Titlebook: Cyclical Variability in Stellar Winds; Proceedings of the E Lex Kaper,Alexander W. Fullerton Conference proceedings 1998 Springer-Verlag Be

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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




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書目名稱Cyclical Variability in Stellar Winds網(wǎng)絡(luò)公開度學(xué)科排名




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書目名稱Cyclical Variability in Stellar Winds被引頻次學(xué)科排名




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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

Conjuction

Antioxidant

N防腐劑

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

烤架

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,

CAJ

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 They are repeated here to compare with the unpublished spectrum from 1978 (thick lines).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

CAJ

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

菊花

interference

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

projectile

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