Cosmic age problem

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The cosmic age problem is a historical problem in astronomy concerning the age of the universe. The problem was that at various times in the 20th century, some objects in the universe were estimated to be older than the time elapsed since the Big Bang,[1] as estimated from measurements of the expansion rate of the universe known as the Hubble constant, denoted H0. (This is more correctly called the Hubble parameter, since it generally varies with time).

Since around 1997–2003, the problem is believed to be solved by most cosmologists: modern measurements give an accurate age of the universe of 13.8 billion years, and recent age estimates for the oldest objects are either younger than this, or consistent allowing for measurement uncertainties.

Early years[edit]

Following theoretical developments of the Friedmann equations by Alexander Friedmann and Georges Lemaitre in the 1920s, and the discovery of the expanding universe by Edwin Hubble in 1929, it was immediately clear that tracing this expansion backwards in time predicts that the universe had almost zero size at a finite time in the past. This concept, initially known as the "Primeval Atom" by Lemaitre, was later elaborated into the modern Big Bang theory. If the universe had expanded at a constant rate in the past, the age of the universe now (i.e. the time since the Big Bang) is simply the inverse of the Hubble constant, often known as the Hubble time. For Big Bang models with zero cosmological constant and positive matter density, the actual age must be somewhat younger than this Hubble time; typically the age would be between 66% and 90% of the Hubble time, depending on the density of matter.

Hubble's early estimate of his constant[2] was 550 (km/s)/Mpc, and the inverse of that is 1.8 billion years. It was believed by many geologists such as Arthur Holmes in the 1920s that the Earth was probably over 2 billion years old, but with large uncertainty.[citation needed] The possible discrepancy between the ages of the Earth and the universe was probably one motivation for the development of the Steady State theory in 1948 as an alternative to the Big Bang;[3] in the (now obsolete) steady state theory, the universe is infinitely old and on average unchanging with time. The steady state theory postulated spontaneous creation of matter to keep the average density constant as the universe expands, and therefore most galaxies still have an age less than 1/H0. However, if H0 had been 550 (km/s)/Mpc, our Milky Way galaxy would be exceptionally large compared to most other galaxies, so it could well be much older than an average galaxy, therefore eliminating the age problem.


In the 1950s, two substantial errors were discovered in Hubble's extragalactic distance scale: first in 1952, Walter Baade discovered there were two classes of Cepheid variable star. Hubble's sample comprised different classes nearby and in other galaxies, and correcting this error made all other galaxies twice as distant as Hubble's values, thus doubling the Hubble time.[4] A second error was discovered by Allan Sandage and coworkers: for galaxies beyond the Local Group, Cepheids were too faint to observe with Hubble's instruments, so Hubble used the brightest stars as distance indicators. Many of Hubble's "brightest stars" were actually HII regions or clusters containing many stars, which caused another underestimation of distances for these more distant galaxies.[citation needed] Thus, in 1958 Sandage[5] published the first reasonably accurate measurement of the Hubble constant, at 75 (km/s)/Mpc, which is close to modern estimates of 68–74 (km/s)/Mpc.[6]

The age of the Earth (actually the Solar System) was first accurately measured around 1955 by Clair Patterson at 4.55 billion years,[7] essentially identical to the modern value. For H0 ~ 75 (km/s)/Mpc, the inverse is 13.0 billion years; so after 1958 the Big Bang model age was comfortably older than the Earth.

However, in the 1960s and onwards, new developments in the theory of stellar evolution enabled age estimates for large star clusters called globular clusters: these generally gave age estimates of around 15 billion years, with substantial scatter.[citation needed] Further revisions of the Hubble constant by Sandage and Gustav Tammann in the 1970s gave values around 50–60 (km/s)/Mpc,[8] and an inverse of 16-20 billion years, consistent with globular cluster ages.


