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The solar coronal heating is a longstanding mystery in astrophysics.Considering that the solar magnetic field is spatially inhomogeneous withconsiderable magnetic gradient from solar surface to the corona, this workproposes a magnetic gradient pumping (MGP) mechanism and try to explain theformation of hot plasma upflows, such as the hot type II spicules and hotplasma ejections, etc. In MGP mechanism, the magnetic gradients drive theenergetic particles to move upwards from the underlying solar atmosphere andform hot upflows. These upflow energetic particles deposit in corona and makeit becoming very hot. Roughly estimations indicate that the solar corona can beheated to above 1 million degrees, and the upflow velocity is about 40 km/s inchromosphere and about 130 km/s in the corona. The solar magnetic flux tubesact as pumpers to extract energetic particles from the underlying thermalphotosphere, convey them and deposit in the corona. The deposition of energeticparticles will make the corona become hot, and their escaping from thephotosphere will make the underlying photosphere a bit cold. This mechanismpresent a natural explanation to the mystery of solar coronal heating.

Coronal Heating Driven by A Magnetic-gradient Pumping Mechanism in Solar Plasmas