extending from 1 to 10 millibars. We averaged the data using a bin of 20 degrees of longitude and latitudes in order to increase signal-to-noise ratios. The resultant images show interesting wave structure in Jupiter`s stratosphere. Fourier transform analyses of these images yield wavenumbers 5 - 7 at mid-Northern and mid-Southern latitudes, and these results are different from those resulted from previous ground-based observations and recent Cassini CIRS, suggesting temporal variations on the stratospheric infrared pattern. The comparisons of the Voyager 1 and 2 spectra also show evidence of temporal intensity variations not only on the infrared hydrocarbon polar brightenings of hydrocarbon emissions but also on the stratospheric infrared structure in the temperate regions of Jupiter over the 4 month period between the two Voyager encounters. Short running title: Stratospheric Images of Jupiter derived from Voyager IRIS Spectra.

We present the characteristics of the dust comae of two comets, 126P/IRAS, a member of the Halley family (a near-isotropic comet), and 2P/Encke, an ecliptic comet. We have primarily used mid- and far-infrared data obtained by the ISOPHOT instrument aboard the Infrared Space Observatory (ISO) in 1996 and 1997, and mid-infrared data obtained by the SPIRIT III instrument aboard the Midcourse Space Experiment (MSX) in 1996. We find that the dust grains emitted by the two comets have markedly different thermal and physical properties. P/IRAS's dust grain size distribution appears to be similar to that of fellow family member 1P/Halley, with grains smaller than 5 microns dominating by surface area, whereas P/Encke emits a much higher fraction of big (20 μm and higher) grains, with the grain mass distribution being similar to that which is inferred for the interplanetary dust population. P/Encke's dearth of micron-scale grains accounts for its visible-wavelength classification as a “gassy” comet. These conclusions are based on analyses of both imaging and spectrophotometry of the two comets; this combination provides a powerful way to constrain cometary dust properties. Specifically, P/IRAS was observed preperihelion while 1.71 AU from the Sun, and seen to have a 15-arcmin long mid-infrared dust tail pointing in the antisolar direction. No sunward spike was seen despite the vantage point being nearly in the comet's orbital plane. The tail's total mass at the time was about 8×109 kg. The spectral energy distribution (SED) is best fit by a modified greybody with temperature T=265±15 K and emissivity e proportional to a steep power law in wavelength λ: e∝λ−α, where α=0.50±0.20 (2σ) . This temperature is elevated with respect to the expected equilibrium temperature for this heliocentric distance. The dust mass loss rate was between 150–600 kg/s (95% confidence), the dust-to-gas mass loss ratio was about 3.3, and the albedo of the dust was 0.15±0.03. Carbonaceous material is depleted in the comet's dust by a factor of 2–3, paralleling the C2 depletion in P/IRAS's gas coma. P/Encke, on the other hand, observed while 1.17 AU from the Sun, had an SED that is best fit by a Planck function with T=270±15 K and no emissivity falloff. The dust mass loss rate was 70–280 kg/s (95% confidence), the dust-to-gas mass loss ratio was about 2.3, and the albedo of the dust was about 0.06±0.02. These conclusions are consistent with the strongly curved dust tail and bright dust trail seen by Reach et al. (2000; Icarus 148, 80) in their ISO 12-μm imaging of P/Encke. The observed differences in the P/IRAS and P/Encke dust are most likely due to the less evolved and insolated state of the P/IRAS nuclear surface. If the dust emission behavior of P/Encke is typical of other ecliptic comets, then comets are the major supplier of the interplanetary dust cloud.

Infrared heterodyne spectroscopy (λ/Δλ⩾106) enabled the precision measurement of lineshapes of 168 ethylene absorption transitions for 12C2H4 and 88 absorption transitions for 13 C 12 CH 4 . Of the 168 12C2H4 transitions, 96 are assigned to ν7, 17 to ν10, 10 to ν4, and 45 to hotband transitions. The 88 13 C 12 CH 4 transitions have not been assigned. Measurements were made at gas temperatures in the range of 293– 297 K and at pressures in the range of 0.05– 0.5 Torr . Absolute line frequencies and line intensities were retrieved for each of the transitions. Frequencies and absolute intensities of unblended strong lines were determined to better than 5×10 −5 cm −1 and 10%, respectively.

