21. The Green Bank Ammonia Survey: Dense Cores Under Pressure in Orion A Kirk+ ApJ in press
GAS

Herschel YSOSpitzer YSO

JCMT
prestellar
core

JCMT
protostellar
core

prestellar core

protostellar core

surface pressure

G dominatedpotential
P dominatedkinetic energy-(ΩG+ΩP)= 2ΩK

Virial Equilibrium
Surprisingly, we find that almost none of the dense cores are sufficiently massive to be bound when considering
only the balance between self-gravity and the thermal and non-thermal motions present in the dense gas.
Including the additional pressure binding imposed by the weight of the ambient molecular cloud material andadditional smaller pressure terms, however, suggests that most of the dense cores are pressure-confined.

22. HP2 survey: III The California Molecular Cloud– A Sleeping Giant Revisitedby Lada, Lewis, Lombardi, Alves Aap in press
SFR = 1/10 of Ori
Herschel data SED fit à (T, τ850)
TStructure Function

τ850

Ak=γτ850+δ
γ=3593.75 mag
δ=-0.110±0.006 mag∝Ak-q
where dS (AK ) is an element of cloudsurface area at an extinction AK.
derivative of this functiondS(>AK)/dAK=S’(>AK)∝Ak-n
proportional to the column density PDF
èn=4.0±0.1
èq=3.0 (q=2 Ori A, B and Per)èsteeper slope than the GMCs

Schmidt Law
protostellar surface density: thresholded Schmidt relationèβ=3.31±0.23, κ=0.36±0.09 stars pc-2 mag-3.31, AK,0=0.51 mag.

measured

unknownmeasured

if power law à p=β-n = -0.69 ±0.27
Our observations suggest that variations both in the slope ofthe Schmidt relation and in the sizes of the protostellar
populations between GMCs are largely driven by variationsin the slope, n, of PDFN(AK).

∝Akp

23. Mid-Infrared Polarization of Herbig Ae/Be Discs by Dan Li+, MNRAS in press
The translation of mm/submm polarization maps into the B-field morphology (projectedon the plane-of-sky) was once thought to be straightforward, but recent studies haveemphasized that scattered emission can also contribute to the observed mm/submm
polarization if dust grains much larger than their ISM (interstellar medium) counterparts
are present in discs (Kataoka et al. 2015; Yang et al. 2016; Tazaki et al. 2017).
(1) Observation: a mid-infrared (mid-IR) polarimetry using Canari-Cam(2) Object: Herbig Ae/Be (HAeBe) stars (i.e., premain sequence stars of 2–8 M⊙).
(3) detected: the brightest and most compact inner regions of the discs.
(4) Band: Si-2 (λ=8.7μm), Si-4 (λ=10.3μm), Si-6 (λ=12.5μm)
AB Aur (Li+ 2016)
r>70AU ring-like (scattering),
Pol. E vec. r<70AU PA~165deg (dichroic emission ofPol. Intensity elongated particles aligned in a disk B-field[poloidal axis is offset from disk axis])
Stokes Iabsorption
pcombined
Q/I

U/Iemission

not inconsistent with
2 component modelà scattering24. The Formation of Stellar Clusters in Magnetized, Filamentary Infrared Dark Clouds
Pak Shing Li et al. MNRAS in press
InfraRed Dark Cloud Σ~10^22cm^-2 ρ~10^4cm^-3 M~10^2~10^3 M_solλ >> 2c_s^2/G ~16.6 (T/10K) M_sol/pc(1) Would stars form throughout the lament, or would the formation propagate along
the lament?
(2) How efficient is protostellar feedback in destroying or disrupting a lament?
(3) Would the geometry of long filamentary clouds affect the properties of a
protostellar cluster, such as the protostellar mass function (PMF) and the companion
multiplicity?
Model and Method
Numerical Methods:orion2 adaptive mesh renement (AMR) code
Turbulence: M=10, M_A=1 driving turbulence, T=10K, M=3110M_sol, V=(4.55pc)^3
sink particle:
stellar feedback: Luminosity + outflow (momentum+energy)
fw=Mdot ej/Mdot acc=0.3; outflow speed v_w=min[v_Kep(R_*)/3, 100km/s]

100 most massive clumps
zoom-in region=refine upto 6 levels
Krumholz+12 à high z gal 0.015
Heyer+16 à Class I 0.02
εff=0.067
Chabrier IMF05
Mass Funcevolution
M*tot=SFE=M*/(Mg+M*)

Padoan+14 à1.75
Li+15,Murray+17 à2
Luminosity Prob è resolved
1st protostar is madetheoretical IMF

25. The properties of the inner disk around HL Tau: Multi-wavelength modeling of thedust emission by Yao Liu+ AAp in press
Carrasco-Gonzalez+2016
VLA 7mm cont.

Fig.6: larger grains
are trapped in thefirst bright ring.
ALMA wavelengths of 2.9, 1.3, and 0. 87mm revealed a pattern of bright and dark rings.
(1) embedded planets in the gaps (Dong+2015; Dipierro+ 2015; Picogna & Kley 2015)à
Large Binocular Telescope, however, excluded the presence of massive planets (~ 10 −15MJup ) in two gaps ~70AU (Testi+2016)(2) non ideal MHD (Flock+2015)(3) sintering（焼結）-induced dust rings (Okuzumi+ 2016 ),(4) dust coagulation triggered by condensation zones of volatiles (Zhang et al. 2015 ),(5) secular gravitational instability (Takahashi & Inutsuka 2016 ).
Since radiation λ=2.9mm optically thick, longer wavelength λ=7mm (JVLA)Flared disk

ξ>0 smaller dust has a larger scaleheightàβ>1dust size distribution a=(0.01μm,7mm)
p=-3.5 or spatially varies

Central Star M*=1.7M8, T=4000K, L=11L8(A) Modeling with a homogeneous grain size distribution èNO(B) Modeling with two power-law grain size distributions
cf. Pinte+2016 model p=-3.5 @ r<75AU; -4.5 @ r>75AU(C) mass fraction fsize @ size=+0.1+0.2
pinner = −3.5 −0.2 @ r<50AU; pouter = −3.9 −0.1 @ r>50AU
2.82, 0.95, 0.45, and 0.29mm
Model
0.87mm
Obs
1.3mm

2.9mm
7mm

AU Auriamaxλ