研究者業績

鳴沢 真也

ナルサワ シンヤ  (Shin-ya Narusawa)

基本情報

所属
兵庫県立大学 自然・環境科学研究所 専任講師
学位
博士(理学)(2014年3月)

研究者番号
10984198
J-GLOBAL ID
202301017466103843
researchmap会員ID
R000050542

主要な経歴

 3

論文

 56
  • 鳴沢真也
    分析化学 2024年10月  査読有り招待有り筆頭著者
  • Iijima, T, H. Naito, S. Narusawa
    Publications of the Astronomical Society of Japan, (accepted) 76(5) 1002-1014 2024年10月  査読有り
  • Narusawa,S, Nagi, K, Maeno, S, Nishimura, M, Maehara, H
    Publications of the Astronomical Society of Japan 2024年  査読有り筆頭著者
  • Shin-ya Narusawa, Kazuo Nagai
    VSOLJ Variable Star Bulletin (103) 2022年10月  筆頭著者
  • Yusuke Tampo, Daisaku Nogami, Taichi Kato, Kazuya Ayani, Hiroyuki Naito, Norio Narita, Mitsugu Fujii, Osamu Hashimoto, Kenzo Kinugasa, Satoshi Honda, Hidenori Takahashi, Shin-ya Narusawa, Makoto Sakamoto, Akira Imada
    Publications of the Astronomical Society of Japan 74(2) 460-476 2022年3月21日  査読有り
    Abstract We present our spectroscopic observations of V455 Andromedae during the 2007 superoutburst. Our observations cover this superoutburst from around the optical peak of the outburst to the post-superoutburst stage. During the early superhump phase, the emission lines of the Balmer series, He i, He ii, Bowen blend, and C iv/N iv blend were detected. The He ii 4686 line exhibited a double-peaked emission profile, where Balmer emission lines were single-peaked, which is unexpected from its high inclination. In the ordinary superhump phase, the Balmer series transitioned to double-peaked emission profiles, and high-ionization lines were significantly weakened. These transitions of the line profiles should be related to the structural transformation of the accretion disk, as expected between the early and ordinary superhump transition in the thermal–tidal instability model. The Doppler map of Hα during the early superhump phase exhibits a compact blob centered at the primary white dwarf. In analogy to SW Sex-type cataclysmic variables, this feature could emerge from the disk wind and/or the mass accretion column on to the magnetized white dwarf. The Doppler map of He ii 4686 Å is dominated by the ring-like structure and imposed two flaring regions with the velocity of ∼300 km s−1, which is too slow for a Keplerian accretion disk. The phase of the flaring regions was coincident with the inner spiral arm structure identified during the early superhump phase. Our disk wind model with the enhanced emission from the wind component launched from the inner arm structure successfully reproduced the observed properties of He ii 4686 Å. Therefore, V455 And is the first case in dwarf nova outbursts where the presence of the disk wind is inferred from an optical spectrum.
  • Narusawa, S, Nagai, K
    VSOLJ Variable Star Bulletin (82) 2021年10月  筆頭著者
  • Narusawa, S., Akazawa, H.
    VSOLJ Variabel Star Bulletin (73) 2021年2月  筆頭著者
  • Narusawa, S, Arai, K, Fujii, M, Nagai, K, Yasuda, T
    VSOLJ Variabel Star Bulletin (70) 2021年  筆頭著者
  • Narusawa, S
    VSOLJ Variabel Star Bulletin (71) 2021年  筆頭著者
  • Narusawa, S, Akazawa, H, Arai,.K, Fujii, M, Invernizzi, F, D, Ioroi, M, Ito, Y, Morikawa, K, Ohkura, N
    VSOLJ Variabel Star Bulletin (72) 2021年  筆頭著者
