標題: Titlebook: Astrophysics and Space Science; Volume 255, 1997/199 John Dyson,Susan A. Lamb,P. A. Zaal Book 1998 Springer Science+Business Media New York [打印本頁] 作者: estrange 時間: 2025-3-21 18:31
書目名稱Astrophysics and Space Science影響因子(影響力)
書目名稱Astrophysics and Space Science影響因子(影響力)學科排名
書目名稱Astrophysics and Space Science網(wǎng)絡公開度
書目名稱Astrophysics and Space Science網(wǎng)絡公開度學科排名
書目名稱Astrophysics and Space Science被引頻次
書目名稱Astrophysics and Space Science被引頻次學科排名
書目名稱Astrophysics and Space Science年度引用
書目名稱Astrophysics and Space Science年度引用學科排名
書目名稱Astrophysics and Space Science讀者反饋
書目名稱Astrophysics and Space Science讀者反饋學科排名
作者: 高度表 時間: 2025-3-21 23:24 作者: GREEN 時間: 2025-3-22 00:40 作者: arrogant 時間: 2025-3-22 06:40 作者: Occlusion 時間: 2025-3-22 12:25
https://doi.org/10.1007/978-1-4302-0308-7rina spiral arm at a distance of 2.2 kpc (Chini et al., 1980). The cloud core M17-North is a dust condensation located 10′ north of the exciting stars of M17. It was investigated only by low-resolution studies of the whole cloud complex (e.g. Gatley et al. 1979; Wilson et al. 1979).作者: 合法 時間: 2025-3-22 15:56
The Camera Object and Flash Video,(FCS) with known output power. However, the short-period drifts of the C-100 detectors at the beginning of a measurement are on the same order of magnitude as the response to both faint source fluxes and the corresponding FCS power. Thus other techniques for calibrating ISOPHOT data on faint sources are sought.作者: 東西 時間: 2025-3-22 19:53 作者: GRE 時間: 2025-3-22 23:44
The Intermittently Embedded Herbig AE/BE StarsBe stars which are viewed edge-on to their polarimetrically identified dust and gas disks. The ISO SWS observations confirm the lack of a simple correlation between system age and the profile shape. Comparison with laboratory silicates suggests that much of the observed variation is due to different annealing histories of the grains.作者: Osteons 時間: 2025-3-23 04:30 作者: Frequency-Range 時間: 2025-3-23 06:49 作者: 道學氣 時間: 2025-3-23 12:10 作者: GUISE 時間: 2025-3-23 14:12
ISOPHOT Observations of Vega and Vega-Like Starshigh resolution 60.m scan data to compare with 60.m and 90.m oversampled maps. The dust disk around Vega is clearly resolved. In addition similar maps of HD98800, SAO226057, SAO186777 and α Piscis ustrinus (HR8728) are evaluated, resolving the disks of two Vega-like stars/candidates and providing upper limits for the size of the other two.作者: 哎呦 時間: 2025-3-23 21:04 作者: 招惹 時間: 2025-3-24 01:15 作者: 窗簾等 時間: 2025-3-24 02:39 作者: 揭穿真相 時間: 2025-3-24 07:43
Flash lite mobile entertainment basicsontinued theoretical progress, these observations have pushed our understanding of the overall star formation process to a satisfying level. We now believe that we understand the phases a dense interstellar cloud passes through in the process of becoming a young star, and we have observational examp作者: 抗原 時間: 2025-3-24 13:12 作者: inflame 時間: 2025-3-24 14:53 作者: 建筑師 時間: 2025-3-24 19:00
The future of flash in the mobile world, but it no longer occurs inside a star-forming region, so that it can be considered a transition object between the youngest, embedded, stars and main-sequence objects such as Beta Pic, a phase in which the radiation which characterizes the circumstellar dust disk diminishes.作者: Adenoma 時間: 2025-3-25 00:55
Flash lite mobile entertainment basicsral energy distributions (SEDs) in the far-infrared, attributed to thermal emission of heated circumstellar dust, the remnant of star formation. A significant fraction of the much older main-sequence B and A-type stars also shows excess emission at λ ≥ 25μm (the so-called Vega-phenomenon, Backman an作者: 緯度 時間: 2025-3-25 04:21
https://doi.org/10.1007/978-1-4302-0308-7rina spiral arm at a distance of 2.2 kpc (Chini et al., 1980). The cloud core M17-North is a dust condensation located 10′ north of the exciting stars of M17. It was investigated only by low-resolution studies of the whole cloud complex (e.g. Gatley et al. 1979; Wilson et al. 1979).作者: 的染料 時間: 2025-3-25 11:33 作者: 包裹 時間: 2025-3-25 14:54
