SFN369
29. Testing external photoevaporation in the Orionis cluster with spectroscopy and disk mass measurements(K. Maucó, et al.)
30. Finding substructures in protostellar disks in Ophiuchus (Arnaud Michel et al.)31. Global kinematics study of OH masers in W49N (Mendoza-Torres et al.)32. Constraining the geometry of the reflection nebula NGC 2023 with [O I]: Emission & Absorption (B.
Mookerjea et al.)33. Correlation between the optical veiling and accretion properties: A case study of the classical T Tauri star
DK Tau (M. Nelissen et al.)34. Impact of hot exozodiacal dust on the polarimetric analysis of close-in exoplanets (Kevin Ollmann et al.)35. Dissecting the morphology of star forming complex S193 (Rakesh Pandey et al.)
36. Merging Filaments and Hub Formation in the G083.097+03.270 Molecular Complex (Alik Panja et al.)37. High-resolution [OI] line spectral mapping of TW Hya consistent with X-ray driven photoevaporation (Ch.
Rab et al.)
38. Into the Mystic: ALMA ACA observations of the Mystic Mountains in Carina (Megan Reiter et al.)
39. Protoplanetary and debris disks in the Chamaeleontis Association: A sub-millimeter survey obtained with
APEX/LABOCA (V. Roccatagliata et al.)
40. Early Planet Formation in Embedded Disks (eDisk) IX: High-resolution ALMA Observations of the Class
0 Protostar R CrA IRS5N and its surrounding (Rajeeb Sharma et al.)41. How to make giant planets via pebble accretion (Sofia Savvidou et al.)42. The time evolution of Md/Mdot in protoplanetary discs as a way to disentangle between viscosity andMHD winds (Alice Somigliana et al.)

36. Merging Filaments and Hub Formation in the G083.097+03.270
Molecular Complex (Alik Panja et al.)

Kumar et al.2020
ハブ･フィラメント･パラダイム･ハブでの⼤質量星形成、クラスター形成･フィラメント衝突によるハブ形成Stage I
13CO積分強度
Mon OB1 (Montillaud+2019) G202.3+2.5
NWNE

IRAM
Main
NH2SPIRE
NGC22642km/s
13CO位置速度図

Stage 3/4
G31.41+0.31 Beltran+2022

Class I & II天体の分布

PMO 13.7mΦ
the Milky Way Imaging Scroll Painting (MWISP) survey
D=1.52kpc

N~4.8x1022cm -2
速度分散ピーク

12CO (blue), 13CO (green), and C18O (red)NE

中央値-3.98km/s

NW

Panja+2022
S112領域
2度x0.83度=73pcx30pc

中央値-0.83km/s

D~2.1kpc
three distinctyoung stellar
groups12CO (blue), 13CO (green), and C18O (red)l-V図 13COb-V図Fi-SとFi-NWは2km/sの速度差
橋で連結
Fi-N ⻑さ20.7pc 速度勾配0.084km/s/pc
Fi-S
10.4pccf.Ori Integral Shape Filament
幅 0.7~2.2pc
速度勾配<1km/s/pc
Hub N~4.8x10^22cm^-2Stage II かIIIだ
cf. Mon R2 N~2-3x10^22cm^-2Ori KL 5x10^23 cm^-2(1) YSO(Cls I,II,TD)はFi-Nに沿って分布(2) ハブには⼤質量アウトフロー源(3) Fi-NWに⾼密度クランプがありClass I天体が集中42. The time evolution of Md/Mdot in protoplanetary discs as a way to disentangle between viscosity and MHD winds(Alice Somigliana et al.)
Shakura & Sunyaev (1973) αの観測的制限まとめ(Rossoti 2023)

α降着円盤からMHD円盤⾵
ß観測は、想定されるαより⼩さい

観測的に区別できるか
α粘性による円盤の拡散が⾒えるか？
Class 0 天体の円盤は⼩さい。
理論的に1-2Myrで広がってゆく。
観測的にClass II円盤は時間とともに膨張するか？収縮するか？
ダスト連続波で、円盤は収縮
ßダストのドリフト
ガス円盤は？まだ不明

we normalize the wind torque by the mid-plane thermalpressure and define the dimensionless αDW parameterBenoît Tabone et al. 2022

(6)
(A1)
geometrically thin, isothermal, nearly Kepler rotationvφ=rΩ+δvφ, integrating between disk surface

