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dc.contributor.authorOpher, Meraven_US
dc.contributor.authorDrake, J.F.en_US
dc.contributor.authorSwisdak, M.en_US
dc.contributor.authorZieger, B.en_US
dc.contributor.authorToth, G.en_US
dc.date.accessioned2018-12-06T20:06:43Z
dc.date.available2018-12-06T20:06:43Z
dc.date.issued2017-04-10
dc.identifierhttp://arxiv.org/abs/1702.06178v1
dc.identifier.citationOpher, M., Drake, J. F., Swisdak, M., Zieger, B., & Toth, G. (2017). The Twist of the Draped Interstellar Magnetic Field Ahead of the Heliopause: A Magnetic Reconnection Driven Rotational Discontinuity. The Astrophysical Journal Letters, 839(1), L12. https://doi.org/10.3847/2041-8213/aa692f
dc.identifier.issn2041-8213
dc.identifier.urihttps://hdl.handle.net/2144/32904
dc.description.abstractBased on the difference between the orientation of the interstellar B ISM and the solar magnetic fields, there was an expectation that the magnetic field direction would rotate dramatically across the heliopause (HP). However, the Voyager 1 spacecraft measured very little rotation across the HP. Previously, we showed that the B ISM twists as it approaches the HP and acquires a strong T component (east–west). Here, we establish that reconnection in the eastern flank of the heliosphere is responsible for the twist. On the eastern flank the solar magnetic field has twisted into the positive N direction and reconnects with the southward pointing component of the B ISM. Reconnection drives a rotational discontinuity (RD) that twists the B ISM into the −T direction and propagates upstream in the interstellar medium toward the nose. The consequence is that the N component of B ISM is reduced in a finite width band upstream of the HP. Voyager 1 currently measures angles ($\delta ={\sin }^{-1}({B}_{N}/B)$) close to solar values. We present MHD simulations to support this scenario, suppressing reconnection in the nose region while allowing it in the flanks, consistent with recent ideas about reconnection suppression from diamagnetic drifts. The jump in plasma β (the plasma to magnetic pressure) across the nose of HP is much greater than in the flanks because the heliosheath β is greater there than in the flanks. Large-scale reconnection is therefore suppressed in the nose but not at the flanks. Simulation data suggest that B ISM will return to its pristine value 10–15 au past the HP.en_US
dc.publisherInstitute of Physics Publishingen_US
dc.relation.ispartofAstrophysical Journal Letters
dc.subjectISM: kinematics and dynamicsen_US
dc.subjectSun: heliosphereen_US
dc.subjectSun: magnetic fieldsen_US
dc.subjectPhysical sciencesen_US
dc.subjectAstronomy & astrophysicsen_US
dc.subjectVoyager 1en_US
dc.subjectSolar systemen_US
dc.subjectAstronomical and space sciencesen_US
dc.subjectAstronomy & astrophysicsen_US
dc.titleThe twist of the draped interstellar magnetic field ahead of the heliopause: a magnetic reconnection driven rotational discontinuityen_US
dc.typeArticleen_US
dc.description.versionAccepted manuscripten_US
dc.identifier.doi10.3847/2041-8213
pubs.elements-sourcemanual-entryen_US
pubs.notes19 pages, 5 figures, submitteden_US
pubs.notesEmbargo: No embargoen_US
pubs.organisational-groupBoston Universityen_US
pubs.organisational-groupBoston University, College of Arts & Sciencesen_US
pubs.organisational-groupBoston University, College of Arts & Sciences, Department of Astronomyen_US
pubs.publication-statusPublisheden_US


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