Exciting developments in astronomy and particle physics appear to provide probable, though not yet positive, evidence for the existence of sterile neutrinos and axions (particles that hold the possibility of solving numerous problems in our understanding of the universe and greatly bolstering the evidence for design).
In part 1 of this series I described why the Higgs boson is called the “God particle,” and why the sterile neutrino may be much more deserving of the title. In this article I will review astronomers’ dogged searches over the past twenty years to discover sterile neutrinos and why these searches, to everyone’s surprise, have come up empty so far. I will also describe how these failures have, nevertheless, infused astronomers with new hope that the discovery of sterile neutrinos is at hand.
I frequently use my three-foot crowbar in home-improvement projects around my house. For several months, however, it was lost. I looked in all the reasonable places: my construction sites under the house and in the attic, the garage, and all the closets. Nothing. It wasn’t until I cleaned out the old toys, books, and games my youngest son had crammed under his bed that I found my missing crowbar. Why, I asked David, did he put my crowbar under his bed? He explained he was having bad dreams and had put the crowbar there for self-defense. For me, a crowbar was a construction tool. I never thought of its utility as a weapon. Likewise, astronomers, in focusing on one means for sterile neutrino production, had ignored another and thus failed in their attempts to find their object.
As with my crowbar, astronomers have had no doubts that sterile neutrinos must exist. Sterile neutrinos explain far too many anomalies in astronomy and physics for them not to exist. Still, astronomers and physicists have yet to produce any positive detection that proves sterile neutrinos’ existence.
The “yet” may be short-lived. While sterile neutrinos do not interact with ordinary matter, they can decay. Back in 1990, two physicists at the University of Pisa in Italy, Riccardo Barbieri and Alexandre Dolgov, calculated that with a half-life of more than the age of the universe, sterile neutrinos could decay virtually at rest into a photon and an active neutrino.1 Such decay, given the anticipated mass of a sterile neutrino (a few millionths of the proton’s mass), would produce a comparatively sharp spectral line at X-ray wavelengths.
Detecting the spectral line from the decay of sterile neutrinos is not easy. Almost everywhere astronomers point their telescopes the X-ray background radiation is expected to overwhelm the signal from sterile neutrino decay. Moreover, the signal from sterile neutrino decay may not be as strong as astronomers once thought. Many, if not most, of the missing dwarf and subdwarf galaxies are starting to turn up in deep surveys of galaxies.2 Stars do form early in cosmic history, but according to the final release of the WMAP of the cosmic microwave background radiation (left over from the cosmic creation event), the epoch of first star formation now measures significantly later than what the WMAP first release indicated.3 Thus, the expected number density of sterile neutrinos in the universe is such that these particles almost certainly do not comprise the major fraction of the exotic matter in the universe.
The most frequently exercised detection technique involves pointing the best existing X-ray telescopes at certain regions of the exotic dark matter halos surrounding galaxies where no other known X-ray sources exist. Initial searches already have been attempted for both nearby4 and distant5 galaxies. So far, the best attempted measurements were performed on Segue 1, a dwarf galaxy with the highest known dark matter density, by the X-ray telescope onboard the Swift satellite (see figure 1)6 and on the ultra-faint dwarf galaxy Willman 1 by Chandra X-Ray Observatory (see figure 2).7 The measurements of Segue 1 produced a meaningful upper limit to the density of sterile neutrinos in the 1.6–14 keV mass range, while the measurements on Willman 1 yielded a marginal detection (68 percent confidence of actual detection) consistent with a sterile neutrino mass of 5 keV.
Looking in the Right Places
For the first time astronomers have discovered an X-ray signal that qualifies as more than just a possible detection of sterile neutrinos. In a paper published in the December 20, 2010 Astrophysical Journal Letters A,astronomer Dmitry Prokhorov and famous physicist Joseph Silk, author of several books on big bang cosmology,8 first point out where astronomers may have gone wrong in their search for sterile neutrinos.9 They refer to X-ray observations of dwarf galaxies that apparently rule out measurable production of sterile neutrinos by Barbieri and Dolgov’s proposed mechanism.
Prokhorov and Silk suggest instead that sterile neutrinos are produced from Higgs decays, or more likely, the decay of a very light inflaton. Inflatons refer to particles responsible for generating the scalar field that drove the brief and rapid expansion of the universe between 10-35 and 10-34 seconds after the cosmic creation event—the inflationary era in big bang cosmology. At the very end of 2010, three theoretical physicists submitted a preprint in which they conclude that Silk and Prokhorov’s proposed very light inflaton is probably the axion.10
For nearly a decade now, both astronomers and theoretical physicists have touted axions as the particles that make up the majority of the universe’s exotic matter. Thus, Silk and Prokorov’s proposal could not only solve the problem of the missing sterile neutrinos but also identify the kinds of particles making up most, if not all, of the universe’s exotic matter (predominantly axions complemented by active and sterile neutrinos).
