Lines Of Na Research Articles

Integrated miRNA-mRNA analysis provides potential biomarkers for selective breeding in bay scallop (Argopecten irradians)

Growth traits were compared between selected Argopecten irradians (BA) and non-selected A. irradians (NA; as a control). The results indicated that 1) the BA line exhibited greater average body weight and adductor muscle wet weight increase compared with the NA line at the same age of 10 months. 2) Comparative and integrated microRNA (miRNA) and mRNA transcriptome analyses identified 3373 differentially expressed genes (DEGs), 33 differentially expressed miRNAs (DEMs), and 39 “DEM-DEG” pairs in the BA line compared with the control. DEGs, DEMs, and “DEM-DEG” pairs involved in insulin signaling, immune related pathways, and actin cytoskeleton regulation were identified as candidates correlated with growth improvement in the BA line. A total of 259 positively selected genes were also identified. Collectively, our observations in this study will enrich the molecular information for A. irradians and provide potential biomarkers for future selective breeding and new seed creation in scallops.

Comparison of cephalometric measurements between conventional and automatic cephalometric analysis using convolutional neural network

ObjectiveThe rapid development of artificial intelligence technologies for medical imaging has recently enabled automatic identification of anatomical landmarks on radiographs. The purpose of this study was to compare the results of an automatic cephalometric analysis using convolutional neural network with those obtained by a conventional cephalometric approach.Material and methodsCephalometric measurements of lateral cephalograms from 35 patients were obtained using an automatic program and a conventional program. Fifteen skeletal cephalometric measurements, nine dental cephalometric measurements, and two soft tissue cephalometric measurements obtained by the two methods were compared using paired t test and Bland-Altman plots.ResultsA comparison between the measurements from the automatic and conventional cephalometric analyses in terms of the paired t test confirmed that the saddle angle, linear measurements of maxillary incisor to NA line, and mandibular incisor to NB line showed statistically significant differences. All measurements were within the limits of agreement based on the Bland-Altman plots. The widths of limits of agreement were wider in dental measurements than those in the skeletal measurements.ConclusionsAutomatic cephalometric analyses based on convolutional neural network may offer clinically acceptable diagnostic performance. Careful consideration and additional manual adjustment are needed for dental measurements regarding tooth structures for higher accuracy and better performance.

Study of the departures from LTE in the unevolved stars infrared spectra

ABSTRACT We present a study of departures from Local Thermodynamic Equilibrium (LTE) in the formation of infrared (IR) lines of Na i, Mg i, Al i, S i, K i, and Sr ii in unevolved stars of spectral types F, G, K and metallicities around the solar metallicity. The purpose of this investigation is to identify lines of these species that can be safely treated with the LTE approximation in the IR spectra of these types of stars. We employ a set of 40 stars observed with the GIANO spectrograph at the 3.5 m Telescopio Nazionale Galileo and previously investigated by Caffau et al. We were able to identify many lines that can be treated in LTE for all the above-mentioned species, except for Sr ii. The latter species can only be studied using three lines in the J band, but all three of them display significant departures from LTE. With our small-size, but high-quality sample, we can determine robustly the trends of the abundance ratios with metallicity, confirming the trends apparent from a sample that is larger by several orders of magnitude, but of lower quality in terms of resolution and S/N ratio.

A Christmas gift: Signature of the 24th December 2018 eruption of Mt. Etna on the chemical composition of bulk deposition in eastern Sicily

