Data-constrained Magnetohydrodynamic Simulation for Magnetic Flux Rope Eruptions Driven by Magnetic Reconnection
We conducted data-constrained magnetohydrodynamic (MHD) simulations for solar active region (AR) NOAA AR 11429, which produced two X-class flares within a span of 63 minutes. The simulations were performed using the zero- β MHD approximation, with the initial condition derived from the nonlinear for...
Saved in:
| Main Authors: | , , , |
|---|---|
| Format: | Article |
| Language: | English |
| Published: |
IOP Publishing
2025-01-01
|
| Series: | The Astrophysical Journal |
| Subjects: | |
| Online Access: | https://doi.org/10.3847/1538-4357/adba56 |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| _version_ | 1849767128148738048 |
|---|---|
| author | Nian Liu Satoshi Inoue Ying Wang Haimin Wang |
| author_facet | Nian Liu Satoshi Inoue Ying Wang Haimin Wang |
| author_sort | Nian Liu |
| collection | DOAJ |
| description | We conducted data-constrained magnetohydrodynamic (MHD) simulations for solar active region (AR) NOAA AR 11429, which produced two X-class flares within a span of 63 minutes. The simulations were performed using the zero- β MHD approximation, with the initial condition derived from the nonlinear force-free field extrapolated from the photospheric magnetograms taken 2 hr before the first X5.4 flare. During the simulation, we enhanced magnetic reconnection locally by applying anomalous resistivity in the induction equation within the regions of interest. As a result, the simulations successfully reproduced the expansion of two magnetic flux ropes (MFRs) corresponding to the two observed eruptions. The result shows that the difference in stability between the two MFRs is related to the location of the magnetic reconnection that triggers the solar eruptions. Furthermore, comparison with the analysis of failed MFR eruptions indicates that both the initiation reconnection and the subsequent driving mechanism, torus instability, are equally important for a successful eruption. This simulation reveals a new mechanism in which long loops, formed via tether-cutting reconnection, push up the overlying twisted field lines, leading to their destabilization by torus instability. |
| format | Article |
| id | doaj-art-3802ea4bbdfe46c29a58d1de9da7c3d4 |
| institution | DOAJ |
| issn | 1538-4357 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj-art-3802ea4bbdfe46c29a58d1de9da7c3d42025-08-20T03:04:21ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-0198313810.3847/1538-4357/adba56Data-constrained Magnetohydrodynamic Simulation for Magnetic Flux Rope Eruptions Driven by Magnetic ReconnectionNian Liu0https://orcid.org/0000-0002-6018-3799Satoshi Inoue1https://orcid.org/0000-0001-5121-5122Ying Wang2https://orcid.org/0009-0008-7623-0140Haimin Wang3https://orcid.org/0000-0002-5233-565XInstitute for Space Weather Sciences , New Jersey Institute of Technology, Newark, NJ 07102-1982, USA ; nian.liu@njit.eduInstitute for Space Weather Sciences , New Jersey Institute of Technology, Newark, NJ 07102-1982, USA ; nian.liu@njit.eduInstitute for Space Weather Sciences , New Jersey Institute of Technology, Newark, NJ 07102-1982, USA ; nian.liu@njit.eduInstitute for Space Weather Sciences , New Jersey Institute of Technology, Newark, NJ 07102-1982, USA ; nian.liu@njit.edu; Big Bear Solar Observatory , New Jersey Institute of Technology, 40386 North Shore Lane, Big Bear City, CA 92314-9672, USAWe conducted data-constrained magnetohydrodynamic (MHD) simulations for solar active region (AR) NOAA AR 11429, which produced two X-class flares within a span of 63 minutes. The simulations were performed using the zero- β MHD approximation, with the initial condition derived from the nonlinear force-free field extrapolated from the photospheric magnetograms taken 2 hr before the first X5.4 flare. During the simulation, we enhanced magnetic reconnection locally by applying anomalous resistivity in the induction equation within the regions of interest. As a result, the simulations successfully reproduced the expansion of two magnetic flux ropes (MFRs) corresponding to the two observed eruptions. The result shows that the difference in stability between the two MFRs is related to the location of the magnetic reconnection that triggers the solar eruptions. Furthermore, comparison with the analysis of failed MFR eruptions indicates that both the initiation reconnection and the subsequent driving mechanism, torus instability, are equally important for a successful eruption. This simulation reveals a new mechanism in which long loops, formed via tether-cutting reconnection, push up the overlying twisted field lines, leading to their destabilization by torus instability.https://doi.org/10.3847/1538-4357/adba56Solar flaresMagnetohydrodynamicsSolar active region magnetic fieldsMagnetohydrodynamical simulations |
| spellingShingle | Nian Liu Satoshi Inoue Ying Wang Haimin Wang Data-constrained Magnetohydrodynamic Simulation for Magnetic Flux Rope Eruptions Driven by Magnetic Reconnection The Astrophysical Journal Solar flares Magnetohydrodynamics Solar active region magnetic fields Magnetohydrodynamical simulations |
| title | Data-constrained Magnetohydrodynamic Simulation for Magnetic Flux Rope Eruptions Driven by Magnetic Reconnection |
| title_full | Data-constrained Magnetohydrodynamic Simulation for Magnetic Flux Rope Eruptions Driven by Magnetic Reconnection |
| title_fullStr | Data-constrained Magnetohydrodynamic Simulation for Magnetic Flux Rope Eruptions Driven by Magnetic Reconnection |
| title_full_unstemmed | Data-constrained Magnetohydrodynamic Simulation for Magnetic Flux Rope Eruptions Driven by Magnetic Reconnection |
| title_short | Data-constrained Magnetohydrodynamic Simulation for Magnetic Flux Rope Eruptions Driven by Magnetic Reconnection |
| title_sort | data constrained magnetohydrodynamic simulation for magnetic flux rope eruptions driven by magnetic reconnection |
| topic | Solar flares Magnetohydrodynamics Solar active region magnetic fields Magnetohydrodynamical simulations |
| url | https://doi.org/10.3847/1538-4357/adba56 |
| work_keys_str_mv | AT nianliu dataconstrainedmagnetohydrodynamicsimulationformagneticfluxropeeruptionsdrivenbymagneticreconnection AT satoshiinoue dataconstrainedmagnetohydrodynamicsimulationformagneticfluxropeeruptionsdrivenbymagneticreconnection AT yingwang dataconstrainedmagnetohydrodynamicsimulationformagneticfluxropeeruptionsdrivenbymagneticreconnection AT haiminwang dataconstrainedmagnetohydrodynamicsimulationformagneticfluxropeeruptionsdrivenbymagneticreconnection |