標題: Titlebook: Effects of Mass Loss on Stellar Evolution; IAU Colloquium no. 5 C. Chiosi,R. Stalio Book 1981 D. Reidel Publishing Company, Dordrecht, Holl [打印本頁] 作者: autoantibodies 時間: 2025-3-21 19:57
書目名稱Effects of Mass Loss on Stellar Evolution影響因子(影響力)
書目名稱Effects of Mass Loss on Stellar Evolution影響因子(影響力)學(xué)科排名
書目名稱Effects of Mass Loss on Stellar Evolution網(wǎng)絡(luò)公開度
書目名稱Effects of Mass Loss on Stellar Evolution網(wǎng)絡(luò)公開度學(xué)科排名
書目名稱Effects of Mass Loss on Stellar Evolution被引頻次
書目名稱Effects of Mass Loss on Stellar Evolution被引頻次學(xué)科排名
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書目名稱Effects of Mass Loss on Stellar Evolution年度引用學(xué)科排名
書目名稱Effects of Mass Loss on Stellar Evolution讀者反饋
書目名稱Effects of Mass Loss on Stellar Evolution讀者反饋學(xué)科排名
作者: 食品室 時間: 2025-3-21 20:52 作者: 不自然 時間: 2025-3-22 00:39
Book 1981related to the problem of mass loss from stars - would have spurred thorough discussions on the many aspects and implications of this topic. We hope this goal has been achieved. Furthermore, the most recent observational and theoreti- cal developments on the problem of mass loss from early ty- pe st作者: 要求比…更好 時間: 2025-3-22 08:18
Summary, Conclusions, and Future Work,the WR mass loss may also be important for Of stars (Lamers 1980). A determination of the properties of the WR stellar winds will provide diagnostics which might aid in identifying the mass loss mechanism, and P-Cygni profiles form one important data source for this purpose. With the advent of IUE m作者: 帽子 時間: 2025-3-22 12:38 作者: 天氣 時間: 2025-3-22 15:56 作者: 天氣 時間: 2025-3-22 20:25 作者: 燒瓶 時間: 2025-3-23 00:08 作者: capsaicin 時間: 2025-3-23 03:25 作者: theta-waves 時間: 2025-3-23 07:50
An Introduction to Data Mining,± 100 km s.. Our preliminary evaluation of the associated mass loss rate gives 10. M. yr.. Other planetary nebulae nuclei are studied with low resolution IUE spectra and indications are found of mass loss rates consistent with the above value.作者: NICE 時間: 2025-3-23 10:08 作者: 支形吊燈 時間: 2025-3-23 17:04 作者: 有害 時間: 2025-3-23 21:42
Dimension Reduction and Feature Selectionree-free fluxes. The resultant mass loss rates show a range of only a factor of four. WC stars generally have larger mas loss rates than WN stars, the mean rates being .(WC) = 4.1×10. M.y. and .(WN) = 2.7×10. M.y.. Optical and ultraviolet data have been used to estimate bolometric luminosities for a作者: 專心 時間: 2025-3-24 01:08 作者: Cytokines 時間: 2025-3-24 06:12
Data Mining for Business Applicationsspectrograms were taken with the image-tube spectrographs of the 1-m and 4-m telescopes at the Cerro Tololo Inter-American Observatory (CTIO). The emulsion was always IIIa-J baked in “forming gas” (N2+H2). The “blue” spectrograms extend from 3600 to 5000 ? at 45 ? mm.; the “red” ones extend from 500作者: ALIEN 時間: 2025-3-24 07:32
Guido Cervone,Pasquale Franzeseics of mass loss are discussed with new theoretical calculations of chromospheric line profiles. A general picture of mass loss from cool stars is developed and related to chromospheric and coronal emissions measured by IUE and the HEAO-2 Obgervatory. These winds range in characteristics from the ho作者: Herbivorous 時間: 2025-3-24 11:25
Using Data Mining for CRM Evaluation, less typical of the spectrum of an M2 supergiant, except for their very great widths; 2) a shell spectrum consisting of P Cygni-type profiles of neutral and singly-ionized metallic lines of very low excitation potential; and 3) asymmetric absorption lines, including H., Hβ, FeI lines of intermediat作者: Headstrong 時間: 2025-3-24 16:52 作者: 連鎖 時間: 2025-3-24 21:57 作者: 去世 時間: 2025-3-25 00:46
