標題: Titlebook: Birth and Evolution of Massive Stars and Stellar Groups; Proceedings of a Sym Wilfried Boland,Hugo Woerden Conference proceedings 1985 D. R [打印本頁] 作者: 非決定性 時間: 2025-3-21 17:52
書目名稱Birth and Evolution of Massive Stars and Stellar Groups影響因子(影響力)
書目名稱Birth and Evolution of Massive Stars and Stellar Groups影響因子(影響力)學科排名
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書目名稱Birth and Evolution of Massive Stars and Stellar Groups網(wǎng)絡公開度學科排名
書目名稱Birth and Evolution of Massive Stars and Stellar Groups被引頻次
書目名稱Birth and Evolution of Massive Stars and Stellar Groups被引頻次學科排名
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書目名稱Birth and Evolution of Massive Stars and Stellar Groups年度引用學科排名
書目名稱Birth and Evolution of Massive Stars and Stellar Groups讀者反饋
書目名稱Birth and Evolution of Massive Stars and Stellar Groups讀者反饋學科排名
作者: Rustproof 時間: 2025-3-22 00:07
The Nearest Molecular Cloudsare correlated with the infrared “cirrus” found by IRAS. The mean distance to the clouds is about 100 pc; they are thus the nearest clouds to the Sun and are the small molecular-cloud component of the interstellar medium. The large internal velocity dispersions indicate that the clouds are not gravi作者: BRINK 時間: 2025-3-22 01:19 作者: 季雨 時間: 2025-3-22 06:02
Distribution and Motion of Young Nearby Stars as a Function of Agetial distribution of stars younger than 30·10. years along the inclined plane of Gould’s Belt shows a rather abrupt jump back to the galactic plane at distances coinciding with a discontinuity in the velocity gradients. Table 1 gives velocity parameters for different age groups, and the difficulty t作者: corn732 時間: 2025-3-22 12:39 作者: 悠然 時間: 2025-3-22 15:51
Near-Infrared Spectra of 11 T Tauri Starstriplet behaviour. The stars we have observed fall into three groups according to the values of the equivalent widths of the Ca IIλ 8498 line. Our results are in good agreement with recently proposed chromospheric models.作者: 來就得意 時間: 2025-3-22 19:06
The Turn-On Point of the Pleiades Clusterituated near to spectral type K2, corresponding to a mass of 0.75 to 0.8 M.. This is very close to the expected position based on the cluster age, as derived from the B and early A-star members of the Pleiades, and stellar contraction times. This also means, however, that the pre-main-sequence stars作者: 危機 時間: 2025-3-22 23:12
Two AOV Stars on the Zero-Age Main-Sequence in the Association Cha I HD 97048 and HD 97300 in the Cha I association. The MK spectral classification and apparent visual magnitude for these stars are: B9.5 Ve and V = 8.4; B9V and V = 9.0, respectively. Both objects are presumably ZAMS stars; although HD 97300 has no emission features, it does have many of the properti作者: 安裝 時間: 2025-3-23 03:16
Evolution of Massive Stars: Observational Evidenceith evolutionary models, the observations suggest a galactic gradient in the initial mass function of these stars. Differences in the massive stellar population between the Large and Small Magellanic Cloud are starting to appear. Understanding these differences will provide important insight into th作者: 遣返回國 時間: 2025-3-23 08:50 作者: 無法治愈 時間: 2025-3-23 12:43 作者: Alienated 時間: 2025-3-23 16:13 作者: deface 時間: 2025-3-23 18:18
Supernovae and Pulsarstific career. His own contributions to that history include supernova explosions in close binary systems as an origin for runaway OB stars (most pulsars are also high-velocity objects), and studies of expanding stellar associations that have prompted explanations in terms of supernovae. Of the more 作者: misshapen 時間: 2025-3-24 00:15
