A Magnetic Pressure Front Upstream of the Heliopause and the Heliosheath Magnetic Fields and Plasma, Observed during 2017

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dc.contributor.authorBurlaga, L. F.
dc.contributor.authorNess, N. F.
dc.contributor.authorBerdichevsky, D. B.
dc.contributor.authorJian, L. K.
dc.contributor.authorPark, J.
dc.contributor.authorMostafavi, P.
dc.contributor.authorRichardson, J. D.
dc.date.accessioned2019-10-10T14:10:09Z
dc.date.available2019-10-10T14:10:09Z
dc.date.issued2019-05-21
dc.description.abstractVoyager 1 (V1), moving in the interstellar magnetic field, observed an increase in the daily averages of B beginning on day ≈346, 2016, rising to a local maximum on day ≈382, and declining nearly monotonically for the most part until day 720, measured from 2016.0. A pressure front was observed during a ≈35-day interval beginning on day 346, 2016. The pressure front observed by V1 was not a shock, although one might expect it to evolve into a shock. Voyager 2 (V2) observed the distant heliosheath during 2017. The average B in the heliosheath was relatively high, 0.130 nT. The distribution of azimuthal angles had two nearly equal maxima at approximately 90° and 180°. An unusual transition of the BT component from a large “away” sector to a large “toward” sector occurred during 2017 from day 101 to day 239. Abrupt but small changes in magnetic polarity occurred between day 146 and day 239, when the average BT component of B was close to zero. Changes in the >70 MeV nucleon−1 cosmic-ray intensity were qualitatively related to the B(t) profile described by the CR-B relationship. There was no net decrease in magnetic flux at V2 in the heliosheath during 2017 that might be attributed to ongoing magnetic reconnection in the heliosheath. Small-scale increments in B can be described by a q-Gaussian distribution with q = 1.64 ± 0.02 for hourly averages of B and q = 1.54 ± 0.08 for daily averages of B.en_US
dc.description.sponsorshipJ.P. was supported by an appointment to the NASA Postdoctoral Program at the NASA Goddard Space Flight Center, administered by Universities Space Research Association under contract with NASA. D.B. and N.F.N. were supported by the NASA Voyager Project under a cooperative agreement to the University of Maryland, Baltimore County. L. F.B. was supported by NASA contract 80GSFC19C0012. P.M. was supported by the NASA Earth and Space Science Fellowship Program-grant 16-HELIO16F-0022, and J.R. was supported by NASA under grant 959203 from the Jet Propulsion Laboratory to the Massachusetts Institute of Technologyen_US
dc.description.urihttps://iopscience.iop.org/article/10.3847/1538-4357/ab16f1en_US
dc.format.extent9 pagesen_US
dc.genrejournal articlesen_US
dc.identifierdoi:10.13016/m2gbth-gcma
dc.identifier.citationL. F. Burlaga, et.al, A Magnetic Pressure Front Upstream of the Heliopause and the Heliosheath Magnetic Fields and Plasma, Observed during 2017, The Astrophysical Journal, Volume 877, Number 1, https://doi.org/10.3847/1538-4357/ab16f1en_US
dc.identifier.urihttps://doi.org/10.3847/1538-4357/ab16f1
dc.identifier.urihttp://hdl.handle.net/11603/15019
dc.language.isoen_USen_US
dc.publisherIOP Publishingen_US
dc.relation.isAvailableAtThe University of Maryland, Baltimore County (UMBC)
dc.relation.ispartofUMBC Goddard Planetary Heliophysics Institute (GPHI)
dc.relation.ispartofUMBC Faculty Collection
dc.rightsThis item is likely protected under Title 17 of the U.S. Copyright Law. Unless on a Creative Commons license, for uses protected by Copyright Law, contact the copyright holder or the author.
dc.rights© 2019 The American Astrophysical Journal
dc.subjectISM: magnetic fieldsen_US
dc.subjectSun: heliosphereen_US
dc.subjectSun: magnetic fieldsen_US
dc.titleA Magnetic Pressure Front Upstream of the Heliopause and the Heliosheath Magnetic Fields and Plasma, Observed during 2017en_US
dc.typeTexten_US

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