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• W144954287 abstract "The characteristic signature of Be stars is the Balmer line emission understood to arise in a circumstellar disk. Unlike the accretion disks of protostars or mass-exchange binary systems, the evolved and generally single or wide-binary status of Be stars seems to require that its disk must form from mass ejection (a.k.a. decretion) from the star itself. In this review, I use analogies with launching orbital satellites to discuss candidate processes (radiation, pulsation, magnetic) for driving such orbital mass ejection, with particular emphasis on the role of the rapid, possibly near-critical, rotation of Be stars in facilitating the formation of their signature disks. 1. The Puzzle of Be Disks Be stars are main-sequence or subgiant spectral type B stars characterized by Balmer emission (e.g., Hα) that originates in a circumstellar disk. Understanding the nature of such stars, and in particular the origin of their circumstellar disks, is one of the longest-standing challenges in astronomy ( Slettebak and Snow 1987; Smith, Henrichs, and Fabregat 1999; Porter and Rivinius 2003). Disks are a common consequence in astrophysical accretion systems, wherein they form as a means to provide outward viscous transport of the angular momentum of the infalling material (Shakura & Sunyaev 1973; Frank et al. 2002). Such accretion disks occur, for example, in protostellar nebulae, or in close binary systems with mass exchange. But Be stars are clearly too old to have retained a protostellar disk (indeed, in many Be stars the Balmer emission signatures of a disk are observed to come and go on timescales of months to decades), and moreover they are not generally found to be in close, mass-exchange binary systems. Thus lacking an outside source of material, it seems instead that Be disks must originate from ejection or “decretion” of mass from the underlying star. Identifying the specific dynamical mechanisms for achieving this “insideout” formation of a circumstellar disks is perhaps the central puzzle underlying the Be phenomenon. Dating back to early analyses by Struve (1931), rapid rotation has long been presumed to be a key piece in this puzzle. But as emphasized below, a crucial, still-open question is just how close Be star rotation might be to the “critical” speed, at which the equatorial surface would be in Keplerian orbit. Critical rotation would enable a direct centrifugal ejection of a circumstellar disk or ring, much as first envisioned by Struve, and developed further in modern “Viscous Decretion Disk” models of Lee et al. (1991) that are discussed in the contribution by A. Okazaki to these proceedings. But conventional interpretations of" @default.
• W144954287 created "2016-06-24" @default.
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• W144954287 date "2005-11-01" @default.
• W144954287 modified "2023-10-16" @default.
• W144954287 title "Dynamical Processes in the Formation of Hot-Star Disks" @default.
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