{"status":"ok","message-type":"work","message-version":"1.0.0","message":{"indexed":{"date-parts":[[2026,5,1]],"date-time":"2026-05-01T10:11:59Z","timestamp":1777630319206,"version":"3.51.4"},"reference-count":41,"publisher":"American Association for the Advancement of Science (AAAS)","issue":"4903","content-domain":{"domain":[],"crossmark-restriction":false},"short-container-title":["Science"],"published-print":{"date-parts":[[1989,4,28]]},"abstract":"<jats:p>\n            Evidence is reported for hydrogen sulfide (H\n            <jats:sub>2<\/jats:sub>\n            S) on Io's surface. An infrared band at 3.915 (\u00b1 0.015) micrometers in several ground-based spectra of Io can be accounted for by reflectance from H\n            <jats:sub>2<\/jats:sub>\n            S frost deposited on or cocondensed with sulfur dioxide (SO\n            <jats:sub>2<\/jats:sub>\n            ) frost. Temporal variation in the occurrence and intensity of the band suggests that condensed H\n            <jats:sub>2<\/jats:sub>\n            S on Io's surface is transient, implying a similar variation of H\n            <jats:sub>2<\/jats:sub>\n            S abundance in Io's atmosphere. The band was observed in full-disk measurements of Io at several orbital longitudes, including once at 24\u00b0 (\u223c 0.5 hour after Io's reappearance after an eclipse)\u2014but not after another reappearance at 22\u00b0\u2014and once at 95\u00b0(on Io's leading hemisphere). These results suggest that condensed H\n            <jats:sub>2<\/jats:sub>\n            S is sparse and variable but can be widespread on Io's surface. When present, it would not only produce the infrared band but would brighten Io's typical surface at ultraviolet and visible wavelengths.\n          <\/jats:p>","DOI":"10.1126\/science.244.4903.454","type":"journal-article","created":{"date-parts":[[2006,10,5]],"date-time":"2006-10-05T21:21:28Z","timestamp":1160083288000},"page":"454-457","source":"Crossref","is-referenced-by-count":46,"title":["Hydrogen Sulfide on IO: Evidence from Telescopic and Laboratory Infrared Spectra"],"prefix":"10.1126","volume":"244","author":[{"given":"Douglas B.","family":"Nash","sequence":"first","affiliation":[{"name":"Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, and San Juan Capistrano Research Institute, San Juan Capistrano, CA 92675."}],"role":[{"role":"author","vocabulary":"crossref"}]},{"given":"Robert R.","family":"Howell","sequence":"additional","affiliation":[{"name":"Department of Physics and Astronomy, University of Wyoming, Laramie, WY 82071."}],"role":[{"role":"author","vocabulary":"crossref"}]}],"member":"221","reference":[{"key":"e_1_2_1_1_1","doi-asserted-by":"crossref","first-page":"1082","DOI":"10.1086\/156341","volume":"223","year":"1978","unstructured":"CARLSON, R.W., SODIUM D-LINE EMISSION FROM IO - COMPARISON OF OBSERVED AND THEORETICAL LINE-PROFILES, ASTROPHYSICAL JOURNAL 223: 1082 (1978).","journal-title":"ASTROPHYSICAL JOURNAL"},{"key":"e_1_2_1_2_1","doi-asserted-by":"crossref","first-page":"240","DOI":"10.1016\/0019-1035(80)90007-X","volume":"41","year":"1980","unstructured":"CRUIKSHANK, D.P., INFRARED-SPECTRUM OF LO, 2.8-5.2 MU-M, ICARUS 41: 240 (1980).","journal-title":"ICARUS"},{"key":"e_1_2_1_3_1","doi-asserted-by":"crossref","first-page":"L89","DOI":"10.1086\/182800","volume":"225","year":"1978","unstructured":"CRUIKSHANK, D.P., ABSORPTION-BANDS IN SPECTRUM OF IO, ASTROPHYSICAL JOURNAL 225: L89 (1978).","journal-title":"ASTROPHYSICAL JOURNAL"},{"key":"e_1_2_1_4_1","doi-asserted-by":"crossref","first-page":"761","DOI":"10.1038\/280761a0","volume":"280","year":"1979","unstructured":"Fanale, F. 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