  Apart from regular monitoring by ASM, the compact object SS 433 was observed
with RXTE several times last two/three years. We present the first analysis of
these observations. We also include the results of the recent exciting TOO
campaign made during donour inferior (orbital phase $\phi=0$) and superior
($\phi=0.5$) conjunctions which took place on Oct. 2nd, 2003, and on March
13th, 2004 respectively, when the jet itself was directly pointing towards us
(i.e., precessional phase $\psi \sim 0$). Generally, we found that two distinct
lines fit the spectra taken on all these days. We present some of the
light-curves and the X-ray spectra, and show that the Doppler shifts of the
emitted lines roughly match those predicted by the kinematic model for the
jets. We find that the line with a higher energy can be best identified with a
FeXXVI Ly-$\alpha$ transition while the line with lower energy can be
identified with a FeXXV (1s2p - 1s$^2$) transition. We observe that the X-ray
flux on March 13th, 2004 (when the base of the jet is exposed) is more than
twice compared to that on Oct. 2nd, 2003 (when the base is covered by the
companion). We find the flux to continue to remain high at least till another
orbital period. We believe that this is because SS 433 was undergoing a weak
flaring activity during the recent observation.
