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Journal articles on the topic 'Phi star'

Author: Grafiati

Published: 4 June 2021

Last updated: 11 February 2022

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1

GHORAISHI, S. M. "ON NONINNER AUTOMORPHISMS OF FINITE NONABELIAN -GROUPS." Bulletin of the Australian Mathematical Society 89, no. 2 (June 7, 2013): 202–9. http://dx.doi.org/10.1017/s0004972713000403.

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AbstractA long-standing conjecture asserts that every finite nonabelian $p$-group has a noninner automorphism of order $p$. In this paper the verification of the conjecture is reduced to the case of $p$-groups $G$ satisfying ${ Z}_{2}^{\star } (G)\leq {C}_{G} ({ Z}_{2}^{\star } (G))= \Phi (G)$, where ${ Z}_{2}^{\star } (G)$ is the preimage of ${\Omega }_{1} ({Z}_{2} (G)/ Z(G))$ in $G$. This improves Deaconescu and Silberberg’s reduction of the conjecture: if ${C}_{G} (Z(\Phi (G)))\not = \Phi (G)$, then $G$ has a noninner automorphism of order $p$ leaving the Frattini subgroup of $G$ elementwise fixed [‘Noninner automorphisms of order $p$ of finite $p$-groups’, J. Algebra 250 (2002), 283–287].

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2

Singh, Mahendra, Masahiro Mon, Tomokazu Kogure, and Masakazu Suzuki. "Spectroscopic Observations of The Be Star PHI-PER." International Astronomical Union Colloquium 137 (1993): 804–6. http://dx.doi.org/10.1017/s0252921100018935.

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AbstractBased on a series of high dispersion Coude spectra taken with 188-cm telescope of Okayama Astrophysical Observatory over an extensive period of time (nearly 20 years), spectroscopic behaviours were measured and discussed. Synchronous variations of V/R (intensity ratio of violet to red emission peaksjvariability with the radial velocity curves (RV) for Balmer and Hel 3888 shell absorption lines were confirmed. Using the peak separations of the Balmer emission lines, envelope extension was also estimated. Main difficulty was found in explaining the envelope extension of the primary star of the system which overflows the Roche-lobe limit when we consider the binary nature of the system.

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3

Brunetti, Maurizio, and Francesco Belardo. "Line graphs of complex unit gain graphs with least eigenvalue -2." Electronic Journal of Linear Algebra 37, no. 37 (February 3, 2021): 14–30. http://dx.doi.org/10.13001/ela.2021.5249.

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Let $\mathbb T$ be the multiplicative group of complex units, and let $\mathcal L (\Phi)$ denote a line graph of a $\mathbb{T}$-gain graph $\Phi$. Similarly to what happens in the context of signed graphs, the real number $\min Spec(A(\mathcal L (\Phi))$, that is, the smallest eigenvalue of the adjacency matrix of $\mathcal L(\Phi)$, is not less than $-2$. The structural conditions on $\Phi$ ensuring that $\min Spec(A(\mathcal L (\Phi))=-2$ are identified. When such conditions are fulfilled, bases of the $-2$-eigenspace are constructed with the aid of the star complement technique.

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4

PEDERSEN, THOMAS VILS. "WEAK-STAR PROPERTIES OF HOMOMORPHISMS FROM WEIGHTED CONVOLUTION ALGEBRAS ON THE HALF-LINE." Journal of the Australian Mathematical Society 89, no. 1 (July 20, 2010): 75–90. http://dx.doi.org/10.1017/s144678871000025x.

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AbstractLet L1(ω) be the weighted convolution algebra L1ω(ℝ+) on ℝ+ with weight ω. Grabiner recently proved that, for a nonzero, continuous homomorphism Φ:L1(ω1)→L1(ω2), the unique continuous extension $\widetilde {\Phi }:M(\omega _1)\to M(\omega _2)$ to a homomorphism between the corresponding weighted measure algebras on ℝ+ is also continuous with respect to the weak-star topologies on these algebras. In this paper we investigate whether similar results hold for homomorphisms from L1(ω) into other commutative Banach algebras. In particular, we prove that for the disc algebra $A(\overline {\mathbb D})$ every nonzero homomorphism $\Phi :L^1({\omega })\to A(\overline {\mathbb D})$ extends uniquely to a continuous homomorphism $\widetilde {\Phi }:M(\omega )\to H^{\infty }(\mathbb D)$ which is also continuous with respect to the weak-star topologies. Similarly, for a large class of Beurling algebras A+v on $\overline {\mathbb D}$ (including the algebra of absolutely convergent Taylor series on $\overline {\mathbb D}$) we prove that every nonzero homomorphism Φ:L1(ω)→A+v extends uniquely to a continuous homomorphism $\widetilde {\Phi }:M(\omega )\to A^+_v$ which is also continuous with respect to the weak-star topologies.

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5

Brown, Christopher F. "BV photometry of the binary Be star Phi Persei." Publications of the Astronomical Society of the Pacific 104 (January 1992): 38. http://dx.doi.org/10.1086/132955.

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6

Imran, Muhammad, Adnan Aslam, Sohail Zafar, and Waqas Nazeer. "Further results on edge irregularity strength of graphs." Indonesian Journal of Combinatorics 1, no. 2 (August 23, 2017): 36. http://dx.doi.org/10.19184/ijc.2017.1.2.5.

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<p>A vertex $k$-labelling $\phi:V(G)\longrightarrow \{1,2,\ldots,k\}$ is called irregular $k$-labeling of the graph $G$ if for every two different edges $e$ and $f$, there is $w_{\phi}(e)\neq w_{\phi}(f)$; where the weight of an edge is given by $e=xy\in E(G)$ is $w_{\phi}(xy)=\phi(x)+\phi(y)$. The minimum $k$ for which the graph $G$ has an edge irregular $k$-labelling is called \emph{edge irregularity strength} of $G$, denoted by $es(G)$.\\<br />In the paper, we determine the exact value of the edge irregularity strength of caterpillars, $n$-star graphs, $(n,t)$-kite graphs, cycle chains and friendship graphs.</p>

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7

Zhao, J., and C. G. Tinney. "FIESTA – disentangling stellar variability from exoplanets in the Fourier domain." Monthly Notices of the Royal Astronomical Society 491, no. 3 (November 22, 2019): 4131–46. http://dx.doi.org/10.1093/mnras/stz3254.

