Talk detail

Participant	Kashiyama, Kazumi
Institution	The Pennsylvania State University - 1000 South Allen Street, Apt. B1 - State College - PA - USA

Session	SO4	Accepted		Order	Time
Talk	Oral abstract	Title	White dwarf pulsars as possible cosmic ray electron-positron factories
Co-authors
Abstract	We suggest that white dwarf (WD) pulsars can compete with neutron star (NS) pulsars for producing the excesses of cosmic ray electrons and positrons (e}) observed by the PAMELA, Fermi, and H.E.S.S. experiments. A merger of two WDs leads to a rapidly spinning WD with a rotational energy comparable to the NS case. The birth rate is also similar, providing the right energy budget for the cosmic ray e}. Applying the NS theory, we suggest that the WD pulsars can in principle produce e} up to 10TeV. In contrast to the NS model, the adiabatic and radiative energy losses of e} are negligible since their injection continues after the expansion of the pulsar wind nebula, and hence it is enough that a fraction 1% of WDs are magnetized as observed. The long activity also increases the number of nearby sources. The WD pulsars could dominate the quickly cooling e} above TeV energy as a second spectral bump or even surpass the NS pulsars in the observing energy range 10GeV-1TeV, providing a background for the dark matter signals and a nice target for the future AMS-02, CALET, and CTA experiment.