Self- and nitrogen (N2) broadening of ethylene (C2H4) have been measured for the ν 10 20 11,10 ←19 10,9 ethylene transition at 927.01879 cm −1 . The measurements were made using infrared heterodyne spectroscopy with a spectral resolution of ∼1.7×10−4cm−1. At 296 K , the retrieved self-broadening coefficient for the observed transition is 0.1244(92) cm −1 / atm ; the nitrogen-broadening coefficient is 0.0757(99) cm −1 / atm . These results represent the most conservative treatment of experimental and statistical errors. A different purely statistical approach provides consistent values with uncertainties of only a few percent.

We report on our molecular spectroscopy effort to determine frequencies, intensities, shapes and broadening in fundamental and low-lying hot band transitions for molecules of interest to contemporary planetary atmospheric investigations. The laboratory measurements, obtained with the NASA/GSFC Heterodyne Instrument for Planetary Wind and Composition (HIPWAC), are described in a companion paper in this session (see Blass et al.) which also compares our results to those of other researchers (e.g., Vander Auwera et al.). Herein we present the analysis methodology and interpretation of the laboratory measurements. We identified molecular species of significance to current outer-planet missions such as the Cassini Mission to Jupiter, Saturn and Titan: ethane (C2H6), including both normal and primary hot band (i.e., _9 and _9 + _4 _ _4); ethylene (C2H4); and allene (C3H4). The laboratory measurements which are the basis for the results reported herein were obtained at a spectral resolution of 0.00003 cm_1 (_1MHz) at 12 µm. At this spectral resolution, the rotation-vibration transitions measured under laboratory conditions (ambient temperature and _1 Torr pressure) are fully resolved and identified without ambiguity. The principal objective is to provide critical laboratory truth for the interpretation of infrared spectral observations of the Cassini mission, follow on missions to Titan and the outer planets, and in the re-interpretation of mid-IR emission spectra from Voyager IRIS, ISO, and ground based IR data of the outer planets. Resultant line intensities (

The absolute infrared intensities of transitions in the _9 band of ethane have long been a subject of controversy (Gunson 1996, Daunt 1984, Henry 1983, Auwera 2007, and references therein). Improving the ethane 12 µm database is one of the goals of this work. The spectra here acquired was obtained using the NASA Heterodyne Instrument for Planetary Wind And Composition (HIPWAC) in a laboratory setting. HIPWAC, in this environment, makes use of a blackbody source and a gas absorption cell. Observations were carried out from P(10) at 858.1583905 cm_1 to P(32) at 839.1958112 cm_1 of the 646 laser. The observational range is ± 3GHz centered on each laser line. HIPWAC has the ability to measure spectra by using infrared heterodyne techniques, in which an infrared source is combined with a laser local oscillator and focused on a photomixer, where the difference frequency between the source and laser is retrieved and analyzed. Using these techniques HIPWAC is able to achieve a very high resolution (_/__ > 106 ) and a high frequency specificity (> 10_8 ) in order to study low-pressure gases. The spectra was retrieved using an Acoustic-Optical Spectrometer (AOS) with a sampling interval of 1 MHz. The detector was a liquid Helium cooled HgCdTe Photomixer. The ethane was research grade (99.96 %) obtained from Matheson Gas Products. The gas was contained in a 30 cm straight-path cell with ZnSe windows. The gas pressure was 0.709 Torr, as measured by an MKS Baratron gauge, at a temperature of 26 degrees Celcius. Additional measurements were also done at 1.4 Torr and 2.8 Torr. The spectra acquired is double sided and was fitted using an IDL program. The quantum assignments were taken from previous atlases (Tennessee/GSFC and GEISA). Currently, similar measurements are also being done on Allene and OCS. In the future we would like to incorporate Quantum Cascade Lasers in our system to replace our CO2 gas lasers. Quantum Cascade lasers are very small solid-state devices with an output power of about 100 mW and limited tunability.

The current and prospective status of astronomical research in Ukraine is discussed. A brief history of astronomical research in Ukraine is presented and the system organizing scientific activity is described, including astronomy education, institutions and staff, awarding higher degrees/titles, government involvement, budgetary investments and international cooperation. Individuals contributing significantly to the field of astronomy and their accomplishments are mentioned. Major astronomical facilities, their capabilities, and their instrumentation are described. In terms of the number of institutions and personnel engaged in astronomy, and of past accomplishments, Ukraine ranks among major nations of Europe. Current difficulties associated with political, economic and technological changes are addressed and goals for future research activities presented.

