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THE PERIODICITY OF THE SOLAR FLARE PRODUCTION DURING THE ACTIVITY CYCLE 22
TOHMURA ICHIROH,TOKIMASA NORITAKA,KUBOTA JUN The Korean Astronomical Society 1996 Journal of The Korean Astronomical Society Vol.29 No.suppl1
Using the data on the occurrences of the Ho: and soft X-ray flares for the time interval of January 1, 1986-May :31, 1994, we have studied the middle term(30-300days) pericities of the solar flare production during the activity cycle 22. Power analysis of the time seies of daily H$\alpha$ flare index in the northern hemisphere shows prominent periodicities at 220, 120, 109, and 92 days(see Figures l(a) and l(b)), while in the southern hemisphere, those at 267, 213, 183, 167, and 107 days are apparent, though their peaks are not so distint as those in the northern hemisphere. Periodogram of daily soft X-ray flare index also reveal the periodicities at 279, 205, 164, 117, and 91 days in the northern hemisphere, and at 266, 220, 199, 162, 120, and 100 days in the southern hemisphere. Howeer, the 155-day periodicity reported for the earlier cycles, 19, 20, and 21, could not be confirmed in our analysis. to be submitted to Solar Physics; an extended abstract.
The opposition effect of the asteroid 4 Vesta
Hasegawa, Sunao,Miyasaka, Seidai,Tokimasa, Noritaka,Sogame, Akito,Ibrahimov, Mansur A.,Yoshida, Fumi,Ozaki, Shinobu,Abe, Masanao,Ishiguro, Masateru,Kuroda, Daisuke Oxford University Press 2014 Publications of the Astronomical Society of Japan Vol.66 No.5
Ishiguro, Masateru,Kuroda, Daisuke,Hasegawa, Sunao,Kim, Myung-Jin,Choi, Young-Jun,Moskovitz, Nicholas,Abe, Shinsuke,Pan, Kang-Sian,Takahashi, Jun,Takagi, Yuhei,Arai, Akira,Tokimasa, Noritaka,Hsieh, He IOP Publishing 2014 The Astrophysical journal Vol.792 No.1
<P>We investigated the magnitude-phase relation of (162173) 1999 JU3, a target asteroid for the JAXA Hayabusa 2 sample return mission. We initially employed the International Astronomical Union's H-G formalism but found that it fits less well using a single set of parameters. To improve the inadequate fit, we employed two photometric functions: the Shevchenko and Hapke functions. With the Shevchenko function, we found that the magnitude-phase relation exhibits linear behavior in a wide phase angle range (alpha = 5 degrees-75 degrees) and shows weak nonlinear opposition brightening at alpha < 5 degrees, providing a more reliable absolute magnitude of H-V = 19.25 +/- 0.03. The phase slope (0.039 +/- 0.001 mag deg(-1)) and opposition effect amplitude (parameterized by the ratio of intensity at alpha = 0 degrees.3 to that at alpha = 5 degrees, I(0 degrees.3)/I(5 degrees) = 1.31 +/- 0.05) are consistent with those of typical C-type asteroids. We also attempted to determine the parameters for the Hapke model, which are applicable for constructing the surface reflectance map with the Hayabusa 2 onboard cameras. Although we could not constrain the full set of Hapke parameters, we obtained possible values, w = 0.041, g = -0.38, B-0 = 1.43, and h = 0.050, assuming a surface roughness parameter <(theta)over bar> = 20 degrees. By combining our photometric study with a thermal model of the asteroid, we obtained a geometric albedo of p(v) = 0.047 +/- 0.003, phase integral q = 0.32 +/- 0.03, and Bond albedo A(B) = 0.014 +/- 0.002, which are commensurate with the values for common C-type asteroids.</P>