Three-dimensional features of the outer heliosphere due to coupling between the interstellar and interplanetary magnetic fields. IV. Solar cycle model based on Ulysses observations

Pogorelov, N. V.; Suess, S. T.; Borovikov, S. N.; Ebert, R. W.; McComas, D. J.; Zank, G. P.

doi:10.1088/0004-637X/772/1/2

Title: Three-dimensional features of the outer heliosphere due to coupling between the interstellar and interplanetary magnetic fields. IV. Solar cycle model based on Ulysses observations

Journal Article · Wed Jun 26 00:00:00 EDT 2013 · The Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/772/1/2· OSTI ID:1325985

Pogorelov, N. V. ^[1]; Suess, S. T. ^[2]; Borovikov, S. N. ^[3]; Ebert, R. W. ^[4]; McComas, D. J. ^[5]; Zank, G. P. ^[1]

Univ. of Alabama, Huntsville, AL (United States). Dept. of Physics and Center for Space Plasma and Aeronomic Research
National Space Science and Technology Center, Huntsville, AL (United States)
Univ. of Alabama, Huntsville, AL (United States). Center for Space Plasma and Aeronomic Research
Southwest Research Inst. (SwRI), San Antonio, TX (United States)
Southwest Research Inst. (SwRI), San Antonio, TX (United States); Univ. of Texas in San Antonio, TX (United States)

The solar cycle has a profound influence on the solar wind (SW) interaction with the local interstellar medium (LISM) on more than one timescales. Also, there are substantial differences in individual solar cycle lengths and SW behavior within them. The presence of a slow SW belt, with a variable latitudinal extent changing within each solar cycle from rather small angles to 90°, separated from the fast wind that originates at coronal holes substantially affects plasma in the inner heliosheath (IHS)—the SW region between the termination shock (TS) and the heliopause (HP). The solar cycle may be the reason why the complicated flow structure is observed in the IHS by Voyager 1. Here, we show that a substantial decrease in the SW ram pressure observed by Ulysses between the TS crossings by Voyager 1 and 2 contributes significantly to the difference in the heliocentric distances at which these crossings occurred. The Ulysses spacecraft is the source of valuable information about the three-dimensional and time-dependent properties of the SW. Its unique fast latitudinal scans of the SW regions make it possible to create a solar cycle model based on the spacecraft in situ measurements. On the basis of our analysis of the Ulysses data over the entire life of the mission, we generated time-dependent boundary conditions at 10 AU from the Sun and applied our MHD-neutral model to perform a numerical simulation of the SW-LISM interaction. We analyzed the global variations in the interaction pattern, the excursions of the TS and the HP, and the details of the plasma and magnetic field distributions in the IHS. The resulting numbers are compared with Voyager data as functions of time in the spacecraft frame. We also discuss solar cycle effects which may be reasons for the recent decrease in the TS particles (ions accelerated to anomalous cosmic-ray energies) flux observed by Voyager 1.

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Research Organization:: Univ. of Alabama, Huntsville, AL (United States)

Sponsoring Organization:: USDOE Office of Science (SC), Fusion Energy Sciences (FES); National Science Foundation (NSF)

Grant/Contract Number:: SC0008334

OSTI ID:: 1325985

Journal Information:: The Astrophysical Journal, Vol. 772, Issue 1; ISSN 0004-637X

Publisher:: Institute of Physics (IOP)Copyright Statement

Country of Publication:: United States

Language:: English

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Globally Distributed Energetic Neutral Atom Maps for the “Croissant” Heliosphere Kornbleuth, M.; Opher, M.; Michael, A. T. The Astrophysical Journal, Vol. 865, Issue 2 https://doi.org/10.3847/1538-4357/aadbac	journal	September 2018
Magnetic Turbulence Spectra and Intermittency in the Heliosheath and in the Local Interstellar Medium Fraternale, Federico; Pogorelov, Nikolai V.; Richardson, John D. The Astrophysical Journal, Vol. 872, Issue 1 https://doi.org/10.3847/1538-4357/aafd30	journal	February 2019
The Effect of Suprathermal Protons in the Heliosheath on the Global Structure of the Heliosphere and Heliotail Heerikhuisen, Jacob; Zirnstein, Eric J.; Pogorelov, Nikolai V. The Astrophysical Journal, Vol. 874, Issue 1 https://doi.org/10.3847/1538-4357/ab05e3	journal	March 2019
A Magnetic Pressure Front Upstream of the Heliopause and the Heliosheath Magnetic Fields and Plasma, Observed during 2017 Burlaga, L. F.; Ness, N. F.; Berdichevsky, D. B. The Astrophysical Journal, Vol. 877, Issue 1 https://doi.org/10.3847/1538-4357/ab16f1	journal	May 2019
All-sky Measurement of the Anisotropy of Cosmic Rays at 10 TeV and Mapping of the Local Interstellar Magnetic Field Abeysekara, A. U.; Alfaro, R.; Alvarez, C. The Astrophysical Journal, Vol. 871, Issue 1 https://doi.org/10.3847/1538-4357/aaf5cc	journal	January 2019
All-Sky Measurement of the Anisotropy of Cosmic Rays at 10 TeV and Mapping of the Local Interstellar Magnetic Field Abeysekara, A. U.; Alfaro, R.; Alvarez, C. Deutsches Elektronen-Synchrotron, DESY, Hamburg https://doi.org/10.3204/pubdb-2020-00512	text	January 2019
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
Extended MHD modeling of the steady solar corona and the solar wind Gombosi, Tamas I.; van der Holst, Bart; Manchester, Ward B. arXiv https://doi.org/10.48550/arxiv.1807.00417	text	January 2018

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