Numerical Simulations of Anemone Jets in the Solar Photosphere

In the solar atmosphere, jet phenomena accompanied by bright loops in their footpoint are observed. These jets were first discovered in the corona in the 90's, and then in 2007 by the Hinode satellite, which boasts high spatial resolution, also in the chromosphere. These jets are called anemone jets because their feet look like sea anemones. It should be noted that although anemone jets have 10-1000 times different spatial scales in corona and chromosphere, they have the same shape regardless of the scale and can be explained uniformly by magnetic reconnection (Shibata et al. 2007). From the scale universality of anemone jets, it can be predicted that there will be an anemone jet of about 100 km in the photosphere.However, in the photosphere where magnetic energy is not dominant, can jet be generated by release of magnetic energy by magnetic reconnection like corona and chromosphere where magnetic energy is dominant? In addition, since the density decreases exponentially with height in the photosphere and chromosphere, wave velocity increases rapidly with height to form a shock wave. It is thought that magnetohydrodynamic waves generated from photospheric anemone jets also grow by this mechanism to form shock waves and affect the upper layer, but this is not clear quantitatively. Therefore, we are working on the 3D MHD simulation to determine whether an anemone jets occur in the photosphere. As a result of the simulation, the jets are formed by the magnetic reconnection even in the photosphere. In addition, it is also confirmed that slow mode waves are generated with the jet and propagate toward the upper layer. In this poster, we discuss the mechanism of the magnetic reconnection that generated the jet and the growth of the slow mode waves on the upper layer.