Spectral distribution of the cross helicity in the solar wind

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Spectral distribution of the cross helicity in the solar wind was investigated. It was found that the space plasma turbulence is distributed anisotropically in space relative to magnetic field direction. The cross helicity was found to enter a magnetohydrodynamic description on equal footing with th...

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Autor principal: Milano, L.J
Otros Autores: Dasso, Sergio Ricardo, Matthaeus, W.H, Smith, C.W
Formato: Capítulo de libro
Lenguaje:Inglés
Publicado: 2004
Acceso en línea:Registro en Scopus
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Biblioteca Central Dr. Luis F. Leloir (FCEN) de Universidad de Buenos Aires
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100 1 |a Milano, L.J. 
245 1 0 |a Spectral distribution of the cross helicity in the solar wind 
260 |c 2004 
270 1 0 |m Milano, L.J.; Bartol Research Institute, University of Delaware, Newark, DE 19716, United States 
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504 |a Goldstein, M.L., Roberts, D.A., Deane, A., (2003) AIP Conf. Proc. No. 679, 679, pp. 405-408. , Solar Wind Ten, (AIP, New York) 
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506 |2 openaire  |e Política editorial 
520 3 |a Spectral distribution of the cross helicity in the solar wind was investigated. It was found that the space plasma turbulence is distributed anisotropically in space relative to magnetic field direction. The cross helicity was found to enter a magnetohydrodynamic description on equal footing with the energy. The rotational symmetry of the cross helicity was examined. It was found that the cross helicity is associated more or less equally with all angular components of the fluctuations.  |l eng 
536 |a Detalles de la financiación: Umweltbundesamt 
536 |a Detalles de la financiación: National Aeronautics and Space Administration, NAG5-8134, NAG5-11603 
536 |a Detalles de la financiación: National Science Foundation, ATM 0105254 
536 |a Detalles de la financiación: Consejo Nacional de Investigaciones Científicas y Técnicas, PIP 2693 
536 |a Detalles de la financiación: PC251459 
536 |a Detalles de la financiación: JGREA2 0148-0227 97 , 17 189 ( 1992 ). W. H. M. and L. J. M. acknowledge support by the NSF (ATM 0105254) and NASA (NAG5-8134 and NAG5-11603). S. D. acknowledges partial support by UBA Grant No. UBACYT X329, CONICET Grant No. PIP 2693, and FONCyT-ANPCyT Grant No. PICT 12187. S. D. is a member of the Carrera del Investigador Científico, CONICET. C. W. S. is supported by J.P.L. Contract No. PC251459 under NASA Grant No. NAG5-6912 for support of the ACE/MAG instrument. ACE data was provided by the ACE Science Center. 
593 |a Bartol Research Institute, University of Delaware, Newark, DE 19716, United States 
593 |a Inst. Astronomia y Fis. del Espacio, Buenos Aires, Argentina 
593 |a Departamento de Física, Fac. de Ciencias Exactas y Naturales, Universidad de Buenos Aires, Buenos Aires, Argentina 
593 |a Inst. for Earth, Oceans and Space, University of New Hampshire, Durham, NH 03824, United States 
690 1 0 |a ANISOTROPY 
690 1 0 |a HEATING 
690 1 0 |a MAGNETIC FIELDS 
690 1 0 |a MAGNETOHYDRODYNAMICS 
690 1 0 |a MATHEMATICAL MODELS 
690 1 0 |a STABILITY 
690 1 0 |a THERMAL CONDUCTIVITY OF SOLIDS 
690 1 0 |a TURBULENCE 
690 1 0 |a VECTORS 
690 1 0 |a CROSS HELICITY 
690 1 0 |a SOLAR WIND 
690 1 0 |a WAVE NUMBERS 
690 1 0 |a WAVE VECTORS 
690 1 0 |a PLASMA THEORY 
700 1 |a Dasso, Sergio Ricardo 
700 1 |a Matthaeus, W.H. 
700 1 |a Smith, C.W. 
773 0 |d 2004  |g v. 93  |h pp. 155005-1-155005-4  |k n. 15  |p Phys Rev Lett  |x 00319007  |w (AR-BaUEN)CENRE-386  |t Physical Review Letters 
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856 4 0 |u https://doi.org/10.1103/PhysRevLett.93.155005  |x doi  |y DOI 
856 4 0 |u https://hdl.handle.net/20.500.12110/paper_00319007_v93_n15_p155005_Milano  |x handle  |y Handle 
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963 |a VARI 

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