局所的な降着率は(7)magnetic lever arm parameter
total specific angular momentum
carried away along the MHD disc wind(8)
streamline anchored at r
The total angular momentum lost locally by the disc per unit surface(A2)
the time-averaged radial stress tensor describing the radial
and vertical transport of angular momentum
(2)

=(A6)

質量保存

(3)
Shakra Sunyaev αSSはz-⽅向に積分
(4)

(A3)
(A4)

DWによるoutflow

局所的な降着率はDWの反作⽤で⽣じるinflow
(5)
(A5)

SS 乱流拡散Lodato+2017 SS的

降着円盤の同時代線

104 yrTabone＋2022のDWありの降着円盤<latexit sha1_base64="Q3NIqn8AFPYdVsR7UxbxEAFIKO4=">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</latexit>

代

同sha1_base64="k8iXSSgIMWA9DrNC+Ng88IfS7Ao=">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</latexit><latexit

sha1_base64="uenewp9ekIwWn0V5npTptzuwFc0=">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</latexit><latexit

Lupusのデータ

106 yr<latexit sha1_base64="yCVBtckzBJZCn0YB+IDgm9XC2Xo=">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</latexit>(4)線

時 5 yrt=t=

進化

106 yr10

M0 = 10 2 Ms<latexit sha1_base64="lucKAUhvZl+0Wvi48jSI2Kowz6Y=">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</latexit>

M0 = 10 4 Ms<latexit sha1_base64="6wQgfl9+r1Aq48nrc+FVSCpnsm8=">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</latexit>t>>tν0 (最終状態)は1本に収束Lynden-Bell Pringle 1974の⾃⼰相似解

乱流のみ
M0を忘れる

両⽅DWのみ
DWのみ
同時刻線は

(3)

M0の記憶を保つ

population synthesis

ディスク維持時間の時間進化<tlt>
N~100 stars M* follows IMF↓
Md∝M* λmdM/dt∝M*λacc
これを平均値として、個々のMdとdM/dtは対数正規分布↓
個々の星を解析解(など仮定)で進化させる。
ディスクの消失
乱流降着×、円盤⾵○

今は、MD=10-6M8で達成と仮定

tlt=Md/(dM/dt)

disk windσ(tlt)à時間とともに分散が減少、1つの指数関数に収束

0.1Myr
10Myr
SS disk
0.1Myr
10Myr
disk wind

多分、log-normalの平均値に対する同時代線
à時間がたっても分散は維持

観測不定性⼊りモデルと観測の⽐較
à平均値は系統的にモデルを下回る（Mdの過⼩評価？多重星の効果？ダストの進化？）
à分散から、SS円盤は時間とともに外れる。
円盤⾵効果が⾒えている。

観測不定性付加σobs(Md)=0.1dex
σobs(dM/dt)=0.45dex
SS diskMd

ディスク寿命29. Testing external photoevaporation in the Orionis cluster with spectroscopy and disk massmeasurements (K. Maucó, et al.)OB星からの距離

σOri: O9.5V

OB星からの距離

30. Finding substructures in protostellar disks in Ophiuchus (Arnaud Michel et al.)IRS63

Power Law Core withan exponential Tail (PLCT).

Oph-emb-1
standard Gaussians

simple Gaussians that are offset from the source center31. Global kinematics study of OH masers in W49N (Mendoza-Torres et al.)

32. Constraining the geometry of the reflection nebula NGC 2023 with [O I]: Emission & Absorption (B. Mookerjea et al.)33. Correlation between the optical veiling and accretion properties: A case study of the classical T Tauri star DK Tau(M. Nelissen et al.)34. Impact of hot exozodiacal dust on the polarimetric analysis of close-in exoplanets (Kevin Ollmann et al.)

35. Dissecting the morphology of star forming complex S193 (Rakesh Pandey et al.)37. High-resolution [OI] line spectral mapping of TW Hya consistent with X-ray driven photoevaporation (Ch. Rab et al.)photoevaporation wind(Fang+2023)
観測high-resolution VLT/MUSE spectral mapping of TW Hya
結果: [OI] is confined to within 1 AU radially from the star.

38. Into the Mystic: ALMA ACA observations of the Mystic Mountains in Carina (Megan Reiter et al.)39. Protoplanetary and debris disks in the Chamaeleontis Association: A sub-millimeter survey obtained withAPEX/LABOCA (V. Roccatagliata et al.)40. Early Planet Formation in Embedded Disks (eDisk) IX: High-resolution ALMA Observations of the Class 0
Protostar R CrA IRS5N and its surrounding (Rajeeb Sharma et al.)

41. How to make giant planets via pebble accretion (Sofia Savvidou et al.)