Abstract
We suggest that white dwarf pulsars can compete with neutron star pulsars for producing the excesses of cosmic ray positrons and electrons (e±) observed by the PAMELA, ATIC/PPB‐BETS, Fermi and HESS experiments. A double degenerate white dwarf binary mergers into a white dwarf pulsar with rotational energy (∼1050 erg) comparable to a neutron star pulsar. The birth rate (∼1/100 yr) is also similar, providing the right energy budget. Applying the neutron star theory, we show that the white dwarf pulsars can produce e±, up to ∼10 TeV for high magnetic fields (>108 G). In contrast to the neutron star case, the adiabatic energy losses of e± are negligible since their injection continues after the nebula expansion. The long activity also enhances the nearby sources, potentially dominating the quickly cooled e± above TeV energy, detectable by the future CALET experiment.
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