First Cellulose Langmuir‐Blodgett Films towards Photocurrent Generation Systems

Langmuir‐Blodgett films of a cellulose derivative containing porphyrins, porphyrin‐cellulose, were fabricated in order to construct a cellulose‐based molecular photocurrent generation system. On visible light illumination of the LB monolayer film deposited on an ITO electrode, anodic photocurrents were observed with a quantum yield of 1.6% at an applied potential of 0 V versus SCE, and 3.8–4.6% at 0.2–0.3 V versus SCE. These values indicate that the self‐quenching of the photoexcited porphyrins in the cellulose LB film was suppressed, while porphyrin moieties in the LB film had a densely packed structure. This is because the porphyrins are located at a distance of approximately 1.0 nm along the cellulose backbone.

     

Catalytic asymmetric total synthesis of (+)-lactacystin

Total synthesis of (+)-lactacystin, a potent and selective proteasome inhibitor, was accomplished using a catalytic enantioselective Strecker reaction of a ketoimine as the initial key step. An enone-derived N-phosphinoyl ketoimine 7 was selected as a stable masked alpha-hydroxy ketoimine analogue. Excellent enantioselectivity (98% ee) and practical catalyst activity were produced under the optimized catalyst preparation method using 2.5 mol % Gd{N(SiMe3)2}3 as a metal source and 3.8 mol % D-glucose-derived ligand 8. This reaction was conducted on a 5 g scale. The chiral tetrasubstituted C-5 carbon efficiently controlled the stereochemistry of the other three chiral centers of lactacystin. Chelation-controlled Meerwein-type reduction of ketone 5 using i-PrMgBr (originally reported by Kang in a related substrate) selectively produced the desired secondary alcohol at the C-9 position. The C-6 hydroxy and C-7 methyl groups were introduced via a silyl conjugate addition followed by the Tamao oxidation and Donohoe methylation, respectively, in a highly stereoselective manner. A practical amount of enantiomerically pure clasto-lactacystin beta-lactone (2), the biologically active form of (+)-lactacystin, can be synthesized using this route. clasto-Lactacystin beta-lactone (2) was converted to (+)-lactacystin following the reported procedure.     

Reduction of ion thermal diffusivity associated with the transition of the radial electric field in neutral-beam-heated plasmas in the large helical device

Recent large helical device experiments revealed that the transition from ion root to electron root occurred for the first time in neutral-beam-heated discharges, where no nonthermal electrons exist. The measured values of the radial electric field were found to be in qualitative agreement with those estimated by neoclassical theory. A clear reduction of ion thermal diffusivity was observed after the mode transition from ion root to electron root as predicted by neoclassical theory when the neoclassical ion loss is more dominant than the anomalous ion loss.     

Phase structure of a U(1) lattice gauge theory with dual gauge fields

We introduce a U(1) lattice gauge theory with dual gauge fields and study its phase structure. This system is partly motivated by unconventional superconductors like extended s-wave and d  -wave superconductors in the strongly-correlated electron systems and also studies of the t–J$t\text{–}J$ model in the slave-particle representation. In this theory, the “Cooper-pair” (or RVB spinon-pair) field is put on links of a cubic lattice due to strong on-site repulsion between original electrons in contrast to the ordinary s  -wave pair field on sites. This pair field behaves as a gauge field dual to the U(1) gauge field coupled with the hopping of electrons or quasi-particles of the t–J$t\text{–}J$ model, holons and spinons. By Monte Carlo simulations we study this lattice gauge model and find a first-order phase transition from the normal state to the Higgs (superconducting) phase. Each gauge field works as a Higgs field for the other gauge field. This mechanism requires no scalar fields in contrast to the ordinary Higgs mechanism. An explicit microscopic model is introduced, the low-energy effective theory of which is viewed as a special case of the present model.     

Infrared seed inspection system (IRSIS) on painted car shells

This paper describes a newly-developed automated thermal system for detection of seeds on newly painted car shells. The system’s novel approach is to use thermal emission; previously applied techniques relied on light reflection strategies. The system is described beginning with analytical modeling of the underlying detection theory to verification on a pilot run in an automotive production line. Parker’s flash procedure, using a thermal detector, was performed to extract the thermal properties of inspected panels. New computer logic developed in-house for processing the acquired thermograms is also presented.     

