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Relationship between radar cross section and optical magnitude based on radar and optical simultaneous observations of faint meteors
Planetary and Space Science ( IF 1.8 ) Pub Date : 2020-12-01 , DOI: 10.1016/j.pss.2020.105011
Ryou Ohsawa , Akira Hirota , Kohei Morita , Shinsuke Abe , Daniel Kastinen , Johan Kero , Csilla Szasz , Yasunori Fujiwara , Takuji Nakamura , Koji Nishimura , Shigeyuki Sako , Jun-ichi Watanabe , Tsutomu Aoki , Noriaki Arima , Ko Arimatsu , Mamoru Doi , Makoto Ichiki , Shiro Ikeda , Yoshifusa Ita , Toshihiro Kasuga , Naoto Kobayashi , Mitsuru Kokubo , Masahiro Konishi , Hiroyuki Maehara , Noriyuki Matsunaga , Takashi Miyata , Yuki Mori , Mikio Morii , Tomoki Morokuma , Kentaro Motohara , Yoshikazu Nakada , Shin-ichiro Okumura , Yuki Sarugaku , Mikiya Sato , Toshikazu Shigeyama , Takao Soyano , Hidenori Takahashi , Masaomi Tanaka , Ken'ichi Tarusawa , Nozomu Tominaga , Seitaro Urakawa , Fumihiko Usui , Takuya Yamashita , Makoto Yoshikawa

Abstract Radar and optical simultaneous observations of meteors are important to understand the size distribution of the interplanetary dust. However, faint meteors detected by high power large aperture radar observations, which are typically as faint as 10 mag. In optical, have not been detected until recently in optical observations, mainly due to insufficient sensitivity of the optical observations. In this paper, two radar and optical simultaneous observations were organized. The first observation was carried out in 2009–2010 using Middle and Upper Atmosphere Radar (MU radar) and an image-intensified CCD camera. The second observation was carried out in 2018 using the MU radar and a mosaic CMOS camera, Tomo-e Gozen, mounted on the 1.05-m Kiso Schmidt Telescope. In total, 331 simultaneous meteors were detected. The relationship between radar cross sections and optical V-band magnitudes was well approximated by a linear function. A transformation function from the radar cross section to the V-band magnitude was derived for sporadic meteors. The transformation function was applied to about 150,000 meteors detected by the MU radar in 2009–2015, large part of which are sporadic, and a luminosity function was derived in the magnitude range of − 1.5 – 9.5 mag . The luminosity function was well approximated by a single power-law function with the population index of r = 3.52 ± 0.12 . The present observation indicates that the MU radar has capability to detect interplanetary dust of 10 − 5 – 10 0 g in mass as meteors.

中文翻译:

基于雷达和光学同时观测暗弱流星的雷达截面与光级的关系

摘要 流星的雷达和光学同步观测对于了解行星际尘埃的大小分布非常重要。然而,高功率大孔径雷达观测检测到的微弱流星通常只有 10 mag 微弱。在光学方面,直到最近才在光学观察中被发现,主要是由于光学观察的灵敏度不够。在本文中,组织了两次雷达和光学同时观测。第一次观测是在 2009-2010 年使用中高层大气雷达(MU 雷达)和图像增强型 CCD 相机进行的。第二次观测是在 2018 年使用 MU 雷达和安装在 1.05 米 Kiso Schmidt 望远镜上的马赛克 CMOS 相机 Tomo-e Gozen 进行的。总共检测到 331 颗同时发生的流星。雷达截面和光学 V 波段幅度之间的关系由线性函数很好地近似。对于零星流星,导出了从雷达截面到 V 波段幅度的转换函数。该变换函数应用于 2009-2015 年 MU 雷达探测到的大约 150,000 颗流星,其中大部分是零星的,并且在-1.5-9.5 mag 的星等范围内推导出光度函数。光度函数很好地近似于一个单一的幂律函数,人口指数 r = 3.52 ± 0.12。目前的观测表明,MU 雷达有能力探测质量为 10 − 5 – 10 0 g 的行星际尘埃作为流星。对于零星流星,导出了从雷达截面到 V 波段幅度的转换函数。该变换函数应用于 2009-2015 年 MU 雷达探测到的大约 150,000 颗流星,其中大部分是零星的,并且在-1.5-9.5 mag 的星等范围内推导出光度函数。光度函数很好地近似于一个单一的幂律函数,人口指数 r = 3.52 ± 0.12。目前的观测表明,MU 雷达有能力探测质量为 10 − 5 – 10 0 g 的行星际尘埃作为流星。对于零星流星,导出了从雷达截面到 V 波段幅度的转换函数。该变换函数应用于 2009-2015 年 MU 雷达探测到的大约 150,000 颗流星,其中大部分是零星的,并且在-1.5-9.5 mag 的星等范围内推导出光度函数。光度函数很好地近似于一个单一的幂律函数,人口指数 r = 3.52 ± 0.12。目前的观测表明,MU 雷达有能力探测质量为 10 − 5 – 10 0 g 的行星际尘埃作为流星。5 倍。光度函数很好地近似于一个单一的幂律函数,人口指数 r = 3.52 ± 0.12。目前的观测表明,MU 雷达有能力探测质量为 10 − 5 – 10 0 g 的行星际尘埃作为流星。5 倍。光度函数很好地近似于一个单一的幂律函数,人口指数 r = 3.52 ± 0.12。目前的观测表明,MU 雷达有能力探测质量为 10 − 5 – 10 0 g 的行星际尘埃作为流星。
更新日期:2020-12-01
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