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We study the correlation between the non-thermal velocity dispersion($\sigma_{\rm nth}$) and the length-scale (L) in the neutral interstellarmedium (ISM) using a large number of Hi gas components taken from variouspublished Hi surveys and previous Hi studies. We notice that above thelength-scale ($L$) of 0.40 pc, there is a power-law relationship between$\sigma_{\rm nth}$ and $L$. However, below 0.40 pc, there is a break in thepower-law, where $\sigma_{\rm nth}$ is not significantly correlated with $L$.It has been observed from the Markov chain Monte Carlo (MCMC) method that forthe dataset of $L > 0.40$ pc, the most probable values of intensity ($A$) andpower-law index ($p$) are 1.14 and 0.55 respectively. Result of $p$ suggeststhat the power-law is steeper than the standard Kolmogorov law of turbulence.This is due to the dominance of clouds in the cold neutral medium. This is evenmore clear when we separate the clouds into two categories: one for $L$ is >0.40 pc and the kinetic temperature ($T_k$ ) is < 250 K, which are in the coldneutral medium (CNM) and for other one where L is > 0.40 pc and T k is between250 K and 5000 K, which are in the thermally unstable phase (UNM). Mostprobable values of $A$ and $p$ are 1.14 and 0.67 respectively in the CNM phaseand 1.01 and 0.52 respectively in the UNM phase. A greater number of datapoints is effective for the UNM phase in constructing a more accurate estimateof $A$ and $p$, since most of the clouds in the UNM phase lie below 500 K.However, from the value of $p$ in the CNM phase, it appears that there is asignificant difference from the Kolmogorov scaling, which can be attributed toa shock-dominated medium.

Turbulence measurements in the neutral ISM from Hi-21 cm emission-absorption spectra