The eruption of Mt. Etna which occurred on December 24th 2018 was characterized by strombolian activity and fire fountains, emitted by the New South-East Crater and along a fissure that propagated towards the SE. The influence of volcanic emissions on atmospheric deposition was clearly detectable at several kilometres from the source. Wet and dry (bulk) deposition samples were collected each month, through a network of eleven collectors, in the areas of Milazzo, and Priolo between June 2018 and June 2019. They were analysed for major ions and trace elements concentrations. The pH values range from 3.9 to 8.3, while the EC values range from 7 to 396 μS cm-1. An extensive neutralization of the acidity has been recognised mainly due to the suspended alkaline dust particles, which have a buffering role in rainwater. A high load of Na+ and Cl- was observed at all sites, related to the closeness of the study areas to the coast, showing a high positive correlation (R2 = 0.989) along the line of Na+/Cl- ratio in seawater. During the eruption, the volcanic plume was carried by the winds for long distance (more than 300 km) affecting the area of Priolo but not that of Milazzo, which was upwind with respect to Mt. Etna. The impact of volcanic HF was clearly recognised in the samples collected after the eruption. Volcanic SO2 and HCl had a lower impact due to the overwhelming input of anthropogenic sulfate and marine chloride. On the contrary, the signature of the Mt. Etna eruption can be well recognised in the high concentrations of certain trace elements in the samples collected immediately after the eruption. The strongest contrast between affected and non-affected samples was recognised in Al, Cd, and especially in the volatile elements Tl and Te, which are typically enriched in volcanic emissions. The results showed that volcanic eruptions might have a relevant effect on the atmospheric chemistry and on the composition of rainwater up to distances of 80 km from the emission vents.

Study for Cephalometrics of Facial Bone by Computerized Tomography Images.

Authors tried to investigate the maxillomandibular morphology of Korean nationality with computerized tomography images and establish a series of cephalometric values which should be considered in orthognathic plastic surgery in Korea.The computerized tomography images of 200 patients were retrospectively reviewed with the computer workstation in Sanggye Paik Hospital, Inje University College of Medicine from 2016 to 2017.The mean distance between nasion to point A (NA) line and the maxillary central incisor was 5.07 cm. The mean distance from nasion to point B (NB) line to the mandibular central incisor was 7.11 cm. The mean angle between NA line and the long axis of the maxillary central incisor was 20.58 degree. The mean angle between NB line and the long axis of the mandibular central incisor was 26.47 degree. The mean angle between SN (sella to nasion) line and NA line was 83.18 degree. The mean angle between SN line and NB line was 78.83 degree. The mean angle between NA line and NB line was 4.35 degree. There were no any statistically significant differences between age groups. But there were statistically significant difference in the mean of angle between NB line and the long axis of the mandibular central incisor (P = 0.025, between sex groups) and in the mean of angle between NA line and the long axis of the maxillary central incisor between sex groups in the 51 to 60 age group (P = 0.045).The maxillomandibular profile of Korean adults was established which can be applied for orthognathic surgery of Korean patients.

Landau theory for isotropic, nematic, smectic-A, and smectic-C phases

ABSTRACTWe use the Landau theory of phase transitions to describe the phase diagram of a liquid crystal displaying the isotropic (i), nematic (N), smectic-A and smectic-C phases. The order parameter of the smectic-C phase is defined as the projection of the director on the plane of the smectic layers, vanishing in the smectic-A phase. We present a detailed phase diagram that shows transition between any two of these phases, containing a triple point INA, a Lifshitz point NAC, a tricritical at the NA line, and a critical end point IAC. As one approaches the NC line from the smectic-C phase, the tilt angle approaches a nonzero value, but if the AC line is approached, the tilt angle vanishes according to the distance to the AC line to the power 1/2.

A Study of the Kepler K2 Variable EPIC 211957146 Exhibiting a Variable O’ Connell Effect

Abstract We present the multi-band photometric and spectroscopic study of an over-contact binary system, EPIC 211957146. The light curves exhibit a variable O’ Connell effect, confirmed from our observational data and the Kepler K2 data. The best photometric solution incorporating a dark spot over the primary component unveils that the system has a low-mass ratio (q ∼ 0.17) and a high inclination (i ∼ 85°). To confirm the solution and constrain the uncertainty, Monte-Carlo simulations are performed and the results are reported. Based on the O–C diagram analysis, we see that the variable shows a period increase at the rate of dP/dt ∼ 1.06 × 10−6 days yr−1, which is higher than the theoretically predicted value. Presence of a third body having a period of ∼16.23 years is evident from the O–C diagram. No filled-in effect is observed in the Hα line, while the effect is vividly present in the Na line. From the Kepler K2 data, we found that the primary and secondary minima exhibit an anti-correlated O–C variation followed by an erratic behavior. This is possibly caused by the longitudinal motion of the spot, and hence, we set a lower limit of ∼40 days for the spot modulation. We also observe a possibly associated photometric difference in the primary depth by comparing our light curves with Kepler K2 normalized light curves. This system has a low-mass ratio and a high fill-out factor, and, theoretically, such a physical configuration would lead to a merger.