[1] High-resolution infrared spectroscopy of ethane (C2H6) emission features formed in the stratosphere of Titan was collected on disc center at 11.74 μm wavelength (851 cm−1) on 15 January 2005 UT. The observations were obtained at the Subaru 8.2 m telescope of the National Astronomical Observatory of Japan on Mauna Kea, Hawaii, using the NASA Goddard Space Flight Center Heterodyne Instrument for Planetary Winds and Composition (HIPWAC). Fully resolved rotational-vibrational transitions of C2H6 were measured with resolving power λ/Δλ ≥ 106 by infrared heterodyne spectroscopy (IRHS). The spectrum is reproduced most effectively by vertical profiles of ethane abundance that are uniform through the stratosphere and enhanced within the mesosphere. Profiles in which there is a significant gradient within the stratosphere are not favored. The retrieved stratospheric ethane mole fraction depends weakly on the form invoked for the mesospheric enhancement. Two forms of the ethane mole fraction profile are found to reproduce the observed spectrum effectively: the best fitting results are obtained with a profile in which the mesospheric ethane concentration increases logarithmically versus decreasing pressure, retrieving a stratospheric ethane concentration of 8.2 ± 2.1 × 10−6 (1σ), increasing proportional to p−1.2 from the stratopause through the mesosphere (p is pressure). A second form of profile, in which the mesospheric ethane concentration is enhanced uniformly by a factor of 9.5, retrieves a stratospheric concentration of 9.7 ± 4.9 × 10−6 (1σ), with the enhancement discontinuity at about one scale height above the stratopause. The retrieved stratospheric mole fraction is consistent with earlier retrievals from IRHS and is somewhat less than contemporaneous retrievals from infrared spectroscopy at lower resolution by the Cassini spacecraft. The retrieved mesospheric concentration is consistent with in situ measurements in Titan's thermosphere made by the Cassini Ion Neutral Mass Spectrometer instrument during the Titan flyby (Waite et al., 2005).

International audience; Measurements of stratospheric zonal winds on Titan were made in preparation for and during the time of the descent of the Huygens Probe into Titan's atmosphere on 14 January 2005. Fully resolved emission lines from ethane near 11.7 mum were measured on the east, center, and west positions on Titan using the NASA/GSFC Heterodyne Instrument for Planetary Wind And Composition, HIPWAC, mounted on the National Astronomical Observatory of Japan 8.2 m Subaru Telescope on Mauna Kea, Hawaii. Analysis of the Doppler shifts of the emission line shapes yielded mean prograde gas velocity ~60 +/- 65 m/s at altitudes below ~120 km (~5 mbar). This result is consistent with retrievals from the Huygens Doppler Wind Experiment and from other observations near this altitude range. Current spectral line shapes, however, differed significantly from those obtained in similar measurements on Subaru in 2004 and on the NASA IRTF in 1993-1996, which retrieved prograde zonal winds 190 +/- 90 m/s at 230 km (~0.4 mbar). The cores of the emission lines, which probe the high-altitude region, could not be fitted as before to retrieve wind directly using the accepted atmospheric model for Titan. They imply an approximately tenfold increase in ethane mole fraction (1.2 × 10-4) with strong wind shear above the stratopause, providing a potential probe of the lower mesosphere and possible evidence of temporal and spatial variability. Results contribute to coordinated measurements of winds by various techniques providing information on the altitude distribution of wind velocity in Titan's atmosphere from near the surface to the lower mesosphere.

International audience; The Huygens Probe has successfully entered Titan's atmosphere and landed on its surface on 14 January 2005. With the aim of characterizing the zonal wind flow in Titan's stratosphere close to the time of entry, coordinated observations were carried out at the Very Large Telescope on the nights of 7, 12, 14, and 15 January. As in our previous investigation (Luz et al., 2005), we used the UVES instrument, mounted on the Kueyen-UT2 telescope, simultaneously achieving high spectral resolving power and high spatial resolution. The field has been derotated in order to align the 0.3-arcsec aperture perpendicularly to Titan's rotation axis. In this configuration, spatial information in the east-west direction is preserved in a set of spectra in the direction perpendicular to dispersion. We present measurements of zonal winds obtained with the technique of absolute accelerometry. The observations were made in the wavelength range 4200-6200 Å, probing between 115 and 280 km, with peak contributions at 200 and 170 km for the lower and upper parts of the domain. We detect prograde zonal winds with lower limits 46 and 53 ms-1 at these altitudes. These values are close to our previous measurements.

