@inproceedings{oai:jaxa.repo.nii.ac.jp:00003131,
 author = {梨本, 真志 and 服部, 誠 and 下西, 隆 and 大坪, 貴文 and 山本, 哲生 and 土井, 靖生 and Nashimoto, Masashi and Hattori, Makoto and Shimonishi, Takashi and Otsubo, Takafumi and Yamamoto, Tetsuo and Doi, Yasuo},
 book = {宇宙航空研究開発機構特別資料, JAXA Special Publication: The Cosmic Wheel and the Legacy of the AKARI archive: from galaxies and stars to planets and life},
 month = {Mar},
 note = {第4回「あかり」国際会議 (2017年10月17-20日. 東京大学), 文京区, 東京, The 4th AKARI International Conference: The Cosmic Wheel and the Legacy of the AKARI archive: from galaxies and stars to planets and life (October 17-20, 2017. The University of Tokyo), Bunkyo-ku, Tokyo, Japan, We have been working on construction of the physically motivated Galactic dust emission SED models both for intensity and polarization in order to improve the detection limit of the cosmic microwave background (CMB) B-mode polarization imprinted by primordial gravitational waves. A full treatment of photon absorption processes due to quantum mechanical transitions between two-level systems (TLS) caused by deformation of lattice structure is developed to model absorption coefficients of interstellar dust grains in mm, submm and FIR wavebands. We showed that there are 8 free parameters which control shape and amplitude of emission spectrum of amorphous dust grains. Since interstellar dust consists of two main species, that is carbon and silicate, totally 16 free parameters must be defined to model interstellar dust SED at least. To construct polarization emission model from dust grains, dust grain shapes are modeled by ellipsoids. Continuous distribution of ellipsoids (CDE) is adopted as distributions of ratios of major to minor axes and major to semi-minor axes. We also showed that the degree of polarization of ellipsoidal dust depends only on the real part of the permittivity in the mm wavelength range. On the other hand, the emissivity depends on both real and imaginary parts. Therefore, the complex permittivity of interstellar dust grains is able to be constrained by measuring the frequency dependence of both degree of polarization and intensity. It provides an important clue to clarify physical nature and origin of interstellar dust grains. Our amorphous dust grain models predict that the degree of polarization of the ellipsoidal dust is monotonically decreasing function of the frequency., 形態: カラー図版あり, Physical characteristics: Original contains color illustrations, 資料番号: AA1730026057, レポート番号: JAXA-SP-17-009E},
 pages = {301--304},
 publisher = {宇宙航空研究開発機構(JAXA), Japan Aerospace Exploration Agency (JAXA)},
 title = {A Study of the Galactic Dusts for the Improvement of the CMB Components Separation},
 volume = {JAXA-SP-17-009E},
 year = {2018}
}