標(biāo)題: Titlebook: Evolution of Massive Stars; A Confrontation betw D. Vanbeveren,W. Rensbergen,C. Loore Book 1994 Springer Science+Business Media Dordrecht 1 [打印本頁(yè)] 作者: NK871 時(shí)間: 2025-3-21 16:51
書(shū)目名稱Evolution of Massive Stars影響因子(影響力)
書(shū)目名稱Evolution of Massive Stars影響因子(影響力)學(xué)科排名
書(shū)目名稱Evolution of Massive Stars網(wǎng)絡(luò)公開(kāi)度
書(shū)目名稱Evolution of Massive Stars網(wǎng)絡(luò)公開(kāi)度學(xué)科排名
書(shū)目名稱Evolution of Massive Stars被引頻次
書(shū)目名稱Evolution of Massive Stars被引頻次學(xué)科排名
書(shū)目名稱Evolution of Massive Stars年度引用
書(shū)目名稱Evolution of Massive Stars年度引用學(xué)科排名
書(shū)目名稱Evolution of Massive Stars讀者反饋
書(shū)目名稱Evolution of Massive Stars讀者反饋學(xué)科排名
作者: 痛苦一生 時(shí)間: 2025-3-21 23:49
Das Systemisch-integrative Führungsmodell derived for O—stars show, in general terms, good agreement with predictions from the latest radiation—driven wind models, although some discrepancies are apparent. Several LBVs show similar mass-loss rates at maximum and minimum states, contrary to previous expectations, with the mechanism responsi作者: Hyperopia 時(shí)間: 2025-3-22 02:24
Book 1994olution therefore got a chance in these meetings, but rarely as a prime subject. The state of the art, the physical processes and the uncertainties in stellar evolution were barely touched. Even more, the influence of close binaries in all these massive star meetings slowly disappeared the last, say作者: separate 時(shí)間: 2025-3-22 05:06
ve star evolution therefore got a chance in these meetings, but rarely as a prime subject. The state of the art, the physical processes and the uncertainties in stellar evolution were barely touched. Even more, the influence of close binaries in all these massive star meetings slowly disappeared the last, say978-94-010-4471-4978-94-011-1080-8作者: FLOUR 時(shí)間: 2025-3-22 11:13
Spectral Synthesis of Spectral Populations using Balmer Linesalaxies. The colors of a young starburst as well as most of its spectral features are relatively unaffected by stars of a few solar masses which contribute little to the integrated luminosity and to the ionization and excitation properties. However, as the Balmer lines are much stronger for those st作者: 慷慨不好 時(shí)間: 2025-3-22 13:16
Observations of the Atmospheres and Winds of O-stars, LBVs and Wolf-Rayet Stars derived for O—stars show, in general terms, good agreement with predictions from the latest radiation—driven wind models, although some discrepancies are apparent. Several LBVs show similar mass-loss rates at maximum and minimum states, contrary to previous expectations, with the mechanism responsi作者: 慷慨不好 時(shí)間: 2025-3-22 19:07
http://image.papertrans.cn/e/image/317744.jpg作者: 變化 時(shí)間: 2025-3-23 00:34
Erfolg als theoriegeleitete Kategorie,the SMC are 185, 114, and 9, respectively. Distances and galactic distributions determined by various authors are compared. The single star and binary distributions are discussed in the light of evolutionary studies.作者: 不遵守 時(shí)間: 2025-3-23 01:44
https://doi.org/10.1007/978-3-531-93479-2method to account for the huge number of atomic levels and line transitions is presented. Results of exploratory model calculations examining the effects on the temperature structure, the hydrogen and helium line profiles and UV/EUV fluxes are discussed.作者: AXIOM 時(shí)間: 2025-3-23 08:31 作者: foppish 時(shí)間: 2025-3-23 10:10 作者: Grasping 時(shí)間: 2025-3-23 16:36 作者: mendacity 時(shí)間: 2025-3-23 18:13
LTE and NLTE Abundances in A-Supergiants a Test of Their Evolutionary Statuses between the scenarios depend on the input assumptions for several physical parameters, ., treatments for convection parameters and mass loss rates. A review of the predictions of evolution calculations for 10–30 solar mass stars is given by Fitzpatrick & Garmany (1991).作者: 可用 時(shí)間: 2025-3-24 00:03
https://doi.org/10.1007/978-94-011-1080-8Galaxy; Population; Supernova; astrophysics; galaxies; milky way; photometry; spectroscopy; star; stellar; ste作者: lymphedema 時(shí)間: 2025-3-24 02:34
978-94-010-4471-4Springer Science+Business Media Dordrecht 1994作者: neuron 時(shí)間: 2025-3-24 07:20 作者: 難理解 時(shí)間: 2025-3-24 11:15 作者: overwrought 時(shí)間: 2025-3-24 18:37
https://doi.org/10.1007/978-3-322-82282-6f 30 Doradus in the Large Magellanic Cloud (LMC). Using photometric data for over 2400 stars (complete to .≈ 18 mag), and spectroscopic observations of over 150 stars in the region, the best estimate of the initial mass function (IMF) yields a slope of Г = ?1.5 ± 0.2 for masses > 12.⊙, where the Sal作者: MUMP 時(shí)間: 2025-3-24 21:16
