bluuebunny/crossref_metadata_2025 huggingface dataset:
NH$_{3}$ Survey Observation of Massive Star-Forming Region W 43
Authors: Nishitani Hiroyuki , Sorai Kazuo , Habe Asao , Hosaka Keita , Watanabe Yoshimasa , Ohishi Yukie , Motogi Kazuhito , Minamidani Tetsuhiro , Fujimoto Masayuki Y.
Published: March 2014

We consider the properties of giant molecular cloud complexes in the star-forming region W 43 with a resolution of several pc scale, and discuss their relations to the evolutionary stages of massive star formation. We performed a NH$_{3}$ ($J$, $K$) $=$ (1, 1), (2, 2), and (3, 3) inversion-line survey with the Hokkaido University 11-m telescope. Among 51 observed positions, selected based on integrated intensity maps of $^{13}$CO ($J$$=$ 1–0), these three emissions were detected from 21, 8, and 5 positions, respectively. The integrated intensity of the NH$_{3}$ ($J$, $K$) $=$ (1, 1) line was found to be proportional to the far-infrared luminosity, estimated from IRAS data. The rotation temperatures were deduced to be $\sim\ $15–20 K at eight observed positions. In addition, the upper limits were estimated for 13 positions, which include the relatively low temperatures below 14 K at two positions with a relatively high fractions of NH$_{3}$ for $^{13}$CO and with a low far-infrared luminosity. We derived the ortho-to-para abundance ratio of NH$_{3}$. From the population distribution between the ortho- and para-levels of NH$_{3}$, we also derived temperatures of $\sim\ $6–12 K, which may be interpreted as the temperatures when NH$_{3}$ molecules were formed. We discuss the relevance of the present results of our observations to the massive star-formation process and the current status of the W 43 region while taking into account previous observations of other indicators of massive star formation. It is shown that the complexes contain several regions in different evolutionary stages, or with the distinct characteristics of star formation within a timescales shorter than the lifetime of massive stars.
On the Error Reduction of a Simple Symplectic Integrator
Authors: Ito Takashi , Tanikawa Kiyotaka
Published: March 2014

An analysis of truncation errors of the simplest symplectic integrator is revisited. We performed an analytical error estimate of this integrator within the framework of a canonical perturbation method, taking the two-body system as an example. Our study was motivated by the desire to remove any confusion in the derivation of this issue in one standard literature along this line of research. We repeated the derivation, and examined how a secular numerical error arises in symplectic integration. We showed that it is possible to substantially eliminate a secular numerical error by choosing appropriate initial conditions, as previous studies have shown. On the other hand, depending on boundary parameter values, such as the eccentricity in the two-body system, we could see that it is sometimes impossible to reduce the secular numerical error by changing the starting conditions. We also numerically demonstrated this reduction, or lack of reduction of numerical errors by taking a restricted three-body system as an example. We confirmed that the so-called “iterative start” of symplectic integrators works in certain systems.
Tidal-Force-Induced Precessions of Accretion Disks
Authors: Inoue Hajime
Published: March 2014

The preccession of an accretion disk around a compact star in a close binary has been studied. When the accretion disk tilts, the tidal force from the companion star induces a torque on it, which causes a preccession of the disk. We firstly consider the properties of a preccessing motion of a ring, which is circularly rotating around a compact star, and is preccessing with a slightly tilting angle under the influence of a tidal force from a companion star. We next compare the predicted behaviors of the preccessing ring with observations, and find that several observational facts from Her X-1, SS 433, and some other X-ray binaries can be explained by a tidal-force-induced precession scheme quite reasonably. We further examine the energetics of the preccessing ring as a function of the tilting angle. It is shown that the kinetic and potential energies of the orbiting motions of the ring matter around the compact star increases as the tilting angle increases, while the thermal and effective potential energies for hydro-static balance in the meridian cross section of the ring decreases through adiabatic expansion. Quantitative estimations have shown that when the ring has sufficient thermal energy, the decrease of the energy for the hydro-static balance can be larger than the increase of the energy for circular motion around the compact star until the tilting angle reaches a certain value. It is strongly suggested that preccessions of accretion disks are often realized in close binaries.
Standing Kink Waves with Longitudinal Flow in Fine Threaded Coronal Loops: A New Method for the Coronal Seismology through Beat and Damped Waves
Authors: Pandey Vinay Shankar , Magara Tetsuya , Lee Dong-Hun
Published: March 2014

Stimulated by the first weakly attenuated standing kink oscillations of coronal fine threads filled with cool flowing plasma, seen in a recent Ca II H-line observed by Solar Optical Telescope (SOT) aboard Hinode, in this study we present the effects of longitudinal flow on the standing wave. We have found that flow generates two important consequences: first, it produces a frequency shift, which leads to the phenomenon of wave beating; second, it splits the damping time of the forward and backward waves of the attenuated standing wave (considered here only the resonance absorption) into two different values. A comparative analysis of the beat waves, within the “quarter-beat period approximation” together with attenuated waves, seems to be very appealing for coronal seisomology. We refer a new parameter, modulating time ($\tau_{\rm m}$), which is defined as the time when the amplitude of the beat wave becomes zero for a wave train that lies within a quarter period of the beat envelope, the so-called “quarter beat period approximation”. We can compare this $\tau_{\rm m}$ with the attenuating time ($\tau_{\rm D}$) to discriminate the behaviour of the signal, as follows: if $\tau_{\rm m}~\gt~\tau_{\rm D}$, the envelope of the signal is dominated by attenuation due to resonance absorption, while if $\tau_{\rm m}~\lt~\tau_{\rm D}$, the envelope of the signal is dominated by modulation due to beating. Since observation corresponds to first inequality, the amplitude of the signal seems to be dominated by attenuation due to resonance absorption. Hence, the inequality $\tau_{\rm m}~\geq~\tau_{\rm D}$ imposes an upper bounds for the density contrast and magnetic field for a given value of the observed flow. Besides these, we also find that the flow-generated splitting of the damping time also leads to an $\sim\ $8%–10% uncertainty in our estimation of the radial inhomogeneity across the loop boundary, as compared to the static case, i.e., when the flow is zero.
An Attempt to Describe Frequency Correlations among kHz QPOs and HBOs by Two-Armed Nearly Vertical Oscillations
Authors: Kato Shoji
Published: March 2014

