Solar coronal heating and photospheric magnetic field

The solar coronal heating is one of the most important problem to be solved for the astrophysics. Although it is widely accepted that the magnetic filed emerging from the solar surface plays an essential role for the coronal heating, the detailed mechanism is totally unknown. In this study, we investigated the relationship between the coronal temperature distribution and the properties of small scale magnetic features, magnetic flux tubes, at the base of the corona in detail. We found that coronal temperature distribution depend on the dynamical properties of magnetic flux tubes at the base of the corona. The implication on the coronal heating mechanism is addressed based on our results.