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  • 1
    Electronic Resource
    Electronic Resource
    Colostomy closure (1996)
    Springer
    Diseases of the colon & rectum 39 (1996), S. 605-609 
    Details
    ISSN: 1530-0358
    Keywords: Colostomy closure ; Hartmann's pouch ; Stoma ; Complications
    Source: Springer Online Journal Archives 1860-2000
    Topics: Medicine
    Notes: Abstract PURPOSE: We retrospectively reviewed the records from our past five years of experience with colostomy closure at a large multispecialty hospital to determine postoperative morbidity. RESULTS: From March 1988 to April 1993, 46 patients underwent colostomy closure. Patients ranged in age from 24 to 87 (mean, 41.8) years, and 25 (54 percent) were women. Stomas had been created during emergency operations in 40 patients (87 percent); most operations (54 percent) were for complications of acute diverticulitis. Of the 46 procedures, 40 (87 percent) were end colostomies, and 6 were loop colostomies. Stomas were closed at a range of 11 to 1,357 days after creation (mean, 207 days; median, 116 days). Twenty-six patients (57 percent) underwent colostomy closure alone, and the remainder underwent additional procedures ranging from appendectomy to hepatic lobectomy. Duration of operations ranged from 1 to 9.5 (mean, 4.2) hours, and estimated blood loss averaged 400 ml. Overall hospital stay for closure was 6 to 62 (mean, 11.5) days. Inpatient complications occurred in 15 percent of patients, including congestive heart failure (2 percent), cerebrovascular accident (4 percent), pneumonia (2 percent), enterocutaneous fistula (2 percent), and pulmonary embolus with death (2 percent). The most common longterm complication was midline wound hernia, which occurred in 10 percent of surviving patients. Overall, complications occurred in 24 percent.CONCLUSIONS: Colostomy closure is a major operation; however, with good surgical judgment and technique, associated morbidity and mortality can be minimized.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF02056935
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  • 2
    Electronic Resource
    Electronic Resource
    Incidence of small-bowel obstruction and adhesiolysis after open colorectal and general surgery (1999)
    Springer
    Diseases of the colon & rectum 42 (1999), S. 241-248 
    Details
    ISSN: 1530-0358
    Keywords: Adhesions ; Complications ; Small-bowel obstruction
    Source: Springer Online Journal Archives 1860-2000
    Topics: Medicine
    Notes: Abstract PURPOSE: The study contained herein was undertaken to establish the incidence of small-bowel obstruction, adhesiolysis for obstruction, and additional abdominal surgery after open colorectal and general surgery. METHODS: A retrospective cohort study was performed using patient-specific Health Care Financing Administration data to evaluate a random 5 percent sample of all Medicare patients who underwent surgery in 1993. Of these, 18,912 patients had an index abdominal procedure. Two-year follow-up data documented outcomes of hospitalizations with obstruction, adhesiolysis for obstruction, and/or additional open colorectal or general surgery. RESULTS: Within two years of incision, excision, and anastomosis of intestine (International Classification of Diseases (ICD)-9 code 45), 14.3 percent of patients had obstructions, 2.6 percent required adhesiolysis for obstructions, and 12.9 percent underwent additional open colorectal or general surgery. After other operations of intestine (ICD code 46), 17 percent of patients had obstructions, 3.1 percent required adhesiolysis for obstructions, and 20.2 percent underwent additional open colorectal or general surgery. After operations of rectum, rectosigmoid, and perirectal tissue (ICD code 48), 15.3 percent of patients had obstructions, 5.1 percent required adhesiolysis for obstructions, and 16.4 percent underwent additional open colorectal or general surgery. After other operations on the abdominal region (ICD code 54), 12.4 percent of patients had obstructions, 2.3 percent required adhesiolysis for obstructions, and 8.8 percent underwent additional open colorectal or general surgery. CONCLUSIONS: In this retrospective study of Medicare patients, we learned that bowel obstruction, adhesiolysis for obstructions, and additional abdominal surgery occurred more often after abdominal surgery than was previously published.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF02237135
