High-energy electrons lose energy by the synchrotron and inverse Compton processes during the passage in the Galaxy. By these raidative losses, the TeV electrons can propagate from the sources only within several hundred pc during their lifetimes of about 10 5 yr. After the discovery of the evidence of electrons up to 100TeV in SN1006, the argument for supernova origin of high-energy cosmic-ray electrons has been strongly supported. Several candidates among nearby supernova remnants (SNRs) contributing to the high-energy electrons in the solar system have been investigated. The previous estimate of distance to Vela was 500pc, and too far to contribute effectively to TeV electrons in the solar system. However, the recent accurate estimate reduces this distance to 250 pc. Vela is now the most likely candidate contributing significantly to TeV electrons near the solar system. Comparing to the observed data, some consequences of Vela contribution to the spectrum of electrons in the TeV region, and the astrophysical significance are discussed in this paper.
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