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Segunda parte

Segunda parte. IRAS Vela Shell. Feitzinger & Stüwe 1984.  Pup.  Vel. 14°x14°. IRAS 100µ (30° x 30°). Fig. 1. Pereyra & Magalhães 04. Pereyra & Magalhães 06. Pereyra & Magalhães 06. Estimating Magnetic Fields. Chandrasekhar & Fermi 51. ρ : density ν : turbulent velocity

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Segunda parte

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  1. Segunda parte

  2. IRAS Vela Shell

  3. Feitzinger & Stüwe 1984  Pup  Vel 14°x14° IRAS 100µ (30°x30°) Fig. 1

  4. Pereyra & Magalhães 04

  5. Pereyra & Magalhães 06

  6. Pereyra & Magalhães 06

  7. EstimatingMagneticFields Chandrasekhar & Fermi 51 ρ : density ν : turbulent velocity Δθ: polarization angle dispersion

  8. B = 18 ± 13 μG Pereyra & Magalhães 06

  9. EvaluatingMass-to-Magnetic flux ratio Crutcher 2004 (M / Φ) crit : critical value for the mass can be supported by a magnetic flux N (H2) : H2 column density λ < 1 subcritical regime, magnetic support prevents collapse and star formation

  10. Results support subcritical regime Pereyra & Magalhães 06

  11. Lupus Dark Cloud Alves & Franco 06

  12. Sigue tercera parte

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