Solar Orbiter and SDO Observations, and a Bifrost Magnetohydrodynamic Simulation of Small-scale Coronal Jets
We report high-resolution, high-cadence observations of five small-scale coronal jets in an on-disk quiet Sun region observed with Solar Orbiter’s EUI/HRI _EUV in 174 Å. We combine the HRI _EUV images with the EUV images of SDO/AIA and investigate the magnetic setting of the jets using coaligned lin...
| Main Authors: | , , , , , |
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| Format: | Article |
| Language: | English |
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IOP Publishing
2023-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/aca1c1 |
| _version_ | 1797695818923245568 |
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| author | Navdeep K. Panesar Viggo H. Hansteen Sanjiv K. Tiwari Mark C. M. Cheung David Berghmans Daniel Müller |
| author_facet | Navdeep K. Panesar Viggo H. Hansteen Sanjiv K. Tiwari Mark C. M. Cheung David Berghmans Daniel Müller |
| author_sort | Navdeep K. Panesar |
| collection | DOAJ |
| description | We report high-resolution, high-cadence observations of five small-scale coronal jets in an on-disk quiet Sun region observed with Solar Orbiter’s EUI/HRI _EUV in 174 Å. We combine the HRI _EUV images with the EUV images of SDO/AIA and investigate the magnetic setting of the jets using coaligned line-of-sight magnetograms from SDO/HMI. The HRI _EUV jets are miniature versions of typical coronal jets as they show narrow collimated spires with a base brightening. Three out of five jets result from a detectable minifilament eruption following flux cancelation at the neutral line under the minifilament, analogous to coronal jets. To better understand the physics of jets, we also analyze five small-scale jets from a high-resolution Bifrost MHD simulation in synthetic Fe ix /Fe x emissions. The jets in the simulation reside above neutral lines and four out of five jets are triggered by magnetic flux cancelation. The temperature maps show evidence of cool gas in the same four jets. Our simulation also shows the signatures of opposite Doppler shifts (of the order of ±10 s of km s ^−1 ) in the jet spire, which is evidence of untwisting motion of the magnetic field in the jet spire. The average jet duration, spire length, base width, and speed in our observations (and in synthetic Fe ix /Fe x images) are 6.5 ± 4.0 min (9.0 ± 4.0 minutes), 6050 ± 2900 km (6500 ± 6500 km), 2200 ± 850 km, (3900 ± 2100 km), and 60 ± 8 km s ^−1 (42 ± 20 km s ^−1 ), respectively. Our observation and simulation results provide a unified picture of small-scale solar coronal jets driven by magnetic reconnection accompanying flux cancelation. This picture also aligns well with the most recent reports of the formation and eruption mechanisms of larger coronal jets. |
| first_indexed | 2024-03-12T03:17:52Z |
| format | Article |
| id | doaj.art-1b21b6ed9eb642d1b7e455e54b6687a4 |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-12T03:17:52Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-1b21b6ed9eb642d1b7e455e54b6687a42023-09-03T14:08:22ZengIOP PublishingThe Astrophysical Journal1538-43572023-01-0194312410.3847/1538-4357/aca1c1Solar Orbiter and SDO Observations, and a Bifrost Magnetohydrodynamic Simulation of Small-scale Coronal JetsNavdeep K. Panesar0https://orcid.org/0000-0001-7620-362XViggo H. Hansteen1https://orcid.org/0000-0003-0975-6659Sanjiv K. Tiwari2https://orcid.org/0000-0001-7817-2978Mark C. M. Cheung3https://orcid.org/0000-0003-2110-9753David Berghmans4https://orcid.org/0000-0003-4052-9462Daniel Müller5https://orcid.org/0000-0001-9027-9954Lockheed Martin Solar and Astrophysics Laboratory , 3251 Hanover Street, Bldg. 252, Palo Alto, CA 94304, USA ; panesar@lmsal.com; Bay Area Environmental Research Institute , NASA Research Park, Moffett Field, CA 94035, USALockheed Martin Solar and Astrophysics Laboratory , 3251 Hanover Street, Bldg. 252, Palo Alto, CA 94304, USA ; panesar@lmsal.com; Bay Area Environmental Research