Abstract
Solar surges are collimated flows of plasma that occur in the periphery of active regions (ARs). The kinematics, physical properties, and triggering mechanisms of a solar surge were studied through imaging and spectroscopic diagnosis. The surge has a typical inverted Y-shape, and it moves with a speed of more than 200 km/s in the transition-region (TR) which is much higher than the sound speed of TR. The observational findings suggest that the surge was triggered due to magnetic reconnection. In addition, a hot jet formed after around 03 minutes and propagated at a speed that is comparable to the sound speed of the corona. Hence, most probably, the hot jet forms due to the chromospheric evaporation. The spectroscopic diagnosis reveals that electron densities are log10 10.82±0.90 and log10 9.93±1.27 in the base and spire of the surge, respectively. Further, it is found that the Si iv line ratio is around 1.85 in the base and 1.80 in the spire of the surge. Hence, we say that most of the Si iv profiles are forming under optically thick conditions in the surge. Most importantly, some Si iv spectral profiles from the base and spire of the surge are double peak profiles with a dip close to the central wavelength. Also, in the same region, optically thick conditions exist, therefore, most probably, the central dip in the profiles is a result of the self-absorption. This is the first-ever report of self-absorption in the solar surges.
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Data Availability
The data underlying this article are available at https://iris.lmsal.com/data.html (NASA/IRIS website) and at https://iris.lmsal.com/search/ (LMSAL search website). Note that IRIS data are publicly available with the observation ID OBS 3880356995. The direct link for the data used in this manuscript is provided below. https://www.lmsal.com/hek/hcr?cmd=view-event&event-id=ivo%3A %2F%2Fsot.lmsal.com%2FVOEvent%23VOEvent_IRIS_20141017_ 181131_3880356995_2014-10-17T18%3A11%3A312014-10-17T18 %3A11%3A31.xml
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We gratefully acknowledge the reviewer for their constructive comments that improved the manuscript. We acknowledge the use of IRIS, AIA/SDO. 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. Atmospheric Imaging Assembly onboard Solar Dynamic Observatory
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The data collection and analysis were done by BSB with suggestions provided by PK. BSB has written the first draft of the manuscript. PK and BSB together made the final draft of the manuscript. SCT contributed to some language corrections in the manuscript.
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Appendix: Spatial variations of spectral profiles in base and spire of the surge
Appendix: Spatial variations of spectral profiles in base and spire of the surge
In this appendix, we have shown the spatial variations of the Si iv line profiles from two different locations: one in the base and another one in the spire of the surge. The red line in panel (a) shows the vertical extent within the surge’s base, i.e., from the bottom to the top edge. We have a total of 20 spectral profiles along the red line. Out of 20 profiles, we have shown six key profiles (panels (b) to (g); Fig. 7) to cover the full vertical extent of the surge’s base. The Si iv profiles from the top edge (panel (g)) and bottom edge (panel (b)) are not double peak profiles while other profiles (in between top and bottom edges) are double peak profiles. We do see that both peaks in these profiles (i.e., panels c, d, e, and f) lie at almost the same wavelength as we move from the bottom to the top edge of the surge’s base.
The panel (a) shows IRIS/SJI 1330 Å image during surge’s maximum phase. The red (blue) vertical line covers the full vertical extent from the base (spire) of the surge. Six key profiles from the surge’s base (i.e., from the red line) are displayed from panels (b) to (g). Similarly, six key profiles from the surge’s spire are displayed in panels (h) to (m). The vertical red lines in all spectral profiles (i.e., panel (b) to (m)) correspond to the rest wavelength of Si iv line
Similar to the surge’s base, the blue line shows the vertical extent of the surge’s spire. Here, the full vertical extent of the spire has a total of 11 spectral profiles, and 6 key profiles are displayed from panels (h) to (m) of Fig. 7. The spectral profiles are either double peak or highly blueward asymmetric profiles. We do not see any change in both peaks (see panels (i), (j), and (m)), and also we don’t see any shift in blueward asymmetry (see panels (h), (l), and (m)). Therefore, we can say the nature of spectral profiles stays the same from the bottom to the top edge of the surge’s spire.
We did not find the signature of the rotating motion in the spire region. And, there is no chance for the rotating motion in the surge’s base. But for the sake of completeness, we checked the spectral profiles from the base as well.
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Babu, B.S., Kayshap, P. & Tripathi, S.C. Self-absorption in solar surge as observed by IRIS. Astrophys Space Sci 369, 61 (2024). https://doi.org/10.1007/s10509-024-04323-5
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DOI: https://doi.org/10.1007/s10509-024-04323-5