2015
DOI: 10.1007/s10509-015-2277-8
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Abstract: Transversal oscillations of spicules axes may be related to the propagation of magnetohydrodynamic waves along them. These waves may become unstable and the instability can be of the Kelvin-Helmholtz type. We use the dispersion relation of kink mode derived from linearized magnetohydrodynamic equations. The input parameters of the derived dispersion equation, namely, spicules and their ambient medium densities ratios as well as their corresponding magnetic fields ratios, are considered to be within the range 0… Show more

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Cited by 8 publications
(13 citation statements)
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“…5 in Zhelyazkov 2012a), and 15.64737, respectively, and all they are in good agreement with the highest curve in Fig. 4 in Ajabshirizadeh et al 2015. Another interesting observation is the circumstance that the minima of all computed by us 'v'-shaped (see the red curve in the bottom panel of Fig.…”
Section: Discussionsupporting
confidence: 73%
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“…5 in Zhelyazkov 2012a), and 15.64737, respectively, and all they are in good agreement with the highest curve in Fig. 4 in Ajabshirizadeh et al 2015. Another interesting observation is the circumstance that the minima of all computed by us 'v'-shaped (see the red curve in the bottom panel of Fig.…”
Section: Discussionsupporting
confidence: 73%
“…On the other hand, their curves plotted in Fig. 4 in Ajabshirizadeh et al 2015 seem to be correct. One can see, that according to the curve corresponding to η = 0.1 for b = 0.25 the critical Alfvén Mach number, M cr A , must be a little higher than 4, in fine agreement with our computations.…”
Section: Discussionmentioning
confidence: 83%
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“…In its nonlinear stage, the KHI trigger the wave turbulence which is considered as one of the main heating mechanisms of the solar corona (Cranmer et al, 2015). The development of the KHI in various cylindrical jet-environment configurations has been studied in photospheric jets (Zhelyazkov and Zaqarashvili, 2012), in solar spicules (Zhelyazkov, 2012;Ajabshirizadeh et al, 2015;Ebadi, 2016), in high-temperature and cool solar surges (Zhelyazkov et al, 2015a,b), in magnetic tubes of partially ionized compressible plasma (Soler et al, 2015), in EUV chromospheric jets (Zhelyazkov, Chandra, and Srivastava, 2016;Bogdanova et al, 2018), in soft X-ray jets (Vasheghani Farahani et al, 2009;Zhelyazkov, Chandra, and Srivastava, 2017), and in the twisted solar wind flows (Zaqarashvili et al, 2014). A review on KHI in the solar atmosphere, including some earlier studies, the reader can find in Zhelyazkov, 2015. The first modeling of the KHI in a rotating cylindrical magnetized plasma jet was done by Bondenson, Iacono, and Bhattacharjee (1987).…”
Section: Introductionmentioning
confidence: 99%