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ABSTRACT We propose a new analysis methodology – FourIEr phase SpecTrum Analysis (FIESTA, or $\mathit {\Phi }$ESTA) – for the study of spectral line profile variability in Fourier space. The philosophy of $\mathit {\Phi }$ESTA is highlighted in its interpretation of a line deformation as various shifts of the composing Fourier modes. With this ability, $\mathit {\Phi }$ESTA excels in distinguishing the effects of a bulk shift in a line profile, from changes in a line profile shape. In other words, it can distinguish a radial velocity shift due to orbiting companions like planets, from an apparent radial velocity shift due to stellar variability (often referred to as ‘jitter’). Most importantly, it can quantify the radial velocity impact of stellar jitter on each epoch. Our simulations show that (compared to a model that does not account for stellar activity), $\mathit {\Phi }$ESTA can almost triple the fraction of planets recovered with orbital parameters measured to within 10 per cent of their input parameters, when extracting a 2 m s−1 amplitude planetary signal in the midst of ∼2 m s−1 amplitude starspot jitter for high signal-to-noise ratio (>200 pixel−1) data. $\mathit {\Phi }$ESTA can also be used to identify stellar activity related periods in a periodogram analysis and classify relative amplitudes of stellar jitter and planetary signals, with examples for the analysis of HARPS data of the active star HD 224789 and the active planet-host star HD 103720. In the end, we demonstrate that $\mathit {\Phi }$ESTA’s framework is working as well as other activity indicators in correlating with stellar jitter.

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8

Khostovan, A. A., S. Malhotra, J. E. Rhoads, C. Jiang, J. Wang, I. Wold, Z.-Y. Zheng, et al. "A large, deep 3 deg2 survey of H α, [O iii], and [O ii] emitters from LAGER: constraining luminosity functions." Monthly Notices of the Royal Astronomical Society 493, no. 3 (January 20, 2020): 3966–84. http://dx.doi.org/10.1093/mnras/staa175.

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ABSTRACT We present our measurements of the H α, [O iii], and [O ii] luminosity functions as part of the Lyman Alpha Galaxies at Epoch of Reionization (LAGER) survey using our samples of 1577 z = 0.47 H α-, 3933 z = 0.93 [O iii]-, and 5367 z = 1.59 [O ii]-selected emission line galaxies in a 3 deg2 single, CTIO/Blanco DECam pointing of the COSMOS field. Our observations reach 5σ depths of 8.2 × 10−18 erg s−1 cm−2 and comoving volumes of (1−7) × 105 Mpc3 making our survey one of the deepest narrow-band surveys. We select our emission line galaxies via spectroscopic confirmation, photometric redshifts, and colour–colour selections. We measure the observed luminosity functions for each sample and find best fits of $\phi ^\star = 10^{-3.16^{+0.09}_{-0.09}}$ Mpc−3 and $L^\star = 10^{41.72^{+0.09}_{-0.09}}$ erg s−1 for H α, $\phi ^\star = 10^{-2.16^{+0.10}_{-0.12}}$ Mpc−3 and $L^\star = 10^{41.38^{+0.07}_{-0.06}}$ erg s−1 for [O iii], and $\phi ^\star = 10^{-1.97^{+0.07}_{-0.07}}$ Mpc−3 and $L^\star = 10^{41.66^{+0.03}_{-0.03}}$ erg s−1 for [O ii], with α fixed to −1.75, −1.6, and −1.3, respectively. An excess of bright >1042 erg s−1 [O iii] emitters is observed and may be due to active galactic nucleus (AGN) contamination. Corrections for dust attenuation are applied assuming AHα = 1 mag. We also design our own empirical rest-frame g − r calibration using SDSS DR12 data, test it against our z = 0.47 H α emitters with zCOSMOS 1D spectra, and calibrate it for (g − r) between −0.8 and 1.3 mag. Dust and AGN-corrected star formation rate densities (SFRDs) are measured as log10ρSFR/(M⊙ yr−1 Mpc−3) = −1.63 ± 0.04, −1.07 ± 0.06, and −0.90 ± 0.10 for H α, [O iii], and [O ii], respectively. We find our [O iii] and [O ii] samples fully trace cosmic star formation activity at their respective redshifts in comparison to multiwavelength SFRDs, while the H α sample traces ∼70 per cent of the total z = 0.47 SFRD.

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9

Hummel, W., and S. Štefl. "The circumstellar structure of the Be shell star $\mathsf{\phi}$ Persei." Astronomy & Astrophysics 368, no. 2 (March 2001): 471–83. http://dx.doi.org/10.1051/0004-6361:20000559.

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10

Aschieri, Paolo, Leonardo Castellani, and Marija Dimitrijević. "Dynamical Noncommutativity and Noether Theorem in Twisted $${\phi^{\star 4}}$$ Theory." Letters in Mathematical Physics 85, no. 1 (June 24, 2008): 39–53. http://dx.doi.org/10.1007/s11005-008-0247-6.

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11

Moutard, Thibaud, Marcin Sawicki, Stéphane Arnouts, Anneya Golob, Jean Coupon, Olivier Ilbert, Xiaohu Yang, and Stephen Gwyn. "UV and U-band luminosity functions from CLAUDS and HSC-SSP – I. Using four million galaxies to simultaneously constrain the very faint and bright regimes to z ∼ 3." Monthly Notices of the Royal Astronomical Society 494, no. 2 (March 16, 2020): 1894–918. http://dx.doi.org/10.1093/mnras/staa706.

