標(biāo)題: Titlebook: Mass Loss and Evolution of O-Type Stars; P. S. Conti,C. W. H. Loore Book 1979 International Astronomical Union 1979 spectroscopy.star.stel [打印本頁(yè)] 作者: Clientele 時(shí)間: 2025-3-21 19:24
書(shū)目名稱(chēng)Mass Loss and Evolution of O-Type Stars影響因子(影響力)
書(shū)目名稱(chēng)Mass Loss and Evolution of O-Type Stars影響因子(影響力)學(xué)科排名
書(shū)目名稱(chēng)Mass Loss and Evolution of O-Type Stars網(wǎng)絡(luò)公開(kāi)度
書(shū)目名稱(chēng)Mass Loss and Evolution of O-Type Stars網(wǎng)絡(luò)公開(kāi)度學(xué)科排名
書(shū)目名稱(chēng)Mass Loss and Evolution of O-Type Stars被引頻次
書(shū)目名稱(chēng)Mass Loss and Evolution of O-Type Stars被引頻次學(xué)科排名
書(shū)目名稱(chēng)Mass Loss and Evolution of O-Type Stars年度引用
書(shū)目名稱(chēng)Mass Loss and Evolution of O-Type Stars年度引用學(xué)科排名
書(shū)目名稱(chēng)Mass Loss and Evolution of O-Type Stars讀者反饋
書(shū)目名稱(chēng)Mass Loss and Evolution of O-Type Stars讀者反饋學(xué)科排名
作者: resilience 時(shí)間: 2025-3-21 20:29 作者: eucalyptus 時(shí)間: 2025-3-22 02:23 作者: Connotation 時(shí)間: 2025-3-22 06:36
Analysis of UV Spectrophotometric Observations for O-type Starsesolution of 35–40 A, depending on the channel, in the wavelength range 1350–2550 A. The Copernicus catalogue gives spectra between 1000 and 1450 A for 17 O-type stars, with low reddening, at 0.2 A resolution.作者: evince 時(shí)間: 2025-3-22 10:32
Wolf-Rayet Stars in the Magellanic Clouds4 new WR stars of the WN type, afterwards confirmed by slit spectroscopy. In the LMC, two fields were also observed and 13 new faint WR stars detected. The results presented here mainly concern the SMC WR stars.作者: landfill 時(shí)間: 2025-3-22 13:53 作者: beta-cells 時(shí)間: 2025-3-22 18:05 作者: 幻影 時(shí)間: 2025-3-22 23:57
C IV Resonance Line Profiles in O Starsen 3 and 4 ?, as well as thousands of stars at longer wavelengths and correspondingly lower resolution. An atlas of spectra for types O4 to B5 is illustrated in Paper I. That figure shows that the P Cygni profile is a characteristic of all supergiants earlier than B3 and main sequence stars earlier than 08.作者: 種族被根除 時(shí)間: 2025-3-23 05:24 作者: 共同確定為確 時(shí)間: 2025-3-23 07:27
The O Stars: Optical Reviewss rates may account for a large fraction of the new matter injected into the interstellar medium, and they probably power some significant fraction of the hard X-ray sources in the galaxy, by virtue of the fact that a companion can become a neutron star a) without disrupting the binary and b) while the companion is still a mass losing O star.作者: anagen 時(shí)間: 2025-3-23 13:26
Temperatures and Radii of O Starsws through the stellar atmosphere. Distances have been estimated for all the stars and linear diameters found. The average radius for an 08 to 09.5 supergiant is about 23.3 R .; the radii for luminosity class III and Class V 0 stars lie in the range 6.8 to 10.7. R.作者: BRAWL 時(shí)間: 2025-3-23 16:00 作者: 表示向下 時(shí)間: 2025-3-23 21:31 作者: 抱狗不敢前 時(shí)間: 2025-3-24 00:51
O VI in Stellar Winds velocities to ?1380 and ?1000 km s. respectively. In contrast, the absorptions are narrower with steeper wings in ζ Oph and υ Ori. The latter star also has emission, while in Oph the absorption is split into two components from about ?1550 to ?1280 and ?1280 to ?980 km s..作者: unstable-angina 時(shí)間: 2025-3-24 05:52 作者: 不足的東西 時(shí)間: 2025-3-24 06:41
G. Hammerschlag-Hensbergeg with liquid or solid samples; the combination of high resolution and magic angle spinning (HR/MAS) of solid samples provides a wealth of structural information which is complementary to that obtained by X-ray crystallography. The same suite of techniques, slightly adapted, is now available to thos作者: attenuate 時(shí)間: 2025-3-24 12:10