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  • 3
    Electronic Resource
    Electronic Resource
    Discovery Of Mg-Rich Pyroxenes In Comet C/1995 O1 (Hale-Bopp): Pristine Grains Revealed At Perihelion (1997)
    Springer
    Earth, moon and planets 78 (1997), S. 285-291 
    Details
    ISSN: 1573-0794
    Keywords: Comet ; infrared ; dust ; silicates ; olivine ; pyroxene
    Source: Springer Online Journal Archives 1860-2000
    Topics: Geosciences , Physics
    Notes: Abstract The NASA Ames HIFOGS spectrometer observed comet C/1995 O1 (Hale-Bopp) at epochs including 96 Oct 7–14 UT (2.8 AU), 97 Feb 14–15 UT (1.2 AU), 97 Apr 11 UT (0.93 AU), and 97 Jun 22, 25 UT (1.7 AU). The HIFOGS 7.5–13.5 μm spectrophotometry (R = 360 - 180) of the silicate feature at 2.8 AU is identical in shape to the ISO SWS spectra of comet Hale-Bopp (Crovisier et al., 1997); the strong 11.2 μm peak in the structured silicate feature is identified as olivine. Upon close passage to the sun, the HIFOGS spectra at 1.2 AU and 0.93 AU reveals strong peaks at 9.3 μm and 10.0 μm. The post-perihelion 10 μm silicate feature at 1.7 AU is weaker but has nearly the same shape as the pre-perihelion spectra at 1.2 AU, reverting to its pre-perihelion shape: there is no change in the dust chemistry by close passage to the sun. The appearance of the strong peaks at 9.3 μm and 10.0 μm at rh ≲ 1.7 AU is attributed to the rise in the contribution of pryoxenes (clino-pyroxene and orthopyroxene crystals) to the shape of the feature, and leads to the hypothesis that the pyroxenes are significantly cooler than the olivines. The pyroxenes are radiating on the Wien side of the blackbody at 2.8 AU and transition to the Rayleigh-Jeans tail of the blackbody upon closer approach to the Sun. Composite fits to the observed 10 μm silicate features using IDPs and laboratory minerals shows that a good empirical fit to the spectra is obtained when the pryoxenes are about 150 K cooler than the olivines. The pyroxenes, because they are cooler and contribute signficantly at perihelion, are more abundant than the olivines. The perihelion temperature of the pyroxenes implies that the pyroxenes are more Mg-rich than the other minerals including the olivines, amorphous olivines, and amorphous pyroxenes. The PUMA-1 flyby measurements of comet P/Halley also indicated an overabundance of Mg-rich pryoxenes compared to olivines. Comet Hale-Bopp's pyroxenes are similar to pyroxere IDPs from the ’Spray‘ class, known for their D-richness and their unaltered morphologies: Hale-Bopp's Mg-rich pyroxenes may be pristine relic ISM grains.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1023/A:1006225722620
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    Paper (German National Licenses)
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  • 4
    Electronic Resource
    Electronic Resource
    Near-Infrared Imaging Spectrophotometry Of Comet C/1995 O1 (Hale-Bopp) Near Perihelion (1997)
    Springer
    Earth, moon and planets 78 (1997), S. 259-264 
    Details
    ISSN: 1573-0794
    Keywords: Comet ; dust ; infrared spectra
    Source: Springer Online Journal Archives 1860-2000
    Topics: Geosciences , Physics
    Notes: Abstract We present 1- to 5-μm broadband and CVF images of comet Hale-Bopp taken 1997 February 10.5 UT, 50 days before perihelion. All the images exhibit a nonspherical coma with a bright “ridge” in the direction of the dust tail approximately 10″ from the coma. Synthetic aperture spectrophotometry implies that the optically important grains are of a radius ≤0.4 μm; smallest radius for any comet seen to date. The variation of the integrated surface brightness with radial distance from the coma (ρ) in all the images closely follows the “steady state” ρ−1 model for comet dust ablation (Gehrz and Ney, 1992). The near-infrared colors taken along the dust tail are not constant implying the dust grain properties vary with coma distance.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1023/A:1006265419894
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    Paper (German National Licenses)
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