Fingerprints in the Spectrum: Pulsars vs. Dark Matter ✛ ✎ ✦

Original: "Electrons and Positrons in Cosmic Rays"
· A. D. Panov
arXiv:1303.6118 · 2013-03-25 · arXiv non-exclusive · independent analysis · 2 min
The high-precision electron spectrum measured by the ATIC instrument reveals narrow peaks that cannot be explained by dark matter annihilation but can be explained by nearby pulsars.

The cosmic electron spectrum is like fingerprints at a crime scene. Particles arriving from the depths of the Galaxy carry in their energies the traces of those that produced them. For a long time, the picture was blurred: instruments with wide energy bins, like out-of-focus photographs, did not reveal details. But recently, scientists got a sharp image — a high-precision spectrum measured by the ATIC instrument with a resolution of about 3%. And unexpected lines appeared on it.

The fine structure of the spectrum, three peaks and three dips, is like the grooves on a bullet, by which one can tell from which barrel it was fired.

Previously, it was believed that all positrons in cosmic rays are born as secondaries: protons colliding with interstellar gas produce electron-positron pairs. But data from PAMELA and Fermi/LAT showed that the positron fraction increases with energy, which the secondary model cannot explain. Two main suspects emerged: annihilation of dark matter particles and nearby pulsars — rapidly rotating neutron stars that, like lighthouses, emit streams of particles. Both scenarios described the low-energy data equally well, and they could not be distinguished.

The new ATIC spectrum changed the game. In the 200–600 GeV range, it showed not a smooth curve but a distinct jagged structure: three peaks around 250, 350, and 450 GeV, and three dips between them. The statistical significance is 99.7%, and the structure was reproduced in two independent flights. These are not random fluctuations but real fingerprints.

Dark matter, when annihilating, produces a broad, smooth spectrum — a single smeared trace. It cannot create several narrow peaks. But several nearby pulsars, each injecting electrons of specific energies, naturally produce such a comb.

Fitting the fine structure with several pulsars is possible with reasonable parameters. Moreover, in this case, the positron fraction should rise rapidly with energy, reaching about 0.4 at 400–500 GeV, which is consistent with Fermi/LAT data up to 200 GeV. Thus, the fingerprints begin to form a portrait of specific sources.

Now that we have a sharp image, it remains to confirm it with independent experiments. If the fine structure is reproduced on other instruments, it will become a decisive argument in favor of the pulsar origin of the anomalies. And then the mystery of the positron excess will be solved — not by dark matter, but by familiar cosmic lighthouses.

The ATIC instrument flew on a balloon around the South Pole three times, and in two flights (ATIC-2 and ATIC-4) the fine structure of the electron spectrum was reproduced down to details, despite different conditions.

Scientists
Enrico FermiErnest RutherfordAlbert EinsteinBarry BarishKip ThorneRichard Feynman
Concepts
ultra high energy cosmic ray source cosmic ray composition positron particle acceleration astrophysical polarimetry axion dark matter pulsar electron positron pair photoelectron axion detection neutron stars radio interference polaron pulsar phenomena energy reconstruction asymmetric dark matter radio source synchrotron radiation anomaly pulsation neutron star light emission