PRESSURE PULSES AT
Voyager 1 (V1) crossed the heliopause into the local interstellar medium (LISM) in 2012. The LISM is a dynamic region periodically disturbed by solar transients with outward-propagating shocks, cosmic-ray intensity changes and anisotropies, and plasma wave oscillations. Voyager 2 (V2) trails V1 and...
| Main Authors: | , , , , , |
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| Other Authors: | |
| Format: | Article |
| Language: | en_US |
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IOP Publishing
2017
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| Online Access: | http://hdl.handle.net/1721.1/110180 |
| _version_ | 1826215380744404992 |
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| author | Wang, C. Liu, Y. D. Šafránková, J. Němeček, Z. Kurth, W. S. Richardson, John D. |
| author2 | MIT Kavli Institute for Astrophysics and Space Research |
| author_facet | MIT Kavli Institute for Astrophysics and Space Research Wang, C. Liu, Y. D. Šafránková, J. Němeček, Z. Kurth, W. S. Richardson, John D. |
| author_sort | Wang, C. |
| collection | MIT |
| description | Voyager 1 (V1) crossed the heliopause into the local interstellar medium (LISM) in 2012. The LISM is a dynamic region periodically disturbed by solar transients with outward-propagating shocks, cosmic-ray intensity changes and anisotropies, and plasma wave oscillations. Voyager 2 (V2) trails V1 and thus may observe the solar transients that are later observed at V1. V2 crossed the termination shock in 2007 and is now in the heliosheath. Starting in 2012, when solar maximum conditions reached V2, five possible merged interaction regions (MIRs) have been observed by V2 in the heliosheath. The timing is consistent with these MIRs driving the transients observed by V1 in the LISM. The largest heliosheath MIR was observed by V2 in late 2015 and should reach V1 in 2018. |
| first_indexed | 2024-09-23T16:26:31Z |
| format | Article |
| id | mit-1721.1/110180 |
| institution | Massachusetts Institute of Technology |
| language | en_US |
| last_indexed | 2024-09-23T16:26:31Z |
| publishDate | 2017 |
| publisher | IOP Publishing |
| record_format | dspace |
| spelling | mit-1721.1/1101802022-09-29T19:53:03Z PRESSURE PULSES AT Wang, C. Liu, Y. D. Šafránková, J. Němeček, Z. Kurth, W. S. Richardson, John D. MIT Kavli Institute for Astrophysics and Space Research Richardson, John D Voyager 1 (V1) crossed the heliopause into the local interstellar medium (LISM) in 2012. The LISM is a dynamic region periodically disturbed by solar transients with outward-propagating shocks, cosmic-ray intensity changes and anisotropies, and plasma wave oscillations. Voyager 2 (V2) trails V1 and thus may observe the solar transients that are later observed at V1. V2 crossed the termination shock in 2007 and is now in the heliosheath. Starting in 2012, when solar maximum conditions reached V2, five possible merged interaction regions (MIRs) have been observed by V2 in the heliosheath. The timing is consistent with these MIRs driving the transients observed by V1 in the LISM. The largest heliosheath MIR was observed by V2 in late 2015 and should reach V1 in 2018. Jet Propulsion Laboratory (U.S.) (contract 959203) 2017-06-22T20:30:24Z 2017-06-22T20:30:24Z 2017-01 2016-11 Article http://purl.org/eprint/type/JournalArticle 1538-4357 http://hdl.handle.net/1721.1/110180 Richardson, J. D.; Wang, C.; Liu, Y. D.; Šafránková, J.; Němeček, Z. and Kurth, W. S. “PRESSURE PULSES AT VOYAGER 2: DRIVERS OF INTERSTELLAR TRANSIENTS?” The Astrophysical Journal 834, no. 2 (January 2017): 190 © 2017 The American Astronomical Society en_US http://dx.doi.org/10.3847/1538-4357/834/2/190 Astrophysical Journal Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use. application/pdf IOP Publishing IOP Publishing |
| spellingShingle | Wang, C. Liu, Y. D. Šafránková, J. Němeček, Z. Kurth, W. S. Richardson, John D. PRESSURE PULSES AT |
| title | PRESSURE PULSES AT |
| title_full | PRESSURE PULSES AT |
| title_fullStr | PRESSURE PULSES AT |
| title_full_unstemmed | PRESSURE PULSES AT |
| title_short | PRESSURE PULSES AT |
| title_sort | pressure pulses at |
| url | http://hdl.handle.net/1721.1/110180 |
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