We examine whether the two-armed ($m$$=$ 2) vertical p-mode oscillations trapped in the innermost region of magnetized accretion disks with finite disk thickness can describe kHz quasi-periodic oscillations (QPOs) and horizontal branch oscillations (HBOs) in low-mass X-ray binaries (LMXBs). First, we derive the frequency–frequency correlation of the two basic oscillations (both are fundamental modes in the vertical direction, but one is the fundamental and the other the first overtone in the radial direction), and compare it with the observed frequency correlation of twin kHz QPOs. Results show that the calculated frequency correlation can well describe the observed frequency one with reasonable values of the parameters. Second, we examine whether the observed frequency correlation between kHz QPOs and HBO can be described by regarding HBO as the first overtone oscillation in the vertical direction (and the fundamental in the radial direction). The results suggest that (i) the innermost parts of disks on the horizontal branch are strongly diminished in their vertical thickness (presumably by hot coronae) and (ii) the branch is roughly a sequence of variations of magnetic fields or disk temperature.
Application of the Titius–Bode Rule to the 55 Cancri System: Tentative Prediction of a Possibly Habitable Planet
Authors: Cuntz Manfred
Published: March 2014

Following the notion that the Titius–Bode rule (TBR) may also be applicable to some extrasolar planetary systems, although this number could be relatively small, it is applied to 55 Cancri, which is a G-type main-sequence star currently known to host five planets. Following a concise computational process, we tentatively identified four new hypothetical planetary positions, given as 0.081, 0.41, 1.51, and 2.95 AU from the star. The likelihood that these positions are occupied by real existing planets is significantly enhanced for the positions of 1.51 and 2.95 AU in view of previous simulations on planet formation and planetary orbital stability. For example, Raymond, Barnes, and Gorelick (2008, ApJ, 689, 478) argued that additional planets would be possible between 55 Cnc f and 55 Cnc d, which would include planets situated at 1.51 and 2.95 AU. If two additional planets are assumed to exist between 55 Cnc f and 55 Cnc d, the deduced domains of stability would be given as 1.3–1.6 and 2.2–3.3 AU. The possible planet near 1.5 AU appears to be located at the outskirts of the stellar habitable zone, which is, however, notably affected by the stellar parameters as well as the adopted model of circumstellar habitability. We also computed the distance of the next possible outer planet in the 55 Cnc system, which, if existing, is predicted to be located between 10.9 and 12.2 AU, which is consistent with orbital stability constraints. The inherent statistical significance of the TBR was evaluated following a method by Lynch (2003, MNRAS, 341, 1174). Yet it is up to future planetary search missions to verify or falsify the applicability of the TBR to the 55 Cnc system, and to obtain information on additional planets, if existing.
Alpha-Viscosity Effects in Slender Tori
Authors: HorÁK Jin , Abramowicz Marek A. , Levin Lina , Slapak Rikard , Straub Odele
Published: March 2014

We explore effects of the Shakura–Sunyaev $ \alpha$-viscosity on the dynamics and oscillations of slender tori. We start with a slow secular evolution of the torus. We show that the angular-momentum profile approaches the Keplerian one on a timescale longer than a dynamical one by a factor on the order of 1$ /\alpha$ . We then focus our attention on the oscillations of the torus. We discuss the effects of various angular-momentum distributions. Using a perturbation theory, we have found a rather general result that the high-order acoustic modes are damped by the viscosity, while the high-order inertial modes are enhanced. We calculate viscous growth rates for the lowest-order modes, and show that already the lowest-order inertial mode is unstable for less-steep angular-momentum profiles, or very close to the central gravitating object.
Estimates of Emission-Region Locations of Fermi Flat-Spectrum Radio Quasars
Authors: Yan Dahai , Zeng Houdun , Zhang Li
Published: March 2014

We have studied the location of emission regions through modeling the quasi-simultaneous multifrequency spectral energy distributions of 21 Fermi flat-spectrum radio quasars (FSRQs) in the frame of a multicomponent one-zone leptonic model. In our calculations, we took the detailed broad line region (BLR) structure into account, and discussed the effect of the uncertainty of the BLR structure on constraining the location of the emission regions for each FSRQ; besides, we also included both the internal and the external absorptions. Our results indicate that: (1) the contribution of the external Compton-BLR component to the $ \gamma$-ray emission is important, and the energy density of external target-photon fields depends on the location of the emission region, which can be derived by reproducing the observed $ \gamma$-ray emission; (2) the emission regions of FSRQs with relatively low accretion-disk luminosity lie in the region of (7.9 $ \times$ 10$ ^{16}$ –1.3 $ \times$ 10$ ^{18})$ cm (300–4300 Schwarzschild radii) from central black hole, and for FSRQs with high accretion-disk luminosity, the emission regions are located in a larger region of (2.6 $ \times$ 10$ ^{17}$ –4.2 $ \times$ 10$ ^{18}$ ) cm (300–5600 Schwarzschild radii).
V524 Monocerotis: A Marginal Contact Binary with a Cyclic Period Variation
Authors: Jia-Jia He , Jing-Jing Wang , Sheng-Bang Qian
Published: March 2014