[1] Saturn's satellite, Titan, may have stratospheric winds up to ∼210 m/s, circling Titan in ∼1 terrestrial day compared to its 16-day rotation. Theoretical models explaining such super-rotating winds are not well constrained by observations of Titan or a similar slow rotator, Venus. We report measurements taken in December 2003 of zonal wind near Titan's equatorial region, including the Cassini Huygens probe entry latitude. Super-rotating prograde zonal winds of 190 ± 90 m/s near 220 km altitude are found from Doppler-shifted C2H6 gas emission near 12 μm, confirming high wind velocity even near the equator. Stratospheric temperature constraints and ethane abundance (8 ± 3 ppm) also are retrieved. Results are not inconsistent with earlier measurements and with recent Cassini CIRS results, but indicate possible variations between Titan's hemispheres. Differences in east and west C2H6 spectral line shapes can be accounted for by different vertical distributions of either C2H6 abundance or temperature or by unidentified dynamical effects.

A demonstration-prototype CO2-laser heterodyne spectrometer operating at 9-12 microns and suitable for long-term space missions is described and illustrated with extensive diagrams, drawings, photographs, and graphs of test performance data. The spectrometer has total volume 0.63 cu m, mass 30 kg, and power requirement 60-70 W, compatible with miniature-class Space Shuttle experiment payload specifications. It comprises three modules: (1) an optical front end with reflecting optics, a 2-GHz BW HgCdTe photomixer, and a 0-2-GHz 40-dB RF preamplifier; (2) a local oscillator with an RF-excited waveguide CO2 laser, a 75-percent-efficiency RF amplifier, a stepper-driven grating mode selector, and an etalon stabilized for over 30,000 h of use; and (3) an RF-filter-bank spectral-line receiver with a 25-MHz RF channel, 1.6-GHz IF spectral coverage, onboard instrument control, a serial link to the host computer, and highly integrated design.

An improved CO2 laser heterodyne spectrometer is examined. The present system uses reflective optics to eliminate refocusing at different wavelengths, and the local oscillator is a line-center-stabilized isotopic CO2 laser. A tunable diffraction grating makes possible easy and rapid selection of over 50 transitions per isotope of CO2. The IF (0 to 1.6 GHz) from the HgCdTe photomizer is analyzed by a 128-channel filter bank, consisting of 64 tunable 5-MHz filters and 64 fixed 25-MHz RF filters. These filters provide resolving powers of about 1,000,000 to 10,000,000 and velocity resolution of 50 to 250 m/sec; their output is synchronously detected, integrated, multiplexed and stored in a buffer memory for the desired integration period. Kitt Peak observations show the wide spectral coverage, wide mixer and electronics bandwidth, and high sensitivity of the system.

Investigation of relaxation phenomena using two-pulse and three-pulse electron spin-echo technique was carried out on hydrogen- and gadolinium-doped single-crystal calcium fluoride. Measurements were made on calcium-fluoride crystals singly doped with ${\mathrm{H}}^{0}$ and ${\mathrm{Gd}}^{3+}$ and doubly doped with both ${\mathrm{H}}^{0}$ as well as ${\mathrm{Gd}}^{3+}$. Echo decay functions and phase memory times were determined in the 1.2-2.2 \ifmmode^\circ\else\textdegree\fi{}K temperature range. The results are interpreted using existing theories of electron spin-echo decay. A discussion of the results and of deviations from theories is presented. Three-pulse spin-echo decay measurements are also used to determine the spinlattice relaxation time of spins in the $\frac{5}{2}\ensuremath{\leftrightarrow}\frac{3}{2}{\mathrm{Gd}}^{3+}$ cubic line in Ca${\mathrm{F}}_{2}$.

Heterodyne spectroscopy at infrared (IR) wavelengths is a technique well suited for measuring small velocities in the solar atmosphere. An IR heterodyne spectrometer for solar oscillation measurements has been located at the McMath Solar Telescope of the Kitt Peak National Solar Observatory. It is now being used for single point Doppler shift measurements of 11 micron OH absorption features formed in the upper photosphere, with sampling rates as high as 33 mHz. The instrument employs a stabilized CO2. laser permitting absolute velocity measurements with an uncertainty of < 10 ms−1.