Carlo Morossi,Roberto Stalio,Lucio Crivellariused to prepare new copolymers. Methylenecycloalkanes are polymerized by transition metal complexes to produce polymers via addition polymerization or ring-opening polymerization. Copolymerization of dienes with CO is promoted by late transition metal complexes to give polyketones with vinyl groups 作者: Seminar 時(shí)間: 2025-3-24 18:10 作者: fledged 時(shí)間: 2025-3-24 20:04
S. B. Parsons,J. D. Wray,K. G. Henize,G. F. Benedict作者: exclusice 時(shí)間: 2025-3-25 01:01 作者: 代替 時(shí)間: 2025-3-25 04:26 作者: 高度贊揚(yáng) 時(shí)間: 2025-3-25 09:23
H Alpha Variations in Two Mass Losing Starsatory. The observations have been made at the Cassegrain focus of the 1.93 m. The dispersion of the spectrograph was 17 ?.mm. at H. and the slit was 300μ wide. The detector was a cooled SIT TV camera tube commercially available under the name of “Nocticon”.Details on the observing technique have bee作者: ticlopidine 時(shí)間: 2025-3-25 14:15
Short Term Variability of Line Strengths in Some of and WR Starsate to phenomena which are reasonably well understood, as for example the Beta Canis Majoris stars, which are short period pulsators. In other cases, such as the Of and WR stars, the mechanism responsible for the variation is not fully understood. Models proposed to explain this variability include:作者: 火花 時(shí)間: 2025-3-25 16:57 作者: epinephrine 時(shí)間: 2025-3-25 21:59 作者: 不持續(xù)就爆 時(shí)間: 2025-3-26 02:45 作者: Enervate 時(shí)間: 2025-3-26 06:07 作者: 男學(xué)院 時(shí)間: 2025-3-26 08:28
Wolf-Rayet Stars in the Magellanic Clouds for WR stars in the SMC had ever been made, a survey was carried out with the ESO Objective Prism Astrograph which resulted in the identification of 4 new WR stars of the WN type, afterwards confirmed by slit spectroscopy. In the LMC, two fields were also observed and 13 new faint WR stars detected作者: Accolade 時(shí)間: 2025-3-26 16:28
Stellar Outflow: Relative Motions of Nebulae and of Starsly formed hot stars and the surrounding interstellar medium are sufficiently different so that typical H II regions should consist of material which is continually being replaced by the ambient medium and which should therefore possess the velocity of the medium rather than that of the star. Obvious作者: 使成整體 時(shí)間: 2025-3-26 17:42
An Ultraviolet View of Stellar Windsrtially evident from earlier ground-based observations. Ultraviolet resonance lines of a variety of ionization stages of several common elements provide a comprehensive probe of the low-density, extended winds. Three general types of information have been derived from ultraviolet spectroscopy of mas作者: 失眠癥 時(shí)間: 2025-3-26 21:33 作者: arcane 時(shí)間: 2025-3-27 02:27 作者: 使痛苦 時(shí)間: 2025-3-27 05:36
C IV Resonance Line Profiles in O Stars1 film with a 15 cm aperture objective-prism telescope. everal hundred early-type stars wer observed in the vicinity of 1550 ? with a resolution between 3 and 4 ?, as well as thousands of stars at longer wavelengths and correspondingly lower resolution. An atlas of spectra for types O4 to B5 is illu作者: 策略 時(shí)間: 2025-3-27 10:33
Winds in Hot, Subluminous Starst only do the young, massive OB stars (the subjects of our discussion in this symposium, so far) undergo high-velocity mass-loss, but so also do hot evolved, solar mass stars, among them the central star of planetary nebulae. In this talk, I would like to show ultraviolet spectra of two central star作者: 歡笑 時(shí)間: 2025-3-27 17:41 作者: Host142 時(shí)間: 2025-3-27 17:46
Analysis of UV Spectrophotometric Observations for O-type Stars Measured with Copernicus” (Snow and Jenkins 1976) have been used to try to separate, by means of simple diagrams, O-type stars belonging to different luminosity classes and having different temperatures. The ESA catalogue gives absolute fluxes for 43 O-type stars, mostly reddened, with a spectral r作者: 遷移 時(shí)間: 2025-3-27 22:19
