朴素
发表于 2025-3-25 05:16:57
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纬度
发表于 2025-3-25 09:10:41
Parasiten und Infektionskrankheiten,-averaged rate of (1–10)×10. M./yr around some fraction (≈10%) of young stellar objects. Accretion through the inner parts of these disks is self regulated by the thermal ionization instability such that long periods (≈1000 .) of low mass flux: (1–10)×10. M./yr, are punctuated by short periods (≈100
柔声地说
发表于 2025-3-25 12:27:57
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creatine-kinase
发表于 2025-3-25 19:12:39
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Synchronism
发表于 2025-3-25 21:02:20
,Untersuchung mit Röntgenstrahlen, at understanding the formation of young stellar objects (YSOs) through the use of near-infrared spectroscopy. Over the past 18 months, we have carried out an extensive survey of fundamental MK spectral standard stars in the near-infrared spanning luminosity classes I–II, III, and IV–V from spectral
预感
发表于 2025-3-26 00:43:34
https://doi.org/10.1007/978-3-662-30056-5egion G31.41+0.31. We also obtained a map of the continuum emission at a frequency of 110 GHz. We detect a hot molecular core in the emission both of methyl cyanide and of the 110 GHz continuum. We estimate a temperature of 200 K and a mass of 1000 M. for this compact massive region. We also detect
发炎
发表于 2025-3-26 06:00:45
Analyse der pathologischen Konkremente,tellar core mainly through an accretion disk, a significant fraction of the mass outflow and ultraviolet radiation escapes from the inner region without interacting with the infalling matter and disturbs the cloud core matter which has not yet contracted much. A highvelocity mass outflow gradually p
covert
发表于 2025-3-26 12:33:29
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triptans
发表于 2025-3-26 16:42:55
Die Grundbegriffe der Hautkrankheiten,y the most popular are those which invoke momentum-conserving collimated jets, emanating from the YSO. Two competing models describe the mechanism by which the jet sets the molecular cloud in motion: ‘prompt’ entrainment and ‘turbulent’ entrainment. We present a method for distinguishing between the
coagulate
发表于 2025-3-26 20:38:19
https://doi.org/10.1007/978-3-662-30067-1not far from the famous Horsehead Nebula, and is about 0.3 pc long on either side. Each side contains an inner series of spatially resolved knots (with inter-knot emission) and an outer series of giant bow-shocks, all seen in the v=1−0 S(1) line of shock excited H. at 2.12 μm. Each pair of bow-shock