Solar wind stream interaction regions throughout the heliosphere by Ian G. Richardson

“…Stream interaction regions have been observed near 1 AU, in the inner heliosphere (at $$\sim 0.3$$ ∼0.3 –1 AU) by the Helios spacecraft, in the outer and distant heliosphere by the Pioneer 10 and 11 and Voyager 1 and 2 spacecraft, and out of the ecliptic by Ulysses, and these observations are reviewed. …”
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Velocity-space diffusion of solar wind protons in oblique waves and weak turbulence by E. Marsch, S. Bourouaine

“…Then the model predictions are compared with the detailed in-situ plasma measurements made by the Helios spacecraft on 14 April 1976 at 0.3 AU and found to comply favourably with resonant diffusion of protons in obliquely propagating magnetohydrodynamic waves. …”
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Solar wind low-frequency magnetohydrodynamic turbulence: extended self-similarity and scaling laws by P. Veltri, R. Bruno

“…In this paper we review some of the work done in investigating the scaling properties of Magnetohydrodynamic turbulence, by using velocity fluctuations measurements performed in the interplanetary space plasma by the Helios spacecraft. The set of scaling exponents ξ<i>_q</i> for the <I>q</I>-th order velocity structure functions, have been determined by using the Extended Self-Similarity hypothesis. …”
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Magnetohydrodynamic Perspective on the Disappearance of Mercury’s Bow Shock by Helios Data Exploration by S. H. Lai, Y.-H. Yang, W.-H. Ip

“…To examine the variability of Mercury’s bow shock in response to the solar wind properties, analyses of the observations by the Helios spacecraft at 0.30–0.50 au during 1975–1983, covering solar cycle 21, together with the theoretical solutions and MHD simulations are conducted in this study. …”
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Investigation of Alpha-Proton Drift Speeds in the Solar Wind: WIND and HELIOS Observations by Vamsee Krishna Jagarlamudi, Roberto Bruno, Rossana De Marco, Raffaella D’Amicis, Denise Perrone, Daniele Telloni, Nour E. Raouafi

“…In this paper, we present an analysis of how alpha–proton drift speeds (the difference between the magnitudes of alpha and bulk proton speeds) are constrained in the inner heliosphere using observations from the WIND and twin HELIOS spacecraft. The solar wind is separated based on its bulk proton speed into the fast wind (>600 km/s) and slow wind (<400 km/s). …”
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