  • Narusawa, S, Nakamura, Y
    VSOLJ Variabel Star Bulletin (68) 2020年  筆頭著者
  • T. Iijima, H. Naito, S. Narusawa
    Astronomy & Astrophysics 622 A45-A45 2019年1月24日  査読有り
    Context. CH Cyg is one of the most studied symbiotic stars. Its properties, however, are still not well known. Two main periods, about 15 years and 750 days, are known in the photometric and spectroscopic variations, and two models are proposed for these origins. One is a binary system with an orbital period of 15 years consisting of a hot component and pulsating red giant with a 750-day period. The other is a triple system consisting of an inner symbiotic binary with an orbital period of about 750 days and third component with an orbital period of 15 years. Several active stages have been observed since the 1970s during which the object brightened up by ΔU = 3−5 mag and prominent emission lines appeared. Large mass outflows were observed at some active stages. Aims. The spectral variation of CH Cyg has been monitored at Asiago Observatories to understand the problems mentioned above. We have analysed spectra obtained in the time period from 1995 to 2004 which covers an active stage during the years 1998−2000. Methods. High- and low-resolution optical spectra obtained at the Asiago Observatories are used. Results. Narrow absorption lines of Fe I, Cr I, Ti I, and so on appeared in 1998 at an early phase of the active stage. These lines are clearly distinguished from those of the M-type giant and are typically found on the spectrum of early A-type dwarfs. They were redshifted by about 30 km s−1 with respect to the absorption lines of the M-type giant. Assuming that their radial velocities represent the orbital motion of the hot component, its semi-amplitude is estimated to be 37.0 ± 0.5 km s−1. The masses of the hot component and the M-type giant are estimated to be 0.32 ± 0.02 M and 4.6 ± 0.2 M, respectively, where a circular orbit with a period of 756 days is adopted. If the inner binary system has an elliptical orbit, e = 0.33, and a period of 750.1 days, the masses of the two components are 0.21 ± 0.01 M and 2.2 ± 0.1 M, respectively. Our results lend support to the triple system model, because if the period of the symbiotic binary were 15 years, the mass of the hot component would be expected to exceed the Chandrasekhar limit. Highly blueshifted absorption components of H I and He I lines appeared at a later phase of the active stage. Mass ejections with velocities on the order of 1000 km s−1 seem to have occurred along the orbital plane from December 1998 to March 1999. The highest outflow velocity, − 2383 km s−1, was observed on 1999 February 26. Narrow absorption components of Na I D1, D2, and Fe II lines redshifted by 10−15 km s−1 coexisted with the highly blueshifted broad absorption components of H I and He I lines. This phenomenon might have been related to an inner disc inflow expected in wind-compressed discs. In contrast to the bipolar mass outflows at the past active stages, high-velocity equatorial mass ejections likely occurred at the active stage during the years 1998−2000. There should have been an