標題: Titlebook: Dust and Molecules in Evolved Stars; Proceedings of an In Isabelle Cherchneff,Tom J. Millar Conference proceedings 1998 Springer Science+Bu [打印本頁] 作者: obdurate 時間: 2025-3-21 18:27
書目名稱Dust and Molecules in Evolved Stars影響因子(影響力)
書目名稱Dust and Molecules in Evolved Stars影響因子(影響力)學科排名
書目名稱Dust and Molecules in Evolved Stars網絡公開度
書目名稱Dust and Molecules in Evolved Stars網絡公開度學科排名
書目名稱Dust and Molecules in Evolved Stars被引頻次
書目名稱Dust and Molecules in Evolved Stars被引頻次學科排名
書目名稱Dust and Molecules in Evolved Stars年度引用
書目名稱Dust and Molecules in Evolved Stars年度引用學科排名
書目名稱Dust and Molecules in Evolved Stars讀者反饋
書目名稱Dust and Molecules in Evolved Stars讀者反饋學科排名
作者: jeopardize 時間: 2025-3-21 20:17
https://doi.org/10.1007/978-94-017-1307-8Galaxy; Star; astrophysics; cluster; molecule; spectra; stellar作者: 似少年 時間: 2025-3-22 00:33
978-90-481-5018-2Springer Science+Business Media Dordrecht 1998作者: Osmosis 時間: 2025-3-22 07:56
Theodore Pelagidis,Michael MitsopoulosIn this contribution, we present a few highlights of the guaranteed time program to observe AGB stars with differing chemical compositions and mass loss rates using ISO . SWS. We briefly discuss C.H. absorption in C-stars and 0-rich stars with the 13 μm dust emission.作者: 產生 時間: 2025-3-22 12:27 作者: ARENA 時間: 2025-3-22 13:18 作者: ARENA 時間: 2025-3-22 17:13
IR-Colors for Models of Post-AGB Evolution its effective temperature, .., starts to increase, which soon causes the mass loss rate to decrease significantly. When .. reaches about 30 000 K, the star eventually enters the planetary nebula (PN) phase. The transition from the AGB to the PN stage, believed to last a few thousand years, is called the . phase of evolution.作者: 事先無準備 時間: 2025-3-23 00:00
Theodore Pelagidis,Michael Mitsopoulos known features at 3.3, 6.2, 7.7, 8.6, and 11.3 μm a wealth of weaker features is present as well. These studies also reveal detailed variations from source to source, which may be of key importance in the molecular identification process. The emission from Polycyclic Aromatic Hydrocarbon molecules 作者: aesthetician 時間: 2025-3-23 05:04 作者: Immortal 時間: 2025-3-23 07:58
Theodore Pelagidis,Michael Mitsopouloslicity of their geometry and kinematics, and the large variety in their physical and chemical (C/O<1 as well as >1) characteristics, make them excellent targets for the study of molecular formation processes. This review presents a compilation of estimated molecular abundances, discusses the uncerta作者: Institution 時間: 2025-3-23 12:59 作者: lavish 時間: 2025-3-23 14:15
Theodore Pelagidis,Michael Mitsopoulosof the interstellar UV field can initiate a complex photochemistry. These models use as input the abundances of parent species which are either set from observational data or from LTE abundances, which are valid in the photosphere, and which assume that the molecules pass through the inner layers of作者: Omniscient 時間: 2025-3-23 19:25 作者: Osmosis 時間: 2025-3-24 00:17
No Villainous Mother—The Life of Eva Larkinjects. The observations reveal that there is an observable chemical evolution in the neutral gas as a star evolves beyond the AGB, through the proto-PN and PN phases. Significant changes in the abundances of some key molecules (such as CS, CN, HCO., HCN, and HC.N) take place during the fast evolutio作者: 衍生 時間: 2025-3-24 06:19
No Villainous Mother—The Life of Eva Larkinved stars. Where can we expect circumstellar molecular spectra, why would we want to study these spectra, which molecules might be present, and what can we learn from these studies? We present an overview of reported detections, and discuss some of the results.作者: bromide 時間: 2025-3-24 09:22
No Villainous Mother—The Life of Eva Larkinarbon-rich star with an oxygen-rich circumstellar envelope. The CO emission from both of these disks has a spike with a width near ~2 km s., indicating disk radii of 10. cm. The dust in such disks is therefore quite cold (near T ~ 50 K for the Red Rectangle) and may emit primarily at submillimeter w作者: 相信 時間: 2025-3-24 12:26
Wilhelm R?pke: Why He Was a Conservativeover the entire range observed for carbon Miras. The luminosities are calculated from a period-luminosity relation. Parameters derived are the distance, the dust mass loss rate and the ratio of silicon carbide to amorphous carbon dust. The total mass loss rate is derived from a modified relation bet作者: CLIFF 時間: 2025-3-24 18:28
Wilhelm R?pke and American Conservatismture is not yet well established. This subject has been addressed by several authors and good fits of a large number of IRAS sources (chosen among the carbon stars exhibiting the SiC feature at about 11.3 pm) were obtained. In this work we use the same procedure on a limited number of objects, of th作者: animated 時間: 2025-3-24 20:14 作者: browbeat 時間: 2025-3-25 01:23 作者: Working-Memory 時間: 2025-3-25 04:56
