White dwarf pulsars as possible cosmic ray electron-positron factories
White dwarf pulsars as possible cosmic ray electron-positron factories
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DOI：
10.1103/physrevd.83.023002
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发表时间：
2011-01-07
影响因子：
5
通讯作者：
Kawanaka, Norita
中科院分区：
文献类型：
--
作者：
Kashiyama, Kazumi;Ioka, Kunihito;Kawanaka, Norita
我们认为，白色矮星（WD）可以与中子星星（NS）竞争产生PAMELA、ATIC/PPB-BETS、Fermi和H. E. S. S.实验两个WD的合并导致一个快速旋转的WD，其旋转能量（类似于10（50）erg）与NS情况相当。出生率（类似于10（-2）-10（-3）/年/星系）也是相似的，为宇宙射线e（+/-）提供了正确的能量预算。应用NS理论，我们认为WD型双腔体原则上可以产生高达10 TeV的e（+/-）。与NS模型相反，e（+/-）的绝热和辐射能量损失可以忽略不计，因为它们的注入在脉冲星风星云膨胀后继续进行，因此，如观察到的那样，大约1%的WD被磁化（类似于10（7）-10（9）G）就足够了。长时间的活动也增加了附近源的数量（类似于100），这降低了通量的泊松波动。WD双星可以在TeVenergy以上的快速冷却e（+/-）中占主导地位，作为第二个光谱凸起，甚至在类似于10 GeV-1 TeV的观测能量范围内超过NS双星，为暗物质信号提供背景，并为未来的AMS-02，CALET和CTA实验提供一个很好的目标。
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, ATIC/PPB-BETS, Fermi, and H. E. S. S. experiments. A merger of two WDs leads to a rapidly spinning WD with a rotational energy (similar to 10(50) erg) comparable to the NS case. The birth rate (similar to 10(-2)-10(-3)/yr/galaxy) 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 similar to 10 TeV. 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 similar to 1% of WDs are magnetized (similar to 10(7)-10(9) G) as observed. The long activity also increases the number of nearby sources (similar to 100), which reduces the Poisson fluctuation in the flux. The WD pulsars could dominate the quickly cooling e(+/-) above TeVenergy as a second spectral bump or even surpass the NS pulsars in the observing energy range similar to 10 GeV-1 TeV, providing a background for the dark matter signals and a nice target for the future AMS-02, CALET, and CTA experiment.