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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 (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 $G$ elementwis

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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

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Brunetti, Maurizio, and Francesco Belardo. "Line graphs of complex unit gain graphs with least eigenvalue -2." Electronic Journal of Linear Algebra 37, no. 37 (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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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 (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 {\m

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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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Imran, Muhammad, Adnan Aslam, Sohail Zafar, and Waqas Nazeer. "Further results on edge irregularity strength of graphs." Indonesian Journal of Combinatorics 1, no. 2 (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

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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 (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 appar

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Khostovan, A. A., S. Malhotra, J. E. Rhoads та ін. "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, № 3 (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 red

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Hummel, W., and S. Štefl. "The circumstellar structure of the Be shell star $\mathsf{\phi}$ Persei." Astronomy & Astrophysics 368, no. 2 (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 (2008): 39–53. http://dx.doi.org/10.1007/s11005-008-0247-6.

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11

Moutard, Thibaud, Marcin Sawicki, Stéphane Arnouts, et al. "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 (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 &lt;10−5 Mpc−3. Our FUV and

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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 (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

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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, et al. "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 (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 r

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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 spectra

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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 stud

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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 (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

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19

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 (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 implem

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20

Tetarenko, A. J., P. Casella, J. C. A. Miller-Jones, 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 (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.

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21

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

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22

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 (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

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

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24

Amano, Naoko, Satoshi Narumi, Mie Hayashi, et al. "Genetic defects in pediatric-onset adrenal insufficiency in Japan." European Journal of Endocrinology 177, no. 2 (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 sequenc

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

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26

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

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27

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-s

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Hancock, Cynthia. "DISTINGUISHED FACULTY AND RISING STAR EARLY-CAREER FACULTY AWARD LECTURES." Innovation in Aging 3, Supplement_1 (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, et al. "Pulsations of the SX Phe Star BL Camelopardalis." Publications of the Astronomical Society of the Pacific 131, no. 1000 (2019): 064202. http://dx.doi.org/10.1088/1538-3873/ab0a1a.

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30

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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31

McBride, Mark. "Kearns and Star on Reasons as Evidence." Analytic Philosophy 54, no. 2 (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 (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 (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 та 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, № 2 (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 v

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Balona, L. A., та J. M. Nemec. "A search for SX Phe stars amongKeplerδ Scuti stars". Monthly Notices of the Royal Astronomical Society 426, № 3 (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 (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, et al. "Persistence and Fitness of Multidrug-Resistant Human Immunodeficiency Virus Type 1 Acquired in Primary Infection." Journal of Virology 76, no. 4 (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

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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 chan

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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 (2013): 91–101. http://dx.doi.org/10.1002/star.201200206.

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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 (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

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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 (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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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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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, Fi

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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 (2016): 1290–329. http://dx.doi.org/10.1093/mnras/stw3072.

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Nemec, James M., Luis A. Balona, Karen Kinemuchi, et al. "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 (1997): 446–51. http://dx.doi.org/10.1006/jmsp.1996.7188.

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