"The Science of EST" ep. 9: Solar Coronal Jets

Solar coronal jets are extremely fast ejections of hot plasma triggered by a physical mechanism known as magnetic reconnection. The European Solar Telescope will shed light on this interesting phenomenon.

portrait photo of a young man
Dr. Daniel Nóbrega-Siverio, postdoctoral fellow at Rosseland Centre for Solar Physics, UiO.

Solar coronal jets are impressive plasma ejections that occur in the outermost part of the atmosphere of the Sun. They have extremely high velocities, between 250 000 and 1 450 000 kilometers per hour, which means that the fastest ones can cover the distance from Madrid to Barcelona in just 1.5 seconds.
 
These jets are composed of really hot plasma -more than one million degrees- and are mainly visible in coronal holes (regions with open magnetic field). Solar coronal jets were first observed in the 1990s, using the X-ray telescope onboard the Yohkoh satellite. Since then, they have been a hot topic in solar physics.
 
The physical mechanism responsible for the launch of solar coronal jets is magnetic reconnection: a process in which magnetic field lines of opposite polarities are “cut” and “pasted”, leading to a new configuration of the magnetic field as well as important heating and high-speed ejections. Despite our good knowledge of magnetic reconnection, there are still open questions related to how it is triggered in the case of coronal jets.

Thanks to its extremely high magnetic field sensitivity, the future 4-metre European Solar Telescope (EST) will allow us to study the magnetic field configuration in the lower atmosphere that leads to solar coronal jets. Through coordinated observations of EST and space telescopes, we will be able to get a full understanding of this interesting phenomenon.

solar flares

Solar coronal jet observed on 2007 January 20 with the X-Ray Telescope on Hinode. Image: Moreno-Insertis et al., 2008, ApJ, 673, L211

The figure shows a solar coronal jet observed on 2007 January 20 with the X-Ray Telescope onboard the Hinode satellite in the south coronal hole. The color scale is reversed from the original observation. The coronal jet is the elongated dark structure that resembles an inverted Y (also known as an Eiffel Tower shape).


The science of EST” is a series of short posts for social media where researchers talk in a plain language about a particular topic of their choice and how EST will improve our knowledge on that topic. The aim is to raise awareness among the general public about why solar physicists study the Sun, what the hot topics in today’s solar physics are, and how EST will leap forward our knowledge of the Sun. 

 

All the posts can be found in "The Science of EST" (ext. link).

Tags: Solar coronal jets, magnetic reconnection, solar physics, European Solar Telescope, science of EST By Daniel Nóbrega-Siverio
Published Aug. 26, 2020 1:21 PM - Last modified Aug. 26, 2020 1:21 PM