We have secured and analyzed three-color light curves of V524 Monocerotis with the 2003 version of the Wilson–Devinney code. We confirmed that V524 Mon is a shallow W-type contact binary system with a mass ratio of $q$$=$ 2.099 and a degree of contact factor of $f$$=$ 7.7%. Based on the new eight times of the light minima and those published by previous investigators, we find that the orbital period of the binary shows a long-term decrease ($dp/dt$$=$$-$1.52 $\times$ 10$^{-10}$), while it undergoes a cyclic oscillation ($T_{3}$$=$ 23.93 yr, $A_{3}$$=$ 0.0082 d). The long-term period decrease can be explained by mass transfer from the primary to the secondary. The cyclic change, explained as the light-travel time effect, reveals the presence of a tertiary companion. The marginal contact configuration and the continuous period decrease both suggest that the system may be a newly formed contact binary.
Variation of Meteor Heights and Solar-Cycle Activity
Authors: Porubcan Vladimír , Bucek Marek , Cevolani Giordano , Zigo Pavel
Published: March 2014

Photographic meteor observations of the Perseid meteoroid stream compiled from the IAU Meteor Data Center catalogue are analyzed from the viewpoint of possible long-term variation of meteor heights with the solar-cycle activity, which was previously reported from radio observations. The observed beginning and end-point heights of the Perseids, normalized for the geocentric velocity and the absolute photographic magnitude, do not show a variation consistent with the solar-cycle activity. This result is valid for the mass range of larger meteoroids observed by photographic techniques, and must be still verified also for the range of smaller meteoroids observed by TV and radio methods.
Discovery of Negative Superhumps during a Superoutburst of 2011 January in ER Ursae Majoris
Authors: Ohshima Tomohito , Kato Taichi , Pavlenko Elena P. , Itoh Hiroshi , de Miguel Enrique , Krajci Thomas , Akazawa Hidehiko , Shiokawa Kazuhiko , Stein William , Baklanov Alex , Samsonov Denis , Antonyuk Oksana , Andreev Maksim V. , Imamura Kazuyoshi , Hambsch Franz-Josef , Maehara Hiroyuki , Ruiz Javier , Nakagawa Shin'ichi , Kasai Kiyoshi , Boitnott Boyd , Virtanen Jani , Miller Ian
Published: March 2014

We report on a discovery of “negative” superhumps during the 2011 January superoutburst of ER UMa. During the superoutburst, which started on 2011 January 16, we detected negative superhumps having a period of 0.062242(9) d, shorter than its orbital period by 2.2%. No evidence of a positive superhump was detected during this observation. This finding indicates that the disk exhibited retrograde precession during this superoutburst, contrary to all other known cases of superoutbursts. The duration of this superoutburst was shorter than those of ordinary superoutbursts, and the interval of its normal outbursts was longer than those of ordinary normal outbursts of ER UMa. We suggest the possibility that such unusual outburst properties are likely to be a result of a disk tilt, which is supposed to be a cause of negative superhumps; the tilted disk could prevent the disk from being filled with materials in the outmost region, which is supposed to be responsible for long-duration superoutbursts in ER UMa-type dwarf novae. This discovery signifies the importance of the classical prograde precession in sustaining long-duration superoutbursts. Furthermore, the presence of pronounced negative superhumps in this system with a high mass-transfer rate supports the hypothesis that hydrodynamical lift is the cause of the disk tilt.
Re-Calibration of SDF/SXDS Photometric Catalogs of Suprime-Cam with SDSS Data Release 8
Authors: Yagi Masafumi , Suzuki Nao , Yamanoi Hitomi , Furusawa Hisanori , Nakata Fumiaki , Komiyama Yutaka
Published: March 2014

We present photometric recalibrations of the Subaru Deep Field (SDF) and Subaru/XMM-Newton Deep Survey (SXDS). Recently, Yamanoi et al. (2012, AJ, 144, 40) suggested the existence of a discrepancy between the SDF and SXDS catalogs. We have used the Sloan Digital Sky Survey (SDSS) Data Release 8 (DR8) catalog and compared stars in common between SDF/SXDS and SDSS. We confirmed that there exists a 0.12 mag offset in the $ B$-band between the SDF and SXDS catalogs. Moreover, we found that significant zero-point offsets in the $ i$-band ($ \sim$ 0.10 mag) and the $ z$-band ($ \sim$ 0.14 mag) need to be introduced to the SDF/SXDS catalogs to make it consistent with the SDSS catalog. We report the measured zero point offsets of five filter bands of SDF/SXDS catalogs. We studied the potential cause of these offsets, but the origins are yet to be understood.
Discovery of Metastable Helium Absorption Lines in V1280 Scorpii
Authors: Naito Hiroyuki , Tajitsu Akito , Arai Akira , Sadakane Kozo
Published: March 2014