https://doi.org/10.1007/978-3-322-91326-5le is known about the Be star content of the Magellanic Clouds (MCs). We present a refined method of Be star identification by CCD photometry and apply it to four young clusters and associations in the MCs. We find NGC 330 in the SMC to be exceptionally rich in Be stars, while the fraction is clearl作者: Rodent 時(shí)間: 2025-3-25 00:13
Erfolg mit konsistenten Partnernic goal of studying the upper end of the stellar mass function at ultraviolet wavelengths where the color degeneracy encountered in visual CMDs is less severe. The CMD has been compared to a set of theoretical isochrones, which have been computed using the latest generation of evolutionary models an作者: Orchiectomy 時(shí)間: 2025-3-25 06:06
https://doi.org/10.1007/978-3-8349-6885-2pectrum to synthetic spectra built by adding contributions of stars (or star clusters) of various ages. When the population is young, its visible spectrum is dominated by Balmer lines. These lines have rarely been used for spectral synthesis because Balmer lines in emission are superimposed to the c作者: VICT 時(shí)間: 2025-3-25 08:22 作者: 或者發(fā)神韻 時(shí)間: 2025-3-25 14:41 作者: lattice 時(shí)間: 2025-3-25 18:50 作者: AV-node 時(shí)間: 2025-3-25 21:20
https://doi.org/10.1007/978-3-658-03019-3st luminous Ia stars is close to its equilibrium value. The is also some evidence for more moderate CN abundance anomalies in the B2Ib and B2II supergiants. These results, together with other recent work, imply that the effects of the CNO bi-cycle on the composition of B-supergiant atmospheres are m作者: novelty 時(shí)間: 2025-3-26 00:11 作者: BAIL 時(shí)間: 2025-3-26 06:20 作者: Ardent 時(shí)間: 2025-3-26 08:38
https://doi.org/10.1007/978-3-322-81831-7d by the theory of radiatively driven winds reveals a discrepancy of 0.30 ± 0.05 dex, with the theoretical values being too low. We show that there is not only a mass-loss discrepancy but also a momentum flux discrepancy. The theoretically predicted momentum fluxes are too low by 0.17 ± 0.04 dex. Th作者: 哪有黃油 時(shí)間: 2025-3-26 15:49 作者: NIP 時(shí)間: 2025-3-26 18:18 作者: aspersion 時(shí)間: 2025-3-26 23:22
Wert und Bewertung von Erfolgsideen,omplementary to the submitted paper. Here, we emphasize the advantages and the weak points of our approach and we present additional technical aspects..The models are characterised by a simultaneous solution of the equation of motion, the non-LTE populations of H and He, and radiation transfer in a 作者: 說(shuō)明 時(shí)間: 2025-3-27 02:25
Erfolge mit SAP Business Workflow?Magellanic Clouds***, three of which are of spectral type O3. The data cover the spectral region from 1150 A–2300 A with a resolution of Δλ/λ ≈ 1 A. One O8.5 supergiant, OB78#231, in M31 .is also included in this work. These data are a substantial improvement on previous high resolution IUE observat作者: 涂掉 時(shí)間: 2025-3-27 06:11
,Der Reiseflug – Einführung der Agilit?t,The paper gives a summary of the situation mid-1993 of theory and observations regarding massive stars. I describe: stellar mass loss and its implications, pre-main-sequence evolution, the main sequence, problems of atmospheric instability, Luminous Blue Supergiants, Yellow Hyper-giants, Wolf—Rayet stars and supernovae.作者: 灰姑娘 時(shí)間: 2025-3-27 10:24 作者: 口音在加重 時(shí)間: 2025-3-27 14:24 作者: dowagers-hump 時(shí)間: 2025-3-27 20:45
Blue and Red Supergiants and the Age Structure of the NGC 330 RegionWe analysed new UBVRI CCD photometry of the massive, blue SMC cluster NGC 330 and its surrounding field. The age structure and a new reddening value for the stellar population in this region of the SMC are derived and the implications for star formation in this part of the SMC and for stellar evolution are discussed.作者: 簡(jiǎn)潔 時(shí)間: 2025-3-28 00:20
The Massive Star Distribution in the Galaxy and the Magellanic Cloudsthe SMC are 185, 114, and 9, respectively. Distances and galactic distributions determined by various authors are compared. The single star and binary distributions are discussed in the light of evolutionary studies.作者: PANT 時(shí)間: 2025-3-28 04:44
Massive Star Distribution in External Galaxies and Starburst Regionspes of massive stars. There seems to be little, if any, dependence of the slope of the Intial Mass Function, or the . on the initial composition of the stars. Indirect estimates of numbers of massive stars in various more distant environments are reviewed and discussed within a framework of a . of t作者: STYX 時(shí)間: 2025-3-28 07:22
