Equatorial disk formation around rotating stars due to Ram pressure confinement by the stellar wind

Bjorkman, J. E.; Cassinelli, J. P.

doi:10.1086/172676

Cited by 411 publications

(349 citation statements)

References 0 publications

Supporting

Mentioning

334

Contrasting

Unclassified

Order By: Relevance

“…2. 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.…”

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

View full text Add to dashboard Cite

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.

show abstract

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

View full text Add to dashboard Cite

show abstract

“…In the bottom panel of Figure 1 the stellar mass-loss rates of luminosity class V stars are plotted as given by Kudritzki et al (1989) and Bjorkman & Cassinelli (1993). These mass-loss rates can directly be compared with the observed diskgrowth rates (and/or with the corrected IRAS disk mass-loss rates).…”

Section: The Wind Compressed Disk Modelmentioning

confidence: 97%

Long-term Variability in Be-Star disks

Telting

2000

International Astronomical Union Colloquium

View full text Add to dashboard Cite

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).

show abstract

“…Although a few 2-D models have been devised (e.g., Poe 1987;Bjorkman & Cassinelli 1993), most models are really 1-D models, usually of the equatorial outflow (but sometimes they assume the flow occurs at constant latitude; i.e., on the surface of a cone). Classifying these 1-D models according to the main physical driving mechanism, we have:…”

Section: -D Equatorial Outflow Modelsmentioning

confidence: 99%

“…One method for injecting material into a disk is the Wind-Compressed Disk (WCD) model of Bjorkman & Cassinelli (1993). Note however, that the model in its basic form does not transport angular momentum, so the WCD will not be Keplerian (again an additional mechanism will be needed).…”

Section: Wind-compressed Disksmentioning

confidence: 99%

The Formation and Structure of Circumstellar Disks

Bjorkman

2000

International Astronomical Union Colloquium

View full text Add to dashboard Cite

Abstract. Several theories have been proposed to explain the origin of Be star disks. Among them are Wind-Compressed Disks, accretion disks, decretion disks, and "explosive" ejections. In reviewing these mechanisms, I first concentrate on the current status of the Wind-Compressed Disk model. In particular, I discuss how non-radial forces may prevent disk formation and then discuss various physical effects that may restore the disk. Second, I examine the observational evidence and what it tells us about the structure of the disk. Of particular interest is evidence in favor of Keplerian disks. Finally, I discuss theories for Keplerian disk formation and some of the constraints such theories must satisfy.

show abstract

Equatorial disk formation around rotating stars due to Ram pressure confinement by the stellar wind

Cited by 411 publications

References 0 publications

On the role of duplicity in the Be phenomenon

On the role of duplicity in the Be phenomenon

Long-term Variability in Be-Star disks

The Formation and Structure of Circumstellar Disks

Contact Info

Product

Resources

About