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Outbursts of luminous blue variable stars from variations in the helium opacity

Naturevolume 561pages498501 (2018) | Download Citation

Abstract

Luminous blue variables are massive, evolved stars that exhibit large variations in luminosity and size on timescales from months to years, with high associated rates of mass loss1,2,3,4,5. In addition to this on-going variability, these stars exhibit outburst phases, during which their size increases and as a result their effective temperature decreases, typically to about 9,000 kelvin3,6. Outbursts are believed to be caused by the radiation force on the cooler, more opaque, outer layers of the star balancing or even exceeding the force of gravity, although the exact mechanisms are unknown and cannot be determined using one-dimensional, spherically symmetric models of stars because such models cannot determine the physical processes that occur in this regime7. Here we report three-dimensional simulations of massive, radiation-dominated stars, which show that helium opacity has an important role in triggering outbursts and setting the observed effective temperature during outbursts of about 9,000 kelvin. It probably also triggers the episodic mass loss at rates of 10−7 to 10−5 solar masses per year. The peak in helium opacity is evident in our three-dimensional simulations only because the density and temperature of the stellar envelope (the outer part of the star near the photosphere) need to be determined self-consistently with convection, which cannot be done in one-dimensional models that assume spherical symmetry. The simulations reproduce observations of long-timescale variability, and predict that convection causes irregular oscillations in the radii of the stars and variations in brightness of 10–30 per cent on a typical timescale of a few days. The amplitudes of these short-timescale variations are predicted to be even larger for cooler stars (in the outburst phase). This short-timescale variability should be observable with high-cadence observations.

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The simulation data are available from the corresponding author on request.

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Acknowledgements

We thank J. Insley (ALCF) for helping us to make the image shown in Fig. 3, N. Smith for providing the data for LBVs, and B. Paxton and J. Goodman for conversations and comments. This research was supported in part by the NASA ATP grant ATP-80NSSC18K0560, the National Science Foundation under grant number NSF PHY 11-25915, 17-48958, and in part by a Simons Investigator award from the Simons Foundation (to E.Q.) and the Gordon and Betty Moore Foundation through grant GBMF5076. An award of computer time was provided by the Innovative and Novel Computational Impact on Theory and Experiment (INCITE) programme. This research used resources of the Argonne Leadership Computing Facility and National Energy Research Scientific Computing Center, which are DOE Offices of Science User Facility supported under contract DE-AC02-06CH11357 and DE-AC02-05CH11231. Resources supporting this work were also provided by the NASA High-End Computing (HEC) programme through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center. The Flatiron Institute is supported by the Simons Foundation

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Nature thanks C. Lovekin and S. Owocki for their contribution to the peer review of this work.

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Affiliations

  1. Kavli Institute for Theoretical Physics, University of California, Santa Barbara, CA, USA

    • Yan-Fei Jiang
    •  & Lars Bildsten
  2. Center for Computational Astrophysics, Flatiron Institute, New York, NY, USA

    • Matteo Cantiello
  3. Department of Astrophysical Sciences, Princeton University, Princeton, NJ, USA

    • Matteo Cantiello
    •  & James Stone
  4. Department of Physics, University of California, Santa Barbara, CA, USA

    • Lars Bildsten
    •  & Omer Blaes
  5. Astronomy Department and Theoretical Astrophysics Center, University of California at Berkeley, Berkeley, CA, USA

    • Eliot Quataert

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Contributions

Y.-F.J. ran the simulations, analysed the results and wrote the first draft of the paper. M.C. ran the MESA one-dimensional stellar evolution calculations and made Fig. 1. M.C., L.B., E.Q., O.B. and J.S. read and commented on the manuscript.

Competing interests

The authors declare no competing interests.

Corresponding author

Correspondence to Yan-Fei Jiang.

Supplementary information

  1. Video 1

    The video is in mp4 format and it is 32 seconds long. It shows the evolution of density for the simulation T19L6.4 described in the paper. The video starts from a spherically symmetric initial condition and ends with a fully turbulent envelope.

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DOI

https://doi.org/10.1038/s41586-018-0525-0

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