A Dissection of 30 Doradus and a Discussion of Other Magellanic Cloud OB Associationsf 30 Doradus in the Large Magellanic Cloud (LMC). Using photometric data for over 2400 stars (complete to .≈ 18 mag), and spectroscopic observations of over 150 stars in the region, the best estimate of the initial mass function (IMF) yields a slope of Г = ?1.5 ± 0.2 for masses > 12.⊙, where the Sal作者: 推崇 時(shí)間: 2025-3-28 11:23
Be Stars in Young Clusters in the Magellanic Cloudsle is known about the Be star content of the Magellanic Clouds (MCs). We present a refined method of Be star identification by CCD photometry and apply it to four young clusters and associations in the MCs. We find NGC 330 in the SMC to be exceptionally rich in Be stars, while the fraction is clearl作者: BOAST 時(shí)間: 2025-3-28 15:47 作者: dissolution 時(shí)間: 2025-3-28 22:18
Spectral Synthesis of Spectral Populations using Balmer Linespectrum to synthetic spectra built by adding contributions of stars (or star clusters) of various ages. When the population is young, its visible spectrum is dominated by Balmer lines. These lines have rarely been used for spectral synthesis because Balmer lines in emission are superimposed to the c作者: granite 時(shí)間: 2025-3-29 00:15 作者: debble 時(shí)間: 2025-3-29 04:20 作者: sundowning 時(shí)間: 2025-3-29 11:12
Radiation Driven Winds of Hot Stars: Theory of O-Star Atmospheres as a Spectroscopic Toolms relating to the fomation of UV line spectra the use of accurate atomic data, the inclusion of EUV radiation by shock heated matter, the simulation of photospheric line blocking. A new tool for O-star diagnostics is presented. This is based on the use of wind models to calculate synthetic high res作者: ABIDE 時(shí)間: 2025-3-29 11:23
The Chemical Composition of B-supergiant Atmospheresst luminous Ia stars is close to its equilibrium value. The is also some evidence for more moderate CN abundance anomalies in the B2Ib and B2II supergiants. These results, together with other recent work, imply that the effects of the CNO bi-cycle on the composition of B-supergiant atmospheres are m作者: orthopedist 時(shí)間: 2025-3-29 15:33 作者: 貴族 時(shí)間: 2025-3-29 22:53 作者: 狗舍 時(shí)間: 2025-3-30 01:14 作者: 中國(guó)紀(jì)念碑 時(shí)間: 2025-3-30 07:13
LTE and NLTE Abundances in A-Supergiants a Test of Their Evolutionary Statuses between the scenarios depend on the input assumptions for several physical parameters, ., treatments for convection parameters and mass loss rates. A review of the predictions of evolution calculations for 10–30 solar mass stars is given by Fitzpatrick & Garmany (1991).作者: 蕨類 時(shí)間: 2025-3-30 10:04
A Spectroscopic Analysis of B Stars in the SMC Cluster NGC 330een analyzed in order to determine their atmospheric parameters and the evolutionary status. Stellar parameters are determined by comparison with LTE and NLTE model atmosphere calculations and an HR diagram constructed. Luminosities of the sample stars lie in the range 4.0 < log(.*/.⊙) < 5.0 and spe作者: 暗語(yǔ) 時(shí)間: 2025-3-30 15:19 作者: 是限制 時(shí)間: 2025-3-30 16:55 作者: propose 時(shí)間: 2025-3-30 22:37 作者: ostracize 時(shí)間: 2025-3-31 04:57 作者: 煤渣 時(shí)間: 2025-3-31 08:59
https://doi.org/10.1007/978-3-658-21013-7cts on the mass and helium discrepancies and show that the first one is reduced by the use of spherical, non hydrostatic model atmospheres and that the second one is probably due to exposure of CNO material.作者: 解決 時(shí)間: 2025-3-31 12:28
Book 1994as due to their intrinsic brightness, they offer the (only until now) possibility to study the stellar content and stellar behaviour in distant galaxies. The last, say, 25 years, massive stars have been the subject of numerous meetings discussing the influence of massive stars on population synthesi作者: cartilage 時(shí)間: 2025-3-31 15:18
https://doi.org/10.1007/978-3-322-91326-5rly—type B stars in the investigated MC clusters we find the largest number of Be stars, while in the Milky Way this is shifted to somewhat later types. In the LMC, there may be a second frequency peak around B6.作者: 乳白光 時(shí)間: 2025-3-31 18:52 作者: NOT 時(shí)間: 2025-4-1 00:25 作者: Exonerate 時(shí)間: 2025-4-1 05:18
Be Stars in Young Clusters in the Magellanic Cloudsrly—type B stars in the investigated MC clusters we find the largest number of Be stars, while in the Milky Way this is shifted to somewhat later types. In the LMC, there may be a second frequency peak around B6.
