http://chineseinput.net/에서 pinyin(병음)방식으로 중국어를 변환할 수 있습니다.
변환된 중국어를 복사하여 사용하시면 됩니다.
M.K.A. Shanika(M.K.A. Shanika ),K.S. Kumararathna(K.S. Kumararathna ),S.B. Navarathne(S.B. Navarathne ),V.S. Jayamanne(V.S. Jayamanne ) 한국축산식품학회 2022 Food and Life Vol.2022 No.3
Over gelatinization of extruded rice noodles during open wet steam cooking is a major problem in the food processing industry and occurs due to the condensation of water droplets that come into contact with noodle strings during the steaming process. This issue may arise due to the presence of stuck noodles in the finished product. Therefore, 5 prototype designs; wooden frame enclosed with polythene sheet (A), wooden frame enclosed with gray cloth (B), wooden frame enclosed with a plywood sheet with two steam inlets in the galvanized door (C), wooden frame enclosed with plywood sheet with multiple steam inlets in the galvanized door (D), and completely enclosed galvanized chamber were made (E). All steam chambers had multiple steam inlets in lateral walls except the chamber with gray cloth. Red rice noodles were prepared from the combination (16% w/w moisture, 200 μm, water at ambient temperature (30±2℃), control atmosphere, 20 min) and fed into five different types of prototype designs to complete the cooking (gelatinization) process. The performance of the five prototype designs was evaluated in terms of the percentage of dried noodles coming out of each design in a single straight form. According to the results, the percentage of dried noodles coming out of each design was (A-50.0±7.1%, B-15.0±5.0%, C-15.0±5.0%, D-50.0±7.1%, E-77.5±4.3% w/w) analyzed. The mean values of all designs revealed that the effective prototype design was “design E” (steam chamber consisted of a completely enclosed galvanized chamber with multiple steam inlets in the two lateral sides). It was able to produce a higher percentage of straight single noodles when compared to other designs. In conclusion, design E is the effective steam chamber to produce straight single rice noodles for the market. The design of a steam chamber is also a very important aspect to avoid over gelatinization thus producing straight and single form of rice noodles strings.
Miyake, N.,Udalski, A.,Sumi, T.,Bennett, D. P.,Dong, S.,Street, R. A.,Greenhill, J.,Bond, I. A.,Gould, A.,Kubiak, M.,Szymań,ski, M. K.,Pietrzyń,ski, G.,Soszyń,ski, I.,Ulaczyk, K.,Wyrzyk IOP Publishing 2012 The Astrophysical journal Vol.752 No.2
<P>We report the extremely high-magnification (A > 1000) binary microlensing event OGLE-2007-BLG-514. We obtained good coverage around the double peak structure in the light curve via follow-up observations from different observatories. The binary lens model that includes the effects of parallax (known orbital motion of the Earth) and orbital motion of the lens yields a binary lens mass ratio of q = 0.321 +/- 0.007 and a projected separation of s = 0.072 +/- 0.001 