著者

Tamagawa Toru Hayato Asami Nakamura Satoshi TERADA Yukikatsu BAMBA Aya HIRAGA Junko S. HUGHES John P. HWANG Una KATAOKA Jun KINUGASA Kenzo KUNIEDA Hideyo TANAKA Takaaki TSUNEMI Hiroshi UENO Masaru HOLT Stephen S. KOKUBUN Motohide MIYATA Emi SZYMKOWIAK Andrew TAKAHASHI Tadayuki TAMURA Keisuke UENO Daisuke MAKISHIMA Kazuo

出版者

社団法人日本天文学会

雑誌

PASJ : publications of the Astronomical Society of Japan (ISSN:00046264)

巻号頁・発行日

vol.61, no.1, pp.S167-S174, 2009-01-30

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Tycho's supernova remnant was observed by the XIS and HXD instruments onboard the Suzaku satellite on 2006 June 26-29 for 92 ks. The spectrum up to 30 keV was well fitted with a two-component model, consisting of a power-law with photon index of 2.7 and a thermal bremsstrahlung model with temperature of 4.7 keV. The former component can alternatively be modeled as synchrotron emission from a population of relativistic electrons with an estimated roll-off energy of around 1 keV. In the XIS spectra, in addition to the prominent Fe K_alpha line (6.445 keV), we observe for the first time significant K_alpha line emission from the trace species Cr and Mn at energies of 5.48 keV and 5.95 keV, respectively. Faint K_beta lines from Ca (4.56 keV) and Fe (7.11 keV) are also seen. The ionization states of Cr and Mn, based on their line centroids, are estimated to be similar to that of Fe K_alpha (Fe XV or XVI).

著者

谷津 陽一 片岡 淳 五十川 知子 河合 誠之 水野 恒史 釜江 常好 田島 宏康 高橋 忠幸 斉藤 芳隆 郡司 修一 Yatsu Yoichi Kataoka Jun Ikagawa Tomoko Kawai Nobuyuki Mizuno Tsunefumi Kamae Tsuneyoshi Tajima Hiroyasu Takahashi Tadayuki Saito Yoshitaka Gunji Shuichi

出版者

宇宙航空研究開発機構宇宙科学研究本部

雑誌

第4回宇宙科学シンポジウム = Proceedings of the 4th Space Science Symposium

巻号頁・発行日

pp.453-455, 2004-08

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X線、ガンマ線の偏光はほとんど全ての高エネルギー天文現象と関連し、その物理を研究するための有力なプローブである。しかしながら、これまでの観測例は10keV以下では1970年代のかに星雲、10keV以上ではガンマ線バーストのみである。そこで、30〜200keVの領域での世界初の偏光観測を目標とし気球実験を行う予定であり、これに搭載するためのWell-type硬X線偏光PoGO(Polarized Gamma-ray Observer)の開発を行っている。

著者

片岡 純 カタオカ ジュン Kataoka Jun 佐藤 禮子 サトウ レイコ Sato Reiko

出版者

千葉看護学会

雑誌

千葉看護学会会誌 (ISSN:13448846)