The influence of ultrasound frequency on the shape of the D-line of Na in the sonoluminescence spectra of aqueous solutions of sodium chloride and sodium dodecylsulfate

The multibubble sonoluminescence spectra of aqueous solutions of sodium chloride and sodium dodecylsulfate saturated with argon were measured around the D-line of Na under irradiation with ultrasound with a frequency of 20 and 870 kHz. The Na line had a complex shape and incorporated two overlapping components: an asymmetrically broadened shifted band and a narrow unshifted doublet. The Na line in the spectra of the dodecylsulfate solution was notably narrower than the line in the NaCl solution spectra at both ultrasound frequencies. At the same time, the changes in the line shape observed upon the transition from one frequency to the other in these two solutions were similar. The line was narrower and had a prominent narrow component at a frequency of 870 kHz, and the line was broader with a dominant broad component at a frequency of 20 kHz. The results are discussed within the context of different dynamics of bubbles at high and low ultrasound frequencies.

Bimaxillary protrusion trait in the Indian population: A cephalometric study of the morphological features and treatment considerations

PurposeThe orthodontic literature is discordant with the diagnosis of bimaxillary protrusion with no single anatomic answer and the anomaly has been referred in the literature with protean characteristics. The trait denotes a particular facial configuration and its cephalometric representation in certain ethnic and racial groups revealed a mixed pattern with individual variations. The present study was aimed at analyzing the dento-skeletal characteristics of bimaxillary protrusion in a sample of Indian men and women. Materials and methodsForty-six Indian subjects (28 women and 18 men; 19±3.6 years of age) with Class I malocclusion and interincisal angle ≤110°, who attended orthodontic clinics for a comprehensive fixed orthodontic treatment were included for the study. The lateral films were hand traced and 27 parameters were measured. The data were imported to SPSS version 13 US package and statistical manipulation included means, standard deviation, and coefficient of variation (%). Male and female data were compared by Student's t-test (unpaired). Correlation and regression analysis were performed to assess any relationship between different parameters. ResultsThere was a marked increase in proclination of the maxillary incisors both to the maxillary plane (125.3±5.7°), the NA line (35.1±5.0°) and to sella–nasion (117.7±5.5°). The positional relationship of the mandible to the maxilla with reference to the cranial base was within the normal limits (ANB=3.1±1.3°) and the skeletal pattern was Class I. The effective lengths of maxilla and mandible did not correlate significantly with sagittal skeletal discrepancy. ConclusionUnlike in other ethnic and racial groups, bimaxillary protrusion in Indian subjects is likely a bidental protrusion over normal dento-alveolar bases. The skeletal characteristics suggested a normal relationship of the functional components of the face. The condition could be treated successfully with orthodontic mechanotherapy alone.

LASER-INDUCED BREAKDOWN SPECTROSCOPY FOR THE STUDY OF THE PATTERN OF SILICON DEPOSITION IN LEAVES OF SACCHARUM SPECIES

The spatial distribution pattern of silicon in the leaves of three species of Saccharum has been demonstrated by means of laser induced breakdown spectroscopy (LIBS). The in-situ point detection capability of LIBS was used to determine different elements in leaf samples. The concentrations of silicon and other elements in different parts of the leaves were estimated by measuring the intensities of their corresponding atomic lines. Silicon, deposited in the form of phytoliths, was also isolated by using the dry ash technique. LIBS observations showed that in all three Saccharum species, the concentration of silicon was highest in the midrib followed by that found in margin and vein areas. The concentration of silicon in S. officinarum is higher in comparison to S. spontaneum and S. bengalense. Furthermore, the concentration of silicon at the upper surface of the leaf was larger than at the lower surface. The LIBS spectra of Saccharum species also show the presence of spectral lines of Na, Mg, Ca, Fe, and K.