The Identification of Massive Supernova Progenitorsir rate of occurrence and theoretical considerations on stellar evolution (the latter only for type II supernovae). The pre-explosion masses are derived from the lightcurves (types II and V) and from the absolute magnitude before the explosion (only for type V’s). We find mass ranges of 6 to 16 M., 作者: 獨白 時間: 2025-3-24 04:26 作者: Conscientious 時間: 2025-3-24 10:35
Vereinigung, Zersetzung, Umsetzung,s that of a young cluster containing stars of ages up to that of an average giant molecular cloud, a few 10. years. A few stars in the solar neighborhood may be low-mass, still pre-main-sequence, products of recently dissipated clouds.作者: nitric-oxide 時間: 2025-3-24 12:41 作者: Presbyopia 時間: 2025-3-24 15:28 作者: 罵人有污點 時間: 2025-3-24 22:58 作者: 或者發(fā)神韻 時間: 2025-3-25 03:13
The Nearest Molecular Cloudsand are the small molecular-cloud component of the interstellar medium. The large internal velocity dispersions indicate that the clouds are not gravitationally bound, and that they have ages of ~ 10. yr.作者: farewell 時間: 2025-3-25 04:51
Distribution and Motion of Young Nearby Stars as a Function of Age distances coinciding with a discontinuity in the velocity gradients. Table 1 gives velocity parameters for different age groups, and the difficulty to find simple models to explain the expanding motion of the local group of young stars is discussed.作者: hyperuricemia 時間: 2025-3-25 11:04 作者: MAPLE 時間: 2025-3-25 14:32
The Structure of Star-Forming Regions-The Ages of Subgroups and the Progression of Star Formationo the few hundredths of a parsec structure observed in dense cloud cores. Explanations of both the temporal and spatial progress of star formation are reviewed, and factors which may dominate the process on all scales are considered.作者: affluent 時間: 2025-3-25 16:08 作者: BIAS 時間: 2025-3-25 20:26 作者: Silent-Ischemia 時間: 2025-3-26 04:07 作者: 縱火 時間: 2025-3-26 05:32
Double Stars in Young Stellar Groupsith other investigations. Along the entire main sequence (O-K5) close binaries appear to form with nearly circular orbits. When the orbital dimensions are close to the stellar dimensions complete circularization takes place.作者: Scintigraphy 時間: 2025-3-26 11:11
Photometric Age Determination of OB-Associationse determination of ages of the associations and their subgroups by means of isochrone fitting are investigated. The influence of stellar rotation and undetected duplicity is discussed. Future work on the stellar content of the nearby OB-associations is suggested, in connection with the . mission.作者: 壓迫 時間: 2025-3-26 16:10
Astrophysics and Space Science Libraryhttp://image.papertrans.cn/b/image/188862.jpg作者: FUME 時間: 2025-3-26 20:45
Lehrbuch der Chemie und MineralogieThe recognition of stellar associations as regions of star formation, i.e. regions containing groups of recently formed stars (Ambartsumian 1947), had an important significance for our understanding of the origin and evolution of stars.作者: RADE 時間: 2025-3-26 21:11
Stellar Associations and the Regions of Active Star Formation in themThe recognition of stellar associations as regions of star formation, i.e. regions containing groups of recently formed stars (Ambartsumian 1947), had an important significance for our understanding of the origin and evolution of stars.作者: oblique 時間: 2025-3-27 04:04 作者: fallible 時間: 2025-3-27 06:02 作者: 雜役 時間: 2025-3-27 12:32
https://doi.org/10.1007/978-3-663-15891-2the local galactic neighborhood, which is here defined to encompass a region centered on the Sun and extending to a distance of approximately 500 parsecs..The major features in the distribution of the ISM in the northern local galactic neighborhood are two ‘holes’ (regions of low gas density). One o作者: BAIL 時間: 2025-3-27 14:53 作者: epicondylitis 時間: 2025-3-27 17:54
