Star Formation Newsletter No. 371 #36-47

花輪 知幸 (千葉大)fifi

36. The need for spatially resolved observations of PAHs in protoplanetary discs, Lange et al,A&A
37. β Pictoris b through the eyes of the upgraded CRIRES+, Landman et al. A&A
38. C I Traces the Disk Atmosphere in the IM Lup Protoplanetary Disk, Law et al. ApJL
39. Linking Circumstellar Disk Lifetimes to the Rotational Evolution of Low-mass Stars,Monsch et al. ApJ
40. Line pro les of forbidden emission lines and what they can tell us about protoplanetary
disk winds, Nemer & Goodman, ApJ
41. Identifying the population of T-Tauri stars in Taurus: UV–optical synergy, Nayak et al. J.
Ap & A
42. PDRs4All VI: Probing the Photochemical Evolution of PAHs in the Orion Bar Using
Machine Learning Techniques, Pasquini et al. A&Ap
43. Forming Giant Planets Around Late-M Dwarfs: Pebble Accretion and Planet-Planet
Collision, Pan et al, A & Ap
44. Insight into the Formation of β Pic b through the Composition of Its Parent Protoplanetary
Disk as Revealed by the β Pic Moving Group Member HD 181327, Reggiani et al. AJ
45. An HST Study of the Substellar Population of NGC 2024, Robberto et al. ApJ
46. Massive star-formation in the hub- lament system of RCW 117, Seshadri et al. MNRaS
47. Outcomes of Planetary Collisions: Importance of Gravity and Material Properties,
Smallwood et al. MNRaS

No. 38. C I Traces the Disk Atmosphere in the IM Lup Protoplanetary Disk, Law et al. ApJL, 959, L27[CI] 3P1-3P0 ALMA archival project 2015.1.01137.S (T. Tsukagoshi), Pascucci (2023, ApJ, 953, 183)
PA = 144°. 5, incl = 47°. 5, vsys = 4.5 km s−1, and M* = 1.1 Mo ΔR. A. = + 0 75 and Δdecl. = − 0 02,z0 = 0.515, ϕ = 1.457, rtaper, 3..917, ψ = 2.2

ModelCleeves et al. (2016, 2018)
Ipeak∫

I(v)dv

Tex = 50 K

No. 45. An HST Study of the Substellar Population of NGC 2024, Robberto et al. ApJ, 960, 49 (2024)
1.4 μm に H2Oの吸収バンド
赤丸(🔴 ) は系外天体
H2O吸収が見えない

青線は1 Myr 等時線

R=F139M, G=F130N and B=F105W.

電子カタログ (全測光天体 812, クラスター内の低質量星候補天体 397 [M, Av])

赤化の非線型性を考慮

ここまで丁寧に補正してもAvを過大評価した天体が多数出る。それらはクラスターの中心領域に集中している。
Appendixに興味深い形状の天体の画像

IRS1

光度関数

No. 37. β Pictoris b through the eyes of the upgraded CRIRES+, Landman et al. A&A
VLT CIRES+ λ = 2.06-2.57 μm, λ/Δλ 〜 104.

Forward modeling

惑星の位置でも 主星からのもれこみが100倍近く明るい。

CO2, CH4,HCN, NH3 はfi検出できなかった。

We nd a slightly sub-solar C/O ratio, v sin(i)= 19.9 ± 1.0 km/s, which gives a rotation
period of 8.7 ± 0.8 hours and a radial velocityof 31.9 ± 0.3 km/s in the barycentric restframe.No. 44. Insight into the Formation of β Pic b through the Composition of Its Parent Protoplanetary Disk as Revealed by theβ Pic Moving Group Member HD 181327, Reggiani et al. AJ 167, 45 (2024).
β Pic b の形成過程を調べるため、母体となった分子ガスの化学組成を探る
β Pic はA型星で化学組成に異常が見られ不適。同じmoving group の調べやすい星を分光して調べる。
K型星は変光が激しく不向き。M型は複雑。F型は2つだが、そのうち1つは自転が早い。良い候補は1つ。

HD181327 と β Pic b の化学組成も違う

No. 41 Identifying the population of T-Tauri stars in Taurus: UV–optical synergy, Nayak et al. J. Ap & A, 44, 83
Gaia-DR3 (distance, proper motion), GALEX GR6/7 (UV) with follow-up by Indian telescope
TTS19星新発見 11
分光で確認済み

Gomez de Castro (2015) のnew TTS の多く
は距離が TMCの範囲にない
７つは彼らのカタログと一致
明るい天体が抜けているのも不一致の原因

WD

Epslin & Lehman (2019) とは3天体が一致
可視光 CMD

紫外線 CMD

FUV 1528 Å, NUV 2310 Å

Epslin & Lehman (2019)

Bimodal distribution ? (Cf. Flemming+19)

d =130 pc と160 pc に2グループがあるらしい。
近い方が空間的にも速度的にもまとまっている。
Class II, III で差は見られない。
どちらも年齢は同じくらい。

No. 42 PDRs4All VI: Probing the Photochemical Evolution of PAHs in the Orion Bar Using Machine
Learning Techniques, Pasquini et al. A&ApJWST

3.2 - 3.6 μm

10.9 - 11.6 μm

他に 6.0-6.6 と 7.2 - 8.9 μm の波長域でもデータあり

No. 40. Line pro les of forbidden emission lines and what they can tell us about protoplanetary disk winds, Nemer & Goodman, to appear in ApJ

Bai+16

No. 46. Massive star formation in the hub– lament system of RCW 117, Seshadri et al. MNRaS, 527, 4244

No. 47 Outcomes of Planetary Collisions:
Importance of Gravity and Material
Properties, Smallwood et al. MNRaS

反発力だけ考慮すれば十分?
(Ki + Kj)(D − rij )fi

fi

22