標(biāo)題: Titlebook: Cyclical Variability in Stellar Winds; Proceedings of the E Lex Kaper,Alexander W. Fullerton Conference proceedings 1998 Springer-Verlag Be [打印本頁] 作者: Enkephalin 時(shí)間: 2025-3-21 18:50
書目名稱Cyclical Variability in Stellar Winds影響因子(影響力)
書目名稱Cyclical Variability in Stellar Winds影響因子(影響力)學(xué)科排名
書目名稱Cyclical Variability in Stellar Winds網(wǎng)絡(luò)公開度
書目名稱Cyclical Variability in Stellar Winds網(wǎng)絡(luò)公開度學(xué)科排名
書目名稱Cyclical Variability in Stellar Winds被引頻次
書目名稱Cyclical Variability in Stellar Winds被引頻次學(xué)科排名
書目名稱Cyclical Variability in Stellar Winds年度引用
書目名稱Cyclical Variability in Stellar Winds年度引用學(xué)科排名
書目名稱Cyclical Variability in Stellar Winds讀者反饋
書目名稱Cyclical Variability in Stellar Winds讀者反饋學(xué)科排名
作者: Conjuction 時(shí)間: 2025-3-21 21:01 作者: Antioxidant 時(shí)間: 2025-3-22 03:20 作者: N防腐劑 時(shí)間: 2025-3-22 05:05
Using ISO to Probe the Acceleration of Wolf-Rayet Windsiles formed in spherically symmetric outflows. The method has been applied to three He . lines (9-7 at 2.83.m, 7-6 at 3.09 .m, and 8-7 at 4.76 .m) observed with the ISO SWS for the stars WR 134 (WN6) and WR 136 (WN6). Of these, the 2.83 .m line probes deepest into the wind owing to the dominant free作者: 烤架 時(shí)間: 2025-3-22 11:20
A Critical Evaluation of Mass-Loss Rates and Wind Properties of Evolved Late-Type Starsnuum emission. Our test cases include the stars . TrA (K4 II), . Vel (K4 Ib-II), and . Aur (K4 Ib + B5 V). Of particular interest is the sensitivity of the line profiles to the wind parameters ., .., .., β, and ... We are finding that while accurate and reliable values of . are difficult to obtain, 作者: CAJ 時(shí)間: 2025-3-22 13:37
Variable Winds in Yellow Supergiantsicki (1992). They are repeated here to compare with the unpublished spectrum from 1978 (thick lines). Although not cyclical, the variability in the wind is apparent. Non-LTE analysis (see Gesicki 1992) results in a mass-loss rate of about 5 × 10. M. yr. in 1978, which is higher than in 1970. These r作者: CAJ 時(shí)間: 2025-3-22 18:06
Numerical Simulations of Dust-Driven AGB Winds: A Two-Fluid Model to explore the parameter space associated with these winds. Since the behaviour of both the dust and gas have to be followed in order to achieve the desired self-consistent description of the outflow in two dimensions, I have written a two-fluid hydrocode. This code uses spherical symmetry. Centere作者: 菊花 時(shí)間: 2025-3-23 00:40 作者: interference 時(shí)間: 2025-3-23 04:33
On the Origin of Relativistic Winds from Accreting Starsn the sheared component of the magnetospheric field of the accreting star. This energy is released by the reconnection of magnetic field lines, which is governed by the dissipative tearing mode of instability. During this process, charged particles are accelerated in the magnetopause by magnetic-fie作者: projectile 時(shí)間: 2025-3-23 09:05
The Solar Wind in Three Dimensionshe new results from Ulysses summarized here are the following: 1. On the declining phase of the solar activity cycle and near solar minimum solar wind variability is largely confined to a relatively narrow latitude band centered on the heliographic equator. 2. Solar wind speed far from the Sun is an作者: Carcinoma 時(shí)間: 2025-3-23 10:43 作者: Infelicity 時(shí)間: 2025-3-23 15:14
Variable Dust Emission Observed in Mirasins when T < 1200 K in the shell. During their pulsational cycle Miras vary in luminosity, forcing the dust that has formed in the circumstellar shells alternately to evaporate and re-condense in the inner parts of their shells. Hence, emission from the dust will vary during the pulsational cycle. T作者: dithiolethione 時(shí)間: 2025-3-23 19:18
Systematic Variability in OB-Star Winds. I summarize evidence for cyclic wind variability and rotational modulation, based on extended time-series UV data sets (including the ‘. MEGA Campaigns’). The constraints provided by these data indicate that the modulating ‘clocks’ apparent in some hot star winds must ultimately have an origin at 作者: 恫嚇 時(shí)間: 2025-3-24 00:40 作者: MEAN 時(shí)間: 2025-3-24 03:35 作者: encyclopedia 時(shí)間: 2025-3-24 09:45
Jaydip Singh,Srishti Nagu,Jyotsna Singhnclude the differential rotation of the fluid and the influence of the radiative force in an optically thin stellar atmosphere (Kakouris & Moussas 1997). The solutions use a new thermo-radiative mechanism in order to describe self-consistently outflows from early-type supergiants, for which the radi作者: cunning 時(shí)間: 2025-3-24 12:53 作者: CEDE 時(shí)間: 2025-3-24 17:23
