Spectroscopic observations of periodic bursty ejections during a dome-spire-shaped jet
Abstract
Context: The study investigates the complexity of the formation and evolution of a dome-spire-shaped jet (or anemone jet) that originated in an active region and was presumably driven by null-point magnetic reconnection. Aims: We aim to provide a quantitative estimation of multi-temperature plasma dynamics and physical parameters of the jet and its blob-like features, together with its temporal evolution in three-dimensional perspective. Methods: For this, we analyze unique sit-and-stare spectral (Si IV, Mg II k, and C II) and slit-jaw imaging 1400 Å and 2796 Å observations obtained with the Interface Region Imaging Spectrograph (IRIS), with a slit uniquely positioned just above the assumed reconnection site. Co-observations taken with the Fast Imaging Solar Spectrograph of the Goode Solar Telescope in the chromospheric Hα and Ca II 8542.10 Å lines were also analyzed. These data are complemented by EUV imaging information from the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory. Results: The IRIS observations reveal that the jet is formed by multiple periodic (∼30 s) plasma ejections with blob-like appearance, each associated with strongly blueshifted Si IV 1402.77 Å transition-region emission reaching about −300 km/s. More importantly, the ejections are grouped into well-defined packets, each lasting approximately 3--5 min. In contrast, only a single Doppler component is observed in the chromospheric Ca II line. Multi-Gaussian decomposition of the Si IV line profiles reveals a highly accelerated plasma, with line-of-sight speed toward the observer increasing linearly from ∼30 to 112 km/s over 66 s, corresponding to an acceleration of 1.3 km/s2. The kinetic energy release rate is estimated in the range of ∼1.0×1024--1.0×1025 erg\,s−1.
Related
- Tiny Quiet-Sun EUV Ejections Revealed by High-resolution Multiwavelength Observations
- Evidence for Interacting Coronal Mass Ejections in a Magnetic-cloud-like Ejecta: Insights from Multipoint Observations and Polytropic Analysis
- Simultaneous photometric, spectroscopic, and FAST radio observations of AD Leo
- Identifying Cosmic Ray Over-Flagging in STIS CCD Spectroscopic Observations
- Analysis of Aditya-L1/VELC [Fe XIV ] 5303 Å Spectroscopic Observations of the Solar Corona: Development of a Data-processing Pipeline
BibTeX
@misc{yang2026spectroscopic,
title = {{Spectroscopic observations of periodic bursty ejections during a dome-spire-shaped jet}},
author = {Heesu Yang and Maria S. Madjarska and Kyoung-Sun Lee and Klaus Galsgaard},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2610.41343},
eprint = {2610.41343},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2610.41343},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - Spectroscopic observations of periodic bursty ejections during a dome-spire-shaped jet
AU - Heesu Yang
AU - Maria S. Madjarska
AU - Kyoung-Sun Lee
AU - Klaus Galsgaard
PY - 2026
DA - 2026/10/30
PB - arXiv
DO - 10.48550/arxiv.2610.41343
UR - https://arxiv.org/abs/2610.41343
AB - Context: The study investigates the complexity of the formation and evolution of a dome-spire-shaped jet (or anemone jet) that originated in an active region and was presumably driven by null-point magnetic reconnection. Aims: We aim to provide a quantitative estimation of multi-temperature plasma dynamics and physical parameters of the jet and its blob-like features, together with its temporal evolution in three-dimensional perspective. Methods: For this, we analyze unique sit-and-stare spectral (Si IV, Mg II k, and C II) and slit-jaw imaging 1400 Å and 2796 Å observations obtained with the Interface Region Imaging Spectrograph (IRIS), with a slit uniquely positioned just above the assumed reconnection site. Co-observations taken with the Fast Imaging Solar Spectrograph of the Goode Solar Telescope in the chromospheric Hα and Ca II 8542.10 Å lines were also analyzed. These data are complemented by EUV imaging information from the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory. Results: The IRIS observations reveal that the jet is formed by multiple periodic (∼30 s) plasma ejections with blob-like appearance, each associated with strongly blueshifted Si IV 1402.77 Å transition-region emission reaching about −300 km/s. More importantly, the ejections are grouped into well-defined packets, each lasting approximately 3--5 min. In contrast, only a single Doppler component is observed in the chromospheric Ca II line. Multi-Gaussian decomposition of the Si IV line profiles reveals a highly accelerated plasma, with line-of-sight speed toward the observer increasing linearly from ∼30 to 112 km/s over 66 s, corresponding to an acceleration of 1.3 km/s^2. The kinetic energy release rate is estimated in the range of ∼1.0×10^24--1.0×10^25 erg\,s^−1.
ER -