Mass Loss Rates of OB Stars Derived from Infrared Observationstometry of 70 southern OB stars of various luminosity class has been secured. Program stars have been selected, among those bright enough in the infrared to give a suitable photometric accuracy, in order to cover a wide range of spectral types (Fig. 1).作者: 中子 時間: 2025-3-25 05:44
https://doi.org/10.1007/978-94-009-8500-1Accretion; Galaxy; star; stars; stellar作者: Fantasy 時間: 2025-3-25 08:09 作者: Hemiparesis 時間: 2025-3-25 12:32 作者: entail 時間: 2025-3-25 18:09
Effects of Mass Loss on Stellar Evolution978-94-009-8500-1Series ISSN 0067-0057 Series E-ISSN 2214-7985 作者: agitate 時間: 2025-3-25 23:12
https://doi.org/10.1007/978-1-4842-3159-3erved in the ultraviolet with IUE. From an analysis of the UV spectra we determine a terminal velocity of 3560 ± 100 km s. and a mass loss rate of (4.2 .) 10. M. yr.. A comparison is made with the stars of similar spectral type.作者: 失眠癥 時間: 2025-3-26 03:40 作者: 植物茂盛 時間: 2025-3-26 07:30 作者: 制定 時間: 2025-3-26 08:44
Organizing and Managing Queries,In addition to certain manifestation of a stellar wind during steady states of WR-stars that we have heard here about I have two notes on their extremal stages of evolution which may be also connected to such a hydrodynamical event.作者: comely 時間: 2025-3-26 14:08 作者: motor-unit 時間: 2025-3-26 17:53
A survey of Clustering AlgorithmsAG Car is a variable supergiant surrounded by a small ring nebula. Its ultraviolet and optical spectrum, and UV to IR energy distribution are similar to those of P Cyg with v. = -290 km s.. Also the strength of the 2200 A band is the same and suggests E(B-V) = 0.55 both stars. The possible variability of the infrared flux is discussed.作者: 創(chuàng)新 時間: 2025-3-26 22:34 作者: deciduous 時間: 2025-3-27 03:25
Robert P. Trueblood,John N. Lovett Jr.Contrary to the results of some investigators, the ratio of terminal to escape velocities (V∞/Vesc) observed for the winds in early-type stars is found to be linearly correlated with log г — г being the ratio of stellar to Eddington’s luminosities.作者: FRAX-tool 時間: 2025-3-27 08:22 作者: 執(zhí)拗 時間: 2025-3-27 10:05
Is a Stellar Wind Inherent in WR-Stars Throughout the Whole of their Evolution?In addition to certain manifestation of a stellar wind during steady states of WR-stars that we have heard here about I have two notes on their extremal stages of evolution which may be also connected to such a hydrodynamical event.作者: colony 時間: 2025-3-27 14:27 作者: 令人悲傷 時間: 2025-3-27 21:14
Mass Outflow in AG Carinae and a Comparison with P CygniAG Car is a variable supergiant surrounded by a small ring nebula. Its ultraviolet and optical spectrum, and UV to IR energy distribution are similar to those of P Cyg with v. = -290 km s.. Also the strength of the 2200 A band is the same and suggests E(B-V) = 0.55 both stars. The possible variability of the infrared flux is discussed.作者: Override 時間: 2025-3-28 01:39
Mass Loss from Hot Stars Below the Main SequenceThe evolutionary implications of mass loss from post-asymptotic giant branch stars is discussed, with reference to the UV observations of sdO’s.作者: 注視 時間: 2025-3-28 04:38 作者: Mercantile 時間: 2025-3-28 06:40 作者: 憂傷 時間: 2025-3-28 13:17 作者: 消息靈通 時間: 2025-3-28 18:15 作者: sterilization 時間: 2025-3-28 20:54
The Velocity Characteristics of WR Stellar Winds transitions of common ions and generally occur in the UV, and typical resonance lines of SiIV, CIV, NV and OVI are well known P-Cygni signatures of stellar winds in luminous OB stars. Analyses of these profiles can lead to important information concerning the velocity, density and temperature struc作者: Bmd955 時間: 2025-3-29 01:35 作者: 故意釣到白楊 時間: 2025-3-29 06:51 作者: llibretto 時間: 2025-3-29 09:30