G. Hammerschlag-Hensbergeto gases, liquids, liquid crystals and solids (including polymers). Biochemists use it routinely for determining the structures of peptides and proteins, and it is also widely used in medicine (where it is often called MRI, Magnetic Resonance Imaging). With the advent of spectrometers operating at v作者: Gesture 時(shí)間: 2025-3-28 05:14
Carlo Morossi,Roberto Stalio,Lucio Crivellarion polymerization of 1,3-butadiene produces.-1,4-,.-1,4-, syndio-1,2-, and iso-1,2-polymers which are obtained selectively by choosing the catalysts and the reaction conditions. Lanthanides catalyze polymerization of 1,3-butadiene to produce the.-1,4-polymer with excellent selectivity. The lanthanoc作者: indignant 時(shí)間: 2025-3-28 09:09 作者: genesis 時(shí)間: 2025-3-28 11:03 作者: 集聚成團(tuán) 時(shí)間: 2025-3-28 18:39 作者: 禁令 時(shí)間: 2025-3-28 20:59
On the Formation of Continuous Spectrum and Emission Line Profiles of P CygniThe attempts to interpret the values of the observed radio and infrared fluxes of P Cygni via simple mass outflow models (constant outflow velocity or usual radiative acceleration outflow) lead to a strongdiscrepancy between the observed and the calculated values.作者: 枯萎將要 時(shí)間: 2025-3-29 01:32 作者: 頭盔 時(shí)間: 2025-3-29 04:48
Mass Loss Effects in the Spectrum of the O 6.5f Binary HD 153919ntified as OIII show an emission component. These lines indicate that the Of star is losing mass at a high rate. A detailed analysis of the radial velocities obtained from 76 spectrograms indicates that the outflow of the wind is not spherically symmetric: at the side where the Of star faces its companion the velocity of the wind has increased.作者: 可商量 時(shí)間: 2025-3-29 07:15
Mass Loss of B1Ia-O Supergiants and Evolutionary Consequencesabout B1Ia-O supergiants in this Symposium. Extensive high dispersion spectroscopic observations of four luminous B1 supergiants of the southern hemisphere have been carried out during 1972 and 1975 at ESO, La Silla. Some characteristic data of the program stars are summarized in Table 1.作者: 死亡 時(shí)間: 2025-3-29 13:37
Evidence for Non-Isotropic Mass Loss from Central Stars of Some Emission Nebulae–5, an H II region with striking symmetry, NGC 2359 a “ring nebula” and M1–67. The exciting stars in all three are centrally located and are of spectral types 06f (showing P Cygni profiles), WN 5 and WN 8 respectively.作者: 怒目而視 時(shí)間: 2025-3-29 19:17 作者: 隼鷹 時(shí)間: 2025-3-29 22:20
2366-2573 ry, but interwoven, analysis and critical discussion of the .This volume wholeheartedly engages with the current climate in higher education and provides not only a thorough analysis of the foundational elements constituting higher education but also a critical discussion of possible connections to 作者: 瘋狂 時(shí)間: 2025-3-30 01:56 作者: Myelin 時(shí)間: 2025-3-30 06:40 作者: 糾纏 時(shí)間: 2025-3-30 08:15
https://doi.org/10.1007/978-3-662-01208-6, the Optima XL-I centrifuge (developed by Beckman, Palo Alto, CA) is equipped with both a new photoelectric scanning absorption optical system enabling exact measurement of concentration profiles at wavelengths of 190-800 nm and an interference optical system allowing the measurement of much higher作者: 柔聲地說(shuō) 時(shí)間: 2025-3-30 12:24 作者: 放逐 時(shí)間: 2025-3-30 19:34 作者: EWER 時(shí)間: 2025-3-30 22:34 作者: 北極人 時(shí)間: 2025-3-31 01:47
Annette Riedel,Anne-Christin LindeHilfestellung bei moralischen Konflikten im Pflegealltag.Entwicklung und Bedeutung der Ethikberatung in der Praxis.Ethisch fundiertes Handeln nach dem Pflegeberufereformgesetz verstehen und konkret um作者: upstart 時(shí)間: 2025-3-31 06:53 作者: parallelism 時(shí)間: 2025-3-31 12:20
Leitfaden des Baubetriebs und der Bauwirtschafthttp://image.papertrans.cn/k/image/540098.jpg
