<Table> Competing heating mechanisms <Tr> <Th_colspan="3"> Heating Models </Th> </Tr> <Tr> <Th> Hydrodynamic </Th> <Th_colspan="2"> Magnetic </Th> </Tr> <Tr> <Td> <Ul> <Li> No magnetic field </Li> <Li> Slow rotating stars </Li> </Ul> </Td> <Th> DC (reconnection) </Th> <Th> AC (waves) </Th> </Tr> <Tr> <Td> <Ul> <Li> B - field stresses </Li> <Li> Reconnection events </Li> <Li> Flares - nanoflares </Li> <Li> Uniform heating rates </Li> </Ul> </Td> <Td> <Ul> <Li> Photospheric foot point shuffling </Li> <Li> MHD wave propagation </Li> <Li> High Alfvén wave flux </Li> <Li> Non-uniform heating rates </Li> </Ul> </Td> </Tr> <Tr> <Th> </Th> <Th_colspan="2"> Competing theories </Th> </Tr> </Table> <Tr> <Th_colspan="3"> Heating Models </Th> </Tr> <Tr> <Th> Hydrodynamic </Th> <Th_colspan="2"> Magnetic </Th> </Tr> <Tr> <Td> <Ul> <Li> No magnetic field </Li> <Li> Slow rotating stars </Li> </Ul> </Td> <Th> DC (reconnection) </Th> <Th> AC (waves) </Th> </Tr>

The corona of the sun has a temperature