eclipse of the hot component by the M-type giant in the inner binary system in the time period of December 1998 to January 1999. A clear light curve of the eclipse, however, was not detected. Possibly, the luminosity of the hot component was due mainly to free-free emission from the ejected circumstellar matter which was likely more extended than the M-type giant. On the other hand, another eclipse by the third component with the period of 15 years began at the end of May 1999 during which the hot component as well as the emitting regions of Hβ and Fe II lines were well eclipsed. The obscuring matter around the third component should have been much more extended than the M-type giant, and it was likely semi-transparent, because the spectrum of the M-type giant was well seen during the eclipse. The third component appears to be similar to the invisible secondary component in the long-period eclipsing binary ϵ Aur.
  • Shin-ya Narusawa, Tatusya Aota, Ryo Kishimoto
    New Astronomy 60 61-64 2018年4月1日  査読有り筆頭著者
    In the case of radio SETI, there are predicted frequencies which extraterrestrial beings select to send messages to other civilizations. Those are called “magic frequencies. Considering the optical region, terrestrial technologies can not transmit arbitrary wavelengths of high-power optical lasers, easily. In this article, we discuss communications among civilizations with the same level of technology as us to enhance the persuasive power. It might be possible to make a reasonable assumption about the laser wavelengths transmitted by extraterrestrial intelligences to benefit optical SETI (OSETI) methods. Therefore, we propose some “magic wavelengths” for spectroscopic OSETI observations in this article. From the senders point of view, we argue that the most favorable wavelength used for interstellar communication would be the one of YAG lasers, at 1.064 µm or its Second Harmonic Generation (532.1 nm). On the contrary, there are basic absorption lines in the optical spectra, which are frequently observed by astrophysicists on Earth. It is possible that the extraterrestrials used lasers, which wavelengths are tuned to such absorption lines for sending messages. In that case, there is a possibility that SHG and/or Sum Frequency Generation of YAG and YLF lasers are used. We propose three lines at, 393.8 nm (near the Ca K line), 656.5 nm (near the Hα line) and 589.1 nm (Na D2 line) as the magic wavelengths.
  • Masateru Ishiguro, Yoonyoung Kim, Junhan Kim, Fumihiko Usui, Jeremie J. Vaubaillon, Daisuke Ishihara, Hidekazu Hanayama, Yuki Sarugaku, Sunao Hasegawa, Toshihiro Kasuga, Dhanraj S. Warjurkar, Ji-Beom Ham, Jeonghyun Pyo, Daisuke Kuroda, Takafumi Ootsubo, Makoto Sakamoto, Shin-ya Narusawa, Jun Takahashi, Hiroki Akisawa, Jun-ichi Watanabe
    The Astrophysical Journal 778(1) 19-19 2013年10月29日  査読有り
  • Shin-Ya Narusawa
    Publications of the Astronomical Society of Japan 65(5) 105-105 2013年10月25日  査読有り筆頭著者
  • H. Naito, S. Mizoguchi, A. Arai, A. Tajitsu, S. Narusawa, M. Yamanaka, M. Fujii, T. Iijima, K. Kinugasa, M. Kurita, T. Nagayama, H. Yamaoka, K. Sadakane
    Astronomy & Astrophysics 543 A86-A86 2012年7月2日  査読有り