Creating and Playing Flash Video,6 IR and Cep A East. Excitation temperatures and masses were derived from the low-lying pure rotational levels of H2 and are 490 and 740 K and 0.04 and 0.007 M⊙ for S106 and Cep A, respectively. The observations were compared to theoretical models for PDRs and dissociative and non-dissociative shock作者: Glossy 時間: 2025-3-25 18:15 作者: Debark 時間: 2025-3-25 23:08
https://doi.org/10.1007/978-1-4302-0578-4ometer (LWS). The selected targets show a range of pre-main sequence evolutionary phases. Whereas some objects still show interstellar ice features, the most evolved objects are coincident with ultracompact HII regions and show strong emission lines from atomic species and polycyclic aromatic hydroc作者: 載貨清單 時間: 2025-3-26 01:48
Creating and Playing Flash Video,l be discussed. The dust is understood to represent debris related to planet formation, and the known disk systems may be dense analogs of the Kuiper Belt structure in our outer solar system. ISO observing programs plan to address questions regarding how common planetary material is around normal st作者: 神圣不可 時間: 2025-3-26 04:33
Going Small and Going Big with Flash Video,e usually skips when thinking about stellar evolution. In early and in late stages of evolution, stars interact much more intensely with their environment. It is this interaction and the circumstellar material involved rather than the star itself which makes them an interesting subject of infrared a作者: decode 時間: 2025-3-26 09:14 作者: 使人煩燥 時間: 2025-3-26 13:40 作者: semiskilled 時間: 2025-3-26 20:35 作者: 助記 時間: 2025-3-26 23:54 作者: 注意到 時間: 2025-3-27 04:50
The Camera Object and Flash Video,In this paper we present a comparison of the observed absorption band at about 660 cm. (15.1 μm) toward NGC7538 IRSI attributed to the bending mode of solid CO. with laboratory spectra of ion irradiated mixtures.作者: keloid 時間: 2025-3-27 07:57
https://doi.org/10.1007/978-1-4302-0578-4The DEBRIS project is a search for infrared excess around Sun-like main sequence stars, and other types of stellar targets, using the Infrared Space Observatory.. Some results, calibration issues, and changes to our original program are presented. Future platforms for advancing this project after the conclusion of the ISO mission are indicated.作者: 構(gòu)想 時間: 2025-3-27 09:39 作者: 1FAWN 時間: 2025-3-27 16:01 作者: 現(xiàn)暈光 時間: 2025-3-27 21:03
Relation Between Stellar Evolution and Circumstellar Processes evolution of the central body. On the contrary, during main-sequence (MS) and post-MS phases the central star determines the evolution of the circumstellar medium (CS). In these late phases the CS material can provide a most useful diagnosis on stellar evolution, particularly on the amount of mater作者: HILAR 時間: 2025-3-28 01:13
Protostars and Protoplanetary Disksontinued theoretical progress, these observations have pushed our understanding of the overall star formation process to a satisfying level. We now believe that we understand the phases a dense interstellar cloud passes through in the process of becoming a young star, and we have observational examp作者: mastopexy 時間: 2025-3-28 06:06
ISO Observations of Isolated Herbig AE/BE Starsrsity of emission features of carbon-rich and oxygen-rich rains. The similarity of the forsterite spectra observed for Comet Hale-Bopp and the Haebe star HD100546 is particularly striking and provides a new argument that huge comet swarms are formed in the disks surrounding young stars. While the da作者: foodstuff 時間: 2025-3-28 09:06 作者: 狂亂 時間: 2025-3-28 13:30 作者: 赤字 時間: 2025-3-28 15:52 作者: ORE 時間: 2025-3-28 19:09 作者: 強所 時間: 2025-3-29 00:41 作者: 名字的誤用 時間: 2025-3-29 05:15
PDRs and Shocks in S106 IR and Cep A East6 IR and Cep A East. Excitation temperatures and masses were derived from the low-lying pure rotational levels of H2 and are 490 and 740 K and 0.04 and 0.007 M⊙ for S106 and Cep A, respectively. The observations were compared to theoretical models for PDRs and dissociative and non-dissociative shock作者: Hot-Flash 時間: 2025-3-29 08:35