Institute , NASA Research Park, Moffett Field, CA 94035, USA; Rosseland Centre for Solar Physics, University of Oslo , P.O. Box 1029 Blindern, NO-0315 Oslo, Norway; Institute of Theoretical Astrophysics, University of Oslo , P.O. Box 1029 Blindern, NO-0315 Oslo, NorwayLockheed Martin Solar and Astrophysics Laboratory , 3251 Hanover Street, Bldg. 252, Palo Alto, CA 94304, USA ; panesar@lmsal.com; Bay Area Environmental Research Institute , NASA Research Park, Moffett Field, CA 94035, USALockheed Martin Solar and Astrophysics Laboratory , 3251 Hanover Street, Bldg. 252, Palo Alto, CA 94304, USA ; panesar@lmsal.comSolar-Terrestrial Centre of Excellence—SIDC , Royal Observatory of Belgium, Ringlaan -3- Av. Circulaire, B-1180 Brussels, BelgiumEuropean Space Agency , ESTEC, P.O. Box 299, 2200 AG Noordwijk, The NetherlandsWe report high-resolution, high-cadence observations of five small-scale coronal jets in an on-disk quiet Sun region observed with Solar Orbiter’s EUI/HRI _EUV in 174 Å. We combine the HRI _EUV images with the EUV images of SDO/AIA and investigate the magnetic setting of the jets using coaligned line-of-sight magnetograms from SDO/HMI. The HRI _EUV jets are miniature versions of typical coronal jets as they show narrow collimated spires with a base brightening. Three out of five jets result from a detectable minifilament eruption following flux cancelation at the neutral line under the minifilament, analogous to coronal jets. To better understand the physics of jets, we also analyze five small-scale jets from a high-resolution Bifrost MHD simulation in synthetic Fe ix /Fe x emissions. The jets in the simulation reside above neutral lines and four out of five jets are triggered by magnetic flux cancelation. The temperature maps show evidence of cool gas in the same four jets. Our simulation also shows the signatures of opposite Doppler shifts (of the order of ±10 s of km s ^−1 ) in the jet spire, which is evidence of untwisting motion of the magnetic field in the jet spire. The average jet duration, spire length, base width, and speed in our observations (and in synthetic Fe ix /Fe x images) are 6.5 ± 4.0 min (9.0 ± 4.0 minutes), 6050 ± 2900 km (6500 ± 6500 km), 2200 ± 850 km, (3900 ± 2100 km), and 60 ± 8 km s ^−1 (42 ± 20 km s ^−1 ), respectively. Our observation and simulation results provide a unified picture of small-scale solar coronal jets driven by magnetic reconnection accompanying flux cancelation. This picture also aligns well with the most recent reports of the formation and eruption mechanisms of larger coronal jets.https://doi.org/10.3847/1538-4357/aca1c1Solar magnetic fieldsSolar magnetic reconnectionJetsSolar coronaSolar chromosphere |
| spellingShingle | Navdeep K. Panesar Viggo H. Hansteen Sanjiv K. Tiwari Mark C. M. Cheung David Berghmans Daniel Müller Solar Orbiter and SDO Observations, and a Bifrost Magnetohydrodynamic Simulation of Small-scale Coronal Jets The Astrophysical Journal Solar magnetic fields Solar magnetic reconnection Jets Solar corona Solar chromosphere |
| title | Solar Orbiter and SDO Observations, and a Bifrost Magnetohydrodynamic Simulation of Small-scale Coronal Jets |
| title_full | Solar Orbiter and SDO Observations, and a Bifrost Magnetohydrodynamic Simulation of Small-scale Coronal Jets |
| title_fullStr | Solar Orbiter and SDO Observations, and a Bifrost Magnetohydrodynamic Simulation of Small-scale Coronal Jets |
| title_full_unstemmed | Solar Orbiter and SDO Observations, and a Bifrost Magnetohydrodynamic Simulation of Small-scale Coronal Jets |
| title_short | Solar Orbiter and SDO Observations, and a Bifrost Magnetohydrodynamic Simulation of Small-scale Coronal Jets |
| title_sort | solar orbiter and sdo observations and a bifrost magnetohydrodynamic simulation of small scale coronal jets |
| topic | Solar magnetic fields Solar magnetic reconnection Jets Solar corona Solar chromosphere |
| url | https://doi.org/10.3847/1538-4357/aca1c1 |
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