  • 新井彰, 高木悠平, 本田敏志, 坂元誠, 鳴沢真也, 伊藤洋一
    西はりま天文台年報 (22) 34-39 2012年  
  • 高木悠平, 新井彰, 高橋隼, 坂元誠, 鳴沢真也, 伊藤洋一
    西はりま天文台年報 (22) 27-33 2012年  
  • Narusawa,Shin-ya, Jun Takahashi, Jun, Kazuo Nagai, Kazuo
    Annual Report of the Nishi-Harima Astronomical Observatory (22) 1-5 2012年  筆頭著者
  • Narusawa,Shin-ya
    Annual Report of the Nishi-Harima Astronomical Observatory (21) 1-3 2011年  筆頭著者
  • Masateru Ishiguro, Jun-ichi Watanabe, Yuki Sarugaku, Takafumi Ootsubo, Daisuke Kuroda, Mitsuhiko Honda, Takashi Miyata, Kenshi Yanagisawa, Hiroyuki Mito, Hideo Fukushima, Takahiro Niwa, Makoto Sakamoto, Shin-ya Narusawa, Hiroki Akisawa
    The Astrophysical Journal 714(2) 1324-1333 2010年4月19日  査読有り
  • 佐藤匡史, 島ノ江純, 山岡仁, 鳴沢真也, 圓谷文明, 石田俊人
    西はりま天文台年報 (20) 1-9 2010年  
  • Kazuo Hiroi, Daisaku Nogami, Yoshihiro Ueda, Yuuki Moritani, Yuichi Soejima, Akira Imada, Osamu Hashimoto, Kenzo Kinugasa, Satoshi Honda, Shin-ya Narusawa, Makoto Sakamoto, Ryo Iizuka, Kentaro Matsuda, Hiroyuki Naito, Takashi Iijima, Mitsugu Fujii
    Publications of the Astronomical Society of Japan 61(4) 697-705 2009年8月25日  査読有り
  • Masayuki Yamanaka, Hiroyuki Naito, Kenzo Kinugasa, Naohiro Takanashi, Masaomi Tanaka, Koji S. Kawabata, Shinobu Ozaki, Shin-ya Narusawa, Kozo Sadakane
    Publications of the Astronomical Society of Japan 61(4) 713-720 2009年8月25日  査読有り
  • Nogami, D, Hiroi, K, Suzuki, Y, Moritani, Y, Soejima, Y, Imada, A, Hashimoto, O, Kinugasa, K, Honda, S, Ayani, K, Narusawa, S, Naito, H, Sakamoto, M, Iijima, T, Fujii, M, Narita, N
    The Eighth Pacific Rim Conference on Stellar Astrophysics: A Tribute to Kam-Ching Leung ASP Conference Series, Vol. 404, proceedings of the conference held 5-9 May, 2008, at Merlin Beach Hotel, Phuket, Thailand. Edited by B. Soonthornthum, S. Komonjinda, K.S. Cheng, and K.C. Leung San Francisco: Astronomical Society of the Pacific 404 52-+ 2009年  査読有り
    We carried out intensive spectroscopic observations of two WZ Sge-type dwarf novae, GIN Lib, and V455 And during their superoutbursts in 2007, at 6 observatories. The observations covered the whole of both superoutbursts from the very maximum to the fading tail. We found evidence of the winds having a speed of similar to 1000 km s(-1) which blew in GW Lib during the rising phase. The evolution of the hydrogen, helium, and carbon lines suggests flaring of the accretion disk and emergence of the temperature inversion layer on the disk.
  • A. Fukui, F. Abe, K. Ayani, M. Fujii, R. Iizuka, Y. Itow, K. Kabumoto, K. Kamiya, T. Kawabata, S. Kawanomoto, K. Kinugasa, R. A. Koff, T. Krajci, H. Naito, D. Nogami, S. Narusawa, N. Ohishi, K. Ohnishi, T. Sumi, F. Tsumuraya
    The Astrophysical Journal 670(1) 423-427 2007年11月20日  査読有り
  • Ken’ichi Tanaka, Kozo Sadakane, Shin-ya Narusawa, Hiroyuki Naito, Eiji Kambe, Jun-ichi Katahira, Ryuko Hirata
    Publications of the Astronomical Society of Japan 59(4) L35-L39 2007年8月25日  査読有り
  • 松田健太郎, 鳴沢真也, 内藤博之
    西はりま天文台年報 (17) 16-24 2007年  
  • Narusawa, S, Naito, H, Sakamoto, M, Imada, A, Nogami, D
    Central Bureau Electronic Telegrams, No. 923, #1 (2007). Edited by Green, D. W. E. 2007年  筆頭著者
