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Generalized similarity in finite range solar wind magnetohydrodynamic turbulence

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Chapman, Sandra C. and Nicol, R. M.. (2009) Generalized similarity in finite range solar wind magnetohydrodynamic turbulence. Physical Review Letters, Vol.103 (No.24). Article no. 241101 . ISSN 0031-9007

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Abstract

Extended or generalized similarity is a ubiquitous but not well understood feature of turbulence that is realized over a finite range of scales. The ULYSSES spacecraft solar polar passes at solar minimum provide in situ observations of evolving anisotropic magnetohydrodynamic turbulence in the solar wind under ideal conditions of fast quiet flow. We find a single generalized scaling function characterizes this finite range turbulence and is insensitive to plasma conditions. The recent unusually inactive solar minimum-with turbulent fluctuations down by a factor of similar to 2 in power-provides a test of this invariance.

Item Type: Journal Article
Subjects: Q Science > QB Astronomy
Q Science > QC Physics
Divisions: Faculty of Science > Physics
Library of Congress Subject Headings (LCSH): Solar wind, Magnetohydrodynamics, Finite size scaling (Statistical physics)
Journal or Publication Title: Physical Review Letters
Publisher: American Physical Society
ISSN: 0031-9007
Official Date: 11 December 2009
Volume: Vol.103
Number: No.24
Number of Pages: 4
Page Range: Article no. 241101
Identification Number: 10.1103/PhysRevLett.103.241101
Status: Peer Reviewed
Publication Status: Published
Funder: Engineering and Physical Sciences Research Council (EPSRC), Science and Technology Facilities Council (Great Britain) (STFC), Culham Centre for Fusion Energy (CCFE)
References:

[1] F. Moisy, P. Tabeling, and H. Willaime, Phys. Rev. Lett.
82, 3994 (1999).
[2] G. I. Barenblatt and A. J. Chotin, Proc. Natl. Acad. Sci.
U.S.A. 101, 15 023 (2004).
[3] K. R. Sreenivasan and A. Bershadskii, J. Fluid Mech. 554,
477 (2006).
[4] S. Grossmann, D. Lohse, V. L’vov, and I. Procaccia, Phys.
Rev. Lett. 73, 432 (1994).
[5] B. Dubrulle, Eur. Phys. J. B 14, 757 (2000).
[6] R. Benzi et al., Phys. Rev. E 48, R29 (1993).
[7] V. Carbone, R. Bruno, and P. Veltri, Geophys. Res. Lett.
23, 121 (1996).
[8] C. Pagel and A. Balogh, Nonlinear Proc. Geophys. 8, 313
(2001).
[9] S. C. Chapman et al., Astrophys. J. Lett. 695, L185 (2009).
[10] R. M. Nicol, S. C. Chapman, and R. O. Dendy, Astrophys.
J. 679, 862 (2008).
[11] R. Bruno and V. Carbone, Living Rev. Solar Phys. 2, 4
(2005).
[12] W. H. Matthaeus et al., Phys. Rev. Lett. 95, 231101
(2005).
[13] W. H. Matthaeus and M. L. Goldstein, Phys. Rev. Lett. 57,
495 (1986).
[14] W. H. Matthaeus et al., Astrophys. J. Lett. 657, L121
(2007).
[15] K. H. Kiyani et al., Phys. Rev. Lett. 103, 075006 (2009).
[16] O. Alexandrova, V. Carbone, P. Veltri, and L. Sorriso-
Valvo, Planet. Space Sci. 55, 2224 (2007).
[17] O. Alexandrova, V. Carbone, P. Veltri, and L. Sorriso-
Valvo, Astrophys. J. 674, 1153 (2008)
[18] O. Alexandrova et al., Phys. Rev. Lett. 103, 165003
(2009).
[19] S. D. Bale et al., Phys. Rev. Lett. 94, 215002 (2005).
[20] T. S. Horbury, A. Balogh, R. J. Forsyth, and E. J. Smith,
Astron. Astrophys. 316, 333 (1996).
[21] R. Bruno et al., Phys. Plasmas 14, 032901 (2007).
[22] E. Marsch and C.-Y. Tu, Nonlinear Proc. Geophys. 4, 101
(1997).
[23] L. Sorriso-Valvo et al., Planet. Space Sci. 49, 1193 (2001).
[24] L. F. Burlaga and M. A. Forman, J. Geophys. Res. 107,
1403 (2002).
[25] L. J. Milano, S. Dasso, W. H. Matthaeus, and C.W. Smith,
Phys. Rev. Lett. 93, 155005 (2004).
[26] S. C. Chapman and B. Hnat, Geophys. Res. Lett. 34,
L17 103 (2007).
[27] T. S. Horbury, M. Forman, and S. Oughton, Phys. Rev.
Lett. 101, 175005 (2008).
[28] B. Hnat, S. C. Chapman, and G. Rowlands, Phys. Rev.
Lett. 94, 204502 (2005).
[29] V. Carbone et al., Phys. Rev. Lett. 103, 061102 (2009).
[30] R. M. Nicol, S. C. Chapman, and R. O. Dendy, Astrophys.
J. 703, 2138 (2009).
[31] L. Sorriso-Valvo et al., Phys. Rev. Lett. 99, 115001
(2007).
[32] D. J. McComas et al., Geophys. Res. Lett. 35, L18 103
(2008).
[33] E. J. Smith and A. Balogh, Geophys. Res. Lett. 35, L22103
(2008).
[34] K. Issautier et al., Geophys. Res. Lett. 35, L19101 (2008).
[35] R. G. Marsden, E. J. Smith, J. F. Cooper, and C. Tranquille,
Astron. Astrophys. 316, 279 (1996).
[36] K. Kiyani, S. C. Chapman, and B. Hnat, Phys. Rev. E 74,
051122 (2006).
[37] K. Kiyani, S. C. Chapman, B. Hnat, and R. M. Nicol, Phys.
Rev. Lett. 98, 211101 (2007).
[38] T. S. Horbury, A. Balogh, R. J. Forsyth, and E. J. Smith,
Geophys. Res. Lett. 22, 3401 (1995).
[39] T. S. Horbury, A. Balogh, R. J. Forsyth, and E. J. Smith,
Astron. Astrophys. 316, 333 (1996).
[40] Y. Narita, K.-H. Glassmeier, and R. A. Treumann, Phys.
Rev. Lett. 97, 191101 (2006).
[41] D. Sundkvist, A. Retino, A. Vaivads, and S. D. Bale, Phys.
Rev. Lett. 99, 025004 (2007).
URI: http://wrap.warwick.ac.uk/id/eprint/16763

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