THE HELIOTAIL

Pogorelov, N. V.; Heerikhuisen, J.; Borovikov, S. N.

doi:10.1088/2041-8205/812/1/L6

Title: THE HELIOTAIL

Journal Article · Sat Oct 10 00:00:00 EDT 2015 · Astrophysical Journal Letters

DOI:https://doi.org/10.1088/2041-8205/812/1/L6· OSTI ID:22518850

Pogorelov, N. V.; Heerikhuisen, J. ^[1]; Borovikov, S. N. ^[2]

Department of Space Sciences, The University of Alabama in Huntsville, AL 35805 (United States)
Center for Space Plasma and Aeronomic Research, The University of Alabama in Huntsville, AL 35805 (United States)

The heliotail is formed when the solar wind (SW) interacts with the local interstellar medium (LISM) and is shaped by the interstellar magnetic field (ISMF). While there are no spacecraft available to perform in situ measurements of the SW plasma and heliospheric magnetic field (HMF) in the heliotail, it is of importance for the interpretation of measurements of energetic neutral atom fluxes performed by Interstellar Boundary Explorer. It has been shown recently that the orientation of the heliotail in space and distortions of the unperturbed LISM caused by its presence may explain the anisotropy in the TeV cosmic ray flux detected in air shower observations. The SW flow in the heliotail is a mystery itself because it is strongly affected by charge exchange between the SW ions and interstellar neutral atoms. If the angle between the Sun’s magnetic and rotation axes is constant, the SW in the tail tends to be concentrated inside the HMF spirals deflected tailward. However, the twisted field soon becomes unstable and the reason for the SW collimation within a two-lobe structure vanishes. We demonstrate that kinetic treatment of the H atom transport becomes essential in this case for explaining the lobe absence further along the tail. We show that the heliotail flow is strongly affected by the solar cycle that eliminates artifacts, which is typical of solutions based on simplifying assumptions. The heliopause in the tail is subject to Kelvin–Helmholtz instability, while its orientation and shape are determined by the ISMF direction and strength.

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OSTI ID:: 22518850

Journal Information:: Astrophysical Journal Letters, Vol. 812, Issue 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 2041-8205

Country of Publication:: United States

Language:: English

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The Original Anisotropy of TeV Cosmic Rays in the Local Interstellar Medium Zhang, Ming; Pogorelov, N. V.; Zhang, Y. The Astrophysical Journal, Vol. 889, Issue 2 https://doi.org/10.3847/1538-4357/ab643c	journal	January 2020
Predicting the Solar Wind at the Parker Solar Probe Using an Empirically Driven MHD Model Kim, T. K.; Pogorelov, N. V.; Arge, C. N. The Astrophysical Journal Supplement Series, Vol. 246, Issue 2 https://doi.org/10.3847/1538-4365/ab58c9	journal	February 2020
Heliosheath Processes and the Structure of the Heliopause: Modeling Energetic Particles, Cosmic Rays, and Magnetic Fields Czechowski, A.; Stone, E. C.; Pogorelov, N. V. Springer https://doi.org/10.7892/boris.105629	text	January 2017
Constraining the Evolution of the Proton Distribution Function in the Heliotail Zirnstein, E. J.; Kumar, R.; Heerikhuisen, J. Institute of Physics Publishing IOP https://doi.org/10.7892/boris.124959	text	January 2018
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COSMOLOGY AND ASTRONOMY
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Title: THE HELIOTAIL

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