  • Narusawa Shin-ya, Morimoto Masaki
    Annual Report of the Nishi-Harima Astronomical Observatory (17) 1-3 2007年  筆頭著者
  • Shin-ya Narusawa, Shinobu Ozaki, Eiji Kambe, Kozo Sadakane
    Publications of the Astronomical Society of Japan 58(3) 617-625 2006年6月25日  査読有り筆頭著者
  • Shin‐ya Narusawa, Shinobu Ozaki, Masami Okyudo, Ryo Takano, Yasuhisa Nakamura
    Publications of the Astronomical Society of the Pacific 118(844) 809-813 2006年6月  査読有り筆頭著者
  • 藤下光身, 鳴沢真也, 藤下基線, 川瀬徳一
    九州東海大学工学部紀要 (33) 7 2006年  
  • Narusawa, Shin-ya, Fujii, Mitsugu, Ioroi, Kayo, Honkawa, Masami
    Annual Report of the Nishi-Harima Astronomical Observatory (ISSN 0917-6926) (15) 1-2 2005年  筆頭著者
  • Mitsumi Fujishita, Shin-ya Narusawa, Motosuji Fujishita, Tokuichi Kawase
    International Astronautical Federation, 56th International Astronautical Congress 59(IAC-05-A4.(CD)) 346-348 2005年  査読有り
  • Narusawa, Shin-ya, Ioroi, Masayuki
    Annual Report of the Nishi-Harima Astronomical Observatory, ISSN 0917-6926 (13) 1-2 2003年  筆頭著者
  • Shin-ya Narusawa, Atsuma Yamasaki, Mitsuo Fukata, Masao Takeda, Yasuhisa Nakamura, Akira Okazaki
    Publications of the Astronomical Society of Japan 54(1) 139-151 2002年2月25日  査読有り筆頭著者
  • Waki, Yoshifumi, Narusawa, Shin-Ya, Ishitsuka Iba, Jose Kaname, Ioroi, Masayuki
    Annual Report of the Nishi-Harima Astronomical Observatory (12) 1-2 2002年  
  • Narusawa, Shin-ya, Waki, Yoshifumi, Ioroi, Masayuki, Nakamura, Yasuhisa, Takeuti, Mine
    Annual Report of the Nishi-Harima Astronomical Observatory, No. 12, 2002, Nishi-Harima Astronomical Observatory, ISSN 0917-6926 (12) 3-11 2002年  筆頭著者
  • Narusawa, S, Waki, Y, Ioroi, M, Takeuti, M
    Information Bulletin on Variable Stars (5279) 2002年  査読有り筆頭著者
  • Osamu Ohshima, Shin-ya Narusawa, Hidehiko Akazawa, Kikuichi Arai, Mitsugu Fujii, Tetsuya Kawabata, Koichi Morikawa, Nobuo Ohkura, Mine Takeuti
    The Astronomical Journal 122(1) 418-424 2001年7月  査読有り
  • 内藤博之, 佐伯圭一, 重富裕也, 鳴沢真也, 時政典孝, 山岡均
    西はりま天文台年報 (10) 11-12 2000年  
  • 石岡涼子, 木全理恵, 松田健太郎, 前田豊, 太田耕司, 鳴沢真也, 石田俊人
    西はりま天文台年報 (9) 1-12 1999年  
  • 川口美紀, 辻本寿太, 野田信之, 鳴沢真也, 山岡均
    西はりま天文台年報 (8) 1-17 1998年  
  • Narusawa, S, Yamasaki, A, Nakamura, Y
    Highlights of Astronomy Vol. 11A, as presented at Joint Discussion 14 of the XXIIIrd General Assembly of the IAU, 1997. Edited by Johannes Andersen. Kluwer Academic Publishers 371 1998年  筆頭著者
  • Ohshima, Osamu, Narusawa, Shin-ya, Akazawa, Hidehiko, Fujii, Mitsugu, Kawabata, Tetsuya, Ohkura, Nobuo
    Information Bulletin on Variable Stars (4581) 1998年  査読有り
  • Tadashi Mukai, Toyoichiro Iwata, Sen Kikuchi, Ryuko Hirata, Masafumi Matsumura, Yasuhisa Nakamura, Sin-ya Narusawa, Akira Okazaki, Munezo Seki, Kaori Hayashi
    Icarus 127(2) 452-460 1997年6月  査読有り
  • 高野 亮, 細井淑子, 中村泰久, 鳴沢真也, 石田俊人
    西はりま天文台年報 (7) 1-21 1997年  
  • Narusawa, Shin-ya, Arai, Kikuichi, Nagai, Kazuo, Ohmori, Shigeo, Fujii, Mitsugu, Yasuda, Takeshi
    Information Bulletin on Variable Stars (4502) 1997年  査読有り筆頭著者
  • 田邉和孝, 眞銅雅子, 小野智子, 鳴沢真也, 山岡 均
    西はりま天文台年報 (6) 1-11 1996年  

MISC

 171

主要な書籍等出版物

 39

主要な講演・口頭発表等

 234

所属学協会

 6

共同研究・競争的資金等の研究課題

 5

主要な社会貢献活動

 852

主要なメディア報道

 143

その他

 1