Multi-wavelength spectroscopic observation of EUV jet in AR 10960

TL;DR

This study investigates the velocity and temperature relationship of a solar EUV jet using multi-wavelength spectroscopy, revealing simultaneous chromospheric evaporation and magnetic acceleration during the jet event.

Contribution

It provides the first detailed analysis of the true velocity and temperature correlation of a solar EUV jet using stereoscopic and spectral data, highlighting concurrent physical processes.

Findings

Cool jet velocity exceeds chromospheric evaporation limit (~220 km/s)

Hot line velocities are higher than cool lines, indicating different acceleration mechanisms

Chromospheric evaporation and magnetic acceleration occur simultaneously

Abstract

We have studied the relationship between the velocity and temperature of a solar EUV jet. The highly accelerated jet occurred in the active region NOAA 10960 on 2007 June 5. Multi-wavelength spectral observations with EIS/Hinode allow us to investigate Doppler velocities at the wide temperature range. We analyzed the three-dimensional angle of the jet from the stereoscopic analysis with STEREO. Using this angle and Doppler velocity, we derived the true velocity of the jet. As a result, we found that the cool jet observed with \ion{He}{2} 256 \AA $\log_{10}T_e[\rm{K}] = 4.9$ is accelerated to around $220 \rm{km/s}$ which is over the upper limit of the chromospheric evaporation. The velocities observed with the other lines are under the upper limit of the chromospheric evaporation while most of the velocities of hot lines are higher than that of cool lines. We interpret that the chromospheric evaporation and magnetic acceleration occur simultaneously. A morphological interpretation of this event based on the reconnection model is given by utilizing the multi-instrumental observations.