A combination of statistical studies and 18 case studies have been used to investigate the structure of the induced Martian magnetosphere. The different plasma and magnetic pressure forces on the dayside of the induced magnetosphere of Mars have been studied using 3.5 years of Mars Atmosphere and Volatile Evolution (MAVEN) and Mars Express (MEX) observations. We present estimates of typical values for the dominant pressure terms, i.e., the thermal pressures of the ionosphere and the magnetosheath, the magnetic pressure of the magnetic pile‐up region, and the solar wind dynamic pressure. For 18 typical orbits the altitudes and relative distances of the pressure balance boundaries, the photoelectron boundary (PEB), the ion composition boundary (ICB), and the induced magnetosphere boundary (IMB) are estimated. The Magnetic Pile‐up Boundary (MPB) is discussed but not further studied since earlier characterisations of the MPB do not agree with our results.This study focuses on the transition region between the ionosphere and the magnetosheath on the dayside of Mars. We show that earlier definitions of the PEB, ICB, and IMB do not characterise the transition region well, mainly because each boundary is based on measurements from only one or two instruments. In order to characterise the transition region correctly changes in magnetic field strength and fluctuations, dominant ion species, electron and ion densities and energy distributions, need to be considered. This article confirms a complex interaction between Mars and the solar wind and can explain why previous studies have had difficulties to describe the force balance.