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  • 1
    Online Resource
    Online Resource
    Cambridge University Press (CUP) ; 1994
    In:  Symposium - International Astronomical Union Vol. 162 ( 1994), p. 311-324
    In: Symposium - International Astronomical Union, Cambridge University Press (CUP), Vol. 162 ( 1994), p. 311-324
    Abstract: A large fraction of Be stars show periodic light and line profile variations with a timescale of about one day. The mechanism which causes these periodic variations has been attributed to nonradial pulsation (NRP) or rotational modulation (RM). The authors present arguments supporting the two opposing points of view with the purpose of stimulating subsequent discussion by the Symposium participants.
    Type of Medium: Online Resource
    ISSN: 0074-1809
    Language: English
    Publisher: Cambridge University Press (CUP)
    Publication Date: 1994
    SSG: 16,12
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  • 2
    Online Resource
    Online Resource
    Cambridge University Press (CUP) ; 1994
    In:  Symposium - International Astronomical Union Vol. 162 ( 1994), p. 305-306
    In: Symposium - International Astronomical Union, Cambridge University Press (CUP), Vol. 162 ( 1994), p. 305-306
    Abstract: Many previous surveys of the rapid variability of Be stars (e.g., Balona et al. 1987, Cuypers et al. 1989, Balona et al 1992) were limited to the Strömgren b -band only. We have undertaken a new observational effort with the specific aim of studying colour variations. A search for new rapidly variable stars should provide us with statistical material needed to generalize properties of the phenomenon with respect to the stellar parameters. Some preliminary results of these items are presented here.
    Type of Medium: Online Resource
    ISSN: 0074-1809
    Language: English
    Publisher: Cambridge University Press (CUP)
    Publication Date: 1994
    SSG: 16,12
    Location Call Number Limitation Availability
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  • 3
    Online Resource
    Online Resource
    American Astronomical Society ; 1992
    In:  The Astronomical Journal Vol. 103 ( 1992-2), p. 573-
    In: The Astronomical Journal, American Astronomical Society, Vol. 103 ( 1992-2), p. 573-
    Type of Medium: Online Resource
    ISSN: 0004-6256
    RVK:
    Language: Unknown
    Publisher: American Astronomical Society
    Publication Date: 1992
    detail.hit.zdb_id: 2207625-6
    detail.hit.zdb_id: 2003104-X
    SSG: 16,12
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  • 4
    Online Resource
    Online Resource
    Cambridge University Press (CUP) ; 1994
    In:  Symposium - International Astronomical Union Vol. 162 ( 1994), p. 307-308
    In: Symposium - International Astronomical Union, Cambridge University Press (CUP), Vol. 162 ( 1994), p. 307-308
    Abstract: The reality of the previously reported triple-wave light curve (Cuypers et al. 1989, A & A Suppl. 81, 151), and relations between rapid line profile and brightness variations of the B1-2III-Ve star η Cen (HD 127972) were investigated by means of simultaneous high-resolution spectroscopy (4 nights, 86 Si III 455.2622 nm profiles) and two-station uvby photometry (14 nights) secured in 1992. To this database were added the uvby photometry by Cuypers et al. and unpublished b observations by L.A.B. from 1988–1991.
    Type of Medium: Online Resource
    ISSN: 0074-1809
    Language: English
    Publisher: Cambridge University Press (CUP)
    Publication Date: 1994
    SSG: 16,12
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  • 5
    Online Resource
    Online Resource
    American Society for Microbiology ; 1991
    In:  Journal of Clinical Microbiology Vol. 29, No. 9 ( 1991-09), p. 1934-1939
    In: Journal of Clinical Microbiology, American Society for Microbiology, Vol. 29, No. 9 ( 1991-09), p. 1934-1939
    Abstract: The ability of seven methods to detect high-level gentamicin (58 strains) and streptomycin resistance (56 strains) among 107 Enterococcus faecalis isolates was investigated at the University of Chicago Medical Center and the University of Nebraska Medical Center. Methods included a standard agar screen plate, high-content disk diffusion, Remel (Lenexa, Kans.) EF Synergy Quad plates, standard microdilution panels prepared in house, Pasco MIC Gram-Positive panels (Difco Laboratories, Detroit, Mich.), MicroScan MIC Type 5 dry panels (Baxter Healthcare Corp., MicroScan Div., West Sacramento, Calif.), and Vitek GPS-TA cards (Vitek Systems Inc., Hazelwood, Mo.). Results indicating false resistance were not obtained by any method, and there was 100% agreement between the results of the disk diffusion and standard agar screen methods. Prolonging incubation from 24 to 48 h increased resistance detection for both agar and microdilution screens. EF Synergy Quad plates inoculated with micropipettes detected 100% of the streptomycin- and gentamicin-resistant isolates. Resistance detection for streptomycin and gentamicin, respectively, was 93 and 96% by standard microdilution, 93 and 98% by Pasco panels, 88 and 89% by MicroScan panels, and 88 and 91% by Vitek GPS-TA cards. False susceptibility occurred more frequently with streptomycin-resistant isolates than it did with gentamicin-resistant strains and appeared to be strain related in some instances. The use of an increased inoculum size enhanced resistance detection with these strains, but it complicated interpretation of results and led to the selection of streptomycin-resistant mutants. Until results of further studies delineate optimum test conditions, a delay in the final interpretation of agar and microdilution screen results until 48 h for isolates showing no or light growth at 24 h may help to minimize the occurrence of false susceptibility reporting.