https://doi.org/10.1007/978-3-642-16809-3nuum emission. Our test cases include the stars . TrA (K4 II), . Vel (K4 Ib-II), and . Aur (K4 Ib + B5 V). Of particular interest is the sensitivity of the line profiles to the wind parameters ., .., .., β, and ... We are finding that while accurate and reliable values of . are difficult to obtain, 作者: Proclaim 時(shí)間: 2025-3-24 21:56
Example 1 Audio FPGA Passthroughicki (1992). They are repeated here to compare with the unpublished spectrum from 1978 (thick lines). Although not cyclical, the variability in the wind is apparent. Non-LTE analysis (see Gesicki 1992) results in a mass-loss rate of about 5 × 10. M. yr. in 1978, which is higher than in 1970. These r作者: 閑聊 時(shí)間: 2025-3-25 02:00 作者: Modicum 時(shí)間: 2025-3-25 04:52 作者: 上釉彩 時(shí)間: 2025-3-25 10:04 作者: HAIL 時(shí)間: 2025-3-25 11:51
Preliminary Test and Stein-Rule Estimatorshe new results from Ulysses summarized here are the following: 1. On the declining phase of the solar activity cycle and near solar minimum solar wind variability is largely confined to a relatively narrow latitude band centered on the heliographic equator. 2. Solar wind speed far from the Sun is an作者: 焦慮 時(shí)間: 2025-3-25 17:55 作者: Thymus 時(shí)間: 2025-3-25 20:10 作者: nostrum 時(shí)間: 2025-3-26 00:29
A Model for Microstructure Characterization. I summarize evidence for cyclic wind variability and rotational modulation, based on extended time-series UV data sets (including the ‘. MEGA Campaigns’). The constraints provided by these data indicate that the modulating ‘clocks’ apparent in some hot star winds must ultimately have an origin at 作者: 不規(guī)則的跳動(dòng) 時(shí)間: 2025-3-26 05:57
Cyclical Variability in Stellar Winds978-3-540-68597-5Series ISSN 1431-2433 Series E-ISSN 1611-6143 作者: 現(xiàn)代 時(shí)間: 2025-3-26 10:07 作者: 斷言 時(shí)間: 2025-3-26 15:09
Ekata Nandy,Subhasis Chattopadhyaye radiation pressure as a stellar mass-loss mechanism. Some highlights of this and subsequent observational and theoretical developments are recalled. In addition, recent progress in solving the momentum problem of Wolf-Rayet winds with the same mechanism is reviewed.作者: Diverticulitis 時(shí)間: 2025-3-26 20:16 作者: enormous 時(shí)間: 2025-3-27 00:09 作者: Sedative 時(shí)間: 2025-3-27 03:33 作者: 燒烤 時(shí)間: 2025-3-27 07:42
Michele Trimarchi,Paolo Manzelli89 Herculis (F2Ia/Ib) is a pulsating binary (Smolinski et al. 1980; Waters et al. 1993) fulfilling the criteria for low-mass post-AGB stars.作者: 地名詞典 時(shí)間: 2025-3-27 12:30
https://doi.org/10.1007/978-3-030-67956-9We observed the 22 GHz water maser emission in VX UMa (M8e, M=388.) and V778 Cyg (C5,5J, SRb=300.) from 1987-1992. The spectra of both stars show three distinct components. All three components vary periodically in intensity. We interpret these features as being produced by a rotating circumstellar disk作者: 河潭 時(shí)間: 2025-3-27 14:50 作者: 隼鷹 時(shí)間: 2025-3-27 19:41 作者: Console 時(shí)間: 2025-3-28 01:40 作者: Matrimony 時(shí)間: 2025-3-28 04:26
Variable Water Maser Emission from Circumstellar DisksWe observed the 22 GHz water maser emission in VX UMa (M8e, M=388.) and V778 Cyg (C5,5J, SRb=300.) from 1987-1992. The spectra of both stars show three distinct components. All three components vary periodically in intensity. We interpret these features as being produced by a rotating circumstellar disk作者: 憤憤不平 時(shí)間: 2025-3-28 07:37 作者: FLOUR 時(shí)間: 2025-3-28 13:16
978-3-662-11392-9Springer-Verlag Berlin Heidelberg 1998作者: 漂亮才會(huì)豪華 時(shí)間: 2025-3-28 15:30 作者: 薄荷醇 時(shí)間: 2025-3-28 19:11
ESO Astrophysics Symposiahttp://image.papertrans.cn/d/image/241996.jpg作者: 分離 時(shí)間: 2025-3-29 00:28 作者: 不利 時(shí)間: 2025-3-29 05:55 作者: 商店街 時(shí)間: 2025-3-29 09:33
Wind Variability in the Hypergiant HR 8752 instability region (Nieuwenhuijzen & de Jager 1995). One of the direct consequences of this instability seems to be brief periods of enhanced mass loss that occur when the star comes close to the edge of the instability region during its blueward evolution.作者: cinder 時(shí)間: 2025-3-29 14:54
1431-2433 se form. The proceedings will provide a useful, up-to-date overview of the observations, interpretation, and modelling of the time-dependent mass outflows from all sorts of stars.978-3-662-11392-9978-3-540-68597-5Series ISSN 1431-2433 Series E-ISSN 1611-6143 作者: sultry 時(shí)間: 2025-3-29 15:37
