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THE FORMATION OF BINARY STARS THE FORMATION OF COMMON-ENVELOPE, PRE-MAIN-SEQUENCE BINARY STARSJ.E. TOHLINE, J.E. CAZES, AND H.S. COHLLouisiana State UniversityDepartment of Physics & Astronomy,202 Nicholson Hall,Baton Rouge, LA 70803-4001 U.S.A.1. IntroductionRecent observational investigations of the frequency of occurrenceof pre-main-sequence binary stars have reinforced earlier suspicions that ''binary formation is the primary branch of the star-formation process'' (Mathieu 1994). As Bodenheimer et al. (1993) have reviewed, a number of different theories have been proposed to explain the preponderance of binary stars. Klein et al. (1998) show how the directfragmentation of protostellar gas clouds may occur in early phases of collapse (at cloud densities n = 103 - 1010 cm-3). But at higher densities, clouds are unable to cool efficiently upon contraction. Consequently, direct fragmentation becomes problematical. Because higher mean densities are associated with systems having shorter dynamical times, one is led to consider mechanisms other than direct cloud fragmentation for forming binary systems with orbital periods less than a few hundred years. Here we investigate whether such binaries can formby spontaneous fission of rapidly rotating protostars.2. The Classical Fission HypothesisAs Chandrasekhar (1969) has reviewed (see also Durisen & Tohline 1985), if protostellar objects are assumed to be self-gravitating, incompressible fluids with uniform vorticity, one can show analytically that their allowed equilibrium configurations are defined by spheroids or ellipsoids. Classically, models describing the slow contraction of rotating protostellar gas clouds have been formulated around such analyticallyprescribable equilibrium configurations. For example, a large, slowly rotating gas cloud with a relatively small ratio of rotational to gravitational potential energy T/|W| will resemble a Maclaurin spheroid. As it contracts conserving angular momentum and mass,its evolution will proceed along the Maclaurin sequence through progressively flatter configurations of higher T/|W|. At a sufficiently high T/|W|, one finds that the axisymmetric configuration is no longer the lowest energy state available. Instead, there is an ellipsoidal configuration to which the gas cloud will prefer to evolve.Furthermore, if one follows evolution alonga more and more distorted ellipsoidal sequence (such as the Jacobisequence or any one of the Riemann sequences), one finds that eventuallyother configurations with even higher order surface distortions becomeenergetically favorable. For example (see Fig. 3 of Durisen &Tohline 1985), there is a ''dumbbell-binary sequence'' that branchessmoothly off of the Jacobi ellipsoid sequence. One might imagine, therefore,that binary stars form from the slow contraction of a rapidly rotatinggas cloud along the Maclaurin, then Jacobi (or Riemann), then dumbbell-binary sequences. In reality, the picture is not this clear. Most significantly, detailed work on ellipsoidal figures of equilibrium has only been completed for incompressible fluid systems. It is not at all clear to what extent the results carry over to more realistic structures having compressible equations of state.3. Problems Promoting the Fission Hypothesis While examining the structure of rotatinggas clouds that form the compressible analogues of Maclaurin spheroids, Ostriker & Bodenheimer (1968) showed thatmodels with reasonable degrees of compressibility must incorporate a significant degree of differential rotationif they are to possess reasonably high values of T/|W| and, therefore, be physically interesting in the context of the fission hypothesis. Employing 3D numerical hydrodynamics techniques, Durisen et al. (1986), Williams & Tohline (1988), and Houser et al. (1994) have examined the relative stability of rapidly rotating, compressible gas clouds that are initially in axisymmetric equilibrium but which reside just past a critical bifurcation point along the axisymmetric sequence according to Ostriker & Bodenheimer (1968). Invariably these simulations have shown that models with T/|W|> 0.27 are dynamically unstable toward the growth of a nonaxisymmetric deformationbut, unlike their uniformly rotating, incompressible counterparts, the eigenmode to which these structures appear to be unstable has a spiral character. Movie1  Quicktime (5,907K) Employing a significantly improved finite-difference simulation code and improved spatial resolution (1283 grid zones), we recently have repeated the simulation that was first reported in Durisen et al. (1986). Movie1 shows the nonlinear development of the two-armed, spiral-mode instability.The evolution is shown in the inertial reference frame and covers 20 central initial rotation periods. Each frame of Movie1 displays four nested isodensity contours at r/rmax = 0.8, 0.4, 0.04, and 0.004. Via the trailing spiral structure, gravitational torques are able to effectively redistribute angular momentum on a dynamical time scale; a relatively small amount of material is shed into an equatorial disk (this disk material is not visible in Movie1 because rdisk < 0.004 rmax);and the central object (containing most of the initial object's mass) settles down into a new equilibrium configuration. Clearly, evolution to a binary star system as suggested by the classical fission hypothesis does not occur.It is primarily because simulations of this type have not produced a binary star system that the classical fission hypothesis haslost favor within the star formation community over the past decade(Bodenheimer et al. 1993). 