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Francini K.J. Yatsu,Greice S. Borghetti,Valquiria L. Bassani 한국식품영양과학회 2011 Journal of medicinal food Vol.14 No.4
The present work was designed to produce an Ilex paraguariensis spray-dried powder (SDP), in semi-industrial scale, in order to characterize its technological and chemical properties as well as to evaluate the thermal stability and photostability of the main polyphenol constituents. The yield of the spray-drying process was satisfactory (67%). The resulting SDP showed to be a material presenting spherical particles with a mean size of 19.6 μm, smooth surface, and good flow properties. The four polyphenol compounds previously reported for the species—neochlorogenic acid, chlorogenic acid, cryptochlorogenic acid, and rutin—were identified. Regarding the photostability test, the polyphenols present in the SDP proved to be stable against ultraviolet C radiation for 48 hours, independently of the packaging material. In the thermal stability test, the polyphenols were demonstrated to be hygroscopic and responsive to temperature (40°C) under an atmosphere of high relative humidity (75%) for 4 months, especially when the SDP was conditioned in permeable flasks. These findings demonstrate that heat and residual moisture content play an important role in the stability of the polyphenols and reinforce the relevance of conditioning SDP in humid tight packages under low temperatures.
Katsuda, Satoru,Maeda, Keiichi,Ohira, Yutaka,Yatsu, Yoichi,Mori, Koji,Aoki, Wako,Morihana, Kumiko,Raymond, John C.,Ghavamian, Parviz,Lee, Jae-Joon,Shimoda, Jiro,Yamazaki, Ryo American Astronomical Society 2016 ASTROPHYSICAL JOURNAL LETTERS - Vol.819 No.2
<P>We present high-resolution long-slit spectroscopy of a Balmer-dominated shock in the northeastern limb of the Cygnus Loop with the Subaru high dispersion spectrograph. By setting the slit angle along the shock normal, we investigate variations of the flux and profile of the H alpha line from preshock to postshock regions with a spatial resolution of similar to 4 x 10(15) cm. The Ha line profile can be represented by a narrow (28.9 +/- 0.7 km s(-1)) Gaussian in a diffuse region ahead of the shock, i.e., a photoionization precursor, and narrow (33.1 +/- 0.2 km s(-1)) plus broad (130-230 km s(-1)) Gaussians at the shock itself. We find that the width of the narrow component abruptly increases up to 33.1 +/- 0.2 km s(-1), or 38.8 +/- 0.4 km s(-1) if we eliminate projected emission originating from the photoionization precursor, in an unresolved thin layer (less than or similar to 4 x 10(15) cm at a distance of 540 pc) at the shock. We show that the sudden broadening can be best explained by heating via damping of Alfven waves in a thin cosmic-ray (CR) precursor, although other possibilities are not fully ruled out. The thickness of the CR precursor in the Cygnus Loop (a soft gamma-ray emitter) is an order of magnitude thinner than that in Tycho's Knot g (a hard gamma-ray emitter), which may be caused by the different energy distribution of accelerated particles between the two sources. In this context, systematic studies might reveal a positive correlation between the thickness of the CR precursor and the hardness of the CR energy distribution.</P>
Optical and Infrared Lightcurve Modeling of the Gamma-ray Millisecond Pulsar 2FGL J2339.6-0532
Yen, Tzu-Ching,Kong, Albert Kwok-Hing,Yatsu, Yoichi,Hanayama, Hidekazu,Nagayama, Takahiro,OISTER 한국우주과학회 2013 Journal of Astronomy and Space Sciences Vol.30 No.3
We report the detection of a quasi-sinusoidally modulated optical flux with a period of 4.6343 hour in the optical and infrared band of the Fermi source 2FGL J2339.7-0531. Comparing the multi-wavelength observations, we suggest that 2FGL J2339.7-0531 is a γ-ray emitting millisecond pulsar (MSP) in a binary system with an optically visible late-type companion accreted by the pulsar, where the MSP is responsible for the γ-ray emission while the optical and infrared emission originate from the heated side of the companion. Based on the optical properties, the companion star is believed to be heated by the pulsar and reaches peak magnitude when the heated side faces the observer. We conclude that 2FGL J2339.7-0531 is a member of a subclass of γ-ray emitting pulsars -the ‘black widows’- recently revealed to be evaporating their companions in the late-stage of recycling as a prominent group of these newly revealed Fermi sources.
Optical and Infrared Lightcurve Modeling of the Gamma-ray Millisecond Pulsar 2FGL J2339.6-0532
Tzu-Ching Yen,Albert Kwok Hing Kong,Yoichi Yatsu,Hidekazu Hanayama,Takahiro Nagayama 한국우주과학회 2013 Journal of Astronomy and Space Sciences Vol.30 No.3
We report the detection of a quasi-sinusoidally modulated optical flux with a period of 4.6343 hour in the optical and infrared band of the Fermi source 2FGL J2339.7-0531. Comparing the multi-wavelength observations, we suggest that 2FGL J2339.7-0531 is a γ-ray emitting millisecond pulsar (MSP) in a binary system with an optically visible late-type companion accreted by the pulsar, where the MSP is responsible for the γ-ray emission while the optical and infrared emission originate from the heated side of the companion. Based on the optical properties, the companion star is believed to be heated by the pulsar and reaches peak magnitude when the heated side faces the observer. We conclude that 2FGL J2339.7-0531 is a member of a subclass of γ-ray emitting pulsars -the ‘black widows’- recently revealed to be evaporating their companions in the late-stage of recycling as a prominent group of these newly revealed Fermi sources.
DISCOVERY OF AN UNIDENTIFIED <i>FERMI</i> OBJECT AS A BLACK WIDOW-LIKE MILLISECOND PULSAR
Kong, A. K. H.,Huang, R. H. H.,Cheng, K. S.,Takata, J.,Yatsu, Y.,Cheung, C. C.,Donato, D.,Lin, L. C. C.,Kataoka, J.,Takahashi, Y.,Maeda, K.,Hui, C. Y.,Tam, P. H. T. IOP Publishing 2012 ASTROPHYSICAL JOURNAL LETTERS - Vol.747 No.1
<P>The Fermi gamma-ray Space Telescope has revolutionized our knowledge of the gamma-ray pulsar population, leading to the discovery of almost 100 gamma-ray pulsars and dozens of gamma-ray millisecond pulsars (MSPs). Although the outer-gap model predicts different sites of emission for the radio and gamma-ray pulsars, until now all of the known gamma-ray MSPs have been visible in the radio. Here we report the discovery of a 'radio-quiet' gamma-ray-emitting MSP candidate by using Fermi, Chandra, Swift, and optical observations. The X-ray and gamma-ray properties of the source are consistent with known gamma-ray pulsars. We also found a 4.63 hr orbital period in optical and X-ray data. We suggest that the source is a black widow-like MSP with a similar to 0.1 M-circle dot late-type companion star. Based on the profile of the optical and X-ray light curves, the companion star is believed to be heated by the pulsar while the X-ray emissions originate from pulsar magnetosphere and/or from intrabinary shock. No radio detection of the source has been reported yet, and although no gamma-ray/radio pulsation has been found we estimate that the spin period of the MSP is similar to 3-5 ms based on the inferred gamma-ray luminosity.</P>