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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.
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
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.