The envelopes accreted by white dwarf stars from their hydrogen-rich companions1 experience thermonuclear-powered runaways2,3 observed as classical nova eruptions4,5 peaking at 105–106 solar luminosities6,7,8,9. Virtually all nova progenitors—‘nova-like variables’—exhibit high mass transfer rates to their white dwarfs before and after an eruption10. Surprisingly, 10–1,000 times lower mass transfer rate11 binaries, exhibiting accretion-powered ‘dwarf nova’ outbursts12, exist at identical orbital periods. Nova shells surrounding dwarf novae13,14,15,16 demonstrate that at least some novae metamorphize into dwarf novae17,18, though the mechanisms and timescales governing mass transfer rate variations are poorly understood. Here, we report simulations of the multi-Gyr evolution of novae modelling every eruption’s thermonuclear runaway, mass and angular momentum losses, feedback due to irradiation and variable mass transfer rate, and orbital size and period changes. These feedback-dominated simulations reproduce the observed range of mass transfer rates at a given orbital period, with large and cyclic kyr–Myr timescale changes. They also demonstrate Myr-long deep hibernation (complete stoppage of mass transfer), but only in short-period binaries; that initially different binaries converge to become nearly identical systems; low-mass-transfer-rate dwarf novae occasionally generate novae; and that the masses of white dwarfs decrease monotonically, but only slightly while their red dwarf companions are consumed.
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All data pertaining to each simulation is available upon reasonable request from Y.H.
Kraft, R. Binary stars among cataclysmic variables. III. Ten old novae. Astrophys. J. 139, 457–475 (1964).
Starrfield, S., Truran, J. W., Sparks, W. M. & Kutter, G. CNO abundances and hydrodynamic models of the nova outburst. Astrophys. J. 176, 169–176 (1972).
Prialnik, D., Shara, M. & Shaviv, G. The evolution of a slow nova model with a Z = 0.03 envelope from pre-explosion to extinction. Astron. Astrophys. 62, 339–348 (1978).
Warner, B. Cataclysmic Variable Stars (Cambridge Univ. Press, 1995).
Yaron, O., Prialnik, D., Shara, M. M. & Kovetz, A. An extended grid of nova models. II. The parameter space of nova outbursts. Astrophys. J. 623, 398–410 (2005).
Shara, M. M. Recent progress in understanding the eruptions of classical novae. Publ. Astron. Soc. Pac. 101, 5–31 (1989).
José, J. & Hernanz, M. Nucleosynthesis in classical nova explosions. J. Phys. G Nucl. Part. Phys. 34, R431–R458 (2007).
Bode, M. F. The outbursts of classical and recurrent novae. Astron. Nachr. 331, 160–168 (2010).
Starrfield, S., Iliadis, C. & Hix, W. R. The thermonuclear runaway and the classical nova outburst. Publ. Astron. Soc. Pac. 128, 051001 (2016).
Collazzi, A. C. et al. The behavior of novae light curves before eruption. Astron. J. 138, 1846–1873 (2009).
Knigge, C., Baraffe, I. & Patterson, J. The evolution of cataclysmic variables as revealed by their donor stars. Astrophys. J. Suppl. Ser. 194, 28–76 (2011).
Dubus, G., Otulakowska-Hypka, M. & Lasota, J.-P. Testing the disk instability model of cataclysmic variables. Astron. Astrophys. 617, A26 (2018).
Shara, M. M. et al. An ancient nova shell around the dwarf nova Z Camelopardalis. Nature 446, 159–162 (2007).
Shara, M. M. et al. AT Cnc: a second dwarf nova with a classical nova shell. Astrophys. J. 758, 121–126 (2012).
Miszalski, B. et al. Discovery of an eclipsing dwarf nova in the ancient nova shell Te 11. Mon. Not. R. Astron. Soc. 456, 633–640 (2016).
Shara, M. M. et al. Proper-motion age dating of the progeny of Nova Scorpii ad 1437. Nature 548, 558–560 (2017).
Vogt, N. The structure and outburst mechanisms of dwarf novae and their evolutionary status among cataclysmic variables. Mitt. Astron. Gessell. 57, 79–118 (1982).
Shara, M., Livio, M., Moffat, A. & Orio, M. Do novae hibernate during most of the millennia between eruptions? Links between dwarf and classical novae, and implications for the space densities and evolution of cataclysmic binaries. Astrophys. J. 311, 163–171 (1986).
Drew, J. Inclination and orbital-phase-dependent resonance line-profile calculations applied to cataclysmic variable winds. Mon. Not. R. Astron. Soc. 224, 595–632 (1987).
Gill, C. D. & O’Brien, T. J. Hubble Space Telescope imaging and ground-based spectroscopy of old nova shells—I. FH Ser, V533 Her, BT Mon, DK Lac and V476 Cyg. Mon. Not. R. Astron. Soc. 314, 175–182 (2000).
Kovetz, A., Prialnik, D. & Shara, M. M. What does an erupting nova do to its red dwarf companion? Astrophys. J. 325, 828–836 (1988).
Ritter, H., Zhang, Z.-Y. & Kolb, U. Irradiation and mass transfer in low-mass compact binaries. Astron. Astrophys. 360, 969–990 (2000).
Baraffe, I. & Kolb, U. On the late spectral types of cataclysmic variable secondaries. Mon. Not. R. Astron. Soc. 318, 354–360 (2000).