We report on the discovery of blue-shifted metastable He I* absorption lines at 3188 Å and 3889 Å with multiple components on high-resolution spectra ($ R$$ \sim$ 60000) of V1280 Scorpii. Similar multiple absorption lines associated with the Na I D doublet as well as Ca II H and K were observed. Na I D doublet absorption lines have been observed since 2009, while the metastable He I* absorption lines were absent in 2009, but were detected in 2011 (four years after the burst). We have found different time variations in the depths and velocities of blue-shifted absorption components among He I*, Na I, and Ca II. The complex time evolutions of these lines can be explained by assuming changes in the density and recombination/ionization rate when the ejecta expands and the photosphere contracts to become hotter. The multiple absorption lines originate in ejected materials consisting of clumpy components, which obscure a significant part of the continuum emitting region. We estimate the total mass of the ejected material to be on the order of $ \sim$ 10$ ^{-4}$$ M_{\odot}$ , using metastable He I*$ \lambda\lambda$ 3188 and 3889 absorption lines.
Disk Origin Narrow Metallic Absortion Lines Observed during the 2009–2011 Eclipse of ∊ Aurigae
Authors: Sadakane Kozo , Kambe Eiji , Hashimoto Osamu , Honda Satoshi , Sato Bun'ei
Published: March 2014

Frequent high-resolution spectroscopic observations of $\epsilon$ Aur during the 2009–2011 eclipse revealed temporal appearances of low-excitation absorption lines of neutral iron peak elements. Several 0 eV lines of Fe I were detected near the end of the first half of the eclipse. They had migrated toward shorter wavelength, became much strong after the third contact, and then disappeared after the fouth contact. Curiously, the widths of these temporal absorption lines became broader for about a 100-d period just before the third contact. The radial velocity measured for these lines follows that of the K I line at 7699 Å, implying that these lines originated in a rotating disk around the secondary star, which occulted the primary star. Weak and sharp absorption lines of low excitation neutral metals, such as Sc I, Ti I, V I, Cr I, and Mn I, were observed only for a short period from the third contact to the fourth contact, and they were all blue-shifted by $\sim$ 40 km s$^{-1}$. These observations show that the rotating disk around the secondary star is not axially symmetric, but suggest that a clump of cool gas concentrated in a region observed projected on the primary star near at the end of the eclipse.
Lithium, Carbon, and Oxygen Abundances of Hyades F–G Type Stars
Authors: Takeda Yoichi , Honda Satoshi , Ohnishi Takashi , Ohkubo Michiko , Hirata Ryuko , Sadakane Kozo
Published: March 2014

In an attempt to carry out a systematic study on the behavior of the photospheric abundances of Li, C, and O (along with Fe) for Hyades main-sequence stars in the $ T_{\rm eff}$ range of $ \sim$ 5000–7000 K, we conducted an extensive spectrum-synthesis analysis applied to four spectral regions (comprising lines of Fe-group elements, Li I 6708 line, C I 7111–7119 lines, and O I 6156–8 lines), based on the high-dispersion spectra of 68 selected F–G type stars belonging to this cluster. The abundances of C and O turned out to be fairly uniform in a marginally supersolar level, such as like the case of Fe: $ \langle$ [C$ /$ H]$ \rangle$$ =$$ +$ 0.15 ($ \sigma$$ =$ 0.08), $ \langle$ [O$ /$ H]$ \rangle$$ =$$ +$ 0.22 ($ \sigma$$ =$ 0.14), and $ \langle$ [Fe$ /$ H]$ \rangle$$ =$$ +$ 0.11 ($ \sigma$$ =$ 0.08), suggesting that the primordial abundances are almost retained for these elements. Strictly, however, they show a slightly increasing trend with a decrease in $ T_{\rm eff}$ (typically on the order of $ \sim$ 10$ ^{-4}$ dex K$ ^{-1}$ ); while this might be due to an improper choice of atmospheric parameters, we found it difficult to give a quantitatively reasonable explanation. Regarding Li, we confirmed the well-known $ T_{\rm eff}$-dependent trend in the Li abundance reported so far (a conspicuous Li-trough at 6300 K $ ≲$$ T_{\rm eff}$$ ≲$ 6700 K and a progressive decrease toward a lower $ T_{\rm eff}$ at $ T_{\rm eff}$$ ≲$ 6000 K), which means that the surface Li of Hyades stars is essentially controlled only by $ T_{\rm eff}$ ; other parameters, such as the rotational velocity, are almost irrelevant.
Suzaku Observation of Strong Solar-Wind Charge-Exchange Emission from the Terrestrial Exosphere during a Geomagnetic Storm
Authors: Ishikawa Kumi , Ezoe Yuichiro , Miyoshi Yoshizumi , Terada Naoki , Mitsuda Kazuhisa , Ohashi Takaya
Published: March 2014

We present an analysis of X-ray data exhibiting strong solar-wind charge-exchange emission obtained with the Suzaku satellite during a geomagnetic storm that occurred on 2005 August 31. A temporal variation of diffuse soft X-ray emission, correlating with the solar-wind proton flux, was found. The diffuse emission consisted of exospheric solar-wind charge exchange (geocoronal SWCX). We extracted the variable component of the spectrum, which is dominated by a sum of C V, C VI, N VI, N VII, O VII, and O VIII emission lines, predicted by the theoretical SWCX model. An analysis of any time correlation between the solar wind and the O VII line flux was conducted using the solar-wind data taken with the ACE and WIND satellites. We found that the observed SWCX intensity was 4–10 times higher than that calculated using a model of exospheric hydrogen density, and the O$ ^{7+}$ flux observed with ACE at the L1 point. This suggests that the exospheric hydrogen density can be higher than that predicted by the hydrogen model, and/or that additional O$ ^{7+}$ ions to the measured ACE fluxes could exist in the magnetosphere. Comparing this observation to past incidences of SWCX emission, as recorded by Suzaku, it was found that the SWCX intensity in this observation was strong, in spite of the fact that the line-of-sight direction did not traverse the sub-solar magnetosheath nor the magnetospheric cusps, where higher SWCX emission would be expected.
Rosette Modes of Oscillations of Rotating Stars Caused by Close Degeneracies. I. Axisymmetric Modes
Authors: Takata Masao , Saio Hideyuki
Published: March 2014