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ABSTRACT We constrain the rest-frame FUV (1546 Å), NUV (2345 Å), and U-band (3690 Å) luminosity functions (LFs) and luminosity densities (LDs) with unprecedented precision from z ∼ 0.2 to z ∼ 3 (FUV, NUV) and z ∼ 2 (U band). Our sample of over 4.3 million galaxies, selected from the CFHT Large Area U-band Deep Survey (CLAUDS) and HyperSuprime-Cam Subaru Strategic Program (HSC-SSP) data lets us probe the very faint regime (down to MFUV, MNUV, MU ≃ −15 at low redshift), while simultaneously detecting very rare galaxies at the bright end down to comoving densities <10−5 Mpc−3. Our FUV and NUV LFs are well fitted by single-Schechter functions, with faint-end slopes that are very stable up to z ∼ 2. We confirm, but self-consistently and with much better precision than previous studies, that the LDs at all three wavelengths increase rapidly with lookback time to z ∼ 1, and then much more slowly at 1 < z < 2–3. Evolution of the FUV and NUV LFs and LDs at z < 1 is driven almost entirely by the fading of the characteristic magnitude, $M^\star _{\rm UV}$, while at z > 1 it is due to the evolution of both $M^\star _{\rm UV}$ and the characteristic number density $\phi ^\star _{\rm UV}$. In contrast, the U-band LF has an excess of faint galaxies and is fitted with a double-Schechter form; $M^\star _{U}$, both $\phi ^\star _{U}$ components, and the bright-end slope evolve throughout 0.2 < z < 2, while the faint-end slope is constant over at least the measurable 0.05 < z < 0.6. We present tables of our Schechter parameters and LD measurements that can be used for testing theoretical galaxy evolution models and forecasting future observations.

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12

SONG, Maengseok, Haiyan SHAO, Anwer MUJEEB, Thomas L. JAMES, and Walter L. MILLER. "Molten-globule structure and membrane binding of the N-terminal protease-resistant domain (63–193) of the steroidogenic acute regulatory protein (StAR)." Biochemical Journal 356, no. 1 (May 8, 2001): 151–58. http://dx.doi.org/10.1042/bj3560151.

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The first step in steroidogenesis is the movement of cholesterol from the outer to inner mitochondrial membrane; this movement is facilitated by the steroidogenic acute regulatory protein (StAR). StAR has molten-globule properties at low pH and a protease-resistant N-terminal domain at pH4 and pH8 comprising residues 63–193. To explore the mechanism of action of StAR we investigated the structural properties of the bacterially expressed N-terminal domain (63–193 StAR) using CD, limited proteolysis and NMR. Far- and near-UV CD showed that the amount of secondary structure was greater at acidic than at neutral pH, but there was little tertiary structure at any pH. Unlike 63–193 StAR liberated from N-62 StAR by proteolysis, biosynthetic 63–193 StAR was no longer resistant to trypsin or proteinase K at pH7, or to pepsin at pH4. Addition of trifluoroethanol and SDS increased secondary structure at pH7, and dodecylphosphocholine and CHAPS increased secondary structure at pH2, pH4 and pH7. However, none of these conditions induced tertiary structure, as monitored by near-UV CD or NMR. Liposomes of phosphatidylcholine, phosphatidylserine and their mixture increased secondary structure of 63–193 StAR at pH7, as monitored by far-UV CD, and stable protein–liposome complexes were identified by gel-permeation chromatography. These results provide further evidence that the N-terminal domain of StAR is a molten globule, and provide evidence that this conformation facilitates the interaction of the N-terminal domain of StAR with membranes. We suggest that this interaction is the key to understanding the mechanism of StAR's action.

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13

Lipiec, A. "$\Delta \eta $--$\Delta \phi $ Correlations of Identified Particles in the Beam Energy Scan Program at STAR." Acta Physica Polonica B Proceedings Supplement 12, no. 2 (2019): 301. http://dx.doi.org/10.5506/aphyspolbsupp.12.301.

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14

Gies, Douglas R., Chilinda Y. Willis, Laura R. Penny, and David McDavid. "The He I 6678-wavelength emission line of Phi Persei - New evidence of the companion star." Publications of the Astronomical Society of the Pacific 105 (March 1993): 281. http://dx.doi.org/10.1086/133143.

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15

Ocran, E. F., A. R. Taylor, M. Vaccari, C. H. Ishwara-Chandra, I. Prandoni, M. Prescott, and C. Mancuso. "The evolution of the low-frequency radio AGN population to z ≃ 1.5 in the ELAIS N1 field." Monthly Notices of the Royal Astronomical Society 500, no. 4 (November 13, 2020): 4685–702. http://dx.doi.org/10.1093/mnras/staa3538.

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ABSTRACT We study the cosmic evolution of radio sources out to z ≃ 1.5 using a GMRT 610 MHz survey covering ∼1.86 deg2 of the ELAIS N1 field with a minimum/median rms noise 7.1/19.5 μJy beam−1 and an angular resolution of 6 arcsec. We classify sources as star forming galaxies (SFGs), radio-quiet (RQ) and radio-loud (RL) Active Galactic Nuclei (AGNs) using a combination of multiwavelength diagnostics and find evidence in support of the radio emission in SFGs and RQ AGN arising from star formation, rather than AGN-related processes. At high luminosities, however, both SFGs and RQ AGN display a radio excess when comparing radio and infrared star formation rates. The vast majority of our sample lie along the $\rm {SFR - \mathit{ M}_{\star }}$ ‘main sequence’ at all redshifts when using infrared star formation rates. We derive the 610 MHz radio luminosity function for the total AGN population, constraining its evolution via continuous models of pure density and pure luminosity evolution with $\rm {\Phi ^{\star }\, \propto \, (\, 1+\, \mathit{ z})^{(2.25\pm 0.38)-(0.63\pm 0.35)z}}$ and $\rm {\mathit{ L}_{610\, MHz}\, \propto \, (\, 1+\, \mathit{ z})^{(3.45\pm 0.53)-(0.55\pm 0.29)\mathit{ z}}}$, respectively. For our RQ and RL AGN, we find a fairly mild evolution with redshift best fitted by pure luminosity evolution with $\rm {\mathit{ L}_{610\, MHz}\, \propto \, (\, 1+\, \mathit{ z})^{(2.81\pm 0.43)-(0.57\pm 0.30)\mathit{ z}}}$ for RQ AGN and $\rm {\mathit{ L}_{610\, MHz}\, \propto \, (\, 1+\, \mathit{ z})^{(3.58\pm 0.54)-(0.56\pm 0.29)\mathit{ z}}}$ for RL AGN. The 610 MHz radio AGN population thus comprises two differently evolving populations whose radio emission is mostly SF-driven or AGN-driven, respectively.

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Lumbreras-Calle, A., J. Méndez-Abreu, and C. Muñoz-Tuñón. "The stellar host in star-forming low-mass galaxies: Evidence for two classes." Astronomy & Astrophysics 632 (November 21, 2019): A15. http://dx.doi.org/10.1051/0004-6361/201935288.