Nonthermal emission which occurs in the cores of the 9.4- and 10.4-μm CO 2 bands on Mars has been recently identified as a natural atmospheric laser. The emission is believed to be excited by absorption of near-ir solar flux, followed by collisional transfer to the 00°1 state of CO 2 . A numerical model based on this mechanism is developed which includes the solar pumping contributed by ∼2 × 10 4 near-ir CO 2 lines. The non-Local Thermodynamic Equilibrium (NLTE) radiative transfer problem is solved to obtain the 00°1 vibrational state population. This model successfully reproduces the existing center-to-limb observations, although higher spatial resolution observations are needed for a definitive test. The model also predicts total fluxes which are close to the observed values. The strength of the emission is predicted to be closely related to the instantaneous near-ir solar heating rate. Calculation of the CO 2 level populations in this model supports the identification of this emission as a natural atmospheric laser. Both Mars and Venus are predicted to exhibit level inversions; at large zenith distances several percent of the emergent intensity will be due to stimulated emission. While the stimulated emission present in these lines is not large enough to be of importance to mesospheric radiative equilibrium, it has other interesting consequences. The construction of large-volume radiation-pumped lasers, which utilize CO 2 planetary mesospheres as a gain medium, is theoretically possible.

An ultra-high resolution diode laser heterodyne spectrometer for observational and laboratory use has been developed for operation between 7.5 and 8.5 microns. The local oscillator is a PbSe tuneable diode laser kept continuously at operating temperatures of 12-60 K using a closed-cycle cooler. The laser output frequency is controlled and stabilized using a high-precision diode current supply, constant temperature controller, and a shock isolator mounted between the refrigerator cold tip and the diode mount. Reflecting optics are used whenever possible to minimize losses from internal reflection and absorption, and to eliminate chromatic effects. The spectrometer is used with a 64-channel RF spectral line receiver for a resolving power of 1.5 X 10° and an IF coverage of 1600 MHz. Heterodyne observations of the sunspot spectrum near 1200 cm1 have revealed fully resolved absorption features in the v = 1-0 and v = 2-1 rotation-vibration bands of silicon monoxide. The instrument has also been used for continuum observations of the infrared object IRC+10-216 as well as for measurements of terrestrial N2O, 03 and CH4.© (1982) COPYRIGHT SPIE--The International Society for Optical Engineering. Downloading of the abstract is permitted for personal use only.

Heterodyne spectroscopy at infrared (IR) wavelengths is a technique well suited for measuring small velocities in the solar atmosphere. An IR heterodyne spectrometer for solar oscillation measurements has been located at the McMath Solar Telescope of the Kitt Peak National Solar Observatory. It is now being used for single point Doppler shift measurements of 11 micron OH absorption features formed in the upper photosphere, with sampling rates as high as 33 mHz. The instrument employs a stabilized CO2 laser permitting absolute velocity measurements with an uncertainty of < 10 ms-1.

The research was predisposed for a progressing increase in incidence of the temporomandibular joint dysfunction, low effectiveness of traditional treatment as well as the necessity of implementation of high-effective etiopathogenetic therapy methods. The necessity of systematizing diagnostics and treatment planning is evident, considering the cause-effect mechanisms of the disease initiation and complex individual approach, required for improving the effectiveness of prevention and pathogenetic therapy in early rehabilitation of the patients with the temporomandibular dysfunction, The visualization model will provide for planning certain treatment stages using a virtual system, synchronizing and combining them with the modern methods of the prosthetic construction fabrication, which will represent a new quality stage of stomatological treatment. The chosen theme is not only of multidisciplinary medical importance, but of the social one as well. The wide coverage of the theme in stomatological sources evidences about urgency of searching for the new diagnostic sources and treatment methods and proves actuality of the topic. The article presents urgent aspects of the temporomandibular dysfunction development pathogenetic mechanisms, depicts new methods of diagnostics and early clinical manifestations, reviewed by the Ukrainian and foreign scientists over the previous 10 years.

Published data on a select group of SiO maser sources have been analyzed for velocity variations as a function of phase. No apparent correlation was found to a level of about 2 km/s. This places constraints on the location of the maser molecules. Such a correlation should be present at some level. The implications for future high resolution infrared measurements are discussed.

Absorption features from the 8 micron SiO fundamental (upsilon = 1-0) and hot bands (upsilon = 2-1) have been observed in sunspots at sub-Doppler resolution using a ground-based tunable diode laser heterodyne spectrometer. The observed line widths suggest an upper limit of 0.5 km/s for the microturbulent velocity in sunspot umbrae. Since the silicon monoxide abundance is very sensitive to sunspot temperature, the measured equivalent widths permit an unambiguous determination of the temperature-pressure relation in the upper layers of the umbral atmosphere. In the region of SiO line formation (log P sub g = 3.0-4.5), the results support the sunspot model suggested by Stellmacher and Wiehr (1970).