Jaydip Singh,Srishti Nagu,Jyotsna Singhsas 1998). Fig. 1 illustrates the logarithmic density contours for our model of the wind of the hypergiant P Cygni, which was computed by using the optically thin radiative force given by Chen & Marlborough (1994) and the acceleration in the envelope determined by Lamers (1986). The results resemble the three-zone envelope of Nugis et al. (1979).作者: IVORY 時(shí)間: 2025-3-29 23:36
Chapter 8: Introduction to Verificationm, and energy for an (ideal) gas and a single dust component. Both sets of equations are coupled by the condensation of gas onto dust grains and the transfer of momentum between dust and gas. Condensation is described by the source term in the continuity equations, .., in which .. is the condensation rate and .. > 0:..作者: 遭受 時(shí)間: 2025-3-30 02:10
Chapter 8: Introduction to Verification magnetic field geometries are controversial. The time-variability of the outflows is poorly understood; observations of the interactions of jets with the circumstellar medium suggest that the outflows are variable on almost all time scales, but are punctuated by substantial bursts which may be related to FU Ori-like events of high disk accretion.作者: 我不死扛 時(shí)間: 2025-3-30 05:50
Preliminary Test and Stein-Rule Estimatorsin the high-speed wind, the plasma beta there typically being ~3.0. 5. Corotating interaction regions have opposed north-south tilts in the northern and southern hemispheres. 6. A new class of forward-reverse shock pairs associated with over-expanding coronal mass ejections has been identified at high heliographic latitudes.作者: 規(guī)章 時(shí)間: 2025-3-30 09:36
A Thermo-Radiatively Driven, Analytical 2-D Model for Stellar Outflowssas 1998). Fig. 1 illustrates the logarithmic density contours for our model of the wind of the hypergiant P Cygni, which was computed by using the optically thin radiative force given by Chen & Marlborough (1994) and the acceleration in the envelope determined by Lamers (1986). The results resemble the three-zone envelope of Nugis et al. (1979).作者: SOBER 時(shí)間: 2025-3-30 14:57
Numerical Simulations of Dust-Driven AGB Winds: A Two-Fluid Modelm, and energy for an (ideal) gas and a single dust component. Both sets of equations are coupled by the condensation of gas onto dust grains and the transfer of momentum between dust and gas. Condensation is described by the source term in the continuity equations, .., in which .. is the condensation rate and .. > 0:..作者: 血友病 時(shí)間: 2025-3-30 16:58 作者: 無目標(biāo) 時(shí)間: 2025-3-30 20:44
The Solar Wind in Three Dimensionsin the high-speed wind, the plasma beta there typically being ~3.0. 5. Corotating interaction regions have opposed north-south tilts in the northern and southern hemispheres. 6. A new class of forward-reverse shock pairs associated with over-expanding coronal mass ejections has been identified at high heliographic latitudes.作者: 雜役 時(shí)間: 2025-3-31 03:34
Variable Winds in Yellow Supergiantsates were calculated by assuming the solar abundance for barium. Our mass-loss rates are sensitive to this assumption, because the abundance of s-processed elements like barium can be significantly increased after the third dredge-up phase.作者: Jacket 時(shí)間: 2025-3-31 07:55
Conference proceedings 1998s to present the state of the art in a concise form. The proceedings will provide a useful, up-to-date overview of the observations, interpretation, and modelling of the time-dependent mass outflows from all sorts of stars.作者: comely 時(shí)間: 2025-3-31 12:36
Using ISO to Probe the Acceleration of Wolf-Rayet Windserved with the ISO SWS for the stars WR 134 (WN6) and WR 136 (WN6). Of these, the 2.83 .m line probes deepest into the wind owing to the dominant free-free opacity. The winds of both WR 134 and WR 136 have attained only 75% of their respective terminal speeds at the radii where the 2.83 .m line is formed.作者: 蘆筍 時(shí)間: 2025-3-31 13:42
A Critical Evaluation of Mass-Loss Rates and Wind Properties of Evolved Late-Type Starsf the line profiles to the wind parameters ., .., .., β, and ... We are finding that while accurate and reliable values of . are difficult to obtain, the most reliable values come from the application of two or more independent techniques.作者: Adenoma 時(shí)間: 2025-3-31 19:53 作者: Baffle 時(shí)間: 2025-4-1 00:45
Variable Dust Emission Observed in Mirass alternately to evaporate and re-condense in the inner parts of their shells. Hence, emission from the dust will vary during the pulsational cycle. These variations have been observed in the low-resolution spectra (LRS) of Miras obtained by IRAS.作者: inconceivable 時(shí)間: 2025-4-1 05:33