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Context. The morphological evolution of star-forming galaxies provides important clues to understand their physical properties, as well as the triggering and quenching mechanisms of star formation. Aims. We analyze the morphology of galaxies hosting star-forming events at low redshift (z < 0.36). We aim at connecting morphology and star-formation properties of low-mass galaxies (median stellar mass ∼108.5 M⊙) beyond the local Universe. Methods. We use a sample of mediumband selected star-forming galaxies from the GOODS-North field. Hα images for the sample are created combining both spectral energy distribution fits and HST data. Using them, we mask the star forming regions to obtain an unbiased two-dimensional model of the light distribution of the host galaxies. For this purpose we use PHI, a new Bayesian photometric decomposition code. We applied it independently to 7 HST bands, from the ultraviolet to the near-infrared, assuming a Sérsic surface brightness model. Results. Star-forming galaxy hosts show low Sérsic index (with median n ∼ 0.9), as well as small sizes (median Re ∼ 1.6 kpc), and negligible change of the parameters with wavelength (except for the axis ratio, which grows with wavelength in 46% of the sample). Using a clustering algorithm, we find two different classes of star-forming galaxies: A more compact, redder, and high-n (class A) and a more extended, bluer and lower-n one (class B). This separation holds across all seven bands analyzed. In addition, we find evidence that the first class is more spheroidal-like (according to the distribution of observed axis ratios). We compute the color gradients of the host galaxies finding that 48% of the objects where the analysis could be performed show negative gradients, and only in 5% they are positive. Conclusions. The host component of low-mass star-forming galaxies at z < 0.36 separates into two different classes, similar to what has been found for their higher mass counterparts. The results are consistent with an evolution from class B to class A. Several mechanisms from the literature, like minor and major mergers, and violent disk instability, can explain the physical process behind the likely transition between the classes.

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Sharma, T. Karthikeya, G. Amba Prasad Rao, and K. Madhu Murthy. "Prediction of HCCI Engine Performance with Three Zone Extended Coherent Flame Combustion Model." Applied Mechanics and Materials 592-594 (July 2014): 1738–45. http://dx.doi.org/10.4028/www.scientific.net/amm.592-594.1738.

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Soot, NOx paradox in compression ignition engines is an extremely challenging issue. Low temperature combustion followed by Homogeneous charge compression ignition (HCCI) type of combustion is capable of reducing nitrogen oxides and soot simultaneously. Homogeneous charge compression ignition (HCCI) has a potential for high fuel conversion efficiency and extremely low emissions of particulate matter and oxides of nitrogen (NOx). However, feasibility of HCCI is also posing certain issues .In this paper, three zone extended coherent flame combustion model of STAR-CD package has been used to study the CI engine in both conventional and HCCI mode. A comparison of important parameters like in-cylinder pressure, temperatures, CO, NOx emissions, in conventional and HCCI mode are predicted. Relatively Low in-cylinder pressures and temperatures are realized in HCCI mode when compared to conventional mode of combustion. Uniform mixing of fuel-air, turbulent kinetic energy and velocity contours are obtained in HCCI mode. Key Words: HCCI, ECFM-3Z, Phi-T charts, Piston Work, Turbulent Kinetic energy.

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Debattista, Victor P., David J. Liddicott, Tigran Khachaturyants, and Leandro Beraldo e Silva. "Box/peanut-shaped bulges in action space." Monthly Notices of the Royal Astronomical Society 498, no. 3 (September 7, 2020): 3334–50. http://dx.doi.org/10.1093/mnras/staa2568.

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ABSTRACT We introduce the study of box/peanut (B/P) bulges in the action space of the initial axisymmetric system. We explore where populations with different actions end up once a bar forms and a B/P bulge develops. We find that the density bimodality due to the B/P bulge (the X-shape) is better traced by populations with low radial, ${\it J}_{R,0}$, or vertical, ${\it J}_{z,0}$, actions, or high azimuthal action, ${\it J}_{\phi ,0}$. Generally, populations separated by ${\it J}_{R,0}$ have a greater variation in bar strength and vertical heating than those separated by ${\it J}_{z,0}$. While the bar substantially weakens the initial vertical gradient of ${\it J}_{z,0}$, it also drives a strikingly monotonic vertical profile of ${\it J}_{R,0}$. We then use these results to guide us in assigning metallicity to star particles in a pure N-body model. Because stellar metallicity in unbarred galaxies depends on age as well as radial and vertical positions, the initial actions are particularly well suited for assigning metallicities. We argue that assigning metallicities based on single actions, or on positions, results in metallicity distributions inconsistent with those observed in real galaxies. We therefore use all three actions to assign metallicity to an N-body model by comparing with the actions of a star-forming, unbarred simulation. The resulting metallicity distribution is pinched on the vertical axis, has a realistic vertical gradient, and has a stronger X-shape in metal-rich populations, as found in real galaxies.

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Denny, DBA, Diane, Sarah Hizon, Lauren Caldarello, Scott Hartman, and Maurie Markman. "Electronic physician ratings and reviews process." Journal of Clinical Oncology 36, no. 30_suppl (October 20, 2018): 209. http://dx.doi.org/10.1200/jco.2018.36.30_suppl.209.

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209 Background: According to JAMA, Public Awareness, Perception, and Use of Online Physician Rating Sites; 35% of patients selected a physician based on good ratings, and 37% avoided one with bad ratings. Yet, there exists a stark difference between unstructured (i.e. Yelp) online reviews as compared to validated survey-generated data. A national network of hospitals that specializes in treating patients with complex cancer had been collecting patient satisfaction data using a validated tool administered by a 3rd party for some time. An electronic physician rating and review process was implemented as an adjunct to that survey process, providing a new mechanism for consumers visiting the networks’ website with accurate information about patients’ satisfaction with its oncologists. Methods: Physician ratings are obtained directly from patients who had an encounter using two specific questions regarding confidence and likelihood to recommend. Ratings are posted by physician and maintained on a 12-month rolling basis once a minimum of 30 ratings is achieved. Likert scale survey data are converted to a one-to-five star rating. De-identified verbatim comments are also posted. Criteria are in place to review comments prior to posting with limited exclusions, such as comments containing PHI or slanderous content. Physicians receive an email to review comments 15 days prior to posting, allowing a process for advance notice or appeal. Both positive and negative reviews are published. Results: Physician performance scores were 4.7 stars pre-launch compared to 4.8 stars post-launch. Additional performance statistics are provided below. Conclusions: Sharing information on the talent of physicians is an important component of transparency and arming patients with information to make informed treatment decisions. As a result, physicians have become more engaged with their data and utilizing reviews to identify improvement opportunities. This translates to a culture of accountability and deepened understanding of patients’ perceptions about care.[Table: see text]

