Scientists tracking the continuous evolution of the energy state of the core of a solar eruption that occurred on July 20, 2017, have found it strangely maintained a constant temperature as it erupted energetic and highly magnetised plasma from the solar corona into space. The finding can improve our understanding of how such eruptions can impact communication systems on Earth.
Coronal Mass Ejections (CMEs) are large-scale eruptions of charged particles (plasma) and magnetic fields from the solar atmosphere into space. They can disrupt a range of ground- and space-based technologies and satellites on Earth. Thus, it is crucial to understand their evolution and propagation through interplanetary space. There is a wide range of plasma temperatures within CMEs, from cold chromospheric material (around 104 K) to hot plasma (around 107 K). When CMEs propagate, several processes can exchange energy (electrical, kinetic, potential, thermal, and so on.), thereby heating or cooling the plasma. To understand the underlying processes, it is important to study the evolution of thermodynamic properties (such as density, temperature, thermal pressure, etc.) of CMEs. This will help our ability to monitor space weather.
In the past, scientists had studied the thermal evolution of CMEs in the solar corona. However, these earlier studies were limited to larger distances from the Sun (more than 1.5 times the radius of the Sun or RSun). It has been known that CME shows peculiar kinematics such as rapid expansion, and impulsive acceleration, in the heights below 3 times the radius of the Sun. However, the evolution of thermodynamic properties of CMEs is not yet well understood, primarily due to the lack of suitable observations in these heights.
A team of scientists consisting of Dr. Vaibhav Pant and Prof. Dipankar Banerjee and researcher Ms. Jyoti Sheoran from Aryabhatta Research Institute of Observational Sciences (ARIES), Nainital, an autonomous institute of the Department of Science & Technology (DST), Govt. of India, and Dr. Ritesh Patel from Southwest Research Institute, Boulder, USA tracked the continuous evolution of the thermodynamic properties of the core of a solar eruption that occurred on July 20, 2017.
In a study published in the journal Frontiers in Astronomy and Space Sciences journal, they estimated the temperature and density of this CME core and found that strangely the CME core maintains a constant temperature as it propagates from 1.05 to 1.35 Rsun despite the expected adiabatic cooling due to the expansion of the core. They used data from the ground-based instruments MLSO (Mauna Loa Solar Observatory) /K-Cor (K-cronagraph) and MLSO/CoMP (Coronal Multichannel Polarimeter) as well as data from the space-based SDO (Solar Dynamics Observatory) /AIA (Atmospheric Imaging Assembly) telescopes for the purpose and also established that the density of the CME core decreased by a factor of around 3.6 as it propagated outwards. The authors conclude that the expansion of this CME core behaves more like an isothermal than an adiabatic process (thermodynamic process in which there is no exchange of heat from the system to its surrounding).
Figure 1: (a) July 20, 2017, CME observed by the MLSO/K-Cor. All three parts of CME are clearly visible. (b) The MLSO/CoMP 10747 Å channel image, and (c) SDO/AIA 193 Å channel image. Only the core of the CME is visible in CoMP & AIA FOV. The yellow rectangular box shows the ROI chosen for the analysis. (d) The zoomed version of CoMP ROI and an artificial slit 3 is shown by a yellow dashed line. (e) The evolution of log temperature and electron density with height and time.
The Visible Emission Line Coronagraph (VELC) onboard Aditya-L1, India’s first solar mission will be launched soon and it will perform both spectroscopy and imaging of the CMEs in the inner corona. A similar kind of analysis using VELC data will provide new insights of the evolution of CME thermodynamic properties in the inner corona.
Details could be found in the following links:
https://doi.org/10.3389/fspas.2023.1092881
https://arxiv.org/abs/2301.13184
For more details, Dr. Vaibhav Pant (vaibhav[dot]pant[at]aries[dot]res[dot]in) may be contacted.
