Inhibition of Wind-Compressed Disk Formation by Nonradial Line Forces in Rotating Hot-Star Winds

Owocki, S. P.; Cranmer, Steven R.; Gayley, K. G.

doi:10.1086/310372

Cited by 197 publications

(199 citation statements)

References 11 publications

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“…Outflow models Several attempts were made to explain the origin of Be envelopes as a spheroidal outlow of gaseous material from the underlying star: the stellar-wind model by Gerasimovič (1934Gerasimovič ( , 1935, the variable mass flux model by Doazan & Thomas (1987) and Doazan (1987), the "bi-stable" or "axi-symmetric" radiation-driven wind model by Lamers & Pauldrach (1991), Araújo et al (1994) and Stee & Araújo (1994) and the wind-compressed disk model by Bjorkman & Cassinelli (1993) (see also the review by Bjorkman 2000). The latest one was considered as a very promising idea several years ago but the radiation-hydrodynamics simulations by Owocki et al (1996) showed that the small non-radial components in line forces inhibit formation of an equatorial disk by the windcompressed model. Also, this model could have problems providing strong enough stellar winds in Be stars of later spectral subclasses.…”

Section: Attempts To Explain the Be Phenomenonmentioning

confidence: 99%

On the role of duplicity in the Be phenomenon

Harmanec

Bisikalo

Boyarchuk

et al. 2002

A&A

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Abstract. This paper begins a new series of studies devoted to a critical re-examination of the role of duplicity for the Be phenomenon and for the variability patterns observed for many Be stars. Based on both dynamical and energy considerations and a numerical gas-dynamical modelling, a new hypothesis of the formation of Be envelopes in binaries, via an outflow from a rapidly rotating B star in a detached binary, is outlined. It is shown that such an outflow is facilitated by the presence of a companion to the B star and leads to the formation of an envelope but not to any significant mass exchange between the binary components.

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Section: Attempts To Explain the Be Phenomenonmentioning

confidence: 99%

On the role of duplicity in the Be phenomenon

Harmanec

Bisikalo

Boyarchuk

et al. 2002

A&A

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“…Owocki et al (1996) additionally accounted for non-radial line force components <7Q nes and g$ nes (acting in the polar and azimuthal direction, respectively) and gravity darkening.…”

Section: Winds From Rotating Early-type Starsmentioning

confidence: 99%

Selfconsistent Models of Winds from Rotating Early-Type Stars – Application to B[e] star winds

Petrenz¹,

Puls²

2000

International Astronomical Union Colloquium

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Abstract. We present results of 2.5-D radiation hydrodynamical simulations of winds from rapidly rotating stars. For the first time, we consider the dependence of the line statistics on local density and radiation temperature implying a spatial variation of the force-multiplier parameters k, a and S which control the dynamics of the flow. We apply our models to the problem of disk formation in B[e]-star winds. Winds from rotating early-type starsIn recent years, the actual structure of radiation driven winds from rotating early-type stars has been discussed without resolution. Bjorkman & Cassinelli (1993) dropped for the first time the assumption of spherical symmetry and solved for the particle trajectories in the polar plane, thus adopting only azimuthal symmetry about the rotational axis. In the equations of motion, they considered additionally to the inertial accelerations a purely radial line force calculated within the force-multiplier concept, where the corresponding forcemultiplier parameters (fmps) kcAK, <*, 5 (cf. Castor et al. 1975, Abbott 1982 were assumed to be constant throughout the wind, i.e., independent both of distance r and co-latitude 0 .This model predicts a polar deflection of the wind material towards the equatorial plane leading to the formation of a wind-compressed disk (WCD) in the equatorial plane for extreme rotation rates Q > 0.9(0.5) for 0-(B-)stars (for a confirmation by radiation hydrodynamical simulations, see Owocki et al. (1994). Owocki et al. (1996) additionally accounted for non-radial line force components <7Q nes and g$ nes (acting in the polar and azimuthal direction, respectively) and gravity darkening.The negative <7Q nes inhibits the disk formation and redistributes the wind material towards the poles, and the negative <7$ nes spins down the wind (by up to < 35% of the value given by angular momentum conservation). The gravity darkening implies an enhanced (reduced) photon flux over the poles (in the equatorial plane) and thus leads, in combination with the non-radial line force components, to an unambigously prolate wind, which is dense and fast over the poles and slower and thinner in the equatorial plane. These results are entirely contradictory to the predictions by the simple BC model and, meanwhile, have been independently confirmed by Petrenz (1999).However, also these investigations suffer from the assumption of fccAK, ct, 8 constant throughout the wind, which have been adopted from 1-D non-LTE 626 terms of use, available at https://www.cambridge.org/core/terms. https://doi

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“…I have given evidence that for the WCD model it is difficult to explain the disk-growth rate of the late-type Be star Pleione. Other arguments against the WCD model have been raised by Owocki et al (1996) and Porter (1997). Observations of \i Cen show that for this star disk growth is due to pulsationally induced photospheric outbursts.…”

Section: Discussionmentioning

confidence: 99%

Long-term Variability in Be-Star disks

Telting

2000

International Astronomical Union Colloquium

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Abstract.Be stars can switch between non-disk, gradual disk growth, disk-loss events, and shell-line phases. Many aspects of this Be phenomenon are still not understood. In this paper I review recent work on variability in Be-star disks, divided in four different topics: disk growth (Section 1), long-term V/R variations and global disk oscillations (Section 2), spectacular variations (Section 3), and, concisely, the disk variability in Be/X-ray binaries (Section 4).

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Inhibition of Wind-Compressed Disk Formation by Nonradial Line Forces in Rotating Hot-Star Winds

Cited by 197 publications

References 11 publications

On the role of duplicity in the Be phenomenon

On the role of duplicity in the Be phenomenon

Selfconsistent Models of Winds from Rotating Early-Type Stars – Application to B[e] star winds

Long-term Variability in Be-Star disks

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