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Tetarenko, A. J., P. Casella, J. C. A. Miller-Jones, G. R. Sivakoff, J. A. Paice, F. M. Vincentelli, T. J. Maccarone, et al. "Measuring fundamental jet properties with multiwavelength fast timing of the black hole X-ray binary MAXI J1820+070." Monthly Notices of the Royal Astronomical Society 504, no. 3 (March 22, 2021): 3862–83. http://dx.doi.org/10.1093/mnras/stab820.

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ABSTRACT We present multiwavelength fast timing observations of the black hole X-ray binary MAXI J1820+070 (ASASSN-18ey), taken with the Karl G. Jansky Very Large Array (VLA), Atacama Large Millimeter/Sub-Millimeter Array (ALMA), Very Large Telescope (VLT), New Technology Telescope (NTT), Neutron Star Interior Composition Explorer (NICER), and XMM–Newton. Our data set simultaneously samples 10 different electromagnetic bands (radio – X-ray) over a 7-h period during the hard state of the 2018–2019 outburst. The emission we observe is highly variable, displaying multiple rapid flaring episodes. To characterize the variability properties in our data, we implemented a combination of cross-correlation and Fourier analyses. We find that the emission is highly correlated between different bands, measuring time-lags ranging from hundreds of milliseconds between the X-ray/optical bands to minutes between the radio/sub-mm bands. Our Fourier analysis also revealed, for the first time in a black hole X-ray binary, an evolving power spectral shape with electromagnetic frequency. Through modelling these variability properties, we find that MAXI J1820+070 launches a highly relativistic ($\Gamma =6.81^{+1.06}_{-1.15}$) and confined ($\phi =0.45^{+0.13}_{-0.11}$ deg) jet, which is carrying a significant amount of power away from the system (equivalent to $\sim 0.6 \, L_{1-100{\rm keV}}$). We additionally place constraints on the jet composition and magnetic field strength in the innermost jet base region. Overall, this work demonstrates that time-domain analysis is a powerful diagnostic tool for probing jet physics, where we can accurately measure jet properties with time-domain measurements alone.

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21

Glos, Derek. "The Star Factor." Performance Improvement 53, no. 6 (July 2014): 35–37. http://dx.doi.org/10.1002/pfi.21419.

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Widodo, Charles, Marchellius Yana, and Halim Agung. "IMPLEMENTASI TOPOLOGI HYBRID UNTUK PENGOPTIMALAN APLIKASI EDMS PADA PROJECT OFFICE PT PHE ONWJ." JURNAL TEKNIK INFORMATIKA 11, no. 1 (May 4, 2018): 19–30. http://dx.doi.org/10.15408/jti.v11i1.6472.

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ABSTRAK Penggunaan aplikasi EDMS di project office PT PHE ONWJ dinilai masih belum optimal karena masih lambat dalam pengunaan aplikasi EDMS. Oleh karena itu dilakukanlah penelitian ini dengan tujuan untuk mengoptimalkan jaringan yang digunakan untuk mengakses aplikasi EDMS pada project office PT PHE ONWJ. Pengoptimalan jaringan yang dimaksud adalah dengan membangun topologi di project office PT PHE ONWJ dan menerapkan metro sebagai perantara topologi star di project office dan topologi star dikantor pusat sehingga menciptakan topologi hybrid. Topologi hybrid yang dimaksud adalah penggabungan antara topologi star yang ada di jaringan pusat, metro sebagai perantara kantor pusat dengan project office PT PHE ONWJ dan topologi star yang akan dibangun di project office PT ONWJ. Diharapkan setelah menerapkan topologi yang telah dirancang dapat mengoptimalkan penggunaan aplikasi EDMS. Topologi star di project office PT ONWJ dan metro sebagai perantara 2 topologi kantor pusat dan project office menghasilkan topologi hybrid. Kesimpulan dari penelitian ini adalah penerapan topologi dalam jaringan dapat memberikan optimalisasi dibandingkan dengan tanpa menerapkan topologi. Hasil rata-rata ping saat pengaksesan aplikasi EDMS sebelum menerapkan topologi hybrid mendapatkan hasil sebesar 392,98 ms dan setelah menerapkan topologi hybrid mendapatkan hasil sebesar 143,50 ms, sehingga disimpulkan bahwa penerapan topologi hybrid lebih baik dalam menjalankan aplikasi EDMS. ABSTRACT The use of EDMS application in PT PHE ONWJ project office is considered not optimal because it is still slow in the use of EDMS applications. Therefore this study was conducted with the aim to optimize the network used to access the EDMS application on the PT PHE ONWJ project office. Network optimization in question is to build a topology in the project office of PT PHE ONWJ and apply the metro as an intermediate star topology in the project office and star topology at the headquarters so as to create a hybrid topology. Hybrid topology in question is a merger between the star topology in the central network, metro as an intermediary head office with PT PHE ONWJ project office and star topology to be built at PT ONWJ project office. It is expected that after applying the topology that has been designed to optimize the use of EDMS applications. Star topology in PT ONWJ project office and metro as intermediary 2 topology headquarters and project office produce hybrid topology. The conclusion of this research is application of topology in network can give optimization compared with without applying topology. The average result of ping when accessing EDMS application before applying hybrid topology got 392.98 ms result and after applying hybrid topology get result of 143,50 ms, so it is concluded that application of hybrid topology is better in running EDMS application. How To Cite : Widodo, C. Yana, M. Agung, H. (2018). IMPLEMENTASI TOPOLOGI HYBRID UNTUK PENGOPTIMALAN APLIKASI EDMS PADA PROJECT OFFICE PT PHE ONWJ. Jurnal Teknik Informatika, 11(1), 19-30. doi 10.15408/jti.v11i1.6472 Permalink/DOI: http://dx.doi.org/10.15408/jti.v11i1.6472

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Novotný, Vojtěch. "State-of-the-art PCI for coronary artery chronic total occlusion." Intervenční a akutní kardiologie 19, no. 1 (June 1, 2020): 31–38. http://dx.doi.org/10.36290/kar.2020.016.

