Search

本稿では，彗星の近赤外線スペクトルにおいて1μm波長帯で主な輝線を生じるCN分子を取り上げ，その発光モデルの詳細化について検討した結果を報告する。1μm波長帯はこれまでにくわしいサーベイがされておらず，京都産業大学神山天文台に設置された世界屈指の感度を誇る近赤外線高分散分光器WINEREDを用いた未同定分子のサーベイが進行中である。そうした未同定分子（CN分子の同位体を含む）は微弱な輝線を有すると考えられるため，その検出には，主な輝線を発するCN分子の同定と除去が必要となる。そこで，高精度な実験室分光データを元にした彗星CN分子輝線モデルの構築を行った。, In this study we discuss about emission lines caused by CN radicals in cometary coma. We have a plan to survey cometary emission lines（including unidentified lines）in 1-micron wavelength region by the high-sensitivity and high-resolution near-infrared spectrometer WINERED equipped with the 1.3m-Araki telescope in Koyama Astronomical Observatory, Kyoto-Sangyo University, Japan. In the target wavelength region（0.9 - 1.3 microns）emission lines from CN radicals are prominent and to be subtracted in order to search for weaker emission lines（isotopologues of CN and other complex molecules）. Accurate emission model for CN in cometary coma has been developed based on the recent laboratory studies and theoretical works., 9, KJ00010262519, P, 研究活動報告, Activity Reports

本稿では，遅い新星V2676 Ophに見られた，極大可視光度付近における分子生成について，神山天文台および他の天文台で行われた観測結果をもとに考察し，新星エンベロープ中における分子生成の条件について考察を行った。C₂やCN分子を作るような新星では，その分子バンド吸収スペクトルから炭素および窒素の同位体比を決定できる。こうした観測条件を満たすような新星の同定に向けた基礎的研究を行った。, In this study the molecular formation in classical novae is investigated, especially for the formation conditions of simple diatomic molecules like CO, CN, and C₂ in novae. From the absorption spectra of CN and C₂, it is known that the isotopic ratios of carbon and nitrogen can be obtained. Therefore, future observations of molecules in novae are important from the viewpoints of the origin of the solar system and also of the Galactic chemical evolution., 9, KJ00009857379, P, 研究活動報告, Acitivity Reports

[Abstract] In order for the primordial solar nebula to be stable against fragmentation, Shakra-Sunyaev parameter a must be sufficiently large. We show in this article that the large value of a is derived naturally from the Hoiland instability.

Meteorites have a hot origin as planetary materials derive from a supernova, similar to SN1987A, and were acquired by a nearby nova, the Sun. The supernova plasmas became zoned around the nova, mainly by their electromagnetic properties. Carbon and carbide dusts condensed first, followed, within the Inner Planetary Zone, by Ca–Mg–Al oxides and then by iron and nickel metal droplets. In the inner Asteroid Belt, the metals aggregated into clumps as they solidified but over a much longer time in the Inner Zone. ‘Soft’ collisions formed larger (