4. Fission Hypothesis RevivedInterestingly, the instability illustrated by Movie1 produces a final steady-state object (hereafter referred to as the ''final bar'') that is dynamically stable, has a T/|W| = 0.25, and has a decidedly nonaxisymmetric structure. In many respects this final bar appearsto be a compressible analog of a Riemann ellipsoid but, as Movie2 illustrates, the configuration possesses nontrivial internal motions. In the first frame of Movie2, 108 test particles have been lined up along the major axis of the final bar. Thereafter the particles are followed as they move along equatorial-plane streamlines of the flow, as viewed in a frame of reference that is rotating with the overall pattern speed of the final bar. The illustrated flow is entirely prograde and largely differential, but there is a smallvolume near the center of the configuration that is moving harmonically.In Movie3 we illustrate the 3D flow-field of the final bar. In the first frame of Movie3, a vertical sheet of test particles has been alligned with the major axis of the final bar. The subsequentmotion of these particles illustrates that there is relatively little vertical fluid motion and, although it varies with R and q, the angular velocityw(x) is almost independent of z.It may be possible, therefore, to understand thisand similar systems in terms of the properties of simpler, 2D nonaxisymmetric structures. Movie2  Quicktime (5,747K) Movie3  Quicktime (3,376K) Andalib (1998) recently has developed a self-consistent-field technique that can be used to Movie4  Quicktime (6,927K) construct equilibrium models of infinitesimally thin, self-gravitating gaseous disks with (a) compressible equations of state, (b) nonaxisymmetric structures, and (c) nontrivial internal motions. By demandingthat the disks have uniform vortensity (defined as the ratio of vorticity to mass density),Andalib has successfully constructed equilibrium disks with polytropic indices 0 < n < 1.3 and minor-to-major axis ratiosin the range 0.06 < b/a < 0.80. Movie4 illustrates the internal flow of four of Andalib's compressible disks with nonaxisymmetric structures: one with fully retrograde internal motions (R); one with fully prograde internal motions (P); one with vortices sandwiched between separate regions of prograde and retrograde flow (V);and a common-envelope binary (dumbbell-shaped) configuration (D). The similarity between the flow illustrated in Movie2 and the flow in Andalib's model P (Movie4)is striking. Apparently Andalib's model provides a good 2D analog of the 3D ''final bar'' that formed as a result of our fully hydrodynamic simulation of the two-armed, spiral mode instability (Movie1). Furthermore, Andalib's work demonstrates that model P is just one among a series of compressible models with nontrivial internal flows that definesa smooth elliptical-dumbbell-binary sequence.We suspect, therefore, that the final bar sits on an analogous (3D) sequence and that, if it is cooled slowly,it will evolve along the sequence to a common-envelopebinary configuration such as the one illustrated by model D inMovie4. Additional support for this conjecture comes fromNew & Tohline (1997) who have demonstrated that stable, equal-masscommon-envelope binaries can be constructed for fully 3D fluid systems with a sufficiently compressible equation of state. In summary, it seems clear that a wide variety of rapidly rotating, nonaxisymmetric systems can be constructed with compressible equations of state. This work gives us renewed confidence that fission offers a viableroute to binary star formation. Future investigations designed to model the slow cooling and contraction of initially nonaxisymmetricconfigurations like the final bar described above should demonstrate whether or not this scenario is correct.5. AcknowledgmentsThis work has been supported, in part, by the U.S. National ScienceFoundation through grant AST-9528424and, in part, by grants ofhigh-performance-computing time at the San Diego Supercomputer Centerand through the PET programof the NAVOCEANO DoD Major Shared Resource Center in Stennis, MS.6. ReferencesAndalib, S.W. (1998), The Structure and Stability of Selected, 2-D Self-Gravitating Systems, Ph.D. Dissertation, Louisiana State UniversityBodenheimer, P., Ruzmaikina, T. and Mathieu, R.D. (1993), in Protostars and Planets, III, ed. E.H. Levy and J.I. Lunine. University of Arizona Press, Tucson, AZ, U.S.A. p. 367Chandrasekhar, S. (1969), Ellipsoidal Figures of Equilibrium. Yale University Press, New Haven, CT, U.S.A.Durisen, R.H., Gingold, R.A., Tohline, J.E. and Boss, A.P. (1986), Ap.J., 305 , p. 281Durisen, R.H. and Tohline, J.E. (1985), in Protostars and Planets, II, ed. D.C. Black and M. Mathews. University of Arizona Press, Tucson, AZ, U.S.A. p. 534Houser, J.L., Centrella, J.M. and Smith, S.C. (1994), Phys. Rev. Lett., 72, p. 1314Klein, R.I, McKee, C.F. and Fisher, R. (1998), These proceedingsMathieu, R.D. (1994), Ann. Rev. Astr. Ap., 32, p. 465New, K.B.C. and Tohline, J.E. (1997), Ap.J., 490, p. 311Ostriker, J.P. and Bodenheimer, P. (1968), Ap.J., 151, p. 1089Williams, H.A. and Tohline, J.E. (1988), Ap.J., 334, p. 449 |
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