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Amano, Naoko, Satoshi Narumi, Mie Hayashi, Masaki Takagi, Kazuhide Imai, Toshiro Nakamura, Rumi Hachiya, et al. "Genetic defects in pediatric-onset adrenal insufficiency in Japan." European Journal of Endocrinology 177, no. 2 (August 2017): 187–94. http://dx.doi.org/10.1530/eje-17-0027.

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Context Most patients with pediatric-onset primary adrenal insufficiency (PAI), such as 21-hydroxylase deficiency, can be diagnosed by measuring the urine or serum levels of steroid metabolites. However, the etiology is often difficult to determine in a subset of patients lacking characteristic biochemical findings. Objective To assess the frequency of genetic defects in Japanese children with biochemically uncharacterized PAI and characterize the phenotypes of mutation-carrying patients. Methods We enrolled 63 Japanese children (59 families) with biochemically uncharacterized PAI, and sequenced 12 PAI-associated genes. The pathogenicities of rare variants were assessed based on in silico analyses and structural modeling. We calculated the proportion of mutation-carrying patients according to demographic characteristics. Results We identified genetic defects in 50 (85%) families: STAR in 19, NR0B1 in 18, SAMD9 in seven, AAAS in two, NNT in two, MC2R in one and CDKN1C in one. NR0B1 defects were identified in 78% of the male patients that received both glucocorticoid and mineralocorticoid replacement therapy and had normal male external genitalia. STAR defects were identified in 67% of female and 9% of male patients. Seven of the 19 patients with STAR defects developed PAI at age two or older, out of whom, five did not have mineralocorticoid deficiency. Conclusions Molecular testing elucidated the etiologies of most biochemically uncharacterized PAI patients. Genetic defects such as NR0B1 defects are presumed based on phenotypes, while others with broad phenotypic variability, such as STAR defects, are difficult to diagnose. Molecular testing is a rational approach to diagnosis in biochemically uncharacterized PAI patients.

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Kara, Murat, Bayram Kaymak, Ayşe Merve Ata, Özden Özkal, Özgür Kara, Aysun Baki, Gözde Şengül Ayçiçek, et al. "STAR—Sonographic Thigh Adjustment Ratio." American Journal of Physical Medicine & Rehabilitation 99, no. 10 (April 6, 2020): 902–8. http://dx.doi.org/10.1097/phm.0000000000001439.

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Rodríguez, E., A. Rolland, and P. López De Coca. "The SX Phe stars." Astrophysics and Space Science 169, no. 1-2 (July 1990): 113–15. http://dx.doi.org/10.1007/bf00640695.

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Vleugels, Nele, John Leys, Isabelle Knockaert, and Paul Declerck. "Effect of Stabilizing versus Destabilizing Interactions on Plasminogen Activator Inhibitor-1." Thrombosis and Haemostasis 84, no. 11 (2000): 871–75. http://dx.doi.org/10.1055/s-0037-1614130.

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SummaryPlasminogen activator inhibitor-1 (PAI-1) is a unique member of the serpin family, as it spontaneously converts into a latent conformation. However, the exact mechanism of this conversion is not known. Previous studies reported that neutralizing monoclonal antibodies as well as reversal or removal of charges on the s3C-s4C turn results in a destabilization of PAI-1 leading to an accelerated conversion to its latent form.In this study the effect of the reversal or removal of charges in this “gate region” (R186E/R187E, H190E/K191E, H190L/K191L and R356E) on a stable PAI-1-variant (PAI-1-stab) was investigated. Whereas PAI-1-stab has a half-life of 150 ± 66 h, PAI-1-stab-R186ER187E, PAI-1-stab-H190E-K191E, PAI-1-stab-H190L-K191L and PAI-1-stab-R356E have a strongly decreased half-life (p< 0.005 versus PAI-1-stab) of 175 ± 48 min, 75 ± 34 min, 68 ± 38 min and 79 ± 16 min, respectively. Wild-type PAI-1 (wtPAI-1) had a half-life of 55 ± 19 min. These data indicate that the stabilization induced by the mutated residues in PAI-1-stab is counteracted by the additional mutations, resulting in half-lives similar to that of wtPAI-1, thereby suggesting that the stabilizing and destabilizing forces act mainly independently in these mutants. Extrapolation of these data to other (stable) serpins leads to the hypothesis that the s3C-s4C turn and the distal hinge region of the reactive site loop plays a role for the stability of serpins in general.

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Hancock, Cynthia. "DISTINGUISHED FACULTY AND RISING STAR EARLY-CAREER FACULTY AWARD LECTURES." Innovation in Aging 3, Supplement_1 (November 2019): S381—S382. http://dx.doi.org/10.1093/geroni/igz038.1400.

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Abstract The Distinguished Faculty Award acknowledges individuals whose teaching stands out as exemplary, innovative, or influential—or any combination thereof. The Distinguished Faculty Award lecture will feature an address by 2019 recipient Gayle Doll, PhD, of Kansas State University. The Rising Star Early-Career Faculty Award acknowledges new faculty whose teaching and leadership stand out as influential and innovative. The Rising Star Early-Career Faculty Award lecture will feature an address by 2019 recipient Katarina Felstedof, PhD, of the University of Utah.

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Zong, Peng, Ali Esamdin, Jian Ning Fu, Hu Biao Niu, Guo Jie Feng, Tao Zhi Yang, Chun Hai Bai, Yu Zhang, and Jin Zhong Liu. "Pulsations of the SX Phe Star BL Camelopardalis." Publications of the Astronomical Society of the Pacific 131, no. 1000 (April 26, 2019): 064202. http://dx.doi.org/10.1088/1538-3873/ab0a1a.

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Yu, I., T. Ebrahimi, S. G. Hatzikiriakos, and P. Mehrkhodavandi. "Star-shaped PHB–PLA block copolymers: immortal polymerization with dinuclear indium catalysts." Dalton Transactions 44, no. 32 (2015): 14248–54. http://dx.doi.org/10.1039/c5dt02357b.

