Star Formation News Letter No. 30
58. Complex organic molecules in low-mass protostars on solar system scales – I.
Oxygen- bearing species, van Gelder et al. A&Ap
59. Is the gap in the DS Tau disc hiding a planet? Veronesi et al. MNRAS
60. Catalogue of new Herbig Ae/Be and classical Be stars. A machine learning
approach to Gaia DR2, Vioque et al. A&Ap
61. Thermal evolution of protoplanetary disks: from β-cooling to decoupled gas
and dust temperatures, Vorobyov et al. A&Ap
62. A Study of Millimeter Variability in FUor Objects, Wendeborn et al., ApJ
63. Non-ideal magnetohydrodynamics vs turbulence I: Which is the dominant
process in protostellar disc formation? Wurster et al. MNRAS
64. Non-ideal magnetohydrodynamics vs turbulence II: Which is the dominant
process in protostellar disc formation?
65. The role of Galactic H ii regions in the formation of filaments High-resolution
submilimeter imaging of RCW 120 with ArTéMiS, Zavagno et al., A&Ap
61-62は一連の論文

花輪 知幸

58. Complex organic molecules in low-mass protostars on solar system scales – I.
Oxygen- bearing species, van Gelder et al. A&Ap, 639, A87 (2020)

灰色IRAS 2A, IRAS4A, HH 212, IRAS 16293A,

IRAS 16293B

Band 3 cold COMs
Tex 〜 60 K
Band 6 hot/warm COMs
Tex 〜 200 K

COM のいくつか(i.e., CH2DOH, CH3OCHO, CH3OCH3, CH3COCH3,(CH2OH)2) は領域によらず似ている。
D/H比は数% (〜15 Kで形成されたと想像される)

59. Is the gap in the DS Tau disc hiding a planet?
Veronesi et al. MNRAS, 495, 1913
34.5 au に惑星 2 MJ

分子輝線に惑星の影響 (kink) が現れる?

60. Catalogue of new Herbig Ae/Be and classical Be stars⋆
A machine learning approach to Gaia DR2Vioque et al. A&Ap, 638, A21 (2020)
学習データ
機械学習で Herbig Ae/Be を網羅的に探索
Gaia DR2, 2MASS, WISE, and IPHAS and VPHAS+G (0.59 μm), GBP (0.5 μm), GRP (0.77 μm), r (0.62μm), Hα (0.66 μm), J (1.24 μm), H (1.66 μm), Ks(2.16 μm), W1 (3.4 μm), W2 (4.6 μm), W3 (12 μm),and W4 (22 μm)変動の有意性variability

FG and e(FG) are the GaiaG band flux and its associated uncertainty
Heterogeneous variability

色の変動色に変換してから学習(主成分解析は12成分で99.99%説明)

教師
正確さ

既存のカタログ (Vinoque+18)

回収率

全体

既知

全体

位置精度の良いもの

8470 new PMS candidates

61. Thermal evolution of protoplanetary disks: from β-cooling to decoupled gas
and dust temperatures, Vorobyov et al (松木場, 大向) A&Ap, 638, A102 (2020)
円盤の熱進化の取り扱いを改善する.. 2次元 thin disk model
1.

β model (現象論)2.

β model + 照射3.

照射 +輻射冷却, Tdust = Tgas

4.

2温度モデル (輻射, 分子輝線)

TdustTgas

62. A Study of Millimeter Variability in FUor Objects,
Wendeborn et al., ApJ, 897, 54
NOEMA+Lowell discovery tel.

変光を１例発見V1735 Cyg

63-64 Non-ideal magnetohydrodynamics versus turbulence – I. Which is thedominant process in protostellar disc formation? II. Which is the dominant process
in stellar core formation? Wurster & Lewis, MNRAS, 495, 3795 (I), 3807 (II)
初期条件

1 MO, ρ = 7.43×10-18 g cm-3, R= 4×1016 cm, cs = 0.22 km s-1, B0 = 163 μG
L = 4 Rにwarm gas super-critical (μ0 = 5)
一様密度、一様回転、乱流、(α = 0.36)
SPH

106 + 5×105 (warm) particles

Non-ideal MHD

sink particle (racc = 1 au)(Ohm抵抗, 両極性拡散, Hall 効果)

原始星形成の後1500 年Non-ideal MHDの効果で円盤が形成される
Non-ideal MHD効果がないと初期磁場が強くなりすぎる65 The role of Galactic HII regions in the formation of filaments
High-resolution submilimeter imaging of RCW 120 with ArTéMiS,Zavagno et al (島尻)., A&Ap, 638, A7 (2020)

分解能 0.05 pc

内側p ≃ 2 and DFlat ≃ 0.08 ± 0.02 pc

Median radial profile

外側p ≃ 1.

フィラメントが(輻射により)圧縮されている。
HII 領域の外にあるフィラメント (前頁 紫)