標題: Titlebook: Be and Shell Stars; Arne Slettebak (Chairman) Book 1976 Springer Science+Business Media Dordrecht 1976 photometry.spectroscopy.star.stella [打印本頁] 作者: 積聚 時間: 2025-3-21 19:12
書目名稱Be and Shell Stars影響因子(影響力)
書目名稱Be and Shell Stars影響因子(影響力)學科排名
書目名稱Be and Shell Stars網(wǎng)絡公開度
書目名稱Be and Shell Stars網(wǎng)絡公開度學科排名
書目名稱Be and Shell Stars被引頻次
書目名稱Be and Shell Stars被引頻次學科排名
書目名稱Be and Shell Stars年度引用
書目名稱Be and Shell Stars年度引用學科排名
書目名稱Be and Shell Stars讀者反饋
書目名稱Be and Shell Stars讀者反饋學科排名
作者: originality 時間: 2025-3-21 23:14
https://doi.org/10.1007/978-3-031-05328-3The early history of the studies on Be stars is reviewed. The importance of keeping in mind a basic model of a Be star is emphasized, and the binary star model is suggested as one serious possibility at least for some Be stars.作者: 絆住 時間: 2025-3-22 02:28
Lecture Notes in Computer ScienceAt the Haute Provence Observatory, a survey of the Be stars brighter than the seventh magnitude was initiated by Herman and her collaborators twenty years ago.作者: Blanch 時間: 2025-3-22 06:59 作者: cortisol 時間: 2025-3-22 11:56
https://doi.org/10.1007/978-1-4899-0936-7A model for the shell star HD 50138 is inferred from the observation of the continuous spectrum from 0.14 to 10 ..作者: 挖掘 時間: 2025-3-22 15:34
https://doi.org/10.1007/978-1-4613-2823-0The appearance of singly ionized iron emission lines in the spectra of early type stars is studied, and the results of a spectroscopic investigation of EW Lac and other Be stars are given. We also discuss the atomic processes of excitation of Fe ti in the stellar envelopes using a two-parameter diagram W, ......作者: genesis 時間: 2025-3-22 17:43 作者: 勉勵 時間: 2025-3-22 21:54 作者: 有斑點 時間: 2025-3-23 03:49
Rapid Variations of H, in Be StarsPhotoelectric spectrum scans of Be stars were analysed to study the short-term variations of H. emission strengths. In . Tau, . Col, PP Car, and . Cen, definite variations of a few percent with time scales of 1 to 3 minutes were found. These variations do not exhibit any periodicity.作者: cloture 時間: 2025-3-23 08:20
A Model for the Shell of HD 50138A model for the shell star HD 50138 is inferred from the observation of the continuous spectrum from 0.14 to 10 ..作者: 酷熱 時間: 2025-3-23 11:22
Singly-Ionized Iron Emission Lines in the Spectra of Early Type StarsThe appearance of singly ionized iron emission lines in the spectra of early type stars is studied, and the results of a spectroscopic investigation of EW Lac and other Be stars are given. We also discuss the atomic processes of excitation of Fe ti in the stellar envelopes using a two-parameter diagram W, ......作者: outskirts 時間: 2025-3-23 16:43
Rapid Variations in the Spectra of , and, , Cas, and , Ophf about one day. Its binary nature is doubtful according to Olsen (1972). We have detected rapid spectroscopic variations in October 1973 when . And had no envelope, that is, when it appeared as a ‘normal’ B star. Spectrograms of 7.2 ? mm. dispersion were obtained at the Haute Provence Observatory with exposure times ranging from 12 min to 52 min.作者: graphy 時間: 2025-3-23 21:09 作者: 獎牌 時間: 2025-3-23 22:30 作者: 復習 時間: 2025-3-24 04:54
Pleione as a Variable Staric observations in the 1930’s. The light curve of this star from the end of the 19th century to 1954 was studied by Binnendijk (1949, 1955). Botsula and Sharov (1959) and Sharov (1961) added some old and new observations and continued the light curve up to 1959.作者: 北極熊 時間: 2025-3-24 10:36
Energy Distributions of Be Starsinuities in emission do exist. Furthermore, the filling in of the Balmer continuum near the discontinuity is usually observed. The continuum emission showing a peak near 1 . is a common feature in the energy distributions presented here..Energy distributions for a number of bright field Be stars are also presented and discussed.作者: diskitis 時間: 2025-3-24 14:08
Be and Shell Stars978-94-010-1498-4Series ISSN 1743-9213 Series E-ISSN 2352-2186 作者: palpitate 時間: 2025-3-24 15:11 作者: 我不重要 時間: 2025-3-24 21:59 作者: 花束 時間: 2025-3-25 02:28
https://doi.org/10.1007/978-1-4899-0936-7e fait partie de notre programme d’observation qui concerne les étoiles Be de magnitude ≤7 et de déclinaison≥ ?15°. Parmi les étoiles les plus chaudes de ce programme, on peut signaler au moins deux catégories:作者: 創(chuàng)造性 時間: 2025-3-25 03:57
