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Impulsive origin of solar spicule-like jets

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Abstract

Using the observations of the coronal hole in Si IV 1393.755 Å line as recorded by interface region imaging spectrograph (IRIS) on 8th October 2013, Chen et al. (Astrophys. J. 873(1):79, 2019) have reported non-Gaussian line profiles showing unusual line broadening that may correspond to the velocity enhancement in the emitting plasma. This observational scenario may be caused by the localized impulsive energy release associated with the footpoint of spicule-like cool jet. We revisit the observations of Chen et al. (Astrophys. J. 873(1):79, 2019) to analyse a specific event showing non-Gaussian profiles in the Si IV 1393.755 Å line, for a lifetime of 3.0 min and Doppler shifts reaching 68 km s\(^{-1}\), which is associated with a spicule-like jet of length 8.0 Mm. We model this jet by implementing an observed velocity enhancement in a magnetized, gravitationally stratified, two-dimensional (2-D) model solar atmosphere. The model atmosphere consists of open magnetic fields and realistic temperature profile. The velocity perturbation of \(\approx\) 68 km s\(^{-1}\), resembling the observed velocity enhancement, launches a thin spicule-like jet whose properties closely match with the observed jet. We also show that non-adiabatic conditions (e.g., thermal conduction and radiative cooling) affect the jet propagation, mass flux, and kinetic energy density. We demonstrate that such spicule-like jets may transport mass and energy into the overlying solar atmosphere. The synthetic images derived from the use of simulation data (e.g., density, temperature) and atomic parameters of Si IV 1393.755 Å from CHIANTI database show that model jet consists of bright plasma as detected in the emissions at transition region temperature. It also consists of a cool core material that indicates its origin in the solar chromosphere. This cool chromospheric material appears as a dark plasma thread seen in the synthetic images that is eventually not evident in the Si IV emissions. IRIS Si IV emissions capture the heated counterpart of the observed jet, which is also evident in the synthetic images as a bright feature. Complementing the recent observations revealing the impulsive origin of the spicule-like jets, our present model emphasizes comprehensively their evolution in both adiabatic and non-adiabatic conditions of the solar atmosphere. The model implicitly displays the presence of the hot and cool components of jet’s plasma. It also demonstrates that the cooling atmosphere affects the kinematics and energetics of the jets.

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Data availability statement

The datasets generated during and/or analysed during the current study are available from the corresponding author on reasonable request.

Notes

  1. https://www.chiantidatabase.org/tech_reports/03_synthetic_spectra/chianti_report_03.pdf.

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Acknowledgements

Authors gratefully acknowledge the reviewer for his/her valuable remarks that improved manuscript considerably. IRIS is a NASA small explorer mission developed and operated by LMSAL with mission operations executed at NASA Ames Research center and major contributions to downlink communications funded by ESA and the Norwegian Space Centre. The IRIS data are publicly available from the Lockheed Martin Solar and Astrophysics Laboratory (LMSAL) website (http://iris.lmsal.com/). The open source SolarSoft code package (http://www.lmsal.com/solarsoft/) is used for the initial data processing. Authors acknowledge the use of PLUTO code in our present work and use of PYTHON libraries for numerical data analysis. BS gratefully acknowledge the Human Resource Development Group (HRDG), Council of Scientific & Industrial research (CSIR) India for providing him a senior research scholar grant. S.K.T. gratefully acknowledges support by NASA contracts NNG09FA40C (IRIS), and NNM07AA01C (Hinode). AKS and MM acknowledge the support of UKIERI Grant for the support of their research. AKS also acknowledge his ISRO Grant (Ref-DS 2B-13-12(2)/26/2022-Scc2) for the support of his research works. AKS thank Piotr Konkol and Dr. González-Avilés for the helpful academic discussions. AKS and DY also acknowledge the ISSI-BJ regarding the science team project on “Oscillatory Processes in Solar and Stellar Coronae”. KM’s work was supported as part of project funded by National Science Centre (NCN) Grant Nos. 2017/25/B/ST9/00506 and 2020/37/B/ST9/00184.

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Authors and Affiliations

  1. Department of Physics, Indian Institute of Technology (BHU), Varanasi, UP, 221005, India

    A. K. Srivastava, Balveer Singh & K. Sharma

  2. Institute of Physics, University of Maria Curie-Sklodowska, Pl. M. Curie-Sklodowskiej 5, 20-031, Lublin, Poland

    K. Murawski

  3. School of Earth and Space Sciences, Peking University, Beijing, 100871, China

    Y. Chen

  4. Max-Planck Institute for Solar System Research, Justus-von-Liebig-Weg 3, 37077, Götingen, Germany

    Y. Chen

  5. Institute of Space Science and Applied Technology, Harbin Institute of Technology, Shenzhen, 518055, Guangdong, China

    D. Yuan

  6. Lockheed Martin Solar and Astrophysics Laboratory, 3251 Hanover Street, Building 252, Palo Alto, CA, 94304, USA

    S. K. Tiwari

  7. Bay Area Environmental Research Institute, NASA Research Park, Moffett Field, CA, 94035, USA

    S. K. Tiwari

  8. Astrophysics Research Centre, Queen’s University, Belfast, BT7 1NN, UK

    M. Mathioudakis

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Srivastava, A.K., Singh, B., Murawski, K. et al. Impulsive origin of solar spicule-like jets. Eur. Phys. J. Plus 138, 209 (2023). https://doi.org/10.1140/epjp/s13360-023-03833-5

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