Talk detail

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

Session	SO4	Accepted	Yes	Order	8	Time	16:30 - 16:50	15' + 5'
Talk	Oral abstract	Title	White dwarf pulsars as possible cosmic ray electron-positron factories
Co-authors	Kunihito Ioka, Norita Kawanaka
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.