Spectroscopic and thermodynamic features of conical bubble luminescence

The influence on luminescence from conical bubble collapse (CBL) with varying Ar gas content while perturbing the liquid 1,2-Propanediol (PD) has been investigated. The temporal, spatial, and spectral features were analysed with regards to the dynamics of collapse and liquid degradation. Sulphuric acid and sodium chloride were added to disturb the liquid. The following three cases were studied: PD/Ar, ( I), (PD + H 2SO 4)/Ar, ( II), and (PD + H 2SO 4 + NaCl)/Ar, ( III). The intensities of those cases decrease as III > II > I. Temporally, single and multiple light emissions were found to occur. The pulse shape exhibited a large variety of profiles with a main maximum and up to two local maxima around the main maximum. These local maxima resembled those generated by laser cavitation. Spatially, no radial symmetry was detected in the light emissions. Spectrally, the Swan, CH and CN lines were observed at low volumes of gas and driving pressure. The OH radical and OH–Ar bands, as well as the Na and K lines, consistently appeared superimposed on an underlying continuum that almost disappeared in ( III). The Na line was observed with two satellite diffuse bands representing Na–Ar complexes in ( I) and ( II), whereas in ( III), only the line of sodium could be seen. Weak and diffuse emission lines from the Ar atom in the near-IR region were observed in ( I) and ( II). The proposed mechanism of bright CBL was based on the energy transfer from electron-excited homolytic cleavage products to the chromophore molecules generated during the collapse-rebound time line (∼8200 K and ∼1 ms of collapse time from model), which had accumulated inside the liquid and remained on the walls of cavity during the repetition of the collapse. A general mechanism for the bright CBL is broached.

THE CARBON MIRA UV AURIGAE AND ITS COMPANION

The carbon Mira UV Aur (photometric period 394 days) and its companion present several interesting spectroscopic issues. The late B-type companion, at a separation of 336, is seen through at least two shells expanding from the C9-type primary, as evidenced by a series of narrow, displaced absorption features at the D1,2 lines of Na I. The (projected) expansion velocity of the fastest shell is about 116 km s–1, much larger than the typical outflow velocity of about 15 km s–1 seen in C-type giants, but reminiscent of the velocities observed in the envelope of another C-type Mira, V Hya. Emission lines of H, Ca II, and Na I are present in UV Aur A; its Balmer emission lines are heavily mutilated by overlying C-type absorptions (much as is seen in Me-type Miras), so they must be formed at a lower level. UV Aur B offers the opportunity to test a speculation that the carriers of the diffuse interstellar bands (DIBs), believed to be a family of carbon-containing polyatomic molecules, may be formed in cool, carbon-rich stars. Moderately strong DIBs are indeed present in the spectrum of UV Aur B at about the same strength and velocity seen in nearby (in the sky) B-type stars. But the essential question is, are DIBs present in the outflow from UV Aur A, at the velocities of the Na I shell components? The answer is no, at least at the level permitted by the signal-to-noise ratio of these Keck/HIRES spectrograms.

Modeling of the R CrB star chromosphere

A model of the R CrB star chromosphere is calculated on the basis of the observed profiles of the Ca II H and K lines and IR triplet and D lines of Na I and H-alpha. The calculated profiles of Ca II H and K lines and IR triplet and H-alpha are in good agreement with the observed ones both for an undisturbed state and for the light minimum. The line profiles for the light minimum are calculated under the assumption that the minimum is attributed to obscuring of the star disc with a dust cloud. In this case, the chromosphere is not hydrostatic since the column density at the chromosphere base is two orders of magnitude higher as compared to that in a hydrostatic model. The model proposed is more extended, less dense at the chromosphere base, and denser in the upper chromosphere. The extension of the calculated chromosphere is about 3 star radii. The density in the chromosphere is 108–1010 atoms per 1 cm3 and the temperature is 5000–7000 K. Agreement of the calculated and observed profiles of Na I D absorption lines is possible if we assume that, around the star, there is a cold envelope containing Na I atoms which expands with a velocity of about 30 km/s. This envelope is beyond the chromosphere, but near enough for the star and the envelope to be observed as a single whole. The optical thickness of the envelope in the Na I D2 line is 1.8. At the brightness minimum, this envelope illuminated with the star light yields additional emission attributed to resonant scattering in the Na I D lines.

