STAR FORMATION NEWSLETTER#306 25 - 34±^\P (ToL)Paper lists

25. A 100 au-Wide Bipolar Rotating Shell Emanating From the HH 212 Protostellar Disk:A Disk Wind?
26. Vortex survival in 3D self-gravitating accretion discs
27. Detection of 40–

25. A 100 au-Wide Bipolar Rotating Shell Emanating From the HH 212
Protostellar Disk: A Disk Wind?
Lee et al.

Accepted by ApJ

http://arxiv.org/pdf/1802.03668

S02outflow shell, inner disk
atmosphere,7>5S0 outflow shell, collimated jet,7>5(dusty diskoptically thick✖)SO maps
Fig3(a)x(|voff| < 3 km s-1)2¬a wide-opening outflow
a collimated jet along the jet axis
Fig3(b)Blueshifted/redshifted emission p)-> mainly radially expanding
Fig3(c)cx4.67iCSO2 maps
Fig4(a), (b)x(|voff| < 3 km s-1)minnerdisk atmosphere,7>5Fig4(b)CH2DOH$Y'*¥
rotation sense
Fig4(c)cx4.67iCSiO4.67¥blueshifted emissionredshifted emission&(Y'*)

Fig.7(a)the redshifted emission in the eastand blueshifted emission in the west-> rotating disk atmosphereKeplerian rotation velocity profile(magenta curves)«Bthe outer part of theatmosphere is not only rotating but alsoexpanding (Hirota et al. 2017)-> atmosphere outflow shellA)(a) -> (g) minor axis` (-> expansion motion &( )(a) -> (g) major axisx-axis!y­-> expansion fFig.6(a) indicating that the shell is also rotating around the jet axis,in addition to the expansion mentioned above.
Fig.6(b)The outflow edges are too faint in SO2 to appear in this figure.

outflow shell radius becomes wideroutsideinside~40 au km s-1~50 auoutside regionBWPVa-> Zs¢J((Fig.7)

 specific angular momentum Zs
*disk windA???(k1=9m)
X wind model* OK?

As discussed later, the wind’s source can be on the disk 2–3 au from the protostar.
In HH212,
52 au resolution,
outflow extend out from the disk & rotates (Tabone+ 17)
Now, 16 au resolution,compact 2 outflows; a wide-angle outflow shell and a collimated jet.
shell disk windh,7>5)ud-> shellab:07=
shell wide-angle radial wind&~
dask%atmosphereud-> :07=radial_,_eHNXG'

r*



Fig.6-> z = CR2+0”02 in the cylindrical coordinate system(C  14 arcsec−1)
Lee+00 (In the cylindrical coordinate system,)shell material is moving along-> vR = v0R and vz = 2v0z-> v0 ~ 42 km s-1 (Fig.11 solid curves)
shell material is radially expanding,-> vR = v0R and vz = v0z-> v0 ~ 45 km s-1 (Fig.11 dashed curves)

28. The straight and isolated G350.54+0.69 filament: density profileand star formation content
Liu et al.

Accepted by MNRAS

http://arxiv.org/pdf/1805.03670

On scales larger than cores, Herschel results
molecular cloud have an approximately uniform inner width of 0.1 pc
common width may be¯ attributed to the sonic scale below° rooted in the dissipation of magneto-hydrodynamic (MHD) waves&(D (&(j©)clouds-> Wider widths (between 0.26 pc and 0.34 pc)
Juvela et al. (2012) find filament widths of 0.1 to 1 pc, with a typical value of ~ 0.2 - 0.3 pc
8</3;?filament widthRgparameter&)$
It is, therefore, necessary to investigate the properties, including the density profile
shape, of star forming gas filaments beyond the Gould Belt.

Ntstar forming filamentary cloud G350.54+0.69 (G350.5 afterwards)-> straight and isolated nature
G350.5-N
Mtot
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T

⇠

590M

⇠

18.2 K⇠Mtot

8.2 ⇥ 1022 cm 2N<latexit sha1_base64=A0JA2hZfInE8HDi3kU0KUHrheOAk=">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</latexit>
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T

⇠

95M

⇠

17.7 K⇠8.2 ⇥ 1021 cm 2

two velocity components

accretion flows&z)¦¨&Larson’s relationship¤*)$&(+  

Plummer-like function fitting-> ⇢c = 2.7 ⇥ 104 cm 3This central gas density represents anunderestimate because at the resolution (0.12 pc)
of our observations the central filament density
profile may be unresolved.
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non-thermal turbulent
pressure dominant overthermal pressure in theentire cloud G350.5

Stutz+13, Ragan+06-> 70μm - 24μmvprotostars¡cenvelope,£Class 0/I&(lIFig. 6-> 670μmQ|[+ 92-UOA) J
YSO candidate

G350.5 -> low mass star formation region,")#SED fitting