Variation Martian proton aurora in different timescales

The aurorae on Mars are divided into diffuse aurora, discrete aurora and proton aurora. Proton aurora is the most common type of aurora on Mars. The proton aurora on Mars is formed when protons in the solar wind pass through the Martian hydrogen corona and undergo charge exchange to form energetic neutral atoms, which deposit energy in the Martian atmosphere. Previous research results showed that the main external factors that affect the occurrence rate, emission enhancement, intensity and peak height of proton aurora are the solar wind particle flux and velocity, solar zenith angle and solar longitude. Here, we extend the previous proton aurora database compiled by Hughes et al. [2019], which was in the descending phase of the last solar cycle between 2014-2018, to present with similar algorithm. Using this new database covering almost one solar cycle, we investigated the long-term variations of the proton aurora on Mars in three timescales, including the solar rotation cycle, Martian season, and solar cycle. The results will help us understand the solar wind-Mars interactions.