Mass Loss from Central Stars of Planetary Nebulae± 100 km s.. Our preliminary evaluation of the associated mass loss rate gives 10. M. yr.. Other planetary nebulae nuclei are studied with low resolution IUE spectra and indications are found of mass loss rates consistent with the above value.作者: 的是兄弟 時間: 2025-3-29 12:08 作者: 釋放 時間: 2025-3-29 19:24
Radio Observations and the Mass Flow Rate of α CYG (A2Ia)icted a 10 GHz radio flux of 2.z mJy. On the other hand Praderie et al. (1980) derived a considerable lower mass loss rate of 1.1 10. ≤ . ≤ 7 10. M. yr. from a curve of growth analysis of the envelope ultraviolet Fell-lines of α Cyg. Radio observations are desirable to make a decision about these di作者: institute 時間: 2025-3-29 21:54 作者: 強所 時間: 2025-3-29 23:57
Observational Evidences of Stellar WindW) and its interaction with the interstellar medium (ISM). Lines arising from excited levels connected radiatively to the ground level tend to be more frequent and/or strong compared to those arising from radiatively forbidden levels of similar excitation as expected from radiatively driven wind. Th作者: 溫和女孩 時間: 2025-3-30 04:47
The Radial Velocity Variations in IC 418spectrograms were taken with the image-tube spectrographs of the 1-m and 4-m telescopes at the Cerro Tololo Inter-American Observatory (CTIO). The emulsion was always IIIa-J baked in “forming gas” (N2+H2). The “blue” spectrograms extend from 3600 to 5000 ? at 45 ? mm.; the “red” ones extend from 500作者: Arrhythmia 時間: 2025-3-30 08:56 作者: 愛花花兒憤怒 時間: 2025-3-30 14:36 作者: Exploit 時間: 2025-3-30 18:39 作者: ensemble 時間: 2025-3-30 23:14 作者: RUPT 時間: 2025-3-31 04:22
Giulia Massini,Stefano Terzi,Massimo Buscemar. from a curve of growth analysis of the envelope ultraviolet Fell-lines of α Cyg. Radio observations are desirable to make a decision about these discrepant results. Therefore we observed α Cyg at 15 GHz with the 100 m telescope of the MPIfR at Effelsberg. The observations are discussed together with recent VLA data of Abbott et al. (1980).作者: CT-angiography 時間: 2025-3-31 08:37
Using Data Mining for CRM Evaluation,ral and singly-ionized metallic lines of very low excitation potential; and 3) asymmetric absorption lines, including H., Hβ, FeI lines of intermediate excitation potential and the infrared triplet of Ca+, which appear to be formed in a relatively warm layer, probably an extended chromosphere.作者: Abominate 時間: 2025-3-31 11:48
Book 1981al Physics, Miramare, Trieste (Italy), under the auspices of the IAU Executive Co~ mittee and the Italian National Council of Research. The planning of this conference began two years ago du- ring the IAU Symposium No. 83 "Mass loss and evolution of 0 type stars" (Qualicum Beach, Victoria, Canada) w作者: 隱士 時間: 2025-3-31 14:38 作者: Orgasm 時間: 2025-3-31 20:00 作者: 神圣在玷污 時間: 2025-4-1 00:57 作者: progestogen 時間: 2025-4-1 05:12
The Radial Velocity Variations in IC 418ate were stored in computer memory and were later added together, in order to improve the signal-to-noise ratio. The resulting intensity tracings reveal more details than had previously been observed (Swings and Struve 1941, Aller and Wilson 1954, Andrillat 1957, Aller and Kaler 1964).作者: 開始沒有 時間: 2025-4-1 08:08
Data Preparation and Training Part I,eir winds in the resonance line P Cygni profiles in the UV region, in the emission lines of Hα and λ4686 He II in the optical spectrum, and in the free-free emission from the ionized plasma as observed in the IR and radio regions of the spectrum.作者: 觀察 時間: 2025-4-1 10:48
https://doi.org/10.1007/978-1-4613-0085-4ories. Absorption lines (P-Cygni like) of C II, Al II, Si II and Mg II shifted shortward by about 300 km s. suggest an expanding shell around the star. As this velocity is smaller than the terminal velocity (880 km s.) the circumstellar shell may have been formed as a result of interaction of SW with ISM.作者: Incorporate 時間: 2025-4-1 17:11