Was Wilhelm R?pke Really a Proto-Keynesian?te and oblate spheroids..It is shown that an asymmetry of the geometry of light scattering by non-spherical particles results in a component of the radiation pressure force . perpendicular to the wave-vector of incident light. For silicate spheroids, this component can exceed 20% of ∣.∣. For small m作者: assent 時間: 2025-3-25 08:12 作者: 朋黨派系 時間: 2025-3-25 13:20
Was Wilhelm R?pke Really a Proto-Keynesian?he geometrical and dynamical structure of winds is also necessary to improve models of mass loss. The fact that mass loss from red giants may be episodic has been recognized early: for example, Sauner (1976) showed multiple absorption components in circumstellar absorption lines Ridgway (1981) analy作者: 半身雕像 時間: 2025-3-25 18:06
Was Wilhelm R?pke Really a Proto-Keynesian? its effective temperature, .., starts to increase, which soon causes the mass loss rate to decrease significantly. When .. reaches about 30 000 K, the star eventually enters the planetary nebula (PN) phase. The transition from the AGB to the PN stage, believed to last a few thousand years, is calle作者: 控訴 時間: 2025-3-25 22:40 作者: Enliven 時間: 2025-3-26 01:55
No Villainous Mother—The Life of Eva Larkinved stars. Where can we expect circumstellar molecular spectra, why would we want to study these spectra, which molecules might be present, and what can we learn from these studies? We present an overview of reported detections, and discuss some of the results.作者: narcissism 時間: 2025-3-26 07:24 作者: 嘲笑 時間: 2025-3-26 10:32 作者: FRAUD 時間: 2025-3-26 16:22
ISO LWS Observations of Evolved Stars and Nebulaenfrared wavelengths by the Infrared Space Observatory (ISO) since its launch in November 1995. The results reported have been obtained mainly using ISO’s Long Wavelength Spectrometer (LWS; Clegg et al. 1996), but for some objects complementary spectra have also been obtained with the Short Wavelengt作者: occurrence 時間: 2025-3-26 18:10 作者: Femine 時間: 2025-3-26 21:19 作者: Hamper 時間: 2025-3-27 01:40
Silicon and Sulphur in the Inner Envelope of IRC+10216of the interstellar UV field can initiate a complex photochemistry. These models use as input the abundances of parent species which are either set from observational data or from LTE abundances, which are valid in the photosphere, and which assume that the molecules pass through the inner layers of作者: Pseudoephedrine 時間: 2025-3-27 08:54
Maser Mapping and Dust Properties of Red Supergiant Windsind is driven by radiation pressure on dust and the structure and kinematics of the masing regions reflect the dust properties. The unbeamed radius of water maser blobs, ~ 10. m, has been measured for the first time. The velocity gradient is used to derive the dust absorption coefficient which incre作者: 仲裁者 時間: 2025-3-27 12:12 作者: 謙虛的人 時間: 2025-3-27 14:02 作者: Measured 時間: 2025-3-27 19:53
Disks around Post-Main Sequence Binariesarbon-rich star with an oxygen-rich circumstellar envelope. The CO emission from both of these disks has a spike with a width near ~2 km s., indicating disk radii of 10. cm. The dust in such disks is therefore quite cold (near T ~ 50 K for the Red Rectangle) and may emit primarily at submillimeter w作者: Assault 時間: 2025-3-27 23:32 作者: 紡織品 時間: 2025-3-28 05:09 作者: 人類 時間: 2025-3-28 08:22 作者: Finasteride 時間: 2025-3-28 11:02
UIR Bands in Carbon Star Spectraiolet radiation in order for the UIR bands to be excited. If, in addition to amorphous carbon and hydrogenated amorphous carbon (HAC) particles, PAHs are able to form in the outflows of cool carbon-rich stars (Cherchneff et al. 1991), then the weak UV radiation field from such stars would be unlikel作者: 巫婆 時間: 2025-3-28 17:16 作者: 貧窮地活 時間: 2025-3-28 19:19
Modeling the Long-Term Evolution of Dusty Outflows of AGB-Starss (typically 10. to 10. M.yr.) dominates over nuclear burning and finally terminates the AGB evolution. It is now generally accepted that the mechanism responsible for the high mass loss rates during the AGB evolution is based on the efficiency of . Shock waves generated by Mira-type stellar pulsati作者: 猛烈責罵 時間: 2025-3-29 00:48
Observations of Shells Around , Cep & CRL2688, and about Episodic Mass Losshe geometrical and dynamical structure of winds is also necessary to improve models of mass loss. The fact that mass loss from red giants may be episodic has been recognized early: for example, Sauner (1976) showed multiple absorption components in circumstellar absorption lines Ridgway (1981) analy作者: RACE 時間: 2025-3-29 05:30
