Star Formation Newsletter No. 358, #1-14

No. 3 Gap-opening Planets Make Dust Rings Wider, Bi et al.
No. 5 Structured Distributions of Gas and Solids in Protoplanetary Disks (PPVII)
No. 9 Episodic accretion and mergers during growth of massive protostars
No. 12 300: An ACA 870 μm Continuum Survey of OrionProtostars and their Evolution, Federman et al.
No. 14 Internal or external magma oceans in the earliest protoplanets – Perspectives from nitrogen and carbon
fractionation, Grewal et al.

花輪 知幸 (千葉大学)

No 2. Sustained FU Orionis-type outbursts from colliding discs in stellar ybys,
Borchert et al., MNRaS, 517, 4436 (2022) Cuello+19, Borchert+22 の続編

L* + Lacc 星を考慮して

伴星: M* = 0.5 Mo, Mdisk = 0.007 Mo, rmin = 1 au, rmax = 17 au

温度分布を求める。
fl

主星: M* =1.4 Mo, Mdisk = 0.02 Mo, rmin = 1 au, rmax = 50 au

No. 4 Survey of Ices toward Massive Young Stellar Objects. I. The 4.90 μm absorption band ofOCS ice is detected in 20 sight lines, more than 5 times the previously known detections.
Boogert et al. ApJ, 941, 32
2–5 μm spectra of 23 massive YSOs, taken with the NASA InfraRed Telescope Facility SpeXspectrometer.
The 4.90 μm absorption band of OCS
ice is detected in 20 sight lines, morethan 5 times the previously known
detections.

CO:CH3OH:OCN−:OCS = 24:20:1.53:0.15.

No 6. The Disk Population in a Distant Massive Protocluster, Cheng et al., ApJ, 940, 124 (2022)
G286.21+0.17 (d = 2.5 kpc) ALMA 1.3 mm, 23 mas (65 au x 50 au) 15 mJy beam-1
2017年秋観測

G286c1

Orion clusterの円盤と似ている
ClassI/Flat 天体が主体
距離と質量・半径の相関は有意ではない• 6円盤が NIR (HST) でも見える• 4円盤がX線源(Chandra)と一致• 16 (11) 円盤がコア (G286c1) に(見かけ)付随カタログが掲載されている。

No. 7 The three-dimensional structure of galactic molecular cloud complexes out to 2.5 kpc,
Dharmawardena et al., MNRaS, 519, 228 (2023)

光赤外線での減光とGaia で求めた距離を使って分子雲(暗黒星雲)の3次元構造を求めた。
計算法の改良がセールスポイントらしいが、その原理は別論文

No 8 Razor-thin dust layers in protoplanetary disks: Limits on the vertical shear instability,
Dullemond et al., A&A, 668, A105 (2022)
原始惑星系円盤が 1.3 mm で幾何的に薄く見えるには VSI が起きていない章子

St > 1 は非現実的
a: ダストの半径

VSI d⌦/dz 6= 0 がある場合の不安定<latexit sha1_base64="YcVBAKXc5Tl8GHPEo11oj6Xlrgs=">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</latexit>

ダストが成長すると、1.3 mm で暗くなる。
観測では τ = 0.3z 方向の turbulence によりダストも持ち上がる
なぜ VSI が安定になる理由を議論

No. 10 The SOFIA Massive (SOMA) Star Formation Survey. IV. Isolated Protostars,Fedriani et al., ApJ, 942, 7 (53pp)∼10–40 μm SOFIA-FORCAST images of 11 isolated protostars

No. 11 Millimeter Dust Emission and Planetary Dynamics in the HD 106906 System,
Fehr et al., ApJ, 939, 5121
HD106906AB = 短周期連星, Debri 円盤 と惑星が付随

No. 13 Diffuse γ -ray emission around the massive star forming region of Carina NebulaComplex, Ge et al., MNRaS, 517, 5121
Fermi LAT 2008-2021 (13年分)

E > 500 MeVHIHI

H2 (CO)HII