https://doi.org/10.1007/978-1-4613-2823-0ic observations in the 1930’s. The light curve of this star from the end of the 19th century to 1954 was studied by Binnendijk (1949, 1955). Botsula and Sharov (1959) and Sharov (1961) added some old and new observations and continued the light curve up to 1959.作者: Canary 時間: 2025-3-25 10:53 作者: 防水 時間: 2025-3-25 15:34
Lecture Notes in Computer Sciencests and knowledge. I hope however at least to mention all forms of observed behaviour within these limitations, but note that as we have specific sessions on energy distributions, rotation, observations at unusual wavelengths (i.e., not from 3500 to 6700 ?), and polarisation, I shall deal less thoro作者: 倫理學 時間: 2025-3-25 16:08 作者: 生氣地 時間: 2025-3-25 20:24
Adam Wojciechowski,Krzysztof Gorzynskihave inferred ages and intrinsic (. — .) colors of Be stars to permit a discussion of their evolutionary states..Rotating stars can become Be stars in their early hydrogen burning evolution away from the main sequence. Both the fraction of stars showing hydrogen emission and the strength of emission作者: 拖網(wǎng) 時間: 2025-3-26 03:28
Lecture Notes in Computer Sciencef about one day. Its binary nature is doubtful according to Olsen (1972). We have detected rapid spectroscopic variations in October 1973 when . And had no envelope, that is, when it appeared as a ‘normal’ B star. Spectrograms of 7.2 ? mm. dispersion were obtained at the Haute Provence Observatory w作者: 分開 時間: 2025-3-26 05:02 作者: chastise 時間: 2025-3-26 11:13 作者: Matrimony 時間: 2025-3-26 13:12
Prefatory Remarks on Part I: Law and Codeentral intensities of both lines vary periodically with the period of velocity changes equal to 46.194 days, reaching two maxima and minima each cycle. Radia-velocity curves of individual Balmer lines differ systematically one from another, the amplitude of the H. variations being largest. The ./. r作者: dithiolethione 時間: 2025-3-26 17:46
Mireille Hildebrandt,Jeanne Gaakeerring their observed profiles of Hγ and H. with those computed from the Princeton model atmospheres and the VCS theory of hydrogen line broadening. The program stars are predominately well-known Be stars and display a wide range of envelope spectra and . sin .. The mean and range in log . for the Be 作者: septicemia 時間: 2025-3-26 23:59
Prefatory Remarks on Part I: Law and Codeity class III. These stars show similar features in the variation of the intensities, the profiles, and the radial velocities of the shell lines. An attempt has been made to explain the evolution of these unstable features.作者: MOCK 時間: 2025-3-27 02:42
https://doi.org/10.1007/978-1-4899-0936-7e fait partie de notre programme d’observation qui concerne les étoiles Be de magnitude ≤7 et de déclinaison≥ ?15°. Parmi les étoiles les plus chaudes de ce programme, on peut signaler au moins deux catégories:作者: 枯萎將要 時間: 2025-3-27 08:19
https://doi.org/10.1007/978-1-4613-2823-0ic observations in the 1930’s. The light curve of this star from the end of the 19th century to 1954 was studied by Binnendijk (1949, 1955). Botsula and Sharov (1959) and Sharov (1961) added some old and new observations and continued the light curve up to 1959.作者: Condense 時間: 2025-3-27 09:35 作者: 歡笑 時間: 2025-3-27 13:46
https://doi.org/10.1007/978-94-010-1498-4photometry; spectroscopy; star; stellar作者: 光亮 時間: 2025-3-27 19:27 作者: 摘要記錄 時間: 2025-3-28 00:45 作者: Endoscope 時間: 2025-3-28 04:10
Book 1976go, a number of participants expressed the wish to organize a symposium on Be and shell stars. If we wish to identify an official ‘Father of IAU Symposium No. 70‘, it would be Mirek Plavec who, in his capacity as President of IAU Commission 42 (Photometric Double Stars) requested and received the co作者: 貴族 時間: 2025-3-28 06:39 作者: Density 時間: 2025-3-28 11:08
A Study of Be Stars in Clustersf the effect, the extreme Be stars would be excellent probes for studies of spiral structure and would also serve as probes for studies of ages and distances of extragalactic systems..Analysis of the corrected colors of the Be stars in clusters suggests that the Lucy and Solomon (1970) mechanism for作者: Indelible 時間: 2025-3-28 14:48
New Observational Data Concerning 4 Her and , Taueral distinct velocity systems are present in the Balmer lines, not a continuous progression. (2) The main absorption component of the H. line does not share the long-term velocity variations, its velocity being always rather close to the systemic velocity +22 kms.. (3) The pseudoperiod of the long-作者: instate 時間: 2025-3-28 20:16