However, in the late 1970s to early 1990s, the age problem re-appeared: new estimates of the Hubble constant gave higher values, with Gerard de Vaucouleurs estimating values 90–100 (km/s)/Mpc,[9] while Marc Aaronson and co-workers gave values around 80-90  (km/s)/Mpc.[10] Sandage and Tammann continued to argue for values 50-60, leading to a period of controversy sometimes called the "Hubble wars".[citation needed] The higher values for H0 appeared to predict a universe younger than the globular cluster ages, and gave rise to some speculations during the 1980s that the Big Bang model was seriously incorrect.

Late 1990s: probable solution[edit]

The age problem was eventually thought to be resolved by several developments between 1995-2003: firstly, a large program with the Hubble space telescope measured the Hubble constant at 72 (km/s)/Mpc with 10 percent uncertainty.[11] Secondly, measurements of parallax by the Hipparcos spacecraft in 1995 revised globular cluster distances upwards by 5-10 percent;[12] this made their stars brighter than previously estimated and therefore younger, shifting their age estimates down to around 12-13 billion years.[13] Finally, from 1998-2003 a number of new cosmological observations including supernovae, cosmic microwave background observations and large galaxy redshift surveys led to the acceptance of dark energy and the establishment of the Lambda-CDM model as the standard model of cosmology. The presence of dark energy implies that the universe was expanding more slowly at around half its present age than today, which makes the universe older for a given value of the Hubble constant. The combination of the three results above essentially removed the discrepancy between estimated globular cluster ages and the age of the universe.[14]

More recent measurements from WMAP and the Planck spacecraft have established a very accurate age of the universe of 13.80 billion years[15] with only 0.3 percent uncertainty (based on the standard Lambda-CDM model), and modern age measurements for globular clusters [16] and other objects are currently smaller than this value (within the measurement errors). A substantial majority of cosmologists therefore believe the age problem is now resolved.[17]


