Star Formation Newsletter No. 338, #1-7
#1 A Theoretical Framework for the Mass Distribution of Gas Giant Planets
Forming through the Core Accretion Paradigm, F. Adams et al., ApJ, 909,
#2 Particle Dynamics in 3D Self-gravitating Disks. I. Spirals, H. Baehr & Z.
Zhu, ApJ, 909, 13#3 Particle Dynamics in 3D Self-gravitating Disks. II. Strong Gas Accretion
and Thin Dust Disks, ApJ, 909, 13#4 A possible far-ultraviolet ux-dependent core mass function in NGC
6357, J. Brand et al., A&#5 Tracers of the ionization fraction in dense and translucent gas: I.
Automated exploitation of massive astrochemical model grids, E. Bron etal. A&A, 645, A28 (open access#6 Radial Velocity Monitoring of the Young Star Hubble 4: Disentangling
Starspot Lifetimes from Orbital Motion, A. Carvalho et al. ApJ#7 The Extraordinary Outburst in the Massive Protostellar System NGC6334 I-MM1: Spatiokinematics of Water Masers during a Contemporaneous
Flare Event, ApJ, 908, 175
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6)

flA

5

花輪 知幸

#1 A Theoretical Framework for the Mass Distribution of Gas Giant Planets
Forming through the Core Accretion Paradigm, F. Adams et al., ApJ, 909,1
円盤は指数関数的に減少するのに、巨大ガス惑星の質量分布が/ MP pとなるのはなぜ？
Core accretion paradigm
Phase I

コアの形成 (微惑星の衝突など

Phase II

ゆっくりした降着による成長

Phase III 急速な降着による成長観測と整合的なモデルをつくる円盤を持つ割合

τ = 4-5 Myr)t0 ⇠ 1Myr

Hill 半径の中のガスを獲得

他の値がバラつけば良い。

#2 Particle Dynamics in 3D Self-gravitating Disks. I. Spirals, H. Baehr & Z.
Zhu, ApJ, 909, 13#3 Particle Dynamics in 3D Self-gravitating Disks. II. Strong Gas Accretion
and Thin Dust Disks, ApJ, 909, 136
局所計算 (shearing box)

PENCIL code

初期の Toomre’s Q は 1.02
tc = ⌦ 15ダストは粒子で扱う

パラメータによらず pitch 角 〜10° の Spiral が現れる

#4 A possible far-ultraviolet ux-dependent core mass function in NGC 6357,
J. Brand et al., A&A
450 μm, 850 μm, CO (3-2) (SCUBA-2
70 μm, 160 μm Hi-GAL Herschel
total, active, quiescent〜25K, 〜35 K

Active1221 cores のうち686 coreをSED
411 (active), 275 (quiescent)Quiescent)fltfi

d = 1.77 ±6860.12 kpc

#5 Tracers of the ionization fraction in dense and translucent gas: I. Automatedexploitation of massive astrochemical model grids, E. Bron et al. A&A, 645, A28
機械学習

強度比から電離度を推定する最良の輝線ペアを探す

Translucent cloud と Dense cloud の別あり: 化学モデル Roueff+15⇢, T , AV , 輻射場, 宇宙線, ortho/para, depletion 固定 定常状態

Translucent

RF = Random Forest fiAnalytical t 強度比から電離度を求める近似式

Cold cloud

電離率決定精度著者たちのお勧め

However, our results show that even in the cold dense gas regime, anddespite including DCO+ in our list of potential tracers, the DCO+/HCO+
column density ratio is not ranked among the best tracers of theionization fraction. In fact, it is ranked as the 38th best tracer in dense
cold gas conditions, with a R2 of 0.57 only(cf. Table B.7).

#6 Radial Velocity Monitoring of the Young Star Hubble 4: Disentangling Starspot
Lifetimes from Orbital Motion, A. Carvalho et al. ApJ?
Hubble 4

K7 型 1.234 Mo + 0.73 Mo 連星 4.1 au

1.5459日周期の変動○2005-2007●2008-201

公転ではない変動が持続

Huerta+08 Bisector の説明

Line Center (RV) と CCF に相関0

RVの変動は 公転＋磁場

#7 The Extraordinary Outburst in the Massive
Protostellar System NGC 6334 I-MM1:
Spatiokinematics of Water Masers during aContemporaneous Flare Event, ApJ, 908, 175
MM1: 2008-2015に70±20倍増光

固有運動

d = 1.30 ± 0.09 kpc