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Identification of slow magnetosonic wave trains and their evolution in 3-D compressible turbulence simulation
Zhang, L.; Yang, L. -P.; He, J. -S.; Tu, C. -Y.; Wang, L. -H.; Marsch, E.; Feng, X. -S.; He, JS (reprint author), Peking Univ, Sch Earth & Space Sci, Beijing 100871, Peoples R China.
Department空间科学部
Source PublicationANNALES GEOPHYSICAE
2015
Volume33Issue:1Pages:13-23
ISSN0992-7689
Language英语
KeywordInterplanetary Physics Mhd Waves And Turbulence
AbstractIn solar wind, dissipation of slow-mode magnetosonic waves may play a significant role in heating the solar wind, and these modes contribute essentially to the solar wind compressible turbulence. Most previous identifications of slow waves utilized the characteristic negative correlation between delta vertical bar B vertical bar and delta rho. However, that criterion does not well identify quasi-parallel slow waves, for which delta vertical bar B vertical bar is negligible compared to delta rho. Here we present a new method of identification, which will be used in 3-D compressible simulation. It is based on two criteria: (1) that V-pB0 (phase speed projected along B-0) is around +/- c(s), and that (2) there exists a clear correlation of delta upsilon(vertical bar vertical bar) and delta rho. Our research demonstrates that if upsilon(A) > c(s), slow waves possess correlation between delta upsilon(vertical bar vertical bar) and delta rho, with delta upsilon(vertical bar vertical bar) = delta upsilon(vertical bar vertical bar) approximate to rho(0)/c(s). This method helps us to distinguish slow-mode waves from fast and Alfven waves, both of which do not have this polarity relation. The criteria are insensitive to the propagation angle theta(kB), defined as the angle between wave vector k and B-0; they can be applied with a wide range of beta if only upsilon(A) > c(s). In our numerical simulation, we have identified four cases of slow wave trains with this method. The slow wave trains seem to deform, probably caused by interaction with other waves; as a result, fast or Alfven waves may be produced during the interaction and seem to propagate bidirectionally away. Our identification and analysis of the wave trains provide useful methods for investigations of compressible turbulence in the solar wind or in similar environments, and will thus deepen understandings of slow waves in the turbulence.
Indexed BySCI ; EI
Document Type期刊论文
Identifierhttp://ir.nssc.ac.cn/handle/122/4664
Collection空间科学部
Corresponding AuthorHe, JS (reprint author), Peking Univ, Sch Earth & Space Sci, Beijing 100871, Peoples R China.
Recommended Citation
GB/T 7714
Zhang, L.,Yang, L. -P.,He, J. -S.,et al. Identification of slow magnetosonic wave trains and their evolution in 3-D compressible turbulence simulation[J]. ANNALES GEOPHYSICAE,2015,33(1):13-23.
APA Zhang, L..,Yang, L. -P..,He, J. -S..,Tu, C. -Y..,Wang, L. -H..,...&He, JS .(2015).Identification of slow magnetosonic wave trains and their evolution in 3-D compressible turbulence simulation.ANNALES GEOPHYSICAE,33(1),13-23.
MLA Zhang, L.,et al."Identification of slow magnetosonic wave trains and their evolution in 3-D compressible turbulence simulation".ANNALES GEOPHYSICAE 33.1(2015):13-23.
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