Characterization of Poly (Methyl Acrylate) Grafted Bleached Sulfite Pulp Fibers using AFM, AEM, EDS and STEM

Sulfite pulp fibers were grafted by poly (methyl acrylate) at a low‐consistency (1% pulp consistency) and medium‐consistency (10% pulp consistency). It is of fundamental interest to determine the distribution of the polymer chains obtained at different fiber concentrations during grafting. In this study, modern analytical tools such as atomic force microscope (AFM), energy dispersive spectrometer (EDS), and scanning transmission electron microscope (STEM) were used for investigating the distribution of the polymer chains in the fiber matrix. AFM images in tapping mode showed that the fiber surface was covered with in‐situ generated polymers. The X‐ray mapping of Na in the cross‐section of the hydrolyzed grafted fibers by using EDS in combination with Na line scans by STEM showed that the distribution of poly (methyl acrylate) was affected by the pulp consistency during grafting; at a medium‐consistency condition the outer region of the fiber structure had a higher polymer concentration than the inner region. On the other hand, at a low‐consistency condition, grafting occurred uniformly across the fiber wall structure.

The optical properties of conical bubble sonoluminescence in glycol

Using an improved conical bubble U tube, the optical properties of conical bubble sonoluminescence in glycol are measured. A strong single flash is observed and the width of light pulse reaches 150 us, which is much higher than that of the results obtained by other methods. The spectrum is a continuum ranging from ultraviolet to visible region, superposed with the spectral line of the 3P-3S transition of sodium around 589 nm. The blue satellite bands of Na-Ar has been measured on the sides of atomic spectral line; the red satellite band of Na-Ar and the 3S-4S atomic spectral line of Na are firstly measured in sonoluminescence.

The Third-Order Angle and the Maxillary Incisor's Inclination to the NA Line

To evaluate the relationship between the angular measurement data (incisor's long axis to NA line) and the third-order angle (TA) according to Andrews' description. The materials in the study included the lateral radiographs and corresponding dental casts of 32 males and 35 females between 10 and 25 years of age, regardless of their skeletal and dental relationships. All subjects were white and none had undergone orthodontic therapy. Using lateral radiographs, upper and lower incisor angulations were assessed in reference to the NA line. These data were compared with third-order angles derived from direct dental cast measurements, which were performed using an incisor inclination recording appliance. The third-order angle measurements recorded from the dental casts were a mean of 16.2 degrees (SD = 5.3 degrees) smaller than the axial inclination according to the NA line. In this sample, there was a range of 42.7 degrees for the TA variable (mean = 5.6 degrees, SD = 9.73 degrees) and 47 degrees for the 1NA/deg variable (mean = 21.7 degrees, SD = 8.67 degrees). A highly significant correlation existed (r = 0.84) between Andrews' angle and the inclination estimated in reference to the NA line. Incisor inclination can be better estimated by recognizing the relationship between the torque angle and the axial inclination referred to the NA line. Third-order measurements using dental casts can offer a simple way to get an objective and rapid vision of the incisor's inclination.

Spectral shift of sodium in a liquid-helium environment: A sequential Monte Carlo time-dependent density-functional-theory study

The excitation lineshift and linewidth of the principal resonance line of Na embedded in liquid He have been obtained using combined Monte Carlo (MC) simulation and quantum mechanics (QM) calculations. The metropolis MC simulation used interatomic potentials obtained from high-level quantum mechanics results. Using the structures of the simulation statistically relevant configurations are sampled for subsequent QM calculations. The transition wavelengths for the $3s\ensuremath{\rightarrow}3p$ principal resonance line of atomic Na were obtained using time-dependent density-functional-theory calculations of the central alkali-metal atom surrounded by the first solvation shell composed of 42 He atoms. The widths are obtained by the statistical distribution of calculated transitions. Three different functionals were used. Statistically converged results using the $\mathrm{PBE}1\mathrm{PBE}∕6\text{\ensuremath{-}}311++\mathrm{G}(\mathrm{d},\mathrm{p})$ give a blueshift of 14.7 nm and a width at half maximum of 7.8 nm. Similar results are obtained using the Beeke-Lee-Yang-Parr three parameter exchange functional and the Becke three-parameter exchange with the Perdew nonlocal correlation functional models. These results seem to give a reasonable statistical representation of the structure of the He cavity enclosing the host Na atom and the consequent solvent effect on the $3s\ensuremath{\rightarrow}3p$ excitation.

