| Name: | Pramod Kumar |
| Affiliation: | S. S. Jain Subodh P. G. (Autonomous) College, Jaipur, Rajasthan, India |
| Conference ID : | ASI2022_159 |
| Title : | A study on various modes of parallel heat conduction in the solar flares using scaling laws |
| Authors : | 1. Dr. Pramod Kumar, Dept. of Physics, S. S. Jain Subodh P. G. (Autonomous) College, Jaipur, Rajasthan, India 2. Dr. R. K Choudhary, Space Physics Laboratory, VSSC, ISRO, Trivandrum, Kerala, India |
| Abstract Type: | Poster |
| Abstract Category : | Sun and the Solar System |
| Abstract : | The study of various modes of parallel heat conduction such as free streaming, collisional-dominate, and turbulent dominated, in the coronal loops is crucial for understanding plasma acceleration, energy release models during solar flares. In this paper, using recently established scaling laws, we have studied the relative importance of these modes of parallel heat conduction in the coronal loops of the small (B-class) and large (X-class) solar flares. The scaling laws relate the maximum loop temperature and heating rate to the loop pressure and loop half-length for collision, turbulence, and free streaming dominated modes of the parallel heat conduction. For a set of values of loop half-length = (2.0 − 3.0) × 10^9 cm, loop pressure= (6.0 − 20.0) erg cm^−3 for the small coronal loops, and loop half-length = (3.0−11.0)×10^9 cm, loop pressure= (1.0−103.0) erg cm^−3 for the large coronal loops at a constant value of mean free path = 10^7.5 cm, our results show that the estimated heating time is ~ 40 – 125 s, which represents a fast heating rate. The estimated maximum loop temperature is found to be less compared to the observed values for the coronal loops of the solar flares. The nature of the positive and negative correlation between the scaling parameters shows that collision-dominated heat conduction is a dominant process in the loops of small flares. The turbulence-dominated process was found to suppress the collision-dominated parallel heat conduction in the coronal loops of large solar flares. In this paper we also discuss instabilities caused by the fast flow of evaporation from the footpoints as the source of the turbulence. |