The origin and evolution of Venus', Earth's, Mars' and Titan's atmospheres are discussed
from the time when the active young Sun arrived at the Zero-Age-Main-Sequence. We show …

The evolution and escape of the martian atmosphere and the planet's water inventory can
be separated into an early and late evolutionary epoch. The first epoch started from the …

Two of the primary goals of the MAVEN mission are to determine how the rate of escape of
Martian atmospheric gas to space at the current epoch depends upon solar influences and …

On 10 September 2017, some of the strongest solar activity occurred in association with
active region 12673 (AR2673), including an X‐class solar flare and a fast coronal mass …

The non-thermal escape of neutral O atoms from Mars at the current epoch is largely due to
dissociative recombination of O2+: There are five energetically allowed channels of this …

We present initial results from the first community-wide effort to compare global plasma
interaction model results for Mars. Seven modeling groups participated in this activity, using …

Aeronomy is a description of the physics and chemistry of the upper atmospheres and
ionospheres of planetary bodies. In this chapter we consider those processes occurring in …

A three‐dimensional (3‐D) atomic oxygen corona of Mars is computed for periods of low and
high solar activities. The thermal atomic oxygen corona is derived from a collisionless …

The crustal remnant field on Mars rotates with the planet at a period of 24 h 37 min,
constantly varying the magnetic field configuration interacting with the solar wind. Until now …

The Mars thermosphere-ionosphere-exosphere (TIE) system constitutes the atmospheric
reservoir (ie available cold and hot planetary neutral and thermal ion species) that regulates …