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The Accelerating Universe: How Exploding Stars Revealed Dark Energy

Cosmologists spent a century assuming that the mutual gravitational pull of galaxies was slowing down the expansion of the universe; two competing teams measuring exploding white dwarf stars discovered that cosmic expansion is speeding up faster and faster. Awarded the 2011 Nobel Prize in Physics, this discovery of Dark Energy proved that empty space contains a repulsive anti-gravity energy that makes up seventy percent of our universe.

Author
Adam G. Riess et al.
Published
1998
Journal
The Astronomical Journal
Last updated
September 2026
The Accelerating Universe: How Exploding Stars Revealed Dark Energy

For decades after Edwin Hubble discovered the expanding universe, every astrophysicist believed that the expansion was gradually slowing down, pulled inward by the gravitational tug of billions of galaxies—much like a baseball thrown into the air slows down as Earth's gravity pulls it back.

Two rival astronomy teams (led by Saul Perlmutter, Brian Schmidt, and Adam Riess) used exploding white dwarf stars (Type Ia supernovae) as standard 100-watt lightbulbs to measure cosmic distances. To their absolute shock, distant supernovae were dimmer than expected—proving that the cosmic car is not braking; it is stepping on the gas pedal.

The accelerating universe earned the 2011 Nobel Prize in Physics. By discovering that invisible Dark Energy makes up seventy percent of the universe, by confirming Einstein's once-abandoned Cosmological Constant, and by predicting that our cosmos will expand forever into a cold, dark freeze, Dark Energy rewrote cosmology.

Reference

Riess, A. G., Filippenko, A. V., Challis, P., Clocchiatti, A., Diercks, A., Garnavich, P. M., Gilliland, R. L., Hogan, C. J., Jha, S., Kirshner, R. P., Leibundgut, B., Phillips, M. M., Reiss, D., Schmidt, B. P., Schommer, R. A., Smith, R. C., Spyromilio, J., Stubbs, C., Suntzeff, N. B., & Tonry, J. (1998). Observational Evidence from Supernovae for an Accelerating Universe and a Cosmological Constant. The Astronomical Journal, 116(3), 1009–1038.

Title

Observational Evidence from Supernovae for an Accelerating Universe and a Cosmological Constant

Abstract

We present spectral and photometric observations of 10 Type Ia supernovae (SNe Ia) in the redshift range 0.16 ≤ z ≤ 0.62. The luminosity distances of these objects are determined by methods that employ relations between SN Ia luminosity and light curve shape. Combined with previous data from our High- z Supernova Search Team and recent results by Riess et al., this expanded set of 16 high-redshift supernovae and a set of 34 nearby supernovae are used to place constraints on the following cosmological parameters: the Hubble constant ( H 0 ), the mass density (Ω M ), the cosmological constant (i.e., the vacuum energy density, Ω Λ ), the deceleration parameter ( q 0 ), and the dynamical age of the universe ( t 0 ). The distances of the high-redshift SNe Ia are, on average, 10%–15% farther than expected in a low mass density (Ω M = 0.2) universe without a cosmological constant. Different light curve fitting methods, SN Ia subsamples, and prior constraints unanimously favor eternally expanding models with positive cosmological constant (i.e., Ω Λ > 0) and a current acceleration of the expansion (i.e., q 0 0 at the 3.0 σ and 4.0 σ confidence levels, for two different fitting methods, respectively. Fixing a "minimal" mass density, Ω M = 0.2, results in the weakest detection, Ω Λ > 0 at the 3.0 σ confidence level from one of the two methods. For a flat universe prior (Ω M + Ω Λ = 1), the spectroscopically confirmed SNe Ia require Ω Λ > 0 at 7 σ and 9 σ formal statistical significance for the two different fitting methods. A universe closed by ordinary matter (i.e., Ω M = 1) is formally ruled out at the 7 σ to 8 σ confidence level for the two different fitting methods. We estimate the dynamical age of the universe to be 14.2 ± 1.7 Gyr including systematic uncertainties in the current Cepheid distance scale. We estimate the likely effect of several sources of systematic error, including progenitor and metallicity evolution, extinction, sample selection bias, local perturbations in the expansion rate, gravitational lensing, and sample contamination. Presently, none of these effects appear to reconcile the data with Ω Λ = 0 and q 0 ≥ 0.

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