in units of the Einstein radius. The parallax parameters allow us to determine the lens distance D-L = 3.11 +/- 0.39 kpc and total mass M-L = 1.40 +/- 0.18 M-circle dot; this leads to the primary and secondary components having masses of M-1 = 1.06 +/- 0.13 M-circle dot and M-2 = 0.34 +/- 0.04 M-circle dot, respectively. The parallax model indicates that the binary lens system is likely constructed by the main-sequence stars. On the other hand, we used a Bayesian analysis to estimate probability distributions by the model that includes the effects of xallarap (possible orbital motion of the source around a companion) and parallax (q = 0.270 +/- 0.005, s = 0.083 +/- 0.001). The primary component of the binary lens is relatively massive, with M-1 = 0.9(-0.3)(+4.6) M-circle dot and it is at a distance of D-L = 2.6(-0.9)(+3.8) kpc. Given the secure mass ratio measurement, the companion mass is therefore M-2 = 0.2(-0.1)(+1.2) M-circle dot. The xallarap model implies that the primary lens is likely a stellar remnant, such as a white dwarf, a neutron star, or a black hole.</P>
Belle Collaboration,Vinokurova, A.,Kuzmin, A.,Eidelman, S.,Arinstein, K.,Aulchenko, V.,Aushev, T.,Bakich, A.M.,Balagura, V.,Barberio, E.,Belous, K.,Bhardwaj, V.,Bondar, A.,Bozek, A.,Bracko, M.,Brodzic North-Holland Pub. Co 2011 Physics letters: B Vol.706 No.2
We report the results of a study of B<SUP>+/-</SUP>→K<SUP>+/-</SUP>η<SUB>c</SUB> and B<SUP>+/-</SUP>→K<SUP>+/-</SUP>η<SUB>c</SUB>(2S) decays followed by η<SUB>c</SUB> and η<SUB>c</SUB>(2S) decays to (K<SUB>S</SUB>Kπ)<SUP>0</SUP>. The results are obtained from a data sample containing 535 million BB@?-meson pairs collected by the Belle experiment at the KEKB e<SUP>+</SUP>e<SUP>-</SUP> collider. We measure the products of the branching fractions B(B<SUP>+/-</SUP>→K<SUP>+/-</SUP>η<SUB>c</SUB>)B(η<SUB>c</SUB>→K<SUB>S</SUB>K<SUP>+/-</SUP>π<SUP>@?</SUP>)=(26.7+/-1.4(stat)<SUB>-2.6</SUB><SUP>+2.9</SUP>(syst)+/-4.9(model))x10<SUP>-6</SUP> and B(B<SUP>+/-</SUP>→K<SUP>+/-</SUP>η<SUB>c</SUB>(2S))B(η<SUB>c</SUB>(2S)→K<SUB>S</SUB>K<SUP>+/-</SUP>π<SUP>@?</SUP>)=(3.4<SUB>-1.5</SUB><SUP>+2.2</SUP>(stat+model)<SUB>-0.4</SUB><SUP>+0.5</SUP>(syst))x10<SUP>-6</SUP>. Interference with the non-resonant component leads to significant model uncertainty in the measurement of these product branching fractions. Our analysis accounts for this interference and allows the model uncertainty to be reduced. We also obtain the following charmonia masses and widths: M(η<SUB>c</SUB>)=(2985.4+/-1.5(stat)<SUB>-2.0</SUB><SUP>+0.5</SUP>(syst)) MeV/c<SUP>2</SUP>, Γ(η<SUB>c</SUB>)=(35.1+/-3.1(stat)<SUB>-1.6</SUB><SUP>+1.0</SUP>(syst)) MeV/c<SUP>2</SUP>, M(η<SUB>c</SUB>(2S))=(3636.1<SUB>-4.2</SUB><SUP>+3.9</SUP>(stat+model)<SUB>-2.0</SUB><SUP>+0.7</SUP>(syst)) MeV/c<SUP>2</SUP>, Γ(η<SUB>c</SUB>(2S))=(6.6<SUB>-5.1</SUB><SUP>+8.4</SUP>(stat+model)<SUB>-0.9</SUB><SUP>+2.6</SUP>(syst)) MeV/c<SUP>2</SUP>.
