A Three-dimensional Map of the Heliosphere from IBEX

Reisenfeld, Daniel Brett; Bzowski, Maciej; Funsten, III, Herbert O.; Heerikhuisen, Jacob; Janzen, Paul H.; Kubiak, Marzena A.; McComas, David J.; Schwadron, Nathan A.; Sokół, Justyna M.; Zimorino, Alex; Zirnstein, Eric J.

doi:10.3847/1538-4365/abf658

A Three-dimensional Map of the Heliosphere from IBEX

Journal Article · Thu Jun 10 00:00:00 EDT 2021 · The Astrophysical Journal. Supplement Series

DOI:https://doi.org/10.3847/1538-4365/abf658· OSTI ID:1890983

^[1]; ^[2]; ^[1]; ^[3]; Janzen, Paul H. ^[4]; ^[2]; ^[5]; ^[6]; ^[7]; Zimorino, Alex ^[4]; ^[5]

Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
Polish Academy of Sciences (PAS), Warsaw (Poland)
Univ. of Waikato, Hamilton (New Zealand)
Univ. of Montana, Missoula, MT (United States)
Princeton Univ., NJ (United States)
Univ. of New Hampshire, Durham, NH (United States)
Southwest Research Institute, San Antonio, TX (United States)

The Interstellar Boundary Explorer (IBEX) mission has shown that variations in the energetic neutral atom (ENA) flux from the outer heliosphere are associated with the solar cycle and longer-term variations in the solar wind (SW). In particular, there is a good correlation between the dynamic pressure of the outbound SW and variations in the later-observed IBEX ENA flux. The time difference between observations of the outbound SW and the heliospheric ENAs with which they correlate ranges from approximately 2 to 6 yr or more, depending on ENA energy and look direction. This time difference can be used as a means of "sounding" the heliosheath, that is, finding the average distance to the ENA source region in a particular direction. Here, we apply this method to build a 3D map of the heliosphere. We use IBEX ENA data collected over a complete solar cycle, from 2009 through 2019, corrected for survival probability to the inner heliosphere. Here we divide the data into 56 "macropixels" covering the entire sky. As each point in the sky is sampled once every 6 months, this gives us a time series of 22 points macropixel^–1 on which to time-correlate. Consistent with prior studies and heliospheric models, we find that the shortest distance to the heliopause, d_HP, is slightly south of the nose direction (d_HP ~ 110–120 au), with a flaring toward the flanks and poles (d_HP ~ 160–180 au). The heliosphere extends at least ~350 au tailward, which is the distance limit of the technique.

View Accepted Manuscript (DOE)

Research Organization:: Los Alamos National Laboratory (LANL), Los Alamos, NM (United States)

Sponsoring Organization:: USDOE Laboratory Directed Research and Development (LDRD) Program; Polish National Science Centre (NCN)

Grant/Contract Number:: 89233218CNA000001

OSTI ID:: 1890983

Alternate ID(s):: OSTI ID: 23163563

Report Number(s):: LA-UR-21-23228

Journal Information:: The Astrophysical Journal. Supplement Series, Journal Name: The Astrophysical Journal. Supplement Series Journal Issue: 2 Vol. 254; ISSN 0067-0049

Publisher:: IOP PublishingCopyright Statement

Country of Publication:: United States

Language:: English

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