IR-Colors for Models of Post-AGB Evolution its effective temperature, .., starts to increase, which soon causes the mass loss rate to decrease significantly. When .. reaches about 30 000 K, the star eventually enters the planetary nebula (PN) phase. The transition from the AGB to the PN stage, believed to last a few thousand years, is calle作者: Kindle 時間: 2025-3-29 10:12
Variation of Silicate Dust Features with Phasen 8/95 & 4/97. With these data, we are attempting to ascertain the relationship of dust formation to optical period. Our ultimate goal is to determine what conditions lead to dust formation and destruction in these environments, and whether or not an evolutionary sequence can be inferred for AGB sta作者: 歪曲道理 時間: 2025-3-29 13:57
Molecules in Envelopes around AGB-Starsnt targets for the study of molecular formation processes. This review presents a compilation of estimated molecular abundances, discusses the uncertainties involved in their estimate, and makes some comparisons with theoretical predictions.作者: 后天習得 時間: 2025-3-29 16:51 作者: CRUE 時間: 2025-3-29 21:06 作者: 樂章 時間: 2025-3-30 02:33 作者: Evocative 時間: 2025-3-30 08:06
No Villainous Mother—The Life of Eva Larkinases with radius from ≤ 0.1 to ≤ 1.0 m. kg.. Comparison with laboratory studies suggests that small crystalline grains are formed near the star and are annealed into astronomical silicates at larger distances.作者: Immunization 時間: 2025-3-30 08:25 作者: 鋼筆記下懲罰 時間: 2025-3-30 14:58
Was Wilhelm R?pke Really a Proto-Keynesian?etallic grains, the radiation pressure force for a spheroid can be 5–10 times greater than that for a sphere of the same volume..A simple light scattering consideration demonstrates that the distinction in the scattering geometry of aligned non-spherical grains can explain the observed wavelength variations of the positional angle of polarization.作者: 抵押貸款 時間: 2025-3-30 17:47 作者: 可忽略 時間: 2025-3-31 00:24
Theodore Pelagidis,Michael Mitsopoulosnt targets for the study of molecular formation processes. This review presents a compilation of estimated molecular abundances, discusses the uncertainties involved in their estimate, and makes some comparisons with theoretical predictions.作者: BRINK 時間: 2025-3-31 03:04
No Villainous Mother—The Life of Eva Larking disk radii of 10. cm. The dust in such disks is therefore quite cold (near T ~ 50 K for the Red Rectangle) and may emit primarily at submillimeter wavelengths. The disks around stars where there is also substantial . loss may not be easily observable; there could be many as yet undiscovered disks around AGB stars作者: 甜瓜 時間: 2025-3-31 07:37 作者: PON 時間: 2025-3-31 09:30
Wilhelm R?pke: Why He Was a Conservativeities to allow heavy elements to condense as grains. These dust particles efficiently scatter and absorb stellar photons, transfer the acquired momentum to the ambient gas via collisions and reradiate the absorbed energy at infrared wavelengths.作者: ambivalence 時間: 2025-3-31 16:49 作者: 母豬 時間: 2025-3-31 19:12 作者: corpuscle 時間: 2025-4-1 00:53 作者: pancreas 時間: 2025-4-1 02:27
Shocks in the Radio Photospheres of Long Period Variable Starsntal questions still remain relating to the movement of mass outwards to a few stellar radii and the conditions under which dust forms. Thus, new approaches to study the region between the optical photosphere and the dust formation zone are extremely valuable.作者: 種屬關系 時間: 2025-4-1 07:27 作者: Maximizer 時間: 2025-4-1 13:18
Maser Mapping and Dust Properties of Red Supergiant Windsases with radius from ≤ 0.1 to ≤ 1.0 m. kg.. Comparison with laboratory studies suggests that small crystalline grains are formed near the star and are annealed into astronomical silicates at larger distances.作者: lethargy 時間: 2025-4-1 18:15
Circumstellar Dust Condensation Scenariosdual nature of the dust forming object are intimately coupled. It is the aim of this contribution to visualize this interplay in a rather schematic and abstract way by focusing on the essential interaction of evolution trajectories and dust formation windows for stationary, pulsational, and episodic situations, as well.作者: narcissism 時間: 2025-4-1 22:01 作者: nonsensical 時間: 2025-4-2 00:06
Conference proceedings 1998om the Infrared Space Observatory. Theastrophysical senarios include late-type stars, novae, Wolf-Rayetstars, Luminous Blue Variables and supernovae. ..Audience:. Researchers and graduate students in the fields ofstellar physics, stellar evolution and astrochemistry.作者: Pelago 時間: 2025-4-2 05:59
results from the Infrared Space Observatory. Theastrophysical senarios include late-type stars, novae, Wolf-Rayetstars, Luminous Blue Variables and supernovae. ..Audience:. Researchers and graduate students in the fields ofstellar physics, stellar evolution and astrochemistry.978-90-481-5018-2978-94-017-1307-8
