The Relation between Solar Spicules and Magnetohydrodynamic Shocks
Spicules are thin, elongated, jet-like features seen in observations of the solar atmosphere, at the interface between the solar photosphere and the corona. These features exhibit highly complex dynamics and are a necessary connecting link between the cooler, denser solar chromosphere and the extrem...
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/ade9b4 |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| _version_ | 1850052280894619648 |
|---|---|
| author | Sankalp Srivastava Piyali Chatterjee Sahel Dey Robertus Erdélyi |
| author_facet | Sankalp Srivastava Piyali Chatterjee Sahel Dey Robertus Erdélyi |
| author_sort | Sankalp Srivastava |
| collection | DOAJ |
| description | Spicules are thin, elongated, jet-like features seen in observations of the solar atmosphere, at the interface between the solar photosphere and the corona. These features exhibit highly complex dynamics and are a necessary connecting link between the cooler, denser solar chromosphere and the extremely hot, tenuous corona. In this work, we explore the spatial and temporal relation between solar spicules and magnetohydrodynamic (MHD) shocks using data from a 2D radiative MHD simulation of the solar atmosphere driven by solar convection. Here, we demonstrate, through direct identification, that slow MHD shocks, which propagate along magnetic field lines, are regions of strong positive vertical acceleration of the plasma that forms the tip of the spicule material during its rise phase. We quantify the effect of pressure and Lorentz forces on the acceleration of the plasma inside the shocks during the rise of spicules. The causality between spicule and shock propagation in the atmosphere of the model is also investigated. It is further shown that the strength of these shocks may play a vital role in determining the height of the spicules, supporting the idea that shocks act as drivers of some spicules. In addition, we also find the presence of structures similar to propagating coronal disturbances (PCDs) in the simulation, linked with the spicules. Here, PCDs appear to be associated with the shock waves driving the spicules that subsequently propagate into the corona and have similar speeds to those reported in observations. |
| format | Article |
| id | doaj-art-737dddd35aa04c44a2bf22b9b128d7fb |
| institution | DOAJ |
| issn | 1538-4357 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj-art-737dddd35aa04c44a2bf22b9b128d7fb2025-08-20T02:52:52ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-0198913910.3847/1538-4357/ade9b4The Relation between Solar Spicules and Magnetohydrodynamic ShocksSankalp Srivastava0https://orcid.org/0009-0000-2614-254XPiyali Chatterjee1https://orcid.org/0000-0002-0181-2495Sahel Dey2https://orcid.org/0000-0002-3369-8471Robertus Erdélyi3https://orcid.org/0000-0003-3439-4127Indian Institute of Astrophysics , 2nd Block, Koramangala, Bengaluru-560034, India; Pondicherry University , R.V. Nagar, Kalapet, Puducherry-605014, IndiaIndian Institute of Astrophysics , 2nd Block, Koramangala, Bengaluru-560034, India; Pondicherry University , R.V. Nagar, Kalapet, Puducherry-605014, IndiaSchool of Information and Physical Sciences, University of Newcastle , University Drive, Callaghan, NSW 2308, AustraliaSolar Physics and Space Plasma Research Centre (SP2RC), School of Mathematical and Physical Sciences, University of Sheffield , Hicks Building, Hounsfield Road, Sheffield, S3 7RH, UK; Department of Astronomy, Eötvös Loránd University , 1/A Pázmány Péter sétány, H-1117 Budapest, Hungary; Gyula Bay Zoltán Solar Observatory (GSO) , Hungarian Solar Physics Foundation (HSPF), Petőfi tér 3., Gyula, H-5700, HungarySpicules are thin, elongated, jet-like features seen in observations of the solar atmosphere, at the interface between the solar photosphere and the corona. These features exhibit highly complex dynamics and are a necessary connecting link between the cooler, denser solar chromosphere and the extremely hot, tenuous corona. In this work, we explore the spatial and temporal relation between solar spicules and magnetohydrodynamic (MHD) shocks using data from a 2D radiative MHD simulation of the solar atmosphere driven by solar convection. Here, we demonstrate, through direct identification, that slow MHD shocks, which propagate along magnetic field lines, are regions of strong positive vertical acceleration of the plasma that forms the tip of the spicule material during its rise phase. We quantify the effect of pressure and Lorentz forces on the acceleration of the plasma inside the shocks during the rise of spicules. The causality between spicule and shock propagation in the atmosphere of the model is also investigated. It is further shown that the strength of these shocks may play a vital role in determining the height of the spicules, supporting the idea that shocks act as drivers of some spicules. In addition, we also find the presence of structures similar to propagating coronal disturbances (PCDs) in the simulation, linked with the spicules. Here, PCDs appear to be associated with the shock waves driving the spicules that subsequently propagate into the corona and have similar speeds to those reported in observations.https://doi.org/10.3847/1538-4357/ade9b4ShocksRadiative magnetohydrodynamicsMagnetohydrodynamical simulationsSolar spiculesSolar chromosphereSolar transition region |
| spellingShingle | Sankalp Srivastava Piyali Chatterjee Sahel Dey Robertus Erdélyi The Relation between Solar Spicules and Magnetohydrodynamic Shocks The Astrophysical Journal Shocks Radiative magnetohydrodynamics Magnetohydrodynamical simulations Solar spicules Solar chromosphere Solar transition region |
| title | The Relation between Solar Spicules and Magnetohydrodynamic Shocks |
| title_full | The Relation between Solar Spicules and Magnetohydrodynamic Shocks |
| title_fullStr | The Relation between Solar Spicules and Magnetohydrodynamic Shocks |
| title_full_unstemmed | The Relation between Solar Spicules and Magnetohydrodynamic Shocks |
| title_short | The Relation between Solar Spicules and Magnetohydrodynamic Shocks |
| title_sort | relation between solar spicules and magnetohydrodynamic shocks |
| topic | Shocks Radiative magnetohydrodynamics Magnetohydrodynamical simulations Solar spicules Solar chromosphere Solar transition region |
| url | https://doi.org/10.3847/1538-4357/ade9b4 |
| work_keys_str_mv | AT sankalpsrivastava therelationbetweensolarspiculesandmagnetohydrodynamicshocks AT piyalichatterjee therelationbetweensolarspiculesandmagnetohydrodynamicshocks AT saheldey therelationbetweensolarspiculesandmagnetohydrodynamicshocks AT robertuserdelyi therelationbetweensolarspiculesandmagnetohydrodynamicshocks AT sankalpsrivastava relationbetweensolarspiculesandmagnetohydrodynamicshocks AT piyalichatterjee relationbetweensolarspiculesandmagnetohydrodynamicshocks AT saheldey relationbetweensolarspiculesandmagnetohydrodynamicshocks AT robertuserdelyi relationbetweensolarspiculesandmagnetohydrodynamicshocks |