Galactic cosmic-ray anisotropy and its modulation in the heliomagnetosphere, inferred from air shower observation at Mt. Norikura

Summary Extensive air showers (EAS) with median primary energy (E _m) of (10¹³÷10¹⁵) eV have been observed since 1970 at Mt. Norikura (2770 m above sea level; geographic latitude 36.1°N, longitude 137.6°E) in order to study a cosmic-ray sidereal daily variation of galactic origin. We report here a summary of the observed results. EAS shows a significant sidereal diurnal variation with an amplitude (0.060±0.003)% and a phase (0.8±0.3) h sidereal local time forE _m≈1.5·10¹³eV. Sidereal semi- and tridiurnal variations also are statistically significant. These variations are proved to be of galactic origin by a method which uses the difference of two directional (eastward and westward) air shower observations. It is found that these variations are subject, as predicted by Nagashimaet al., to the annual variation due to the heliomagnetospheric modulation of the galactic anisotropy, which dominates in the rigidity region ≈10¹²V, and further that the annual variation changes its phase due to the polarity reversal of the polar magnetic field of the Sun, which occurs at the period of the maximum solar activity. This indicates that the anisotropy is produced by the charged cosmic rays, contrary to the expectation from the γ-ray origin hypothesis suggested by Alexeenko and Navara. With the increase ofE _m, the anisotropy seems to be reduced as we have not been able to detect any significant sidereal variation in EAS withE _m≈2·10¹⁴eV. This seems contradictory to the conventional conclusion that the energy spectrum of the anisotropy is flat or slightly increases with energy.

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Riassunto Sono stati osservati sciami cosmici estensivi (EAS) con energia primaria mediana (E _m) di (10¹³⋎10¹⁵) eV dal 1970 a Mt. Norikura (2770m, latitudine geografica 36.1° N, longitudine 137.6° E) per studiare una variazione gionarliera siderale dei raggi cosmici di origine galattica. Si riporta una sintesi dei risultati osservati. EAS mostra una significativa variazione siderale diurna con ampiezza (0.060±0.03)% e fase (0.8±0.3)h in tempo locale siderale perE _m∼1.5·10¹³eV. Le variazioni siderali semi e tri-diurne sono risultate anch'esse statisticamente significative. Si prova che queste variazioni sono d'origine galattica con un metodo che utilizza la differenza tra due osservazioni di sciami cosmici direzionali (est e ovest). Si trova che queste variazioni sono soggette, come previsto da Nagashimaet al., alla variazione annuale dovuta alla modulazione eliomagnetica dell'anisotropia galattica, che domina nella regione di rigidità ∼10¹²V e inoltre che la variazione annuale cambia fase a causa dell'inversione di polarità del campo magnetico polare del Sole, chesi verifica nel periodo di massima attività solare. Ciò indica che l'anisotropia è prodotta da raggi cosmici carichi, contrariamente a quanto previsto dall'ipotesi sull'origine da raggi gamma, suggerita da Alexeenko e Navara. Con l'aumento diE _m, l'anisotropia sembra ridursi in quanto non siamo riusciti a rilevare una variazione siderale significativa in EAS conE _m∼2·10¹⁴ eV. Questo risultato sembra in contraddizione con la conclusione convenzionale che lo spettro di energia dell'anisotropia è piatto o cresce appena con l'energia.

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Резюме Широкие атмосферные ливни со средней первичной энергией (E _m), равной (10¹³⋎10¹⁵) зВ, наблюдались с 1970 года на г. Нарикура (2770 м над уровнем моря; географическая широта 36.1°N, долгота 137.6°E), с целяю исследовать суточное изменение сидерических космических лучей галактической природы. Предлагается обзор полученных результатов. Широкие атмосферные ливни обнаруживают значительное сидерическое суточное изменение с амплитудой (0.060±0.003)% и фазой 0.8±0.3 часа сидерического времени дляE _m∼1.5·10¹³ эВ. Сидерические полу-и трех-суточные изменения являются также статистически заметными. Доказывается, что эти изменения имеют галактическое происхождение. Этот результат получен с помощью метода, который использует разности при наблюдениях атмосферных ливней в двух направлениях (в восточном и западном направлениях). Получено, что эти вариации подчиняются, как было предсказано Нагашима и др., годовому изменению, обусловленному гелиомагнитосферной модуляцией галактической анизотропии, которая доминирует в области жесткости ∼10¹² D, и кроме того, годовая вариация изменяет фазу, в связи с реверсированием полярности магнитного поля Солнца, котороепроисходит в период максимума солнечной активности. Этот реультат показывает, что возникает анизотропия, вызванная заряженными космическими лучами, в противоположность рредсказанию Алексеенко и Навара, связанному с гипотезой происхождения γ-лучей. При увеличенииE _m анизотропия, повидимому, уменьшается, так как мы не смогли зарегистрировать какого-либо существенного сидерического изменения в пироких атмосферных ливнях в случаеE _m∼2·10¹⁴эВ. Это противоречит общепринятому заключению, что энергетический спектр анизотропии является пологим или слегка увеличивается с энергией.

