Ton 34 recently transitioned from non-absorbing quasar into a BALQSO .
Here , we report new HST-STIS observations of this quasar .
Along with CIV absorption , we also detect absorption by NV+Ly \alpha and possibly O VI+Ly \beta .
We follow the evolution of the CIV BAL , and find that , for the slower outflowing material , the absorption trough varies little ( if at all ) on a rest-frame timescale of \sim 2 yr .
However , we detect a strong deepening of the absorption in the gas moving at larger velocities ( -20 , 000 – -23 , 000 km s ^ { -1 } ) .
The data is consistent with a multistreaming flow crossing our line of sight to the source .
The transverse velocity of the flow should be \sim few thousand km s ^ { -1 } , similar to the rotation velocity of the BLR gas ( \approx 2 , 600 km s ^ { -1 } ) .
By simply assuming Keplerian motion , these two components must have similar locations , pointing to a common outflow forming the BLR and the BAL .
We speculate that BALs , mini-BALs , and NALs , are part of a common , ubiquitous , accretion-disk outflow in AGN , but become observable depending on the viewing angle towards the flow .
The absorption troughs suggests a wind covering only \sim 20 % of the emitting source , implying a maximum size of 10 ^ { -3 } pc for the clouds forming the BAL/BLR medium .
This is consistent with constraints of the BLR clouds from X-ray occultations .
Finally , we suggest that the low excitation broad emission lines detected in the spectra of this source lie beyond the wind , and this gas is probably excited by the shock of the BAL wind with the surrounding medium .