What are protostellar outflows are

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Is there infall without outflow ? Very few grav. collapsing objects without outflows All Class 0 protostars drive powerful molecular outflows Class 0 outflows are more powerful than Class I F CO = M.V / t dyn t dyn = R / V F co α L bol for Class I Same mechanism for all sources Outflow energetics are controlled by central object Outflow activity declines with time Bontemps et al. (1996), F CO ≈ 10 -4 M env km s -1 yr -1 F CO and M env are 10x larger for Class 0 / Class I is the same for both classes COSPAR 2012 - Outflows - B. Lefloch
Mass-velocity relation exhibits broken power-law, steeper further out The slope steepens with age and energy in the flow Energy at high velocities of the same magnitude than at low velocities COSPAR 2012 - Outflows - B. Lefloch
Page 1 and 2: Bertrand Lefloch IPAG, Grenoble, Fr
Page 3 and 4: Herbig 1950, 1951; Haro 1952, 1953
Page 5 and 6: What are protostellar outflows are
Page 7 and 8: Outflows • Precess - increases in
Page 9: IRAS 20126+4104 Cesaroni et al. (19
Page 13 and 14: Evolution: opening angle widens wit
Page 15 and 16: A few contributions: Turbulent jet:
Page 17 and 18: HH212: consistent with jet-driving
Page 19 and 20: Ciardi & Hennebelle (2010) COSPAR 2
Page 21 and 22: Shocks are dynamically important :
Page 23 and 24: Outflows interact with the parental
Page 25 and 26: H 2 C-shock J-shock MIR NIR SiO SED
Page 27 and 28: 2.12µm Optical size ~ 2’’ (a f
Page 29 and 30: dN T -a B1 position Nisini et al.
Page 31 and 32: Flower & Pineau des Forets (2010) H
Page 33 and 34: Chemically active outflows L1157 (B
Page 35 and 36: Bachiller et al. (2001) Gueth et al
Page 37 and 38: Rodriguez-Fernandez et al. in prep
Page 39 and 40: PACS HIFI : 490 - 1900 GHz. 27 hrs.
Page 41 and 42: Species detected CO, 13 CO, C 18 O
Page 43 and 44: PACS Spectrum : CO (J up = 14 - 22)
Page 45 and 46: CO : IRAM, CSO, HIFI HIFI Lefloch e
Page 47 and 48: C-type CO Direct evidence for 2 sho
Page 49 and 50: ISO detected strong H 2 O emission
Page 51 and 52: Extended H 2 O emission CSO 325 GHz
Page 53 and 54: B R SiO B R SiO SiO 2-1 Lefloch et
Page 55 and 56: COSPAR 2012 - Outflows - B. Lefloch
Page 57 and 58: COSPAR 2012 - Outflows - B. Lefloch
Page 59 and 60: DG Tau red blue Testi et al. 2002 J
Page 61 and 62:
Origin of molecules in jets ? Sever
Page 63 and 64:
COSPAR 2012 - Outflows - B. Lefloch
Page 65:
A total of 11 emission lines (E up
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What are protostellar outflows are

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