Pulsar velocity with three-neutrino oscillations in non-adiabatic processes

被引:6
作者
Kim, CW [1 ]
Kim, JD
Song, J
机构
[1] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA
[2] Korea Inst Adv Study, Sch Phys, Seoul 130012, South Korea
[3] Seoul Natl Univ, Ctr Theoret Phys, Seoul 151742, South Korea
关键词
D O I
10.1016/S0370-2693(97)01441-X
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We have studied the position dependence of neutrino energy on the Kusenko-Segre mechanism as an explanation of the proper motion of pulsars. The mechanism is also examined in three-generation mixing of neutrinos and in a non-adiabatic case. The position dependence of neutrino energy requires the higher value of magnetic field such as B similar to 3 x 10(15) Gauss in order to explain the observed proper motion of pulsars. It is shown that possible non-adiabatic processes decrease the neutrino momentum asymmetry, whereas an excess of electron neutrino flux over other flavor neutrino fluxes increases the neutrino momentum asymmetry. It is also shown that a general treatment with all three neutrinos does not modify the result of the two generation treatment if the standard neutrino mass hierarchy is assumed. (C) 1998 Elsevier Science B.V.
引用
收藏
页码:279 / 284
页数:6
相关论文
共 26 条
[1]   IMPLICATIONS OF THE GALLEX DETERMINATION OF THE SOLAR NEUTRINO FLUX [J].
ANSELMANN, P ;
HAMPEL, W ;
HEUSSER, G ;
KIKO, J ;
KIRSTEN, T ;
PERNICKA, E ;
PLAGA, R ;
RONN, U ;
SANN, M ;
SCHLOSSER, C ;
WINK, R ;
WOJCIK, M ;
VONAMMON, R ;
EBERT, KH ;
HENRICH, E ;
BALATA, M ;
BELLOTTI, E ;
FERRARI, N ;
LALLA, H ;
STOLARCZYK, T ;
CATTADORI, C ;
CREMONESI, O ;
FIORINI, E ;
PEZZONI, S ;
ZANOTTI, L ;
VONFEILITZSCH, F ;
MOSSBAUER, R ;
SCHANDA, U ;
BERTHOMIEU, G ;
SCHATZMAN, E ;
CARMI, I ;
DOSTROVSKY, I ;
BACCI, C ;
BELLI, P ;
BERNABEI, R ;
DANGELO, S ;
PAOLUZI, L ;
CHARBIT, S ;
CRIBIER, M ;
DUPONT, G ;
GOSSET, L ;
RICH, J ;
SPIRO, M ;
TAO, C ;
VIGNAUD, D ;
HAHN, RL ;
HARTMANN, FX ;
ROWLEY, JK ;
STOENNER, RW ;
WENESER, J .
PHYSICS LETTERS B, 1992, 285 (04) :390-397
[2]  
Bilenky S. M., 1978, Physics Reports. Physics Letters Section C, V41c, P225, DOI 10.1016/0370-1573(78)90095-9
[3]   NEUTRINO OSCILLATIONS IN THE FRAMEWORK OF 3-GENERATION MIXINGS WITH MASS HIERARCHY [J].
BILENKY, SM ;
BOTTINO, A ;
GIUNTI, C ;
KIM, CW .
PHYSICS LETTERS B, 1995, 356 (2-3) :273-281
[4]  
BIRKEL M, ASTROPH9704138
[5]   THE BIRTH OF NEUTRON-STARS [J].
BURROWS, A ;
LATTIMER, JM .
ASTROPHYSICAL JOURNAL, 1986, 307 (01) :178-196
[6]   ELECTROMAGNETIC PROPERTIES OF NEUTRINOS IN A BACKGROUND OF ELECTRONS [J].
DOLIVO, JC ;
NIEVES, JF ;
PAL, PB .
PHYSICAL REVIEW D, 1989, 40 (11) :3679-3687
[7]  
ESPOSITO S, 1996, Z PHYS C, V70, P70
[8]   Solar neutrino data, solar model uncertainties and solar matter-enhanced neutrino oscillations [J].
Fogli, G. L. ;
Lisi, E. .
ASTROPARTICLE PHYSICS, 1994, 2 (01) :91-99
[9]   COMPREHENSIVE ANALYSIS OF SOLAR, ATMOSPHERIC, ACCELERATOR, AND REACTOR NEUTRINO EXPERIMENTS IN A HIERARCHICAL 3-GENERATION SCHEME [J].
FOGLI, GL ;
LISI, E ;
MONTANINO, D .
PHYSICAL REVIEW D, 1994, 49 (07) :3626-3642
[10]   RUNAWAY STARS AND PULSARS NEAR CRAB NEBULA [J].
GOTT, JR ;
GUNN, JE ;
OSTRIKER, JP .
ASTROPHYSICAL JOURNAL, 1970, 160 (02) :L91-&