We present an analysis of unique axisymmetric eigenmodes of oscillations in rigidly rotating stars, which have been recently discovered numerically in the frequency region of low-order gravity modes of the polytropic model with index 3, and named as rosette modes after their structure of the eigenfunctions. We show that the appearance of rosette modes in the presence of slow rotation is caused by a close degeneracy in the frequency among several eigenmodes in the non-rotating case. Regarding the effect of the Coriolis force on stellar oscillations as a small perturbation, and applying quasi-degenerate perturbation theory, we can successfully reproduce the structure of rosette modes as a linear combination of several unperturbed eigenmodes, which have almost the same frequency and successive spherical degrees of the same parity. We confirm that the eigenfrequencies and the structure of the eigenfunctions that are determined by the perturbative technique are consistent with the results of more direct numerical computations, which are based on the decomposition of the eigenfunctions into a series of spherical harmonics. We discuss the characteristics of rosette modes in detail.
The Relationship between the Power-Law Indices of the Temporal Properties on Energy and the Spectral Lag and Photon Flux of Gamma-Ray Burst Pulses
Authors: Peng Zhao-Yang , Zhao Xiao-Hong , Yin Yue , Bao Yu-Ying , Ma Li
Published: March 2014

Previous studies have shown that the dependence of the pulse temporal properties (pulse width, pulse rise width, pulse decay width, and pulse peak time) on energy is a power-law function. In this work we demonstrate that the power-law indices of the pulse width, pulse rise width, pulse decay width, and pulse peak time on energy are correlated with the spectral lag and the relative spectral lag, $ \bigtriangleup t_{31}/w_{3}$ (where $ \bigtriangleup t_{31}$ and $ w_{3}$ are the spectral lag between BATSE channels 1 and 3 and the pulse width of BATSE channel 3, respectively), using a sample including 102 well-separated long-duration gamma-ray burst pulses. In addition, the correlations of the power-law indices with the relative spectral lags are much more tighter than those with the spectral lags. We further find that the power-law indices are also correlated with the pulse photon flux. The possible origins of these correlations are also discussed. We argue that the kinematic effect can explain the correlated properties.
Visible Spectroscopic Observations of a Near-Earth Object, 2012 DA14
Authors: Urakawa Seitaro , Fujii Mitsugu , Hanayama Hidekazu , Takahashi Jun , Terai Tsuyoshi , Ohshima Osamu
Published: March 2014

We present visible spectroscopic observations of a near-earth object (NEO), 2012 DA$_{14}$. The asteroid 2012 DA$_{14}$ came close to the Earth’s surface on 2013 February 15 at a distance of 27700 km. Its estimated diameter is $\sim$ 45 m. The physical properties of such a small asteroid have not yet been well determined. The close encounter was a good opportunity to conduct a variety of observations. The purpose of this paper is to deduce the taxonomy of 2012 DA$_{14}$ based on visible spectroscopic observations using the 0.4 m F/10 telescope at the Fujii Kurosaki Observatory. We conclude that the taxonomy of 2012 DA$_{14}$ is L-type in the visible wavelength region. In addition, we refer to the availability of a small, accessible telescope for NEOs smaller than 100 m.
Abundance Analysis of the Pulsating Primary Component of the Algol-Type System AS Eridani
Authors: Narusawa Shin-Ya
Published: March 2014

We carried out an abundance analysis of the pulsating primary component of an Algol-type binary system, AS Eridani. The spectral data obtained with the Subaru/HDS were used, and the abundances of six elements (Mg, Si, Ca, Ti, Cr, and Fe) were determined relative to an A3V spectroscopic standard star, α PsA. An under-abundance of iron (–0.66 dex) has been established. Other elements, Mg through Cr, are also under-abundant (∼–0.4 dex). No difference in abundances at different orbital phases was found. The physical relation between the metallicities and the pulsational characteristics is discussed.
MAXI/GSC Discovery of the Black-Hole Candidate MAXI J1305–704
Authors: Morihana Kumiko , Sugizaki Mutsumi , Nakahira Satoshi , Shidatsu Megumi , Ueda Yoshihiro , Serino Motoko , Mihara Tatehiro , Matsuoka Masaru , Negoro Hitoshi , Kawai Nobuyuki
Published: March 2014

