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The IMAP Observatory Overview. [PDF]

Space Sci Rev
Hegarty KP, Kubota S, Cully M, McComas DJ, Christian ER, Schwadron NA, Gkioulidou M, Bushman S, Collura C, Dauberman M, Drabenstadt C, Driesman A, Dubill A, Duffy B, Coleman E, Eng D, Ercol CJ, Gerger A, Hall R, Hahn J, Haque M, Hefter S, Jeong D, Jones D, Kelman J, Krupiarz C, Kujawa F, Lippe C, Matlin D, Monaco C, Myers D, Rivera Sepulveda E, Rodriguez D, Roufberg L, Scherrer J, Schwinger M, Shin A, Siddique F, Smith E, Smith R, Tapley M, Vernon S, Vigil C, Weidner S.   +43 more
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Coronal mass ejections and interplanetary shocks

Journal of Geophysical Research: Space Physics, 1985
A comparison between Solwind observations of coronal mass ejections (CME's) and Helios 1 observations of interplanetary shocks during 1979–1982 indicates that 72% of the shocks were associated with large, low‐latitude mass ejections on the nearby limb.
Sheeley Jr., N., Howard, R., Koomen, M., Michels, D., Schwenn, R., Mühlhäuser, K., Rosenbauer, H.   +6 more
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Interplanetary shock collisions: Forward with reverse shocks

Astrophysics and Space Science, 1986
When one interplanetary shock overtakes another, the structure that results depends upon the nature of the interacting shocks. We examine, numerically, the results of collisions of forward with reverse shocks, in two dimensions, and show that the results depend primarily upon shock strength.
Z. K. Smith, M. Dryer, S. M. Han
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Waves upstream of interplanetary shocks

2023
Interplanetary (IP) shocks can be driven in the solar wind by fast coronal mass ejections and by the interaction of fast solar wind with slow streams of plasma. These shocks can be preceded by extended waves and suprathermal ion foreshocks. Shocks characteristics as well as the level of wave activity near them change as they propagate through the ...
Xochitl Blanco-Cano, Domenico Trotta, Heli Hietala, Primoz Kajdic, Diana Rojas-Castillo, Andrew Dimmock, Tim Horbury, Rami Vainio, Lan Jian   +8 more
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Hydromagnetic interplanetary shock waves

Planetary and Space Science, 1968
Adiabatic motion of hydromagnetic fluid behind spherical fast shock wave for Parker solar wind ...
T.S. Lee, T. Chen
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Origin of strong interplanetary shocks

Nature, 1985
Observations of 900 radio sources have been used to study the shape and motion of large-scale interplanetary transients associated with shock disturbances at 1 AU. The variations of plasma density and speed and the zones in the solar atmosphere from which the transients originate suggest an origin related to intermittent flows of enhanced speed from ...
A. Hewish, S. J. Tappin, G. R. Gapper
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STEREO interplanetary shocks and foreshocks

AIP Conference Proceedings, 2013
We use STEREO data to study shocks driven by stream interactions and the waves associated with them. During the years of the extended solar minimum 2007-2010, stream interaction shocks have Mach numbers between 1.1-3.8 and θBn ∼20-86°. We find a variety of waves, including whistlers and low frequency fluctuations.
X. Blanco-Cano, P. Kajdič, E. Aguilar-Rodríguez, C. T. Russell, L. K. Jian, J. G. Luhmann   +5 more
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Observations of interplanetary shocks: Recent progress

Space Science Reviews, 1983
Interplanetary shock observations since the prior Solar Terrestrial Physics Symposium in 1978 are reviewed. Since the interval coincides with the recent solar maximum, emphasis is placed on shocks associated with transient solar phenomena, including coronal transients and eruptive prominences as well as flares.
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Voyager Observations of Interplanetary Shocks

AIP Conference Proceedings, 2005
Data from Voyager 2 are used to compile a shock catalogue covering the 27 years of Voyager 2 solar wind data through the end of 2004. This catalogue is used to investigate the characteristics of shocks as a function of distance out to 75 AU. The shock occurrence frequency decreases with distance.
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The evolution of interplanetary shocks

Journal of Geophysical Research: Space Physics, 1985
Unambiguous identification of the solar events associated with 48 interplanetary (IP) shocks has been facilitated by the observation of radio emission generated by the shocks. This identification makes possible an investigation of the way in which these shocks evolve and of the relationship between solar event “strength” and shock velocity. All but two
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