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1.
Wolfgang Haber 《Umweltwissenschaften und Schadstoff-Forschung》2002,14(4):206-210
Ohne Zusammenfassung 相似文献
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Supportive Breeding and Variance Effective Population Size 总被引:2,自引:0,他引:2
The practice of supporting weak, wild populations through release of individuals bred in captivity is becoming an increasingly important conservation measure. A frequently recommended form of such breeding-release activity refers to supportive breeding: a fraction of the target population is brought into captivity for reproduction, and the resulting progeny are released to mix with the wild segment of the population. We derived an expression for the variance effective size of a population managed through supportive breeding and discuss its relationship to previously published equations that are based on the assumption of random mating. We show that the effect of supportive breeding may be quite different on the inbreeding and the variance effective sizes. Whereas supportive breeding always results in a reduction of the inbreeding effective number, the variance effective number may either decrease, increase, or remain unchanged. We discuss these observations in relation to conservation management and suggest some general guidelines for supportive breeding situations. Our recommendations include making a distinction between inbreeding and variance effective numbers; taking particular care when dealing with organisms with high reproductive potential; assuring that the amount of drift be no larger than it would be without supportive breeding; and focusing primarily on the variance effective size of a population-that is, on the effective number directly related to the rate of loss of gene diversity. 相似文献
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Wolfgang Kundt 《Die Naturwissenschaften》1981,68(2):63-75
There are 109±0.5 neutron stars in the Galaxy. They are born in supernova explosions. Isolated neutron stars are observed as (radio-)pulsars, in some cases also as γ-ray pulsars and as IR-, optical and X-ray pulsars. Binary neutron stars, when accreting mass from their companion, become flickering, periodic and/or bursting X-ray sources, and probably also γ-ray bursters. They may all derive from binary star systems. The masses of population-I-neutron stars are compatible with (1.4 ±0.2)M ⊙; their surface magnetic fields fall almost exclusively within 1012.2 and 1013.2 Gauss (at birth). The radii of population-II-neutron stars are (10 -3 +6 )km. Even in exotic sources like SS 433 and Cyg X-1, the compact core may well be a neutron star. 相似文献
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