List of Figures

• 1.1 Sketch of the Magnetospheric Accretion Geometry.

• 2.1 CGS4 layout.

• 3.1 Example of Object and Sky Observations.
• 3.2 Example of a reduced spectral image.
• 3.3 Example of a spectrum before and after de-rippling.
• 3.4 Removal of Pa Beta from standards.
• 3.5 Corrected GI Tau spectrum using BS1495 and BS1392.
• 3.6 Example of fringing pattern.
• 3.7 Fringing in the Flat Field frame.
• 3.8 FFT modulus of BS1251's positive beam.
• 3.9 Filtered spectrum of BS1251's positive beam.
• 3.10 Examples of removed interference fringes.
• 3.11 Absorption feature removal (UT9512 Br Gamma).
• 3.12 T Tauri stars Pa Beta spectra (UT9512).
• 3.13 T Tauri stars Br Gamma spectra (UT9512).
• 3.14 UT9410 - T Tauri stars spectra.

• 4.1 Photospheric Lines.
• 4.2 Veiling Tests.
• 4.3 Pa Beta Template Stars.
• 4.4 Br Gamma Template Stars.
• 4.5 J veiling vs. K veiling.
• 4.6 Veiling measurements: histograms.
• 4.7 Veiling histograms: lower limits contribution.
• 4.8 Optical versus near infrared veiling.
• 4.9 J and K veiling: comparision with model results.
• 4.10 Veiling at J and K for J veiling equal to one tenth of V veiling.
• 4.11 Mass accretion rate vs. J and K veiling.
• 4.12 K2V vs. M2V veiling determinations.

• 5.1 Pa Beta line profiles.
• 5.2 Br Gamma line profiles.
• 5.3 Pa Beta and Br Gamma FWHM histograms.
• 5.4 Pa Beta and Br Gamma wing maximum velocity histograms.
• 5.5 Velocity of the Pa Beta and Br Gamma line peaks.
• 5.6 Asymmetry factors distributions.
• 5.7 Pa Beta Type I line profiles.
• 5.8 Br Gamma Type I line profiles.
• 5.9 Type I line profiles: FWHM histograms.
• 5.10 Histograms of the wings maximum velocities.
• 5.11 Type I line profiles: histograms of the velocity of the line peaks.
• 5.12 Asymmetry factor distributions for Type I line profiles.
• 5.13 Pa Beta and Br Gamma Types II and III line profiles.
• 5.14 Pa Beta Type IV R line profiles.
• 5.15 Br Gamma Type IV R line profiles.
• 5.16 Type IV R profiles: wings maximum velocities.
• 5.17 Type IV R profiles: velocity of the line peak.
• 5.18 Br Gamma line profile for a spherically symmetric wind model.
• 5.19 Stochastic wind models: high optical depth lines.
• 5.20 Stochastic wind models: intermediate optical depth lines.
• 5.21 Model Br Gamma line profiles from Muzerolle, Calvet & Hartmann (1998).
• 5.22 Influence of the accretion shock in the line profiles.
• 5.23 EW(emission) vs. EW(absorption) for Type IV R (IPC) line profiles.
• 5.24 IPC profiles and spectral types.
• 5.25 Accretion rate vs. absorption EW in Pa Beta IPC lines.
• 5.26 Accretion rate vs. emission EW in Pa Beta IPC lines.
• 5.27 Accretion rate vs. line to continuum ratio at the peak for Pa Beta IPC lines.
• 5.28 Wind Mass Loss Rate vs. Emission EW in Pa Beta IPC lines.
• 5.29 Accretion rate vs. EW in Pa Beta Type I line profiles.
• 5.30 Accretion rate vs. EW in Br Gamma Type I line profiles.
• 5.31 Wind mass loss rate vs. EW in Type I Line Profiles.
• 5.32 Pa Beta line variability I.
• 5.33 Pa Beta line variability II.
• 5.34 Br Gamma line variability.

• 6.1 Model profiles: tests.
• 6.2 Bertout (1984) Figures 1, 4 and 5.
• 6.3 Typical line profiles for a wind model.
• 6.4 Pa Beta and Br Gamma line profiles for different parameters in the wind.
• 6.5 Wind model for CW Tau.
• 6.6 Pa Beta accretion model line profiles.
• 6.7 Br Gamma accretion model line profiles.