We present the first results on a new black-hole candidate, MAXI J1305–704, observed by MAXI/GSC. The new X-ray transient, named as MAXIJ1305–704, was first detected by the MAXI-GSC all-sky survey on 2012 April 9 in the direction to the outer Galactic bulge at $(l,b)=(304_\cdot^\circ 2,-7_\cdot^\circ 6)$. A Swift/XRT follow-up observation confirmed the uncatalogued point source, and localized it to the position at $(13^\textrm h06^\textrm m56_\cdot^\textrm s44,-70^\circ27^\prime4.^{\prime\prime}91)$. The source continued its activity for about five months, until 2012 August. The MAXI/GSC light curve in the 2–10 keV band and the variation of the hardness ratio of the 4–10 keV to the 2–4 keV flux revealed the hard-to-soft state transition on the the sixth day (April 15) in the brightening phase and the soft-to-hard transition on the ∼60th day (June 15) in the decay phase. The luminosity at the initial hard-to-soft transition was significantly higher than that at the soft-to-hard transition in the decay phase. The X-ray spectra in the hard state are represented by a single power-law model with a photon index of ∼2.0, while those in the soft state need such an additional soft component as represented by a multi-color disk blackbody emission with an inner disk temperature of ∼0.5–1.2 keV. All of the obtained features support the source identification of a Galactic black-hole binary located in the Galactic bulge.
Cosmological Fast Radio Bursts from Binary Neutron Star Mergers
Authors: Totani Tomonori
Published: March 2014

Fast radio bursts (FRBs) at cosmological distances have recently been discovered, whose duration is about milliseconds. We argue that the observed short duration is difficult to explain by giant flares of soft gamma-ray repeaters, though their event rate and energetics are consistent with FRBs. Here, we discuss binary neutron star (NS–NS) mergers as a possible origin of FRBs. The FRB rate is within the plausible range of the NS–NS merger rate and its cosmological evolution, while a large fraction of the NS–NS mergers must produce observable FRBs. A likely radiation mechanism is coherent radio emission, like radio pulsars, by magnetic braking when magnetic fields of neutron stars are synchronized to binary rotation at the time of coalescence. Magnetic fields of the standard strength (∼1012-13 G) can explain the observed FRB fluxes, if the conversion efficiency from magnetic braking energy loss to radio emission is similar to that of isolated radio pulsars. Corresponding gamma-ray emission is difficult to detect by current or past gamma-ray burst satellites. Since FRBs tell us the exact time of mergers, a correlated search would significantly improve the effective sensitivity of gravitational wave detectors.
Low-Resolution Spectrum of the Zodiacal Light with the AKARI InfraRed Camera
Authors: Tsumura Kohji , Matsumoto Toshio , Matsuura Shuji , Pyo Jeonghyun , Sakon Itsuki , Wada Takehiko
Published: March 2014

We present near- and mid-infrared zodiacal light spectra obtained with the AKARI Infra-Red Camera (IRC). A catalog of 278 spectra of the diffuse sky covering a wide range of Galactic and ecliptic latitudes was constructed. The wavelength range of this catalog is $1.8-5.3 \mu \textrm m $ with a wavelength resolution of $\lambda/\Delta\lambda \sim20$. Advanced reduction methods specialized for the slit spectroscopy of diffuse sky spectra have been developed for constructing the spectral catalog. Based on a comparison analysis of spectra collected in different seasons and ecliptic latitudes, we confirmed that the spectral shape of the scattered component and the thermal emission component of the zodiacal light in our wavelength range does not show any dependence on location and time, but the relative brightness between them varies with location. We also confirmed that the color temperature of the zodiacal emission at $3-5 \mu \textrm m $ is $300\pm 10 \textrm k$ at any ecliptic latitude. This emission is expected to originate from sub-micron dust particles in interplanetary space.
Microwave Signature of Relativistic Positrons in Solar Flares
Authors: Fleishman Gregory D. , Altyntsev Alexander T. , Meshalkina Nataliia S.
Published: March 2014

Relativistic antiparticles can be created in high-energy nuclear interactions; thus, the detection of antiparticles in an astrophysical source can tell us something remarkable about the underlying high-energy processes and nuclear interactions. However, once created, the antiparticles remain a minor fraction of their conjugant normal particles, so the detection of the antiparticles represents a big science challenge. To address this challenge we employ the imaging and polarimetry of microwave radiation produced as the positrons gyrate in the ambient magnetic field. The key property of the radiation used in this method is that the oppositely charged particles, electrons and positrons, produce radiation with opposite helicity, easily distinguishable by currently operating radio facilities. Analysis of available spatially resolved microwave data augmented by independent magnetic field measurements allows us to remotely detect the relativistic positron component in several solar flares.
Microwave and EUV Observations of an Erupting Filament and Associated Flare and Coronal Mass Ejections
Authors: Alissandrakis Costas E. , Kochanov Alexey A. , Patsourakos Spiros , Altyntsev Alexander T. , Lesovoi Sergey V. , Lesovoya Nadya N.
Published: March 2014

A filament eruption was observed with the Siberian Solar Radio Telescope (SSRT) on 2012 June 23, starting at around 06:40 UT, beyond the west limb. The filament could be followed in SSRT images to heights above 1 R⊙, and coincided with the core of the CME, seen in LASCO C2 images. We briefly discuss the dynamics of the eruption: the top of the filament showed a smooth acceleration up to an apparent velocity of $\sim 1100 \textrm {km} \enspace \textrm s^{-1}$. Images behind the limb from STEREO-A show a two-ribbon flare and the interaction of the main filament, located along the primary neutral line, with an arch-like structure, oriented in the perpendicular direction. The interaction was accompanied by strong emission and twisting motions. The microwave images show a low-temperature component, a high-temperature component associated with the interaction of the two filaments and another high-temperature component apparently associated with the top of flare loops. We computed the differential emission measure from the high-temperature AIA bands and from this the expected microwave brightness temperature; for emission associated with the top of the flare loops, the computed brightness was 35% lower than the observed value.
A single amino acid mutation, R42A, in the Newcastle disease virus matrix protein abrogates its nuclear localization and attenuates viral replication and pathogenicity
Authors: Duan Zhiqiang , Li Juan , Zhu Jie , Chen Jian , Xu Haixu , Wang Yuyang , Liu Huimou , Hu Shunlin , Liu Xiufan
Published: March 2014

