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The Star Newsletter THE HOT STAR NEWSLETTER ? An electronic publication dedicated to A, B, O, Of, LBV and Wolf-Rayet stars and related phenomena in galaxies ed. Philippe Eenens [email protected] No. 15 http://webhead.com/∼sergio/hot/ November-December 1995 http://www.inaoep.mx/∼eenens/hot/ From the editor This issue contains what we hope to be the first of a series of short commentaries. This one is on the photospheric connection. It would be useful to hear your comments, critics and complementary views. If you wish to write a commentary on another topic, please contact the newsletter editor. The news this month include plans for an X-ray observing campaign, notice of the launch of a newsletter on the Magellanic Clouds and information on the Liege colloquium (July) and on a colloquium on LBV stars (October). Best season wishes! Contents of this newsletter Commentary . 2 Abstracts of 10 accepted papers . 5 Abstracts of 5 submitted papers . 10 Abstracts of 3 proceedings papers . 12 Abstract of 1 dissertation thesis . 13 News ......................................................................14 1 Commentary Variability in the Photospheres and Stellar Winds of Hot Stars: The “Photospheric Connection” At Last? Alex Fullerton1,2 and Lex Kaper3 1 Max-Planck-Institut f¨urAstrophysik, Karl-Schwarzschild-Str. 1, 85740 Garching, Germany 2 Universit¨atsSternwarte M¨unchen, Scheinerstr. 1, 81679 M¨unchen, Germany 3 European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany It has been slightly more than 10 years since a seminal workshop on “The Connection Between Non- radial Pulsations and Stellar Winds in Massive Stars” was hosted by JILA and the University of Colorado (Abbott et al. 1986). At that time (see, e.g., the pivotal review by Henrichs 1984), there was a great deal of excitement in the OB- and Be-star communities owing to the recognition that photospheric variability (probably due to one or more modes of nonradial pulsation) coexisted with stellar wind variability (as diagnosed by the discrete absorption components [DACs] in the absorption troughs of UV P Cygni profiles). Since then, the search for observational evidence connecting varia- tions in these two atmospheric regions has been the focus of intense effort, as has been the search for theoretical explanations for the origin of the coupling required to mediate such a connection. From the observational side, the evidence for a connection has proven to be much more elusive than orig- inally anticipated. However, as amply demonstrated by abstracts in recent editions of the Hot-Star Newsletter (HSN), observational evidence supporting the existence of a photospheric connection has been mounting, to the point that we may be on the verge of developing a new paradigm for the at- mospheres of OB stars. In this commentary, we provide a brief (and necessarily incomplete) overview of our interpretation of these developments. The new observational evidence comes from spectroscopic time series observations of a wide range of early-type stars that have been painstakingly collected from ground- and space-based observatories, particularly the stalwart IUE satellite. In the UV, the long-term monitoring program of 10 bright O stars conceived by Henrichs (Kaper et al. 1996a; HSN 13) shows that the recurrence time between repetitions of patterns of DACs and the acceleration of a given component is longer for stars with smaller projected rotational velocities, but that for a given object the pattern of variability seems to remain fixed over at least 6 years. This behaviour suggests that the DACs are related to the underlying rotation rate of the star. Rotation also seems to govern the time scales associated with variability in optical wind lines of BA supergiants (Kaufer et al. 1996; HSN 10), which very often resemble the UV DACs seen in O stars. Indeed, analogs of the UV DACs are also seen at quite small velocities in optical P Cygni profiles of O stars (e.g., Prinja et al. 1996; HSN 14) which, together with the synchronous variability observed between subordinate UV lines and stronger resonance lines (Kaper et al. 1996a) and covariability between DACs and Hα wind profiles (Kaper et al. 1996b) implies that the variability originates deep in the wind. The widespread occurrence of optical line profile variations among the O stars (Fullerton, Gies, & Bolton 1996; HSN 13) and the agreement between the distribution of O-type variables in the H-R diagram and the domain of strange-mode oscillations leave open the possibility that pulsational activity triggers variations in the stellar wind. Direct evidence in favour of a connection comes from the IUE MEGA campaign (Massa et al. 1995; HSN 11), which provided an unprecedented look at stellar wind variability over an interval of ∼16 days (i.e., several consecutive rotational periods) for 3 key objects: HD 50896 (WN5; St Louis et al. 2 1995; HSN 11); HD 64760 (B0.5 Ib; Prinja, Massa, & Fullerton 