6 6 $_{2}$He $^{++}$→ 6 $_{3}$Li +++ + e − + ¯ ν$_{e}$ [25], the high intensity of the 6 $_{2}$He ++ source and a large Lorentz boost factor are necessary. We suggest alternative schemes. One is that in the process e $^{−}$+ p → n + ν$_{e}$ we can employ the very collimated electron beam to bombard the protons at rest. Another is that we can use the lowly accelerated pion beam for π ± → e ± + ¯ ν$_{e}$ ( ν$_{e}$ ) . Even though in the second proposal, the decay rate is sup- pressed by the helicity rule, the branching ratio is still of the order of 10 − 4 [26], so with a large number of pions, it is still plausible. Moreover, a large Lorentz boost factor | p | /m$_{e}$ which determines the spreading solid angle, is easy to obtain and the energy for the pion accelerator needs to be just at O (GeV) . Thus the size of such facilities can be small and the corresponding technique would be relatively simple. We sincerely thank Prof. B.L. Young who introduced the applications of neutrino beams in various fields, especiall y the neutrino tomography, to us. We have greatly benefited from very enlightening discussions on the subject with Prof. Chung Ngoc Leung. In fact, this work was motivated by the discus- sion when he visited the Nankai campus. This work is sup- ported by the National Natural Science Foundation of China (NNSFC) and the Special Grant of the Education Ministry of China for the Ph.D programs. 053; Lindner M, Ohlsson T, Tomas R et al. Astropart. Phys., 2003, 19 : 755-770; Ohlsson T, Winter W. Phys. Lett., 2001, B512 ; 357-364; Jain P, Ralston J P, Frichter G M. Astropart. Phys., 1999, 12 : 193-198; Sugawara H, Hagura H, Sanami T. 2003, arXiv:hep-ph/0305062 [1] Rujula A De, Glashow S L, Wilson R R et al. Phys. Rept., 1983, 99 : 341-396 [2] Ioannisian A N, Smirnov A Y. 2002, arXiv:hep-ph/0201012 [3] Ohlsson T, Winter W. Europhys. Lett., 2002, 60(1) : 34-39 [4] Young B L, in the proceedings for the conference on the ad- vanced topics in the interdiscipilinary fields of particle p hysics, nuclear physics and cosmology, Tengchong, China, Aug., 2008 [5] Wilson T L. Nature, 1984, 309 : 38-42; Gonzalez-Garcia M C, Halzen F, Maltoni M et al. Phys. Rev. Lett., 2008, 100 : 061802; Akhmedov E K, Tortola M A, Valle J W.F. JHEP, 2005, 0506 : [6] CAO Jun. Nucl. Phys. Proc. Suppl., 2006, 155 : 229-230; CHEN Shao-Min. J. Phys. Conf. Ser., 2008, 120 : 052024; White C. J. Phys. Conf. Ser., 2008, 136 : 022012 [7] Dawson J.V. 2009, arXiv:hep-ex/0905.4843 [8] Wolfenstein L. Phys. Rev. D, 1978, 17 : 2369-2374 [9] Mikheev S P, Smirnov A Y. Sov. J. Nucl. Phys., 1985, 42 : 913- 917; Nuovo Cim. C, 1986, 9 : 17-26 [10] Giunti C, Kim C W. Fundamentals of Neutrino Physics and As- trophysics. New York: Oxford, 2007 [11] Winter W. Earth Moon and Planets, 2006, 99 : 285-307 [12] LI Yan-Xing, ZHANG Jing-Hua, ZHOU Wei et al. Chinese J. Geophys., 2009, 52(2) : 519-530(in Chinese) [13] Stacey F D. Physics of the Earth. New York: John Wiley & Sons, 1977 [14] CHEN Zu-An, LIN Bang-Hui, BAI Wu-Ming et al. Chinese J. Geophys., 2009, 52(2) : 408-417(in Chinese) [15] Namgaladze A A, Zolotov O V, Zakharenkova I E et al. Proc. of MSTU, 2009, 12 : 308-315 [16] Pulinets S. TAO, 2004, 15 : 413-435 [17] WANG Xu-Ben, ZHU Ying-Tang, ZHAO Xi-Kui et al. Chinese J. Geophys., 2009, 52(2) : 564-571(in Chinese) [18] ZHOU Yong-Sheng, HE Chang-Rong. Chinese J. Geophys., 2009, 52(2) : 474-484(in Chinese) [19] ZHU Shou-Biao, Zhang Pei-Zhen. Chinese J. Geophys., 2009, 52(2) : 418-427(in Chinese) [20] Fogli G L, Lettera G, Lisi E et al. Phys. Rev. D, 2002, 66 : 093008 [21] XING Zhi-Zhong. Int. J. Mod. Phys. E, 2007, 16 :1361-1372 [22] Nicolaidis A, Jannane M, Tarantola A. J. Geophys. Res., 1991, 96 : 21811-21817 [23] Geer S. Phys. Rev. D, 1998, 57 : 6989-6997 [24] Ioannisian A N, Smirnov A Y. Phys. Rev. Lett., 2004, 93 : 241801 [25] Zucchelli P. Phys. Lett. B, 2002, 532 : 166-172 [26] Particle Data Group. Phys. Lett. B, 2008, 667 : 1-1340