The Newcastle disease virus (NDV) matrix (M) protein is a highly basic and nucleocytoplasmic shuttling viral protein. Previous study has demonstrated that the N-terminal 100 aa of NDV M protein are somewhat acidic overall, but the remainder of the polypeptide is strongly basic. In this study, we investigated the role of the N-terminal basic residues in the subcellular localization of M protein and in the replication and pathogenicity of NDV. We found that mutation of the basic residue arginine (R) to alanine (A) at position 42 disrupted M’s nuclear localization. Moreover, a recombinant virus with R42A mutation in the M protein reduced viral replication in DF-1 cells and attenuated the virulence and pathogenicity of the virus in chickens. This is the first report to show that a basic residue mutation in the NDV M protein abrogates its nuclear localization and attenuates viral replication and pathogenicity.
General approach for in vivo recovery of cell type-specific effector gene sets
Authors: Barsi Julius C. , Tu Qiang , Davidson Eric H.
Published: March 2014

Differentially expressed, cell type-specific effector gene sets hold the key to multiple important problems in biology, from theoretical aspects of developmental gene regulatory networks (GRNs) to various practical applications. Although individual cell types of interest have been recovered by various methods and analyzed, systematic recovery of multiple cell type-specific gene sets from whole developing organisms has remained problematic. Here we describe a general methodology using the sea urchin embryo, a material of choice because of the large-scale GRNs already solved for this model system. This method utilizes the regulatory states expressed by given cells of the embryo to define cell type and includes a fluorescence activated cell sorting (FACS) procedure that results in no perturbation of transcript representation. We have extensively validated the method by spatial and qualitative analyses of the transcriptome expressed in isolated embryonic skeletogenic cells and as a consequence, generated a prototypical cell type-specific transcriptome database.
Standards and innovation in manufacturing and services: the case of ISO 9000
Authors: Mangiarotti Giovanni , A.F. Riillo Cesare
Published: March 2014

Purpose

– The research empirically investigates the firm-level impact of ISO 9000 certification on innovation propensity. The study aims to distinguish between manufacturing and service sectors and adopts different innovation definitions aimed at capturing the peculiarities of innovation in services and small firms.

Design/methodology/approach

– Relying chiefly on Community Innovation Survey data for Luxembourg, the impact of certification on innovation probability is assessed using a logit model that controls for relevant firms characteristics and market features.

Findings

– The innovation potential of services and small firms is understated when adopting innovation definitions restricted to technological aspects and more formalised innovation activities. ISO 9000 certification may promote innovation when adopting definitions that captures sectoral innovation specificities. In particular, certification increases innovation propensity in manufacturing when the focus is on technological innovation and formalised innovation expenditures. On the contrary, when non-technological aspects are included and allowance is made for wider innovation activities, the impact of certification on services tends to emerge. However, sharper statistical evidence for manufacturing indicates a more important role of certification for innovation success in this sector.

Research limitations/implications

– Case-study research could supplement the findings concerning the relative effectiveness of certification in services and manufacturing. The investigation would also benefit from extensions in the econometric analysis to address comparisons across samples and potential causality issues.

Practical implications

– Findings are interesting to practitioners and registrars in order to identify the specific characteristics of firms for which certification provides higher innovative potential.

Originality/value

– The study highlights the relevance of sectoral specificities and innovation definitions for the debate about the effect of ISO 9000 certification on innovation.
Complementary plant nutrient‐acquisition strategies promote growth of neighbour species
Authors: Teste Francois P. , Veneklaas Erik J. , Dixon Kingsley W. , Lambers Hans
Published: March 2014

Greater understanding of positive interspecific interactions in nutrient‐poor soils is a priority, particularly in phosphorus (P)‐limited ecosystems where plants with contrasting nutrient‐acquiring strategies co‐occur. It is also relevant to agro‐ecosystems, since global P stocks are being depleted. In this study, we assess positive interactions between sympatric plants with contrasting nutrient‐acquiring strategies from highly P‐impoverished soils from the biodiversity hotspot of south‐western Australia.

Four plant species (Banksia menziesii, Eucalyptus marginata, Verticordia nitens and Melaleuca preissiana) that are non‐mycorrhizal (cluster‐rooted), ectomycorrhizal (EM), arbuscular (AM) or dual AM/EM, respectively, were grown together in a specially designed ‘common garden’ microcosm with nutrient‐poor or fertilized soil, with or without root intermingling and fungal hyphae contact. We measured growth, mycorrhizal colonization, root intermingling and nutrient uptake to determine positive or negative growth patterns amongst the various plant assemblies.

Growth of the AM/EM host was best when interacting with both the EM host and a non‐mycorrhizal nutrient‐mining plant with cluster roots (Banksia) in microcosms where root intermingling was not possible. Growth promotion was only seen in pots with nutrient‐poor soils, where the better growth of Melaleuca coincided with higher shoot P, manganese, calcium, iron and boron content, whereas an increase in soil nutrient status through fertilizer addition resulted in a decrease in nutrient‐sharing between co‐occurring species. Furthermore, the dual AM/EM Melaleuca exhibited enhanced EM colonization and favoured EM over AM fungi when grown beside Eucalyptus and Banksia. We surmise that mycorrhizal networks were instrumental in the variation in both mycorrhizal type and colonization levels.

