The inner lives of red giants

The natural pulse of a red-giant star provides crucial insight into what makes it shine. Observations of red giants by the Kepler space telescope shed light on a previously untested prediction of stellar evolution theory. See Letter p.608

Just as in Hollywood, the age of a star is not always obvious if you look only at the surface. During certain phases in a star's life, its size and brightness are remarkably constant, even while profound transformations are taking place deep inside. For most of their existence, stars shine from the energy released by nuclear reactions that convert hydrogen into helium, but eventually they begin to burn the helium in their cores to synthesize heavier elements, such as carbon and oxygen. On page 608 of this issue, Bedding et al.1 demonstrate a new technique for distinguishing between these life stages, using continuous 'starquakes' to probe the deepest regions, where the changes are most dramatic.

The objects examined by Bedding and colleagues are known as red giants, the bloated fate of stars such as our Sun as they begin to exhaust their primary source of energy — the hydrogen near the centre that powers nuclear fusion. The resulting helium accumulates in the core, forcing hydrogen in a surrounding shell to burn more vigorously than before. About 5 billion years from now, these processes will gradually cause our own star to expand to more than 100 times its present size, becoming a red giant and destroying some of the inner planets in the Solar System2. Stars that were born before the Sun, as well as heavier stars (which evolve more quickly), have already reached this phase of stellar evolution.

Like the Sun, the surface of a red giant seems to boil as convection brings heat up from the interior and radiates it into the coldness of outer space. These turbulent motions act like continuous starquakes, creating sound waves that travel down through the interior and back to the surface. Some of the sounds have just the right tone — a million times lower than the audible range for humans — to set up standing waves (known as solar-like oscillations) that cause the entire star to change its brightness regularly over hours and days, depending on its size. Inferring the properties of stars from these periodic brightness changes is a technique known as asteroseismology3.

The sound waves generated near the surface of a red giant can interact with buoyancy waves (rather like the waves in the ocean) that are trapped inside the helium core. Under the right conditions, the two types of waves can couple to each other, changing the regularity of the brightness changes at the surface. These 'mixed' oscillation modes are much more sensitive to structure in the core than are the uncoupled sound waves that sample only the stellar envelope (Fig. 1).

Figure 1: Red-giant oscillations.

Turbulent motions inside a red-giant star act like continuous starquakes, creating sound waves that travel down through the interior and back to the surface. Under the right conditions, these standing waves can couple with buoyancy waves trapped inside the helium core. Bedding et al.1 identify these 'mixed' oscillation modes in hundreds of red giants observed by the Kepler space telescope, providing unique tests of stellar evolution theory.

The innovation that allowed Bedding et al.1 to distinguish between red giants at different life stages emerged from precise observations by the Kepler space telescope. Launched in March 2009, Kepler stares at a large patch of sky near the constellation Cygnus, monitoring the brightness of more than 156,000 stars with the goal of detecting Earth-like planets. The mission has been extremely successful at finding alien worlds4, but it is also revolutionizing the study of stellar oscillations by providing many months of continuous data for thousands of stars5,6. Earlier efforts to study red giants from ground-based telescopes were hampered by both the daily interruptions of sunlight and the limited duration of the monitoring.

As mentioned before, the trouble with red giants is that they all look nearly the same on the outside, regardless of their mass and age. Bedding and colleagues1 sought to determine these properties for the hundreds of red giants observed by the Kepler satellite, to measure precisely when stars of a given mass would shift from burning hydrogen in a shell to helium in the core. The regular pattern of standing waves is insufficient to pinpoint which energy source makes a particular red giant shine, but the mixed oscillation modes exhibit a unique pattern7. By deciphering this pattern, Bedding et al.1 demonstrate how the two life stages of red giants can be separated using asteroseismology.

The life story of a red giant theoretically depends not only on its age but also on its mass, with stars smaller than about twice the mass of the Sun experiencing a sudden ignition known as a helium flash. The temperature required to fuse helium is significantly higher than that needed for hydrogen, and in low-mass stars the helium accumulates in the core at very high density until it reaches a critical size and ignites almost instantaneously. In more massive stars, the transition to helium core burning is gradual, so the stars exhibit a wider range of core sizes and never experience a helium flash. Bedding and colleagues show how these two populations can be distinguished observationally using their oscillation modes, providing new data to validate a previously untested prediction of stellar evolution theory.

This extraordinary peek into the inner lives of red giants was made possible by just the first year of observations from the Kepler mission, which is scheduled to operate for at least 3.5 years and might be extended by NASA for a further 2.5 years. The picture that emerges from asteroseismology will steadily improve as the observations continue, so we can expect even better results for the stars examined by Bedding et al.1, as well as similar measurements for other red giants, in the near future.


  1. 1

    Bedding, T. R. et al. Nature 471, 608–611 (2011).

    CAS  ADS  Article  Google Scholar 

  2. 2

    Silvotti, R. et al. Nature 449, 189–191 (2007).

    CAS  ADS  Article  Google Scholar 

  3. 3

    Aerts, C., Christensen-Dalsgaard, J., Cunha, M. & Kurtz, D. W. Sol. Phys. 251, 3–20 (2008).

    ADS  Article  Google Scholar 

  4. 4

    Borucki, W. J. et al. Astrophys. J. 728, 117–137 (2011).

    ADS  Article  Google Scholar 

  5. 5

    Gilliland, R. et al. Publ. Astron. Soc. Pacif. 122, 131–143 (2010).

    ADS  Article  Google Scholar 

  6. 6

    Chaplin, W. J. et al. Science (in the press).

  7. 7

    Beck, P. G. et al. Science doi:10.1126/science.1201939 (2011).

Download references

Author information



Corresponding author

Correspondence to Travis S. Metcalfe.

Rights and permissions

Reprints and Permissions

About this article

Cite this article

Metcalfe, T. The inner lives of red giants. Nature 471, 580–581 (2011).

Download citation


By submitting a comment you agree to abide by our Terms and Community Guidelines. If you find something abusive or that does not comply with our terms or guidelines please flag it as inappropriate.


Nature Briefing

Sign up for the Nature Briefing newsletter — what matters in science, free to your inbox daily.

Get the most important science stories of the day, free in your inbox. Sign up for Nature Briefing