Line-driven disk wind models with an improved line force

We describe an efficient method of calculating the radiation pressure due to spectral lines, including all the terms in the velocity gradient tensor. We apply this method to calculate the two-dimensional, time-dependent structure of winds from luminous disks. Qualitative features of our new models are very similar to those we calculated including only the dominant terms in the tensor (Proga, Stone & Drew 1998, hereafter PSD). In particular, we find that models which displayed unsteady behaviour in PSD are also unsteady with the new method, and gross properties of the winds, such as massloss rate and characteristic velocity are not changed by the more accurate approach. The largest change caused by the new method is in the disk-wind opening angle: winds driven only by the disk radiation are more polar with the new method while winds driven by the disk and central object radiation are typically more equatorial. In the closing discussion, we provide further insight into the way the geometry of the radiation field and consequent flow determines the time properties of the flow.