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Motonori Okabe,1 Kiyotaka Kitagawa,2 Toshiko Yoshida,1 Chika Koike,1 Takeshi Katsumoto,2 Etsuko Fujihara,2 Toshio Nikaido1 1Department of Regenerative Medicine, University of Toyama, Graduate School of Medicine and Pharmaceutical Sciences, Toyama, 2Division of Ophthalmology, Matsue Red Cross Hospital, Japanese Red Cross Society, Shimane, Japan Background: This paper reports on the efficacy of a tissue adhesive, 2-octyl-cyanoacrylate, in the treatment of corneal perforation and glaucoma filtering bleb leak. Methods: Two eyes from two patients with corneal perforation or laceration and two eyes from two patients with bleb leak were included. The patients underwent application of 2-octyl-cyanoacrylate onto the perforated or leaking site, and a hydrogel contact lens was applied as a bandage. We also evaluated the in vitro cell toxicity of 2-octyl-cyanoacrylate in HeLa cells. Results: The two cases of corneal perforation were repaired within 22 days with one application of the tissue adhesive. The two cases of bleb leak were repaired with 2–4 applications of the tissue adhesive over 134 (range 17–134) days). There were no recurrences or adverse effects during a mean follow-up period of 12.7 months. In vitro testing revealed that 2-octyl-cyanoacrylate was markedly toxic to HeLa cells. Conclusion: Four patients with corneal perforation or bleb leak were successfully managed using 2-octyl-cyanoacrylate tissue adhesive. This simple and easy surgical technique may become an alternative therapeutic option for corneal perforation or bleb leak, although several applications of this tissue adhesive may be required. Although 2-octyl-cyanoacrylate was toxic to HeLa cells, no adverse clinical effects were noted using this adhesive. Keywords: corneal perforation, bleb leak, tissue adhesive, 2-octyl-cyanoacrylate

Chiharu Wada-Koike,1,&ast; Ryo Terauchi,1,&ast; Kota Fukai,2 Kei Sano,1 Euido Nishijima,1 Koji Komatsu,1 Kyoko Ito,3 Tomohiro Kato,3 Masayuki Tatemichi,2 Yoshiaki Kabata,4,&ast; Tadashi Nakano1 1Department of Ophthalmology, The Jikei University School of Medicine, Tokyo, Japan; 2Department of Preventive Medicine, Tokai University School of Medicine, Isehara, Japan; 3Centre for Preventive Medicine, The Jikei University School of Medicine, Tokyo, Japan; 4Department of Ophthalmology, Jikei University School of Medicine, Daisan Hospital, Tokyo, Japan&ast;These authors contributed equally to this workCorrespondence: Yoshiaki Kabata, Department of Ophthalmology, Jikei University School of Medicine, Daisan Hospital, 4-11-1 Izumihontyou, Komae-si, Tokyo, 125-8506, Japan, Tel +81 3 3480 1151, Fax +81 3 3480 5700, Email kabata22122@gmail.comPurpose: To examine the variability in glaucoma screening using fundus images among physicians, including non-ophthalmologists.Patients and Methods: Sixty-nine eyes from 69 patients, including 25 eyes with glaucoma, were included from the Jikei University Hospital from July 2019 to December 2022. Fundus images were captured using TRC-NW8 (Topcon Corporation, Tokyo, Japan), and were interpreted by 10 non-ophthalmologists, 10 non-specialist ophthalmologists, and 9 specialists for diagnostic accuracy. We analyzed differences in diagnostic accuracy among the three groups. Sensitivity, specificity, positive predictive value (PPV), negative predictive value (NPV), and Kappa coefficient were compared, using the Kruskal–Wallis test followed by a post hoc Dunn’s test.Results: The sensitivity and specificity were 0.22 and 0.92 for non-ophthalmologists, 0.49 and 0.83 for non-specialist ophthalmologists, and 0.68 and 0.87 for specialists, respectively. Both specialists and non-specialist ophthalmologists showed significantly higher sensitivity than non-ophthalmologists (Dunn’s test, P< 0.001 and P=0.031). There was no significant difference in specificity among the three groups (Kruskal–Wallis test, P=0.086). The PPV did not differ significantly between the groups (Kruskal–Wallis test, P=0.108), while the NPV was significantly higher in specialists compared to non-ophthalmologists (Dunn’s test, P< 0.001). Specialists also had a significantly higher Kappa coefficient than non-ophthalmologists and non-specialist ophthalmologists (Dunn’s test, P< 0.001 and P=0.024).Conclusion: Diagnostic accuracy varied significantly based on the physician’s background.Keywords: glaucoma, fundus images, sensitivity, specificity, health checkup