We conclude that complementarity of plant nutrient‐acquisition strategies can promote growth of neighbour species. The results show a synergistic effect between EM hyphal scavenging and mobilization of limiting nutrients by cluster roots. The positive and negative interactions enable coexistence to go far beyond the traditional view that plants interact mainly through resource depletion. This study improves our understanding of how root interactions could shape plant communities and promote species diversity and packing in nutrient‐impoverished habitats.
Securitization, Risk‐Taking and the Option to Change Strategy
Authors: Lai Rose Neng , Van Order Robert
Published: March 2014

This article models the riskiness of structured securitization deals. The deals are put together by “banks,” which can exercise strategic options over the risk put into the deals. The banks face a trade‐off between the benefits of risk‐taking now and future franchise benefits if the deal pays off. The key insight is a convex relationship between the value of the bank's equity position and the risk in the deal. Although there is a continuum of possible risk, banks choose either the highest or lowest levels of risk open to them. Changes in strategy are discontinuous and unpredictable; a history of low risk‐taking may be a prelude to increased risk‐taking later. Competition, to the extent of reducing franchise value, can lead to more risk‐taking, as can more information in the market. The model provides insights into the risk‐taking that led up to the Great Recession and to institutions that are “Too Big to Fail.”
An Experimental Study of Vertebrate Scavenging Behavior in a Northwest European Woodland Context
Authors: Young Alexandria , Stillman Richard , Smith Martin J. , Korstjens Amanda H.
Published: March 2014

Vertebrate scavengers can modify surface deposited human remains which can hinder forensic investigations. The effects of such scavenging vary between species and regions. Published research into the effects of the scavenging of human remains is dominated by work from North America with few studies covering Northwestern Europe. Forensic scientists, investigators, and police search officers in Northwestern Europe are often left questioning on a basic level as to which scavengers are active and how they might affect human remains. This paper presents the results of a field study utilizing deer (Cervus nippon; Capreolus capreolus) as surface deposits observed by motion detection cameras in a British woodland. The most common avian and rodent scavenger species recorded included the buzzard (Buteo buteo), carrion crow (Corvus corone), wood mouse (Apodemus sylvaticus), and gray squirrel (Sciurus carolinensis). The scavenging behaviors observed were affected by seasonality, rates of decomposition, and insect activity. Scavenging by buzzards, unlike carrion crows, was most frequent during fall to winter and prior to insect activity. Overall, avian scavengers modified and scavenged soft tissue. Rodents scavenged both fresh and skeletonized remains with gray squirrels only scavenging skeletal remains. Wood mice were most active in winter and scavenged both soft tissue and bone.
Postfeeding Larval Dispersal Behavior of Late Season Blow Flies (Calliphoridae) in Southern Ontario, Canada
Authors: Turpin Chantal , Kyle Christopher , Beresford David V.
Published: March 2014

Postfeeding dispersal involves migration of larvae away from their food source in order to pupate. Puparia are difficult to find, yet are important for estimating PMI, and missing puparia during collection can result in inaccurate estimations. This study investigates the late season maggot dispersal patterns for blow flies at coyote carcasses in two habitats with an aim to improving puparia collection procedures. Puparia samples collected from various dispersal distances and directions tested the spatial distribution patterns of the various species using the variance/mean ratio (VMR). Lucilia illustris was the most common species to emerge, with a preferred minimum dispersal distance of more than 50.8 cm and an overall VMR value of 14.91, indicating this species had a clumped distribution pattern. These findings highlight that current collection procedures that use random sampling from under carcasses do not adequately account for the spatial distribution of larvae.
Emotional Reactions of Mothers who have Babies who are Diagnosed with Down Syndrome
Authors: Canbulat Nejla , Demirgöz BAL Meltem , Çoplu Mehtap
Published: March 2014

Purpose

The aim of this study was to explore a deeper insight into experiences of Turkish mothers living with/diagnosed with Down syndrome (DS) baby.

Methods

Individual and audiotaped interviews were carried out with 11 women after amniocentesis in Karaman city of Turkey between August 2012 and February 2013. Transcribed semistructured interviews were qualitatively and analyzed using a thematic analysis approach to code and categorize emerging themes.

Results

Three principal themes emerged from the study: mothers' emotional reaction after diagnosed DS, mother and healthcare professional interactions, and mother's coping with diagnosed DS.

Conclusions

Understanding the experiences of women living with/diagnosed with DS baby enables nurses to devise appropriate strategies to provide better support at every stage and thus helping them to cope with daily life.

Amaç

Bu çalışmanın amacı gebeliğinde Down sendromu tanısı konmuş kadınların derin bir bakışla deneyimlerini saptamaktır.

Yöntem

Çalışma Karaman'da Ağustos 2012 ve Şubat 2013 tarihleri arasında yapılmıştır. Yarı yapılandırılmış görüşme formu ile kişiye özel ses kayıtları alınarak yapılan çalışmada tematik analiz kullanılarak veriler kodlanmış ve kategorize edilmiştir.

Bulgular

Çalışma sonunda sptanan temalar: tanı sonrası kadınların duygusal durumları, anne‐ sağlık personeli ilişkisi, tanı sonrası başetme yollarıdır.

Sonuçlar

Kadınların hislerini anlamak, bu sürecin her aşamasında hemşirelerin daha iyi destek vermek için uygun stratejileri geliştirmelerini sağlayarak, onların günlük yaşamlarını kolaylaştırılabilir.