We present far-ultraviolet spectra of the classical T Tauri star RU Lupi covering the 912–1710 Å spectral range , as observed by the HST /STIS and FUSE satellites .
We use these spectra , which are rich in emission and absorption lines , to probe both the accreting and outflowing gas .
Absorption in the Ly \alpha profile constrains the extinction to A _ { V } \sim 0.07 mag , which we confirm with other diagnostics .
We estimate a mass accretion rate of ( 5 \pm 2 ) \times 10 ^ { -8 } M _ { \odot } yr ^ { -1 } using the optical-NUV accretion continuum .
The accreting gas is also detected in bright , broad lines of C iv , Si iv , and N v , which all show complex structures across the line profile .
Many other emission lines , including those of H _ { 2 } and Fe ii , are pumped by Ly \alpha .
RU Lupi ’ s spectrum varies significantly in the FUV ; our STIS observations occurred when RU Lupi was brighter than several other observations in the FUV , possibly due to a high mass accretion rate .