Stehle, R., Ritter, H. & Kolb, U. An analytic approach to the secular evolution of cataclysmic variables. Mon. Not. R. Astron. Soc. 279, 581–590 (1996).
Hillman, Y., Prialnik, D., Kovetz, A. & Shara, M. Growing white dwarfs to the Chandrasekhar limit: the parameter space of the single degenerate SN Ia channel. Astrophys. J. 819, 168–178 (2016).
Patterson, J. et al. BK Lyncis: the oldest old nova and a Bellwether for cataclysmic variable evolution. Mon. Not. R. Astron. Soc. 434, 1902–1919 (2013).
Mróz, P. et al. The awakening of a classical nova from hibernation. Nature 537, 649–651 (2016).
Townsley, D. & Bildsten, L. Classical novae as a probe of the cataclysmic variable population. Astrophys. J. 628, 395–400 (2005).
Livio, M. & Shara, M. M. Binary system parameters and the hibernation models of cataclysmic variables. Astrophys. J. 319, 819–826 (1987).
Kovetz, A., Yaron, O. & Prialnik, D. A new, efficient stellar evolution code for calculating complete evolutionary tracks. Mon. Not. R. Astron. Soc. 395, 1857–1874 (2009).
Prialnik, D. & Kovetz, A. An extended grid of multicycle nova evolution models. Astrophys. J. 445, 789–810 (1995).
Epelstain, N., Yaron, O., Kovetz, A. & Prialnik, D. A thousand and one nova outbursts. Mon. Not. R. Astron. Soc. 374, 1449–1456 (2007).
Hillman, Y., Prialnik, D., Kovetz, A. & Shara, M. M. Observational signatures of SNIa progenitors, as predicted by models. Mon. Not. R. Astron. Soc. 446, 1924–1930 (2015).
Paxton, B. et al. Modules for Experiments in Stellar Astrophysics (MESA): binaries, pulsations, and explosions. Astrophys. J. Suppl. Ser. 220, 15–59 (2015).
Eggleton, P. Approximations to the radii of Roche lobes. Astrophys. J. 268, 368–369 (1983).
Ritter, H. Turning on and off mass transfer in cataclysmic binaries. Astron. Astrophys. 202, 93–100 (1988).
MacDonald, J. Post thermonuclear runaway angular momentum loss in cataclysmic binaries. Astrophys. J. 305, 251–260 (1986).
Schenker, K., Kolb, U. & Ritter, H. Properties of discontinuous and nova-amplified mass transfer in cataclysmic binaries. Mon. Not. R. Astron. Soc. 297, 633–647 (1998).
Liu, W.-M. & Li, X.-D. Can the friction of the nova envelope account for the extra angular momentum loss in cataclysmic variables? Astrophys. J. 870, 22–30 (2019).
Schreiber, M. R., Zorotovic, M. & Wijnen, T. P. G. Three in one go: consequential angular momentum loss can solve major problems of CV evolution. Mon. Not. R. Astron. Soc. 455, L16–L20 (2016).
Schaefer, B. et al. Precise measures of orbital period, before and after nova eruption for QZ Aur. Mon. Not. R. Astron. Soc. 487, 1120–1139 (2019).
Figueira, J. et al. Three-dimensional simulations of the interaction between the nova ejecta, accretion disk, and companion star. Astron. Astrophys. 613, A8–A17 (2018).
Livio, M. & Truran, J. Spin-up and mixing in accreting white dwarfs. Astrophys. J. 870, 316–325 (1987).
Prialnik, D. & Kovetz, A. The effect of diffusion on prenova evolution: CNO enriched envelopes. Astrophys. J. 281, 367–374 (1984).
Kovetz, A. & Prialnik, D. The composition of nova ejecta from multicycle evolution models. Astrophys. J. 477, 356–367 (1997).
Casanova, J., José, J., Garcia-Berro, E., Shore, S. N. & Calder, A. C. Kelvin–Helmholtz instabilities as the source of inhomogeneous mixing in nova explosions. Nature 478, 490–492 (2011).
José, J., Shore, S. N. & Casanova, J. 123–321 models of classical novae. Astron. Astrophys. 631, A5–A13 (2020).
Livio, M. & Pringle, J. The rotation rates of white dwarfs and pulsars. Astrophys. J. 505, 339–343 (1998).
Brett, J. M. & Smith, R. C. A model atmosphere investigation of the effects of irradiation on the secondary star in a dwarf nova. Mon. Not. R. Astron. Soc. 264, 641–653 (1993).
Günther, H. M. & Wawrzyn, A. C. A method to simulate inhomogeneously irradiated objects with a superposition of 1D models. Astron. Astrophys. 526, 117–125 (2011).
We thank the dozens of observers who have worked diligently, over the past three decades, to test predictions of the hibernation scenario of cataclysmic variables. We also thank C. Tappert, L. Schmidtobreick, B. Schaefer and C. Knigge for valuable constructive criticisms of an earlier draft of this paper.
The authors declare no competing interests.
Peer review information Nature Astronomy thanks Jordi Jose and Steven Shore for their contribution to the peer review of this work.
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Hillman, Y., Shara, M.M., Prialnik, D. et al. A unified theory of cataclysmic variable evolution from feedback-dominated numerical simulations. Nat Astron 4, 886–892 (2020). https://doi.org/10.1038/s41550-020-1062-y
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