Launching of several small- scale successive jets from calcium bright knots and formation of chromospheric anemone jets on the Sun

Abstract Recent space solar observations revealed that solar atmosphere such as corona and chromosphere is full of small- scale jets 1 , associated with small- scale explosions called nanoflares. There is increasing indirect evidence that these jets may be produced by the physical mechanism similar to that of large scale flares, i.e., release of magnetic energy stored in the solar atmosphere through magnetic reconnection 2-4 , and also that these jets and nanoflares may be related to the heating of corona and chromosphere as well as acceleration of solar wind 5,6 . Among small scale jets, the so called chromospheric anemone jets in the active region on the Sun remains puzzling, because they are one of the smallest scale jets so that their footpoints (bright knots) have not been well resolved 7,8,9 . We propose a new model for chromospheric jets using the three-dimensional magnetohydrodynamic (MHD) simulations, which show that the continuous, upward rising of small-scale twisted magnetic flux rope in a magnetized solar chromosphere play an important role in small-scale magnetic reconnections and launching of several small-scale jets during the evolution of the chromospheric anemone jets. Our new, self-consistent, three-dimensional computer modeling of small-scale, but ever-changing flux rope emergence in the magnetized solar atmosphere is found to be fairly consistent with observations.