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The first example of a one-component precursor to star-shaped polyesters, and its utilization in the synthesis of previously unknown star-shaped poly(hydroxybutyrate)–poly(lactic acid) block copolymers, is reported.

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McBride, Mark. "Kearns and Star on Reasons as Evidence." Analytic Philosophy 54, no. 2 (June 2013): 229–36. http://dx.doi.org/10.1111/phib.12017.

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RAFTERY, JUDITH. "Review of Delmendo, The Star-Entangled Banner." Pacific Historical Review 74, no. 3 (August 1, 2005): 477–78. http://dx.doi.org/10.1525/phr.2005.74.3.477.

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KIM, Jinho. "Black Hole, Neutron Star and Numerical Relativity." Physics and High Technology 30, no. 6 (June 30, 2021): 7–13. http://dx.doi.org/10.3938/phit.30.017.

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Compact stars, e.g., black holes and neutron stars, are the most energetic objects in astrophysics. These objects are accompanied by extremely strong gravity and a high velocity, which approaches the speed of light. Therefore, compact objects should be dealt with in Einstein’s relativity. This article will briefly introduce a numerical method that will allow us to obtain general solutions in general relativity. Several applications using numerical relativistic simulations will also be presented.

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Prvák, Milan, Jiří Krtička, and Heidi Korhonen. "The nature of the photometric variability of HgMn stars: a test of simulated light curves of φ Phe against the TESS data." Monthly Notices of the Royal Astronomical Society 492, no. 2 (December 19, 2019): 1834–40. http://dx.doi.org/10.1093/mnras/stz3564.

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ABSTRACT The inhomogeneous surface distribution of heavy elements is known to cause periodic light variability of magnetic chemically peculiar stars. It is unclear to what extent the same paradigm applies to mercury–manganese (HgMn) stars. We aim to model the photometric variability of the HgMn star φ Phe using abundance maps obtained from high-resolution spectroscopy and to study how this variability evolves with time. We compute a grid of atlas12 model atmospheres and the corresponding synspec synthetic spectra. Interpolating within this grid and integrating the specific intensity over the visible stellar surface at different rotational phases, we obtain theoretical light curves of the star. We predict the variability of φ Phe in the ultraviolet and in the visible spectral regions with amplitude of the order of millimagnitudes, mainly caused by absorption in lines of yttrium, chromium, and titanium. We also show how this variability is affected by changes of the distribution of the heavy elements over time. The main characteristics of the predicted light variability of φ Phe correspond roughly to the variability of the star observed with the Transiting Exoplanet Survey Satellite (TESS).

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Balona, L. A., and J. M. Nemec. "A search for SX Phe stars amongKeplerδ Scuti stars." Monthly Notices of the Royal Astronomical Society 426, no. 3 (October 10, 2012): 2413–18. http://dx.doi.org/10.1111/j.1365-2966.2012.21957.x.

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Cummings, Michael. "Star Trek—from space vessels to blood vessels." Practical Diabetes International 20, no. 1 (January 2003): 4–5. http://dx.doi.org/10.1002/pdi.451.

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Thompson, K., and D. W. Coates. "The Rates of Change of the Periods of SX Phe." Publications of the Astronomical Society of Australia 9, no. 2 (1991): 281–82. http://dx.doi.org/10.1017/s1323358000024140.

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Brenner, Bluma G., Jean-Pierre Routy, Marco Petrella, Daniela Moisi, Maureen Oliveira, Mervi Detorio, Bonnie Spira, et al. "Persistence and Fitness of Multidrug-Resistant Human Immunodeficiency Virus Type 1 Acquired in Primary Infection." Journal of Virology 76, no. 4 (February 15, 2002): 1753–61. http://dx.doi.org/10.1128/jvi.76.4.1753-1761.2002.

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ABSTRACT This study examines the persistence and fitness of multidrug-resistant (MDR) viruses acquired during primary human immunodeficiency virus infection (PHI). In four individuals, MDR infections persisted over the entire study period, ranging from 36 weeks to 5 years, in the absence of antiretroviral therapy. In stark contrast, identified source partners in two cases showed expected outgrowth of wild-type (WT) virus within 12 weeks of treatment interruption. In the first PHI case, triple-class MDR resulted in low plasma viremia (1.6 to 3 log copies/ml) over time compared with mean values obtained for an untreated PHI group harboring WT infections (4.1 to 4.3 log copies/ml). Increasing viremia in PHI patient 1 at week 52 was associated with the de novo emergence of a protease inhibitor-resistant variant through a recombination event involving the original MDR virus. MDR infections in two other untreated PHI patients yielded viremia levels typical of the untreated WT group. A fourth patient's MDR infection yielded low viremia (<50 to 500 copies/ml) for 5 years despite his having phenotypic resistance to all antiretroviral drugs in his treatment regimen. In two of these PHI cases, a rebound to higher levels of plasma viremia only occurred when the M184V mutation in reverse transcriptase could no longer be detected and, in a third case, nondetection of M184V was associated with an inability to isolate virus. To further evaluate the fitness of MDR variants acquired in PHI, MDR and corresponding WT viruses were isolated from index and source partners, respectively. Although MDR viral infectivity (50% tissue culture infective dose) was comparable to that observed for WT viruses, MDR infections in each case demonstrated 2-fold and 13- to 23-fold reductions in p24 antigen and reverse transcriptase enzymatic activity, respectively. In dual-infection competition assays, MDR viruses consistently demonstrated a marked replicative disadvantage compared with WT virus. These results indicate that MDR viruses that are generated following PHI can establish persistent infections as dominant quasispecies despite their impaired replicative competence.

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Landes, H., K. R. Bambery, D. W. Coates, and K. Thompson. "Long-Term Changes in the Periods of SX Phe." Publications of the Astronomical Society of Australia 24, no. 1 (2007): 41–45. http://dx.doi.org/10.1071/as06025.