巻号頁・発行日

vol.15, no.2, pp.1-8, 2009-12

被引用文献数

1

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本研究の目的は,外来治療期から寛解期において,悪性リンパ腫患者が病気を克服するための統御力を獲得するプロセスを明らかにすることである。悪性リンパ腫に対する外来治療を終えた通院患者で研究参加に同意の得られた20名を対象に,面接法と参加観察法により資料を収集し,エスノグラフィーの手法を用い分析を行った。悪性リンパ腫患者の統御力獲得は,【[血液のがんではもう駄目だ]の思いが《治せるがんなら治すしかない》思いへ転換する】,【悪性リンパ腫を治すための予定治療を何が何でも完遂させる】,【がん治療を受けながら地域での生活の正常な営みを目指す】,【つきまとう不安を押しのける】,【《人に頼ったって駄目,自分で頑張るしかない》の思いと《支えてくれる人のためにも頑張ろう》の思いが共在する】【命・健康の大切さを肝に銘じて希求する有り様で生きる】,【治療後に残るダメージを軽減して通常生活を取り戻す】,【《自分なら乗り越えられる》思いを獲得する】など9つの局面からなるプロセスであることが明らかになった。患者が悪性リンパ腫罹患を契機として統御力獲得に至るには,①病気克服の意志決定,②主体的療養態度の形成,③出来事の影響を軽減できた自己の能力に対する肯定的評価,④コントロール感覚の獲得,の4つの課題を達成する必要がある。患者の統御力獲得を促進するためには,これらの4つの課題の達成を支援する看護援助が必要である。The purpose of this study was to describe the process by which malignant lymphoma patients in an ambulatory setting acquired mastery to overcome their illness. Twenty outpatients, who finished the treatment for malignant lymphoma in an ambulatory setting, participated in this study. Data were collected by a semi-structured interview and the participant observation, and analyzed using ethnography. Mastery was acquired through nine aspects. The nine aspects were: [Deciding to cure the malignant lymphoma by their own power, if it can be cured], [Completing the schedule of treatment for curing a malignant lymphoma by any means], [Aiming at living a normal life in the community, while undergoing cancer treatment], [Pushing aside the anxiety of hanging around me], [Living by how to desire, as remembering the importance of health and life], [Recovering a normal life by reducing damage after the treatment], [Permitting the anxiety of recurrence and ambiguity], [Acquiring the confidence of "I can overcome difficulties with my own power in the future"], e.t.c. In ordered for malignant lymphoma patients to acquire mastery, it is indispensable to satisfy four tasks. Four tasks are, (1) decision making to overcome the illness, (2) making a positive attitude, (3) fostering the self-efficacy as a result of coping with a problem, and (4) gaining a sense of control. Therefore it is important to provide nursing interventions that assist malignant lymphoma patients to satisfy these tasks on their own.

著者

Koyama Katsuji Hyodo Yoshiaki Inui Tatsuya NAKAJIMA Hiroshi MATSUMOTO Hironori TSURU Takeshi Go TAKAHASHI Tadayuki MAEDA Yoshitomo YAMAZAKI Noriko Y. MURAKAMI Hiroshi YAMAUCHI Shigeo TSUBOI Yohko SENDA Atsushi KATAOKA Jun TAKAHASHI Hiromitsu HOLT Stephen S. BROWN Gregory V.

出版者

日本天文学会

雑誌

PASJ : publications of the Astronomical Society of Japan (ISSN:00046264)

巻号頁・発行日

vol.59, no.1, pp.S245-S255, 2007-01-31

被引用文献数

16 129

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We have observed the diffuse X-ray emission from the Galactic Center (GC) using the X-ray Imaging Spectrometer (XIS) on Suzaku. The high-energy resolution and the low-background orbit provided excellent spectra of the GC diffuse X-rays (GCDX). The XIS found many emission lines in the GCDX near the energy of K-shell transitions of iron and nickel. The most pronounced features are Fe I Kα at 6.4 keV and K-shell absorption edge at 7.1 keV, which are from neutral and/or low ionization states of iron, and the K-shell lines at 6.7 keV and 6.9 keV from He-like (Fe XXV Kα) and hydrogenic (Fe XXVI Lyα) ions of iron. In addition, Kα lines from neutral or low ionization nickel (Ni I Kα) and He-like nickel (Ni XXVII Kα), Fe I Kβ, Fe XXV Kβ, Fe XXVI Lyβ, Fe XXV Kγ and FeXXVI Lyγ were detected for the first time. The line center energies and widths of Fe XXV Kα and Fe XXVI Lyα favor a collisional excitation plasma for the origin of the GCDX. The electron temperature determined from the line flux ratio of Fe XXV Kα/Fe XXV Kβ is similar to the ionization temperature determined from that of Fe XXV Kα/Fe XXVI Lyα. Thus it would appear that the GCDX plasma is close to ionization equilibrium. The 6.7 keV flux and temperature distribution to the galactic longitude is smooth and monotonic, in contrast to the integrated point source flux distribution. These facts support the hypothesis that the GCDX is truly diffuse emission rather than the integration of the outputs of a large number of unresolved point sources. In addition, our results demonstrate that the chemical composition of Fe in the interstellar gas near the GC is constrained to be about 3.5 times solar abundance.