MOA-2010-BLG-073L: AN M-DWARF WITH A SUBSTELLAR COMPANION AT THE PLANET/BROWN DWARF BOUNDARY
Street, R. A.,Choi, J.-Y.,Tsapras, Y.,Han, C.,Furusawa, K.,Hundertmark, M.,Gould, A.,Sumi, T.,Bond, I. A.,Wouters, D.,Zellem, R.,Udalski, A.,Snodgrass, C.,Horne, K.,Dominik, M.,Browne, P.,Kains, N.,Br IOP Publishing 2013 The Astrophysical journal Vol.763 No.1
<P>We present an analysis of the anomalous microlensing event, MOA-2010-BLG-073, announced by the Microlensing Observations in Astrophysics survey on 2010 March 18. This event was remarkable because the source was previously known to be photometrically variable. Analyzing the pre-event source light curve, we demonstrate that it is an irregular variable over timescales >200 days. Its dereddened color, (V - I)(S),(0), is 1.221 +/- 0.051 mag, and from our lens model we derive a source radius of 14.7 +/- 1.3 R-circle dot, suggesting that it is a red giant star. We initially explored a number of purely microlensing models for the event but found a residual gradient in the data taken prior to and after the event. This is likely to be due to the variability of the source rather than part of the lensing event, so we incorporated a slope parameter in our model in order to derive the true parameters of the lensing system. We find that the lensing system has a mass ratio of q = 0.0654 +/- 0.0006. The Einstein crossing time of the event, t(E) = 44.3 +/- 0.1 days, was sufficiently long that the light curve exhibited parallax effects. In addition, the source trajectory relative to the large caustic structure allowed the orbital motion of the lens system to be detected. Combining the parallax with the Einstein radius, we were able to derive the distance to the lens, D-L = 2.8 +/- 0.4 kpc, and the masses of the lensing objects. The primary of the lens is an M-dwarf with M-L,M-1 = 0.16 +/- 0.03 M-circle dot, while the companion has M-L,M-2 = 11.0 +/- 2.0 M-J, putting it in the boundary zone between planets and brown dwarfs.</P>
Park, J W,Moon, C H,Harmache, A,Wargo, A R,Purcell, M K,Bremont, M,Kurath, G Blackwell Publishing Ltd 2011 Journal of fish diseases Vol.34 No.2
<P><B>Abstract</B></P><P>Previously, we demonstrated that a representative M genogroup type strain of infectious haematopoietic necrosis virus (IHNV) from rainbow trout grows well in rainbow trout‐derived RTG‐2 cells, but a U genogroup type strain from sockeye salmon has restricted growth, associated with reduced genome replication and mRNA transcription. Here, we analysed further the mechanisms for this growth restriction of U‐type IHNV in RTG‐2 cells, using strategies that assessed differences in viral genes, host immune regulation and phosphorylation. To determine whether the viral glycoprotein (G) or non‐virion (NV) protein was responsible for the growth restriction, four recombinant IHNV viruses were generated in which the G gene of an infectious IHNV clone was replaced by the G gene of U‐ or M‐type IHNV and the NV gene was replaced by NV of U‐ or M‐type IHNV. There was no significant difference in the growth of these recombinants in RTG‐2 cells, indicating that G and NV proteins are not major factors responsible for the differential growth of the U‐ and M‐type strains. Poly I:C pretreatment of RTG‐2 cells suppressed the growth of both U‐ and M‐type IHNV, although the M virus continued to replicate at a reduced level. Both viruses induced type 1 interferon (IFN1) and the IFN1 stimulated gene Mx1, but the expression levels in M‐infected cells were significantly higher than in U‐infected cells and an inhibitor of the IFN1‐inducible protein kinase PKR, 2‐aminopurine (2‐AP), did not affect the growth of U‐ or M‐type IHNV in RTG‐2 cells. These data did not indicate a role for the IFN1 system in the restricted growth of U‐type IHNV in RTG‐2 cells. Prediction of kinase‐specific phosphorylation sites in the viral phosphoprotein (P) using the NetPhosK program revealed differences between U‐ and M‐type P genes at five phosphorylation sites. Pretreatment of RTG‐2 cells with a PKC inhibitor or a p38MAPK inhibitor did not affect the growth of the U‐ and M‐type viruses. However, 100 μ<SMALL>m</SMALL> of the casein kinase II (CKII) inhibitor, 5,6‐dichloro‐1‐β‐<SMALL>d</SMALL>‐ribofuranosylbenzimidazole (DRB), reduced the titre of the U type 8.3‐fold at 24 h post‐infection. In contrast, 100 μ<SMALL>m</SMALL> of the CKII inhibitor reduced the titre of the M type only 1.3‐fold at 48 h post‐infection. Our data suggest that the different growth of U‐ and M‐type IHNV in RTG‐2 cells may be linked to a differential requirement for cellular protein kinases such as CKII for their growth.</P>
A SUB-SATURN MASS PLANET, MOA-2009-BLG-319Lb
Miyake, N.,Sumi, T.,Dong, Subo,Street, R.,Mancini, L.,Gould, A.,Bennett, D. P.,Tsapras, Y.,Yee, J. C.,Albrow, M. D.,Bond, I. A.,Fouqué,, P.,Browne, P.,Han, C.,Snodgrass, C.,Finet, F.,Furusawa, K IOP Publishing 2011 The Astrophysical journal Vol.728 No.2
<P>We report the gravitational microlensing discovery of a sub-Saturn mass planet, MOA-2009-BLG-319Lb, orbiting a K-or M-dwarf star in the inner Galactic disk or Galactic bulge. The high-cadence observations of the MOA-II survey discovered this microlensing event and enabled its identification as a high-magnification event approximately 24 hr prior to peak magnification. As a result, the planetary signal at the peak of this light curve was observed by 20 different telescopes, which is the largest number of telescopes to contribute to a planetary discovery to date. The microlensing model for this event indicates a planet-star mass ratio of q = (3.95 +/- 0.02) x 10(-4) and a separation of d = 0.97537 +/- 0.00007 in units of the Einstein radius. A Bayesian analysis based on the measured Einstein radius crossing time, t(E), and angular Einstein radius,theta(E), along with a standard Galactic model indicates a host star mass of M-L = 0.38(-0.18)(+0.34) M-circle dot and a planet mass of M-p = 50(-24)(+44)M(circle plus), which is half the mass of Saturn. This analysis also yields a planet-star three-dimensional separation of a = 2.4(-0.6)(+1.2) AU and a distance to the planetary system of D-L = 6.1(-1.2)(+1.1) kpc. This separation is similar to 2 times the distance of the snow line, a separation similar to most of the other planets discovered by microlensing.</P>
Belle Collaboration,Chen, W.T.,Abe, K.,Abe, K.,Adachi, I.,Aihara, H.,Anipko, D.,Aulchenko, V.,Bakich, A.M.,Barberio, E.,Bay, A.,Bedny, I.,Bitenc, U.,Bizjak, I.,Blyth, S.,Bondar, A.,Bozek, A.,Bracko, M North-Holland Pub. Co 2007 Physics letters: B Vol.651 No.1
K<SUB>S</SUB><SUP>0</SUP>K<SUB>S</SUB><SUP>0</SUP> production in two-photon collisions has been studied using a 397.6 fb<SUP>-1</SUP> data sample collected with the Belle detector at the KEKB e<SUP>+</SUP>e<SUP>-</SUP> collider. For the first time the cross sections are measured in the two-photon center-of-mass energy range between 2.4 GeV and 4.0 GeV and angular range |cosθ<SUP>*</SUP>|<0.6. Combining the results with measurements of γγ->K<SUP>+</SUP>K<SUP>-</SUP> from Belle, we observe that the cross section ratio σ(K<SUB>S</SUB><SUP>0</SUP>K<SUB>S</SUB><SUP>0</SUP>)/σ(K<SUP>+</SUP>K<SUP>-</SUP>) decreases from ∼0.13 to ∼0.01 with increasing energy. Signals for the χ<SUB>c0</SUB> and χ<SUB>c2</SUB> charmonium states are also observed.