     

Response and yield functions of neutron monitor, galactic cosmic-ray spectrum and its solar modulation, derived from all the available world-wide surveys

Summary The differential response functionR(p, x, t) of cosmic-ray neutron monitors and its altitude and time dependence are obtained by a new method of analysis which uses all the available data obtained by oversea, overland and airborn surveys at different periods together with those of the space exploration. The simultaneous use of these data enables us to decomposeR(p, x, t) further into three terms; the unmodulated energy spectrumG(U) of galactic cosmic rays, the modulation functionM(p, t) of cosmic rays in solar system and the yield functionY(U, x) of neutrons in the atmosphere (x g/cm²). It is demonstrated that 1) the power exponent ofG(U) shows fairly a good agreement with those so far obtained, 2)Y(U, x) shows also fairly a good agreement with the theoretical expectation in the energy region ≥10 GeV and 3)M(p, t) gives the cosmic-ray mean free path showing a consistent rigidity spectrum with those obtained by the solar proton events. Using these terms, we can obtainR at any time and at any atmospheric depth. A brief historical review of the study of the response function is also made in the introduction.

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Riassunto La funzione di risposta differenzialeR(p,x,t) dei monitor a neutroni dei raggi cosmici e la sua dipendenza dall'altitudine e dal tempo sono ottenuti con un nuovo metodo di analisi che utilizza tutti i dati disponibili ottenuti con rilevamenti aerei, in mare e a terra effettuati in periodi diversi insieme ai dati delle esplorazioni spaziali. L'uso simultaneo di questi dati permette di scomporreR(p,x,t) ulteriormente in tre termini: lo spettro di energia non modulatoG(U) dei raggi cosmici galattici, la funzione di modulazioneM(p,t) dei raggi cosmici nel sistema solare e la funzione di produzioneY(U,x) di neutroni nell'atmosfera (x g/cm²). Si dimostra che 1) l'esponente della potenza diG(U) presenta un buon accordo con quelli ottenuti fino ad ora, 2)Y(U,x) presenta anche un buon accordo con i valori teorici attesi nella regione d'energia ≥10 GeV e 3)M(p,t) dà il percorso libero medio dei raggi cosmici che mostra un consistente spettro di rigidità ottenuto dagli eventi dei protoni solari. Usando questi termini, si può ottenereR in ogni momento e a tutte le profondità atmosferiche. Nell'introduzione c'è una breve rassegna storica dello studio della funzione di risposta.

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Резюме С помощью новочо метода анализа, который использует все имеющие данные мировых исследований в различные периоды вместе с данными космических исследований, получаются дифференциальная функция откликаR(p, x, t) для мониторов космических нейтронов и ее зависимость от высоты и времени. Одновременное испльзование этих данных позволяет нам представитьR(p, x, t) в виде трех членов: немодулированный энергетический спектрG(U) галактических космических лучей, функция модуляцииM(p, t) космических лучей в солнечной системе и функция выходаY(U, x) нейтронов в атмосфере (х·г/см²). Показывается, что 1) показатель экспонентыG(U) довольно хорошо согласуется с полученной величиной, 2)Y(U, x) также довольно хорошо согласуется с теоретическими предсказаниями в области энергий≽10 Гэв и 3)M(p, t) дает величину средней длины свободного пробега космических лучей, которая соответствует величине, полученной для солнечных протонов. Используя эти три члена, мы можем получитьR в любое время и на любой гдубине в атмосфере. Во введении предлагается краткий исторический обзор исследований функции отклика.