Search for H2 Emission from Disks Around T Tauri and Herbig Ae Starsctrometer (SWS) on the Infrared Space Observatory (ISO). The sources are selected to be isolated low- and intermediate-mass young stellar objects, for which the presence of a circumstellar disk has been established by millimeter interferometry. The lowest H. S(0) and S(1) lines are detected in 3 out作者: anus928 時間: 2025-3-29 11:23
Evolution of Southern Star-Forming Regionsometer (LWS). The selected targets show a range of pre-main sequence evolutionary phases. Whereas some objects still show interstellar ice features, the most evolved objects are coincident with ultracompact HII regions and show strong emission lines from atomic species and polycyclic aromatic hydroc作者: PALL 時間: 2025-3-29 16:49
Dust Disks Around Main Sequence Starsl be discussed. The dust is understood to represent debris related to planet formation, and the known disk systems may be dense analogs of the Kuiper Belt structure in our outer solar system. ISO observing programs plan to address questions regarding how common planetary material is around normal st作者: gout109 時間: 2025-3-29 21:19 作者: Cubicle 時間: 2025-3-30 00:20
Calibration of the Debris Project ISOPHOT Data(FCS) with known output power. However, the short-period drifts of the C-100 detectors at the beginning of a measurement are on the same order of magnitude as the response to both faint source fluxes and the corresponding FCS power. Thus other techniques for calibrating ISOPHOT data on faint sources作者: 打谷工具 時間: 2025-3-30 07:14 作者: 我們的面粉 時間: 2025-3-30 08:48 作者: SEMI 時間: 2025-3-30 12:58 作者: Loathe 時間: 2025-3-30 20:16 作者: wangle 時間: 2025-3-30 22:08
Flash lite mobile entertainment basicslieve that we understand the phases a dense interstellar cloud passes through in the process of becoming a young star, and we have observational examples of most of those phases. ISO will play a major role in testing this preliminary understanding of star formation, and in suggesting where it needs to be modified.作者: Aura231 時間: 2025-3-31 04:23
Flash lite mobile entertainment basicsellar ice analogs shows that the 7.24 μm band can be well matched by solid formic acid (HCOOH), while the 7.40 μm band can be fitted both by the formate ion (HCOO.) and acetaldehyde (CH.HCO). The laboratory spectra reveal additional strong features of these molecules which should make a more definite identification straightforward.作者: Statins 時間: 2025-3-31 07:09 作者: 歪曲道理 時間: 2025-3-31 09:19 作者: 形狀 時間: 2025-3-31 16:01
Protostars and Protoplanetary Diskslieve that we understand the phases a dense interstellar cloud passes through in the process of becoming a young star, and we have observational examples of most of those phases. ISO will play a major role in testing this preliminary understanding of star formation, and in suggesting where it needs to be modified.作者: Vertical 時間: 2025-3-31 19:22
ISO-SWS Observations of Weak Bands of Trace Components of Ices Towards the Young Stellar Object W 33ellar ice analogs shows that the 7.24 μm band can be well matched by solid formic acid (HCOOH), while the 7.40 μm band can be fitted both by the formate ion (HCOO.) and acetaldehyde (CH.HCO). The laboratory spectra reveal additional strong features of these molecules which should make a more definite identification straightforward.作者: handle 時間: 2025-3-31 22:54
Evolution of Southern Star-Forming Regionshe most evolved objects are coincident with ultracompact HII regions and show strong emission lines from atomic species and polycyclic aromatic hydrocarbons (PAHs). We discuss the ISO spectra between 2.5–200 .m of selected southern star-forming regions in the context of their evolution.作者: Orchiectomy 時間: 2025-4-1 05:08 作者: insert 時間: 2025-4-1 06:30
PDRs and Shocks in S106 IR and Cep A Easts. The infrared spectrum of S106 IR is dominated by PDR emission while that of Cep A East has a large shock component. We suggest that the difference between these two objects could reflect an evolutionary trend.