Partition energy of complete product of circulant graphs and some new class of graphs
E. Sampathkumar,S. V. Roopa,K. A. Vidya,M. A. Sriraj 장전수학회 2018 Advanced Studies in Contemporary Mathematics Vol.28 No.2
Let G = (V,E) be a graph and Pk = {V1, V2, ..., Vk} be a partition of V . The L-matrix with respect to a partition Pk of the vertex set V of graph G of order n is the unique square symmetric matrix Pk(G) = [aij ] with zero diagonal, whose entries aij with i 6≠ j are defined as follows: (i) If vi, vj ∈ Vr, then aij = 2 or −1 according as vivj is an edge or not. (ii) If vi ∈ Vr and vj ∈ Vs for r 6≠s, then aij = 1 or 0 according as vivj is an edge or not. For all Vi and Vj in Pk, i 6≠j remove the edges between vertices of Vi and Vj and add the edges between the vertices of Vi and Vj which are not in G, the resulting graph is called k-complement of G and is denoted by (G)k. For each set Vr in Pk, remove the edges of G joining the vertices within Vr and add the edges of G (complement of G) joining the vertices of Vr, the graph obtained is called k(i)-complement and is denoted by (G)k(i). The k-partition energy of a graph G with respect to partition Pk is denoted by EPk (G) and is defined as the sum of the absolute values of k-partition eigenvalues of Pk(G). In this paper we construct some graphs such that the graph and its 2-complement are equienergetic with respect to a given partition. We also determine partition energy of complete product of m copies of a circulant graph G and its subgraph, their k-complement and k(i)-complement.
구민진,김수영,방정민,서아영,양희진,윤소람,이윤재,이재은,이지연,정윤경,최수정 이화여자대학교 간호과학대학 2014 이화간호학회지 Vol.- No.48
Purpose: This study aims to analyze the difference in the perception that nursing students and medical students have regarding the image of nurses. Method: The sampling group for this study was made up of 111 nursing students and 117 medicine students, conducted from the 19th August 2013 to 3rd September 2013. The tool used for this study is the “Nurse Image Scale”. The data is analyzed using the SPSS 21.0 program, technical stats, t-test and ANOVA with Scheffe test. Result: There was a notable difference in the results(t=6.94, p<001), with the average image perception score of nurses at 3.84±0.34 amongst nursing students being higher than the 3.50±0.38 amongst Medicine students. The average score of the 4 areas tested, “Qualification of a Nurse”, “Role of a Nurse”, “Social Participation of a Nurse” and “Interpersonal Skills of a Nurse” were all marked higher by the nursing students than the medicine students. The average score became notably higher as the period of practice became shorter with nursing students (F=4.21, p=.043). Furthermore, the average score for the “Qualification of a Nurse” was notably higher as the period of practice became shorter (F=3.98, p=.049). Medical students gave an average score for the “Qualification of a Nurse”(F=3.72, p=.027) and the “Interpersonal Skills of a Nurse”(F=4.11, p=.019) which was relative to the development of a nurse’s image, while the average score for the “Role of a Nurse” was notably higher with a longer period of practice(F=6.65, p=.011). Conclusion: The results of this study suggest that the image perception of a nurse can vary depending on the experience in period of practice. Therefore, together with this study conducted with nursing students and medicine students, there is a need for further studies conducted on image perception of nurses with various experience in period of practice.
MOA-2010-BLG-328Lb: A SUB-NEPTUNE ORBITING VERY LATE M DWARF?
Furusawa, K.,Udalski, A.,Sumi, T.,Bennett, D. P.,Bond, I. A.,Gould, A.,Jørgensen, U. G.,Snodgrass, C.,Prester, D. Dominis,Albrow, M. D.,Abe, F.,Botzler, C. S.,Chote, P.,Freeman, M.,Fukui, A.,Harris, P IOP Publishing 2013 The Astrophysical journal Vol.779 No.2
<P>We analyze the planetary microlensing event MOA-2010-BLG-328. The best fit yields host and planetary masses of M-h = 0.11 +/- 0.01 M-circle dot and M-p = 9.2 +/- 2.2 M-circle dot, corresponding to a very late M dwarf and sub-Neptune-mass planet, respectively. The system lies at D-L = 0.81 +/- 0.10 kpc with projected separation r(perpendicular to) = 0.92 +/- 0.16 AU. Because of the host's a priori unlikely close distance, as well as the unusual nature of the system, we consider the possibility that the microlens parallax signal, which determines the host mass and distance, is actually due to xallarap (source orbital motion) that is being misinterpreted as parallax. We show a result that favors the parallax solution, even given its close host distance. We show that future high-resolution astrometric measurements could decisively resolve the remaining ambiguity of these solutions.</P>