41: Accretion Flows or Outow Cavities? Uncovering the Gas Dynamics around Lupus 3-MMS
Travis J. Thieme et al. ApJ

渦状降着流 Li +2014

L1489IRS Yen+2014
C18O2-1
High V.

C18O2-1
Medum V.

disk
protrusion
outflowと逆の速度成分

C18O2-1
Low V.

Lup 3-MMS
ケプラー円盤を持つ、若いClass 0原始星
CO、13CO、C18O(J=2-1)、SOC18O2-1

12CO2-1

rotating disk
1.3mm

ES1:〜2000AU、red-shift、ディスクの⾚⽅偏移側に接続。
ES2:〜1300AU、Blue-shift gas on red compof outflow、ディスク⽅向へ加速。
ES3:〜1800AU、⾚⽅、⻘⽅偏移ガス混合
ES4:〜1600AU 、⾚⽅、⻘⽅偏移ガス混合j2
r=GM⇤ 1<latexit sha1_base64="7jZ3CwWTZ+I17pjaiEzMk96Ox7s=">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</latexit>

CMU(Cassen-Moosman-Ulrich) Model
点重⼒源へ⾃由落下する軌道を考える。
θ0=90度

1cos ⌫r04 ⌦2rc =GM⇤r 遠⼼⼒半径<latexit sha1_base64="nVz2tmPYkP8dCDM6khOgTzyyou8=">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</latexit>c<latexit sha1_base64="0xOn9MKRWQzYPPIDCFUTIMhgiqM=">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</latexit>

j 2 = r04 ⌦2 sin2 ✓0 θ =45度
0Ω

θ0=90度

M*=0.1M8, rc=100AU, r0=104AU

観測者

θ0=30~150度
φ0=0~360度(C18O PV is) fairly consistent
with the overall structure of
the CMU model.

12CO

12COC18O(1) mostly within the extent of
the model curves(2) C18O emission mostlyavoids these gaps
j=2.7~6.9 10-4kms-1pc

Dendrogram PPV data

Mdot=0.5~1.1 10-6M8yr-1
poorly fitted

S3S3S4S4S1S1S2S5S2S5

42: The VLA/ALMA Nascent Disk and Multiplicity (VANDAM) Survey of Orion Protostars V. A
Characterization of Protostellar Multiplicity by John J. Tobin, et al. ApJ.
主系列星
highest mass ほぼ100%多重星
太陽質量星50%が多重星
軽い星では25−30％前主系列星（Class II, ClassIII）
多重度は主系列と同じか⾼い(Reipurth+2007)。
原始星Class I、Flat Spectrum
前主系列星、太陽質量Field星より多重度同じか⾼いClass 0原始星の多重度は？
多重星形成機構に対する制限
サブmm~cm波の⼲渉計（ALMA、VLA）星周円盤
VLA/ALMA Nascent Disk And Multiplicity(VANDAM) survey Per(済)+Ori
ALMA: λ0.87mm Δθ0.”1(40au) VLA: λ9mm, 0.”08(32AU)HOPS Survey: 94Class0+128ClassI+103Flat Sp./409 HOPS原始星候補天体<latexit sha1_base64="W12bHMQAQQOnnMJxeILB6KYXq2I=">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</latexit>

dlim<dA-Bdlim増やす

Multiplicity fraction (MF)dlimの関数

dlim>dA-B

MF =<latexit sha1_base64="gecsR7S49ckATqdNiV3ybWMaDto=">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</latexit>

Companion fraction (MF)dlimの関数CF =

B+T +Q
S+B+T +Q

B + 2T + 3Q
S+B+T +Q

中⼼点で置き換え
す増や☆bimodalpeak~100auと3000au

d limdlim>dC-D

dlim増やすdlim>dAB-CD

すべてのペア
極⼤値が2つFieldの太陽型星に関する分布☆Fieldの太陽型星の分布とは⼀致しない

中⼼点で置き換え

間隔

Class 0どうしbimodal ○Field×Class Iどうし
bimodal ×
Field×Flat Sp.どうしbimodal ×
Field ○

Class 0含むペア
log flat ×Class I 含むペア
log flat ×MF(20~104AU)

Class 0Flat Sp.含むペア☆MF=0.30±0.03
CF=0.32±0.02
20~104AU separation☆ClassごとのMF/CF
20~104AU sep.でClass 0か1以降で下がる
多重度の減少☆ 20~103AU separation
Flatで上がる（1-1.5σ）
多重度の上昇II+FlatCF(20~104AU)

Flat

Class 0MF(20~103AU)

Class 0I

I+FlatI

I+FlatI+FlatFlat

CF(20~103AU)

Flat

Class 0I

I+FlatFlat

CF(20~500AU)

MF(20~500AU)Class 0I

Flat

Class 0I

I+FlatFlat

HD:>30pc-2
LD:<30pc-2☆環境別のMF/CF変化YSO Density>30pc-2とYSO Density<30pc-2を⽐較☆MF/CF進化は内向き・外向きmigrationか43. Monte-Carlo simulations of evolving rotational distributions of low-massstars in young open clusters. Testing the influence of initial conditions.
M. J. Vasconcelos, J. Bouvier et al. MNRAS

44. A Kpc Scale Molecular Wave in the Inner Galaxy: Feather of the Milky Way?
V. S. Veena, et al.

Giant Molecular Filament
特に⻑いもの、数百pc⻑、銀河⾯に沿って、渦状腕の⾼密度部で「bones/spines」か、渦状腕間の構造で「spurs/feathers」かhighly unusual filamentary cloud at D=5kpc,
galactic center region 324<ℓ<355

350

Data: (1) the structure, excitation, and dynamics
of the inner Galactic interstellar medium SEDIGISM survey
APEX 13CO,C18O J=2-1(2) Three-mm Ultimate Mpora Milky Way Survey(TheUMMS)
Mopra 12CO, 13CO, C18O J=1-0(3) Southen Galactic Plane Survey (SGPS)
ATCA, Parkesm HI340330

Scutum Arm
CO(1-0)ℓ~2.4kpc
HIh<50pc
軸⽐ 60:1
X(13CO2-1)=1x1021cm2(K km/s)-1とするとM~8.7x106M8

Norma Arm3kpc ArmGMF
距離評価：kinematic distanceで遠/近点の判別はHi-GAL（Herschel）のコンパクト点源カタログを⽤いた

vertical oscillation±70pc
λ~600pc

bone（⾻）かspur（蹴⽖）かà今後こんな感じか？

物理的原因：（磁場）⾃⼰重⼒不安定、wiggle不安定性、微分回転によるシア運動、集中した超新星フィードバック45: Mapping physical parameters in Orion KL at high spatial resolution
Olivia H. Wilkins, et al. ApJ

46: Streaming Instability with Multiple Dust Species:II. Turbulence and Dust-Gas Dynamics at Nonlinear
Saturation
Chao-Chin Yang (楊朝欽) and Zhaohuan Zhu (朱照寰) MNRAS