  1. ^ Evidence for the Big Bang by Björn Feuerbacher and Ryan Scranton. January 25, 2006. Retrieved 16 April 2007.
  2. ^ Hubble, E. (15 March 1929). "A relation between distance and radial velocity among extra-galactic nebulae". Proceedings of the National Academy of Sciences. 15 (3): 168–173. Bibcode:1929PNAS...15..168H. PMC 522427Freely accessible. PMID 16577160. doi:10.1073/pnas.15.3.168. 
  3. ^ Kragh, Helge (1999). Cosmology and Controversy. Princeton Univ. Press. ISBN 978-0691005461. 
  4. ^ Baade, W. (February 1956). "The Period-Luminosity Relation of the Cepheids". Publications of the Astronomical Society of the Pacific. 68: 5. Bibcode:1956PASP...68....5B. doi:10.1086/126870. 
  5. ^ Sandage, Allan (1958). "Current Problems in the Extragalactic Distance Scale". Astrophysical Journal. 127: 513. Bibcode:1958ApJ...127..513S. doi:10.1086/146483. 
  6. ^ Riess, A.; Macri, Lucas; Casertano, Stefano; Lampeitl, Hubert; Ferguson, Henry C.; Filippenko, Alexei V.; Jha, Saurabh W.; Li, Weidong; Chornock, Ryan (2011). "A 3% solution: determination of the Hubble constant with the Hubble Space Telescope". ApJ. 730 (119). Bibcode:2011ApJ...730..119R. arXiv:1103.2976Freely accessible. doi:10.1088/0004-637X/730/2/119. 
  7. ^ Patterson, C.; Tilton, G.; Inghram, M. (21 January 1955). "Age of the Earth". Science. 121 (3134): 69–75. Bibcode:1955Sci...121...69P. doi:10.1126/science.121.3134.69. 
  8. ^ Sandage, A.; Tammann, G. A. "Steps toward the Hubble constant. VII - Distances to NGC 2403, M101, and the Virgo cluster using 21 centimeter line widths compared with optical methods: The global value of H sub 0". The Astrophysical Journal. 210: 7. Bibcode:1976ApJ...210....7S. doi:10.1086/154798. 
  9. ^ de Vaucouleurs, G. (23 September 1982). "Five crucial tests of the cosmic distance scale using the Galaxy as fundamental standard". Nature. 299 (5881): 303–307. Bibcode:1982Natur.299..303D. doi:10.1038/299303a0. 
  10. ^ Aaronson, M.; Bothun, G.; Mould, J.; Huchra, J.; Schommer, R. A.; Cornell, M. E. "A distance scale from the infrared magnitude/H I velocity-width relations. V - Distance moduli to 10 galaxy clusters, and positive detection of bulk supercluster motion toward the microwave anisotropy". The Astrophysical Journal. 302: 536. Bibcode:1986ApJ...302..536A. doi:10.1086/164014. 
  11. ^ Madore, Barry F.; Freedman, Wendy L.; Silbermann, N.; Harding, Paul; Huchra, John; Mould, Jeremy R.; Graham, John A.; Ferrarese, Laura; Gibson, Brad K.; Han, Mingsheng; Hoessel, John G.; Hughes, Shaun M.; Illingworth, Garth D.; Phelps, Randy; Sakai, Shoko; Stetson, Peter (10 April 1999). "The Key Project on the Extragalactic Distance Scale. XV. A Cepheid Distance to the Fornax Cluster and Its Implications". The Astrophysical Journal. 515 (1): 29–41. Bibcode:1999ApJ...515...29M. arXiv:astro-ph/9812157Freely accessible. doi:10.1086/307004. 
  12. ^ Reid, N (1998). "Globular clusters, Hipparcos, and the age of the galaxy". Proceedings of the National Academy of Sciences of the United States of America. 95 (1): 8–12. Bibcode:1998PNAS...95....8R. doi:10.1073/pnas.95.1.8. 
  13. ^ Chaboyer, Brian; Demarque, P.; Kernan, Peter J.; Krauss, Lawrence M. (10 February 1998). "The Age of Globular Clusters in Light of  : Resolving the Age Problem?". The Astrophysical Journal. 494 (1): 96–110. Bibcode:1998ApJ...494...96C. arXiv:astro-ph/9706128Freely accessible. doi:10.1086/305201. 
  14. ^ Krauss, Lawrence M.; Chaboyer, Brian (3 January 2003). "Age Estimates of Globular Clusters in the Milky Way: Constraints on Cosmology". Science. 299 (5603): 65–69. Bibcode:2003Sci...299...65K. PMID 12511641. doi:10.1126/science.1075631. 
  15. ^ Planck Collaboration, Planck; Ade, P. A. R.; Aghanim, N.; Armitage-Caplan, C.; Arnaud, M.; Ashdown, M.; Atrio-Barandela, F.; Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.; Bartlett, J. G.; Battaner, E.; Benabed, K.; Benoît, A.; Benoit-Lévy, A.; Bernard, J. -P.; Bersanelli, M.; Bielewicz, P.; Bobin, J.; Bock, J. J.; Bonaldi, A.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Bridges, M.; Bucher, M.; Burigana, C.; Butler, R. C.; et al. (2013). "Planck 2013 results XVI: Cosmological Parameters". arXiv:1303.5076Freely accessible [astro-ph.CO]. 
  16. ^ VandenBerg, Don A.; Brogaard, K.; Leaman, R.; Casagrande, L. (1 October 2013). "THE AGES OF 55 GLOBULAR CLUSTERS AS DETERMINED USING AN IMPROVED $\Delta V^{\rm HB}_{\rm TO}$ METHOD ALONG WITH COLOR-MAGNITUDE DIAGRAM CONSTRAINTS, AND THEIR IMPLICATIONS FOR BROADER ISSUES". The Astrophysical Journal. 775 (2): 134. Bibcode:2013ApJ...775..134V. arXiv:1308.2257Freely accessible. doi:10.1088/0004-637X/775/2/134. 
  17. ^ "Cosmological Parameters" (PDF). Review of Particle Properties 2014. Particle Data Group. 

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