Next week, I will recount where astronomers may have already found sterile neutrinos without realizing it. In part 4, I will explain the connection between sterile neutrinos and another “God particle,” the axion. I will describe where astronomers can quickly garner confirming evidence for both sterile neutrinos and axions, and conclude with a summary of the theological advances we can expect from these discoveries, both current and emerging.
|Part 1 | Part 2 | Part 3 | Part 4|
- R. Barbieri and A. Dolgov, “Bounds on Sterile Neutrinos from Nucleosynthesis,” Physics Letters B 237 (March 22, 1990): 440–45.
- Andrea V. Macciò and Fabio Fontanot, “How Cold Is Dark Matter? Constraints from Milky Way Satellites,” Monthly Notices of the Royal Astronomical Society: Letters 404 (May 2010): L16–L20; Sergey E. Koposov et al., “A Quantitative Explanation of the Observed Population of Milky Way Satellite Galaxies,” Astrophysical Journal 696, no. 2 (May 10, 2009): 2179–94; V. Belokurov et al., “Cats and Dogs, Hair and a Hero: A Quintet of New Milky Way Companions,” Astrophysical Journal 654, no. 2 (January 10, 2007): 897–906; A. M. Brooks et al., “The Origin and Evolution of the Mass-Metallicity Relationship for Galaxies: Results from Cosmological N-Body Simulations,” Astrophysical Journal Letters 655, no. 1 (January 20, 2007): L17–L20; Tom Siegfried, “Middle-Earth Denizens Mob the Milky Way,” Science 315 (January 26, 2007): 455.
- The first release of the WMAP measurement of the temperature fluctuations in the universe’s cosmic microwave background radiation indicated that stars began to form when the universe was roughly 200 million years old. However, the superior second release of the WMAP measurement (five years worth of data compared to three) showed that stars did not begin to form until the universe was 365 million years old. See E. Komatsu et al., “Five-Year Wilkinson Microwave Anisotropy Probe Observations: Cosmological Interpretation,” Astrophysical Journal Supplement 180, no. 2 (February 2009): 330–76.
- Michael Loewenstein, Alexander Kusenko, and Peter L. Biermann, “New Limits on Sterile Neutrinos from Suzaku Observations of the Ursa Minor Dwarf Spheroidal Galaxy,” Astrophysical Journal 700, no. 1 (July 20, 2009): 426–35; S. Riemer-Sorensen and S. H. Hansen, “Decaying Dark Matter in the Draco Dwarf Galaxy,” Astronomy and Astrophysics: Letters 500 (June 3, 2009): L37–L40, 426–35; Alexey Boyarsky, Oleg Ruchayskiy, and Dmytro Iakubovskyi, “A Lower Bound on the Mass of Dark Matter Particles,” Journal of Cosmology and Astroparticle Physics 3 (March 2009): 5; Signe Riemer-Sørensen, Steen H. Hansen, and Kristian Pedersen, “Sterile Neutrinos in the Milky Way: Observational Constraints,” Astrophysical Journal Letters 644, no. 1 (June 10, 2006): L33–L36; Casey R. Watson et al., “Direct X-Ray Constraints on Sterile Neutrino Warm Dark Matter,” Physical Review D 74, no. 3 (August 17, 2006): id 033009; Alexey Boyarsky, Jukka Nevalainen, and Oleg Ruchayskiy, “Constraints on the Parameters of Radiatively Decaying Dark Matter from the Dark Matter Halos of the Milky Way and Ursa Minor,” Astronomy and Astrophysics 471 (August 1, 2007): 51–57.
- A. Boyarsky et al., “Restrictions on Parameters of Sterile Neutrino Dark Matter from Observations of Galaxy Clusters,” Physical Review D 74, no. 10 (November 15, 2006): id 103506; Matteo Viel et al., “Can Sterile Neutrinos Be Ruled Out as Warm Dark Matter Candidates?” Physical Review Letters 97, no. 7 (August 18, 2006): id 071301.
- N. Mirabal, “Swift Observations of Segue 1: Constraints on Sterile Neutrino Parameters in the Darkest Galaxy,” Monthly Notices of the Royal Astronomical Society: Letters 409 (November 2010): L128–L131.
- Michael Loewenstein and Alexander Kusenko, “Dark Matter Search Using Chandra Observations of Willman 1 and a Spectral Feature Consistent with a Decay Line of a 5 keV Sterile Neutrino,” Astrophysical Journal 714, no. 1 (May 1, 2010): 652–62.
- Joseph Silk, The Big Bang, 3rd ed. (New York: W. H. Freeman, 2001).
- Dmitry Prokhorov and Joseph Silk, “Can the Excess in the Fe XXVI Lyɣ Line From the Galactic Center Provide Evidence for 17 keV Sterile Neutrinos?” Astrophysical Journal Letters 725, no. 2 (December 20, 2010): L131–L134.
- Nemanja Kaloper, Albion Lawrence, and Lorenzo Sorbo, “An Ignoble Approach to Large Field Inflation,” (December 30, 2010): arXiv:1101.0028v1 [hep-th].