1995; HSN 11); and ζ Puppis (O4 I(n)f; Howarth, Prinja, & Massa 1995; HSN 11). The repeatability of the variations in the winds of these stars is astonishing. For ζ Pup and HD 64760 (and perhaps also HD 50896), some – though not all – aspects of the variability repeat at intervals that are compatible with the rotational period of the star (ζ Pup) or an integral submultiple of the rotation period (HD 64760). The detection of wind variability that is tied to the underlying star can only mean that the variations originate in the photosphere. Presumably, the wind responds to boundary conditions that vary as a function of position on the stellar surface. Both heuristic, kinematical models (Owocki, Cranmer, & Fullerton 1995; HSN 10) and dynamical simulations (Cranmer & Owocki 1996; HSN 11) of radiation- driven winds that incorporate large-scale basal perturbations of unspecified origin (but neglect the strong, small-scale line-driven instability) produce large-scale, spiral patterns of enhanced density in the wind. These are the “corotating interaction regions” (CIRs) first considered for hot stars by Mullan (1984); their presence introduces significant deviations from spherical symmetry in the azimuthal density distribution of the stellar wind. Synthetic spectra generated from these simulations reproduce several aspects of the observed variability. The results from the MEGA campaign lead to a second, startling inference: in order to have different boundary conditions for the wind at different positions on the star, the photosphere cannot be uniform. Thus, the time-dependent behavior of the stellar winds of at least some OB (and WR?) stars tells us that large-scale inhomogeneities must be present in their photospheres. The prime candidates for the origin of these nonuniformities are nonradial pulsations or magnetic fields, or some combination of both. By themselves, the wind variations do not provide many additional clues to the nature of these photospheric processes, so tests to distinguish between them will have to come from time- series spectroscopy of photospheric lines. Unfortunately, some of these tests may have to be indirect, particularly since extremely small (∼10 G; i.e., probably undetectable) magnetic fields might still have a measurable effect on the emergence of the stellar wind. Both processes may be at work in ζ Puppis, the perennial “archetypical O star” for stationary models of hot-star atmospheres, which has also emerged as an important object for variability studies. Its new prominence may be viewed as another legacy from the 1985 workshop, since it was there that Dietrich Baade announced the detection of line-profile variations in its C IV λλ5801, 5812 doublet, which he interpreted as signatures of nonradial pulsation. This interpretation has now been substantially confirmed by Reid & Howarth (1995; HSN 12), who also detected the pulsation period (8.54 hours) in the near-star wind (as diagnosed by the Hα emission feature). This period was not evident in the MEGA campaign observations of the high-velocity wind, which was instead dominated by two periodic components, one of which probably reflects the rotational period of the star (5.2 days). Howarth et al. (1995) suggest that a magnetic field inclined to the rotation axis of the star (i.e, an oblique rotator model) may cause this modulation. The second period (19.2 hours) reflects the recurrence time of the DACs during the MEGA campaign, and may be related to the 16.7-hour period reported by Bergh¨ofer et al. (1995; HSN 10) in simultaneous observations of Hα and X-ray emission made at an earlier epoch. The periodic nature of these X-ray variations is truly remarkable, and might also be attributable to corotating structures in the wind. These results paint a new, dynamic picture of hot-star atmospheres, one in which time-dependent phenomena in their deep photospheric layers provide shape and structure to their line-driven outflows, much as had been anticipated by the 1985 workshop. At a very basic level, we think that there are two conclusions to be drawn. First, the usual assumption that hot-star winds are uniform and spherically symmetric will probably have to be done away with, once and for all. There needs to be a concerted effort to determine the extent to which the asphericity of the wind’s density distribution in the (r, θ) plane (see, e.g., Ignace, Bjorkman, & Cassinelli 1996; HSN 10) and the presence of CIRs in the (r, φ) 3 plane will alter spectroscopically derived mass-loss rates, particularly those from diagnostics that are sensitive to ρ2. Petrenz & Puls (1996; HSN 14) have taken the first steps in making this assessment for Hα by accounting for the presence of wind-compressed zones in the (r, θ) plane. Second, there is evidently an additional physical process (or processes) at work in the atmospheres of hot stars whose influence has largely been ignored in modelling efforts to date.
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