Classical Novae As Super-Eddington Steady States

Mem. S.A.It. Vol. 0, 0 !c SAIt 2008 Memorie della Classical Novae as Super-Eddington Steady States N. J. Shaviv1 and C. Dotan1 Racah Institute of Physics, Hebrew University of Jerusalem Jerusalem, 91904 Israel Abstract. The high luminosities and long decays of classical novae imply that they should be described as evolving super-Eddington (SED) steady states. We begin by describing how such states can exist—through the rise of a “porous layer”whichreducestheeffective opacity, and then discuss other characteristics of these states, in particular, that a continuum driven wind will arise. We then modify the stellar structure equations to describe these characteristics. The result is a modification of the classical core-mass—luminosity relation to include the super-Eddington state. The evolution of this state through mass loss describes classical nova light curves. Key words. Stars: Novae 1. Introduction - Novae are SED steady states One of the salient characteristics of classical novae is that the peak luminosity of most if not all eruptions is super-Eddington (SED). This can be seen in the peak luminosity of novae in M31 (see fig. 1). Having SED luminosities is not contradic- tory to any classical notion, since SED luminosities can appear in dynamical systems (such as supernovae) which are far from a steady state. However, one would expect in such cases Fig. 1. The visible magnitude–decay rate relation of to develop bulk motions comparable to the lo- novae in M31, from della Valle & Livio (1995) The cal escape speed (since the effective gravity, in- lines denote the Eddington luminosity limit for vari- cluding radiation, is similar to the actual grav- ous cases. The upper line is the highest LEdd theoret- ity but reverse in direction). This implies that ically possible for a Nova. The middle line is a more reasonable upper limit for typical fast novae. we can have a SED system but over a duration no longer than a time scale comparable to the typical size divided by the escape velocity. For one finds that novae could classically be SED the typical sizes of novae envelopes (∼ 1012 for at most a few hours. And indeed, numeri- cm) and typical wind velocities (∼ 1000 km/s), cal simulations of novae can produce SED lu- Shaviv & Dotan: Novae as super-Eddington states 1 minosities for a few hours but not longer (e.g. minosity for a wide range of envelope masses. Prialnik & Kovetz 1992). Within this range, the outer radius of the ob- Nevertheless, a quick inspection of fig. 1 ject is much larger than the core radius. Below clearly reveals that the decay time is typically this Menv range, the CMLR breaks because 10 days or longer. In fact, if one considers the the luminosity starts decreasing with the en- bolometric luminosity, then the problem is ag- velope mass, which extends to heights much gravated since the decay rate of the total lumi- smaller than the core radius. Above this range, nosity is typically a few times slower than the the outer extent of the envelope is so large, that rate observed in the visible (Friedjung 1987; the escape velocity is comparable to the speed Schwarz et al. 2001; Shaviv 2001b). Clearly of sound, and the envelope evaporates. This is then, classical novae should be described as summarized in fig. 2. super-Eddington steady states. This stands in stark contrast to the the- oretical expectation. When the accreted ma- terial on a WD undergoes a thermonuclear runaway, it first passes a dynamic state dur- ing which the atmosphere is puffed up. In this stage, the luminosity can be easily SED. Because of that, a strong continuum driven wind should exist. However, once the system expands and stabilizes dynamically, it should follow the classical core-mass luminosity relation (Paczyński 1970). Since the CMLR is sub-Eddington, the only way to get a signifi- cant, optically thick mass loss is to drive a con- Fig. 2. The luminosity, photospheric temperature tinuum driven wind on opacity maxima (e.g., and photospheric radius as a function of Menv for Kato 1997). However, even in this case, the the standard CMLR of a 1.2 M# object. For a finite maximal mass loss possible is more than an or- range of envelope masses, the luminosity is almost der of magnitude smaller than many observed constant. At larger envelope masses, the escape ve- mass loss rates (Bath & Shaviv 1976; Shaviv locity is smaller than the speed of sound and the envelope evaporates. As lower envelope masses, the 2001b). envelope “width” is smaller than the core radius, The lower mass loss rate in the standard and the luminosity is smaller. The super-Eddington sub-Eddington picture has another interesting core mass (and envelope mass) luminosity relation implication. It implies that the evolution is in is similar except that the “effective” luminosity is many cases driven by the nuclear burning (i.e., constant. changing of the envelope composition and not its mass (e.g., see Hernanz in this volume). To understandwhat sets the luminosity and why it is not a function of the envelope mass, 2. The Classical CMLR we should note that: Before we start modifying the standard CMLR, – To get an envelope which extends to large to see how it can describe super-Eddington radii (much larger than the core radius), the states, we begin by revisiting the standard sound speed at the base of the envelope CMLR. This relation should describe any ob- has to be fixed, irrespective of the envelope ject with an inert degenerate core, and an en- mass. This gives a unique specific radiation velope with a much smaller mass, and nuclear entropy (sr)luminosityrelationthroughthe fusion at its base. Nova eruptions and post- dependence of the energy generation on the AGB stars are the two classical examples of temperature. such objects. Empirically, one finds that such – To get a consistent atmosphere which sat- objects have an envelope mass independent lu- isfies both the hydrostatic and radiative 2Shaviv&Dotan:Novaeassuper-Eddingtonstates transfer equations, there is another relation 4. The modified CMLR between sr and L/LEdd,butonewhichisal- ways sub-Eddington. Moreover, for a fixed The next step is to consider the classical CMLR and modify it following the conclu- opacity, sr is the same everywhere in the envelope. sions from the previous section. The first point to note is that the sr − L relation now ex- The sr – L relations have a unique intersection, pected form the radiative transfer and hydro- which gives a specific L that only depends on static equilibrium will give the same Γeff (cal- the core mass. This is the origin of the CMLR. culated with the effective opacity), however, because κeff is now reduced, the corresponding total luminosity is going to be higher, and it can 3. How can SED states exist? be super-Eddington. This can be seen in fig. 3, Before attempting to modify the CMLR, let us where Leff ≡ (κeff/κ)L behaves the same as the try to understand how SED states can exist. luminosity in the classical CMLR (cf fig. 2), First, we should note that the opacity relevant but the actual luminosity at the top of the at- to radiative transfer in inhomogeneous media mosphere, Lbase,ismuchhigher. is not the microscopic opacity. Instead, it is Although the internal structure (core + envelope) is very similar in the SED state, the $Fκv% appearance of SED states is going to be mark- κ ff = , (1) e $F% ably different from the sub-Eddington counter- parts. The reason is that SED states necessar- where the average is a volume average and κv ily accelerate a thick continuum driven wind is the opacity per unit volume (the extinction). (Shaviv 2001b). As a consequence, the photo- Thus, any introduction of nonlinear structure sphere and general appearance of the wind de- will cause a change in the opacity. For a con- pends on the actual mass loss. stant opacity (e.g., electron scattering) this al- To derive the mass loss, we have to con- ways causes a reduction (Shaviv 1998). sider that the aforementioned opacity reduc- The next point to consider is that as at- tion can only take place as long as the non- mospheres approach LEdd they become unsta- linear structure formed by the instabilities is ble, so that they naturally reduce their opac- optically thick. Once they become optically ity. Such instabilities arise in Thomson scatter- thin, the radiation cannot be funneled around ing atmospheres (Shaviv 2001a) because of the the optical “obstacles”. As a consequence, the vertical stratification. They can also arise on a anti-correlation between the flux and density larger range of length scales under more com- needed for the reduction of the opacity disap- plex conditions, whether a non-constant opac- pears (see eq. 1). ity (Glatzel 1994), or a magnetic field (Arons Since the instabilities are expected to oper- 1992). ate on a length scale comparable to the atmo- The above implies that if we wish to de- spheric vertical scale height, the effective opac- scribe the global structure of luminous atmo- ity will approach the microscopic one where spheres, we should replace the microscopic the optical width of a scale height becomes of opacity by an effective one. Since we do not order unity. From this, one can derive the ex- now yet how the instabilities will saturate, we pected mass loss (Shaviv 2001b): cannot know a priori the form for the opac- L − LEdd ity. In the following analysis, we will con- m˙ wind = W , (2) sider the simplest form which encapsulates the cvs above physics: κeff(Γ) = κ0/(1 +Γ)whereΓ ≡ where vs is the sound speed at the sonic point.

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