Multi-Instrument Observations of Bright Meteors in the Czech Republic

We present detailed data on 8 bright meteors recorded simultaneously by different observational techniques. All meteors were recorded by all-sky cameras at the Czech stations of the European Fireball Network and by image intensified TV cameras placed at Ondrejov and Kunzak observatories. As well as direct photographic and LLLTV recordings, most of meteors were recorded also by the spectral TV camera and some also by photographic spectral cameras. For 6 cases, lightcurves from radiometers with very high time resolution (1200 s−1) are also available. From all these detections we found a significant difference between TV and photographic beginning heights. TV beginnings are in average about 40 km higher than the photographic ones. We found that meteor brightness is up to 2 magnitudes higher in the photographic system than in the TV system. This difference for high velocity meteors is mainly caused by the presence of strong Ca+ lines in the blue part of the spectrum, where the image intensifier is only marginally sensitive. At heights above 110 km, the Na line is usually brighter than the Mg line, while at lower heights both lines have comparable brightness. In one of two captured spectra of short duration luminous trains, a small initial brightening of the Mg and Na lines caused by recombination processes was observed.

Characterization of time resolved, buried layer plasmas produced by ultrashort laser pulses

We report on the characterization of plasmas produced by ultrashort laser irradiation of 500 A ̊ thick layers of NaF buried at varying depths in plastic to reduce plasma gradients. The targets are irradiated with 130 fs, ≈170 mJ laser pulses (λ=400 nm) at an intensity of ≈2×10 18 W cm −2 . The data are spectrally and temporally resolved, with resolutions of λ/Δ λ≈1000 and ≳500 fs , respectively. We use X-ray emission spectroscopy to assess the electron density, N e, and temperature, T e, in the plasma. The density is measured from Stark broadened line profiles of the He-like 1 1S– 3 1 P, He β , and H-like Ly β lines of Na, while the temperature is determined from the intensity ratio of Na He β to Ly β , and also from the dielectronic satellites to these lines. We find peak densities and temperatures of ≳10 23 cm −3 and ≈400 eV , respectively, at 2– 4 ps after the laser pulse. The plasma conditions plateau near these values for 5 ps after that. Atomic data for the kinetics simulations are generated with the HULLAC suite of codes. The Stark broadened line profiles, with full accounting of satellite transitions, are computed with the TOTAL code. Self-absorption effects are included along the observation line of sight using the radiation transport code CRETIN. Steady-state, non-LTE equilibrium plasma conditions are demonstrated suggesting that buried-layer experiments can be used as a test bed to study equation of state and opacity properties in hot, near-solid density matter.

Orionis: further temporal variability and evidence for small-scale structure in the interstellar medium

We report here the detection of both spatial and temporal variations in interstellar absorption in the line of sight to δ Orionis. First, we present new high-resolution (R≈110 000) observations of the interstellar D lines of Na I towards both δ Ori A and C. Comparison of these spectra highlights variations in absorption between the two stars, indicative of small-scale spatial structure in the interstellar medium in this direction over distances of less than ≈15 000 au (the projected separation of the two stars). Components with the largest Na I column densities and lowest velocity dispersions are, in general, found to be subject to the greatest differences; in fact the narrowest component detected is only observed in one of the sightlines. This effect has also been reported by Meyer & Blades. Secondly, we present new ultra-high-resolution (R≈900 000) Na I D1 observations and high-resolution (R≈110 000) Ca II H & K observations of δ Ori A which, through ultra-high-resolution work conducted between 1994 and 2000, has been shown to exhibit a time-variable interstellar Na I absorption component. These new observations, while revealing the further reduction in intensity of the time-variable Na I absorption, indicate constant Ca II absorption over the same period. This results in a dramatic reduction in the Na°/Ca+ abundance ratio, perhaps indicating the line of sight to be gradually probing a less-dense outer region of an absorbing filament.