Vereinigung, Zersetzung, Umsetzung,in order to reproduce the local mass function it is necessary to postulate also that low-mass stars can be produced without OB stars in the conventional proportions. A few extraordinarily dense clusters of young stars in molecular clouds are known, especially that around the Orion Trapezium, but it 作者: Acclaim 時間: 2025-3-28 01:54
Abbau des Wassers. Der Wasserstoff,triplet behaviour. The stars we have observed fall into three groups according to the values of the equivalent widths of the Ca IIλ 8498 line. Our results are in good agreement with recently proposed chromospheric models.作者: 郊外 時間: 2025-3-28 02:42 作者: 大漩渦 時間: 2025-3-28 10:04
Die Lehre von den Atomen und Molekeln, HD 97048 and HD 97300 in the Cha I association. The MK spectral classification and apparent visual magnitude for these stars are: B9.5 Ve and V = 8.4; B9V and V = 9.0, respectively. Both objects are presumably ZAMS stars; although HD 97300 has no emission features, it does have many of the properti作者: 增長 時間: 2025-3-28 10:48
,Das Gesetz der festen Gewichtsverh?ltnisse,ith evolutionary models, the observations suggest a galactic gradient in the initial mass function of these stars. Differences in the massive stellar population between the Large and Small Magellanic Cloud are starting to appear. Understanding these differences will provide important insight into th作者: asthma 時間: 2025-3-28 18:29
Abbau des Wassers. Der Wasserstoff,ith other investigations. Along the entire main sequence (O-K5) close binaries appear to form with nearly circular orbits. When the orbital dimensions are close to the stellar dimensions complete circularization takes place.作者: aplomb 時間: 2025-3-28 20:53
Die Lehre von den Atomen und Molekeln,e determination of ages of the associations and their subgroups by means of isochrone fitting are investigated. The influence of stellar rotation and undetected duplicity is discussed. Future work on the stellar content of the nearby OB-associations is suggested, in connection with the . mission.作者: 放逐 時間: 2025-3-28 23:43
,Das Gesetz der festen Gewichtsverh?ltnisse,WR + 0) are, at the explosion of their initially more massive component, expected to produce runaway 0? stars with velocities typically in the range 30 to 90 km/s, and in a few cases > 100 km/s..At somewhat lower masses, ~ 9–30 M., also relatively wide binaries (ζ Aurigae type), with little mass tra作者: Accord 時間: 2025-3-29 07:07
Abbau des Wassers. Der Wasserstoff,tific career. His own contributions to that history include supernova explosions in close binary systems as an origin for runaway OB stars (most pulsars are also high-velocity objects), and studies of expanding stellar associations that have prompted explanations in terms of supernovae. Of the more 作者: GROVE 時間: 2025-3-29 10:34
Abbau des Wassers. Der Wasserstoff,ir rate of occurrence and theoretical considerations on stellar evolution (the latter only for type II supernovae). The pre-explosion masses are derived from the lightcurves (types II and V) and from the absolute magnitude before the explosion (only for type V’s). We find mass ranges of 6 to 16 M., 作者: 喃喃而言 時間: 2025-3-29 11:25
https://doi.org/10.1007/978-94-009-5478-6Galaxy; astronomy; star; stars; stellar作者: Protein 時間: 2025-3-29 18:25 作者: Verify 時間: 2025-3-29 20:08
Birth and Evolution of Massive Stars and Stellar Groups978-94-009-5478-6Series ISSN 0067-0057 Series E-ISSN 2214-7985 作者: FECK 時間: 2025-3-30 02:37 作者: 想象 時間: 2025-3-30 07:37
Lehrbuch der Chemie für H?here Lehranstalteno the few hundredths of a parsec structure observed in dense cloud cores. Explanations of both the temporal and spatial progress of star formation are reviewed, and factors which may dominate the process on all scales are considered.作者: 啟發(fā) 時間: 2025-3-30 10:19
