ner_tags: O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Model O O O O O O O O O O O O O O O O O B-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Mission I-Mission O O O O O O O O O O O O O O O O O O B-Model I-Model O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation O B-Citation O O B-Formula I-Formula I-Formula I-Formula I-Formula O O O O O O O O B-Model I-Model I-Model O O O O O O O O O O O O O O O O O B-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula O O O O O O O O O O O O O B-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O B-Model I-Model I-Model O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Mission I-Mission O O O O O O O O O O O O O O O O O O O O O B-Formula I-Formula I-Formula I-Formula O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Formula I-Formula I-Formula I-Formula I-Formula I-Formula O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O
tokens: dispersion relation for the slow mode gives for quasi-perpendicular and perpendicular propagations. The weak perpendicular magnetic power can be associated with the Alfvén mode. In this discussion, it is assumed that the plasma temperature is isotropic. However, the presence of temperature anisotropy can modify the dispersion relation of the MHD eigenmodes and/or excite other wave modes, such as the mirror mode, kink mode and sausage mode (e.g., Hasegawa 1975 ; Huang et al. 1988 ; Wang Hau 2003 ; Schoeffler et al. 2011 ). The modification of eigenmodes and the excitation of other modes can also affect the turbulence and hence alter the observed power relation. 7. Summary This paper presents the turbulence spectra of magnetic and electron density fluctuations in situ measured by Voyager 1 in the local ISM. The results can be summarized as follows: 1. The present magnetic spectra obtained by Lomb–Scargle periodogram show a good agreement with the results by Burlaga et al. ( 2015 , 2018 ). At m k ≤ 10 −8.8 , the magnetic spectrum is close to a Kolmogorov power law with a one-dimensional power-law index −5/3. The magnetic SDFs show a bulge of enhanced magnetic power at m k = 10 −8.8 –10 −8.2 . 2. We extend our previous study of the electron density turbulence spectrum (Lee Lee 2019 ) and spans the data coverage to 2019 June. The composite spectrum of both the present in situ measurements and the earlier remote observations shows the Kolmogorov power law in the inertial range (10 6 –10 18 m) and an enhanced power in the kinetic range (50–10 6 m). 3. The electron density turbulence measured by Voyager 1 in the local ISM shows higher intensity than that of the remote observations in the distant ISM by a factor of 10 1.96 ≈ 91. Such an enhanced turbulent power can be resulted from a combination of the energy sources from both the turbulent interstellar plasma and the turbulent solar wind. 4. The relationship between the outer scale L 0 , and the rms values of magnetic and electron density fluctuations are obtained. In the calculation with only in situ measured data of electron density and magnetic field, we obtain and for L 0 = 3 × 10 14 m. Burlaga et al. ( 2018 ) obtained the same outer scale and interpreted this outer scale as the spatial range of the disturbed local ISM, which is separated by the bow wave or bow shock from the undisturbed local ISM. 5. For the typical interstellar cloud size L 0 = 10 18 m, we obtain from the in situ measured magnetic data and obtain by including both the in situ measurements and remote observations in the calculation of electron density SDFs. These rms values of magnetic and electron density fluctuations are much higher than the in situ measured mean values because the turbulence amplitude becomes larger at a longer wavelength. Chepurnov Lazarian ( 2010 ) measured a high electron density fluctuation power at the scale of an interstellar cloud. A high magnetic strength of tens of nanotesla has been observed at the