    Type of Medium: Online Resource
    ISSN: 0095-1137 , 1098-660X
    RVK:
    Language: English
    Publisher: American Society for Microbiology
    Publication Date: 1991
    detail.hit.zdb_id: 1498353-9
    SSG: 12
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  • 6
    Online Resource
    Online Resource
    Cambridge University Press (CUP) ; 1994
    In:  Symposium - International Astronomical Union Vol. 162 ( 1994), p. 271-272
    In: Symposium - International Astronomical Union, Cambridge University Press (CUP), Vol. 162 ( 1994), p. 271-272
    Abstract: Slitless field Hα spectroscopy with a resolution of 0.2 nm has detected numerous Be stars in 3 young open star clusters in the LMC but only a few each in one Galactic and one LMC cluster. The line widths indicate rapid rotation as is typical of Galactic field Be stars. In NGC 2004 (LMC) their distribution seems inconsistent with the assumption of either very similar equatorial rotation velocities or random orientation of the rotation axes or both, which are believed to be valid for Galactic field Be stars.
    Type of Medium: Online Resource
    ISSN: 0074-1809
    Language: English
    Publisher: Cambridge University Press (CUP)
    Publication Date: 1994
    SSG: 16,12
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  • 7
    Online Resource
    Online Resource
    Cambridge University Press (CUP) ; 1994
    In:  Symposium - International Astronomical Union Vol. 162 ( 1994), p. 427-428
    In: Symposium - International Astronomical Union, Cambridge University Press (CUP), Vol. 162 ( 1994), p. 427-428
    Abstract: We sketch a new method for the accurate flux calibration and normalization of stellar spectra. This is of particular importance for the analysis of rapidly rotating early–type stars. Some preliminary log g determinations by profile fitting of H γ are presented.
    Type of Medium: Online Resource
    ISSN: 0074-1809
    Language: English
    Publisher: Cambridge University Press (CUP)
    Publication Date: 1994
    SSG: 16,12
    Location Call Number Limitation Availability
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  • 8
    Online Resource
    Online Resource
    Cambridge University Press (CUP) ; 1994
    In:  Symposium - International Astronomical Union Vol. 162 ( 1994), p. 29-30
    In: Symposium - International Astronomical Union, Cambridge University Press (CUP), Vol. 162 ( 1994), p. 29-30
    Abstract: The β Cephei instability is believed to be caused by the κ-mechanism. Model calculations, based on revised metal opacities, show this mechanism to be strongly sensitive to metallicity (e.g., Dziembowski, W. A. & Pamyatnykh, A. A., 1993: MNRAS , 262, 204). It appears that [Fe/H] must be larger than the solar value in order to drive the β Cephei pulsations. For this reason, the models predict that no β Cephei stars should be found in the Magellanic Clouds. Balona (1992: MNRAS , 256, 425; 1992: ASP Conf. Ser. , Vol. 30, 155; 1993: MNRAS , 260, 795) has tested this prediction by observing three young clusters in the SMC and LMC (NGC 330, NGC 2004 and NGC 2100). He found no β Cephei stars down to a magnitude of V ≈ 16; the threshold for detection of variability on time-scales of a few hours was 10 mmag. Most Galactic β Cephei stars have amplitudes greater than this, but we might expect β Cephei stars in the Magellanic Clouds (if they exist) to have smaller amplitudes, due to the different environment. To test this, we have observed two young clusters NGC 371 (SMC) and NGC 2122 (LMC) with high sensitivity.
    Type of Medium: Online Resource
    ISSN: 0074-1809
    Language: English
    Publisher: Cambridge University Press (CUP)
    Publication Date: 1994
    SSG: 16,12
    Location Call Number Limitation Availability
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