The presence of amorphous silicate particles in interstellar and circumstellar space has been suggested based on the observation of 9.7 and 18 μ m emission bands. We have successfully synthesized amorphous silicate samples of an enstatite and forsterite composition by the mechanical milling of mixed powder consisting of SiO2–MgO and SiO2–Mg(OH)2 reagent-grade particles under different rotation frequencies and milling times. These two types of starting materials are prepared to study the effect of the OH bond on synthesis and crystallization. The amorphous samples were characterized by X-ray diffraction and infrared spectroscopy. Amorphous samples with enstatite composition are synthesized from both SiO2–MgO and SiO2–Mg(OH)2 at 300 rpm and for 300 hr. Amorphous samples with forsterite composition are synthesized from both SiO2–MgO and SiO2–Mg(OH)2. The samples from SiO2–Mg(OH)2 require 400 rpm and a long milling time of 1600 hr. After crystallization, amorphous samples with an enstatite composition synthesized from SiO2–Mg(OH)2 mainly transform into forsterite with small amounts of amorphous silica SiO2 and enstatite depending on the rotation frequencies and milling time, while those from SiO2–MgO become enstatite. The amorphous samples with a forsterite composition are crystallized to forsterite from both starting materials. The presence of H2O or OH bonds significantly affects the final products after the crystallization of amorphous silicates of enstatite composition. [ABSTRACT FROM AUTHOR]

To link to full-text access for this article, visit this link: http://dx.doi.org/10.1016/j.icarus.2009.11.018 Byline: A. Morlok (a)(b), C. Koike (c), N. Tomioka (a), I. Mann (a), K. Tomeoka (a) Keywords: Infrared observations; Comets, Dust; Debris disks; Meteorites Abstract: We present laboratory mid-infrared transmission/absorption spectra obtained from matrix of the hydrated Murchison CM meteorite experimentally shocked at peak pressures of 10-49GPa, and compare them to astronomical observations of circumstellar dust in different stages of the formation of planetary systems. The laboratory spectra of the Murchison samples exhibit characteristic changes in the infrared features. A weakly shocked sample (shocked at 10GPa) shows almost no changes from the unshocked sample dominated by hydrous silicate (serpentine). Moderately shocked samples (21-34GPa) have typical serpentine features gradually replaced by bands of amorphous material and olivine with increasing shock pressure. A strongly shocked sample (36GPa) shows major changes due to decomposition of the serpentine and due to devolatilization. A shock melted sample (49GPa) shows features of olivine recrystallized from melted material. The infrared spectra of the shocked Murchison samples show similarities to astronomical spectra of dust in various young stellar objects and debris disks. The spectra of highly shocked Murchison samples (36 and 49GPa) are similar to those of dust in the debris disks of HD113766 and HD69830, and the transitional disk of HD100546. The moderately shocked samples (21-34GPa) exhibit spectra similar to those of dust in the debris disks of Beta Pictoris and BD+20307, and the transitional disk of GM Aur. An average of the spectra of all Murchison samples (0-49GPa) has a similarity to the spectrum of the older protoplanetary disk of SU Auriga. In the gas-rich transitional and protoplanetary disks, the abundances of amorphous silicates and gases have widely been considered to be a primary property. However, our study suggests that impact processing may play a significant role in generating secondary amorphous silicates and gases in those disks. Infrared spectra of the shocked Murchison samples also show similarities to the dust from comets (C/2002 V1, C/2001 RX14, 9P/Tempel 1, and Hale Bopp), suggesting that the comets also contain shocked Murchison-like material. Author Affiliation: (a) Department of Earth and Planetary Sciences, Faculty of Science, Kobe University, Nada, Kobe 657-8501, Japan (b) CRPG/CNRS, 54501 Vandoeuvre les Nancy, France (c) Department of Earth and Space Science, Graduate School of Science, Osaka University, Toyonaka, Osaka 560-0043, Japan Article History: Received 20 April 2009; Revised 21 October 2009; Accepted 10 November 2009

To link to full-text access for this article, visit this link: http://dx.doi.org/10.1016/j.icarus.2005.03.003 Byline: Y. Kimura (a), K. Tamura (a), C. Koike (b), H. Chihara (b)(c), C. Kaito (a) Keywords: Infrared observations; Interplanetary dust; Solar nebula Abstract: A new method of producing pyrrhotite grains, which are most commonly found in cometary material and interplanetary dust particles, was developed. Pyrrhotite grains in the monophase having a 7C structure were predominately produced using a solid-solid reaction between iron and sulfur grains at room temperature. The characteristic infrared peaks were observed at 602, 563, and 397 cm.sup.-1 (16.6, 17.8, and 25.2 [mu]m). Author Affiliation: (a) Department of Physics, Ritsumeikan University, Noji-higashi 1-1-1, Kusatsu-shi, Shiga 525-8577, Japan (b) Laboratory of Physics, Kyoto Pharmaceutical University, Misasagi, Yamashina, Kyoto 607-8414, Japan (c) Department of Earth and Space Science, Osaka University, 1-1, Machikaneyama, Toyonaka, Osaka 560-0043, Japan Article History: Received 20 April 2004; Revised 24 February 2005