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AbstractWe have used times of maximum light for SX Phe, obtained by ourselves and other workers over 55 years to study the behaviour of the fundamental and first overtone radial pulsation modes of the star. We find (1/P0)dP0/dt to be (+2.53 ± 0.05) × 10−8 yr−1 and (1/P1)dP1/dt to be (−1.60 ± 0.03) × 10−7 yr−1, which differ significantly from the value +1.9 × 10−9 yr−1 expected if the changes are due to standard evolution of the star. The residuals in O–C from a quadratic fit cannot be explained by a light–time effect in a binary. There is some evidence that the amplitudes of the two modes change slowly with time.

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Sáyago-Ayerdi, Sonia G., Juscelino Tovar, Victor M. Zamora-Gasga, and Luis A. Bello-Pérez. "Starch digestibility and predicted glycaemic index (pGI) in starchy foods consumed in Mexico." Starch - Stärke 66, no. 1-2 (February 18, 2013): 91–101. http://dx.doi.org/10.1002/star.201200206.

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41

Martin, Erika G., and Grace M. Begany. "Transforming Government Health Data Into All-Star Open Data." Journal of Public Health Management and Practice 24, no. 6 (2018): E23—E25. http://dx.doi.org/10.1097/phh.0000000000000799.

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Shevchenko, Ivan I. "Habitable worlds of merging stars." International Journal of Astrobiology 19, no. 6 (October 6, 2020): 500–504. http://dx.doi.org/10.1017/s1473550420000282.

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AbstractIt is shown that W UMa-type and SX Phe-type stellar populations are both perfectly and uniquely suited for maintaining hyper-effective biopolymer chain reactions (BCR) on their planets once the planet is in the stellar habitable zone. W UMa-type stars are known to be contact binaries, and SX Phe-type stars are presumably post-binaries, i.e., products of stellar mergers. In case of the contact binaries, the eclipse-driven periodic heating/cooling of planetary surfaces has period-amplitude parameters that perfectly satisfy stringent conditions for maintaining BCR-like reactions. In case of the post-binaries, the stars pulsate with periods and amplitudes also perfectly suited for maintaining the reactions. Therefore, the ‘W UMa – SX Phe’ metamorphosis (from a contact binary to a post-binary, via the merger) seems to provide a potential biosystem reboot on planets in these systems.

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43

Jiayan, Xu, Wang Hongqi, and Zhang Zhiwu. "Realization of a Single Image with Autocollimation for PHA I." Symposium - International Astronomical Union 156 (1993): 89–93. http://dx.doi.org/10.1017/s0074180900172997.

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The First PHotoelectric Astrolabe (PHA I) of China was installed at Shaanxi Obs. in 1971 and came into use later. PHA I has been operating automatically since 1986. Now it is being revised by using a single image with autocollimation, equipped with photon counting system and a tracking diaphragm with a small window to follow the star in zenith direction, which would cut off the most light of the night sky. With all these three approaches, PHA I could improve its limiting magnitude from mag. 6 to mag. 11 or even fainter.

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Barzilai, Nir, and Stephanie Lederman. "Vincent Cristafalo Award Lecture." Innovation in Aging 4, Supplement_1 (December 1, 2020): 866. http://dx.doi.org/10.1093/geroni/igaa057.3199.

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Abstract The Vincent Cristofalo Rising Star Award in Aging Research lecture will feature an address by the 2020 recipient, Sean P. Curran, PhD. This award is given by the American Federation for Aging Research, Inc

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45

Bernstein, G. M., P. Knezek, and W. Offutt. "An SX Phe Variable Star in the Distant Galactic Halo." Publications of the Astronomical Society of the Pacific 107 (June 1995): 521. http://dx.doi.org/10.1086/133586.

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46

Jeon, Young-Beom, Myung Gyoon Lee, Seung-Lee Kim, and Ho Lee. "Double-radial-mode SX Phoenicis stars in the globular clusters NGC 5466 and M71." International Astronomical Union Colloquium 193 (2004): 166–70. http://dx.doi.org/10.1017/s0252921100010551.

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AbstractThrough time-series CCD photometry of the globular cluster NGC 5466, we found three double-radial-mode SX Phe stars, all of which are consistent with the theoretical period ratio of the first overtone mode to the fundamental mode (P1H/PF); their period ratios are 0.7825, 0.7826 and 0.7919, respectively. We also detected a double-radial-mode SX Phe star in M71. Its period ratio is 0.781, which is also consistent with the theoretical value.

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47

Ding-jiang, Luo, and Li Dong-ming. "Photoelectric Astrolabe and Astrolabe Star Catalogues." Symposium - International Astronomical Union 109 (1986): 375–77. http://dx.doi.org/10.1017/s0074180900076798.

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At the Shaanxi Observatory, regular observations with the prototype of the photoelectric astrolabe PAI have been carried out since 1973. Three photoelectric astrolabes of type Mark II (PAII) were mounted at the Shanghai, Beijing and Yunnan Observatories in 1974, 1976 and 1978, respectively. Details of the instruments and the results of the observation were published previously. (Photoelectric Astrolabe Developing Group 1973 and 1975, Second Group, First Divsion Shaanxi Observatory 1974, Astrolabe Data Analysis Group, First Division, Shaanxi Observatory 1975, Wang, L-j 1979, Astrolabe Group, First Division, Shanghai Observatory 1976, Wang, L-z and Luo 1979, Lu and Luo 1979). Time and latitude determinations by these sets of photoelectric astrolabes form a part in the international cooperation of BIH, IPMS as well as in the short campaign of project MERIT.

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Nemec, James M., Luis A. Balona, Simon J. Murphy, Karen Kinemuchi, and Young-Beom Jeon. "Metal-rich SX Phe stars in theKeplerfield." Monthly Notices of the Royal Astronomical Society 466, no. 2 (November 29, 2016): 1290–329. http://dx.doi.org/10.1093/mnras/stw3072.

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Nemec, James M., Luis A. Balona, Karen Kinemuchi, Simon J. Murphy, Young-Beom Jeon, Donald W. Kurtz, and Andrzej Pigulski. "Metal-Rich SX Phe Stars in theKeplerField." EPJ Web of Conferences 101 (2015): 06049. http://dx.doi.org/10.1051/epjconf/201510106049.

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Jackson, M., G. R. Sudhakaran, and E. Gansen. "Far-Infrared Laser Stark Spectroscopy of PH3." Journal of Molecular Spectroscopy 181, no. 2 (February 1997): 446–51. http://dx.doi.org/10.1006/jmsp.1996.7188.

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