For a selected region of the sun during Carringon rotation 1527 (November 1967) we combine synoptic photospheric magnetic field, H &agr;, and coronal EUV observations and associated calculations together with solar wind and interplanetary magnetic field observations of three different space probes with a maximum latitudinal separation of ~13¿. From this we construct a simplified but refined meridional coronal-hole-type field geometry for the lower solar atmosphere, and we calculate the magnetic field and the temperature-density dependence at coronal heights above the transition layer. Questions about coronal heating and the validity of th equations of motion in the lower solar corona are discussed.