Marcin Woliński,Dominika Rogozińskaluminosity stars showing emission, 70 displayed shell structure in Ha at one or both epochs, though in over half of these cases the shell absorption was considered ‘weak’. Thirty of the 70 stars varied in their shell characteristics between the two epochs. The total number of stars whose Hα line var作者: Innovative 時間: 2025-3-29 00:54
Adam Wojciechowski,Krzysztof Gorzynskif the effect, the extreme Be stars would be excellent probes for studies of spiral structure and would also serve as probes for studies of ages and distances of extragalactic systems..Analysis of the corrected colors of the Be stars in clusters suggests that the Lucy and Solomon (1970) mechanism for作者: dura-mater 時間: 2025-3-29 05:20
Prefatory Remarks on Part I: Law and Codeeral distinct velocity systems are present in the Balmer lines, not a continuous progression. (2) The main absorption component of the H. line does not share the long-term velocity variations, its velocity being always rather close to the systemic velocity +22 kms.. (3) The pseudoperiod of the long-作者: 確定 時間: 2025-3-29 07:16
Spectra and Photometry of Be Starsughly, if at all, with these topics. I shall also attempt to incorporate the results of the speakers who follow in this session, in order to save duplication of individual introductions and allow the later presentations to concentrate more on the relevant discussions. I shall deal with nine aspects of Be stars behaviour, under the headings below.作者: FRAUD 時間: 2025-3-29 15:27
1743-9213 er (Cap Cod), Massachusetts, U. S. A. , from September 15th through 18th, 1975. Fifty-three astronomers from Argentina, Belgium, Canada, Czechoslovakia, France, Israel, the United Kingdom, the United States, and the Vatican attended and participated in the Symposium. This volume, which parallels the作者: 改革運動 時間: 2025-3-29 19:28
Caroline Brun,Maud Ehrmann,Guillaume Jacquet months. The other seven showed large and random changes..Warnings are given about the difficulty of tuning such a filter exactly to H. and the need to monitor accurately the filter for long term changes in passband and throughput.作者: 古代 時間: 2025-3-29 21:01
https://doi.org/10.1007/978-94-007-6314-2g Ca II triplet emission without H and K emission is discussed. The implications of this phenomenon on the structure of Be envelopes and possibly the binary nature of some Be stars is discussed..Evidence indicating the presence of cool companions to the Be stars HD 218393 and HR 894 is presented.作者: 畢業(yè)典禮 時間: 2025-3-30 03:41 作者: 先驅(qū) 時間: 2025-3-30 06:58 作者: Canary 時間: 2025-3-30 09:16 作者: 旁觀者 時間: 2025-3-30 13:35 作者: hurricane 時間: 2025-3-30 16:40 作者: SLUMP 時間: 2025-3-31 00:25
Book 1976d), Massachusetts, U. S. A. , from September 15th through 18th, 1975. Fifty-three astronomers from Argentina, Belgium, Canada, Czechoslovakia, France, Israel, the United Kingdom, the United States, and the Vatican attended and participated in the Symposium. This volume, which parallels the actual pr作者: packet 時間: 2025-3-31 04:08 作者: glans-penis 時間: 2025-3-31 08:36 作者: Mindfulness 時間: 2025-3-31 09:22 作者: LUMEN 時間: 2025-3-31 15:32 作者: Abominate 時間: 2025-3-31 17:48 作者: 我要沮喪 時間: 2025-3-31 23:06 作者: Endearing 時間: 2025-4-1 02:25
New Observational Data Concerning 4 Her and , Tauentral intensities of both lines vary periodically with the period of velocity changes equal to 46.194 days, reaching two maxima and minima each cycle. Radia-velocity curves of individual Balmer lines differ systematically one from another, the amplitude of the H. variations being largest. The ./. r作者: 機制 時間: 2025-4-1 06:25
The Surface Gravities of Be Starsring their observed profiles of Hγ and H. with those computed from the Princeton model atmospheres and the VCS theory of hydrogen line broadening. The program stars are predominately well-known Be stars and display a wide range of envelope spectra and . sin .. The mean and range in log . for the Be 作者: Daily-Value 時間: 2025-4-1 12:29
A Comparative Study of the Shell of , Tau and 48 Libity class III. These stars show similar features in the variation of the intensities, the profiles, and the radial velocities of the shell lines. An attempt has been made to explain the evolution of these unstable features.
