星形成セミナー速報
2013. 9.20
fromViscous Evolution and Photoevaporation of Circumstellar
Disks due to External FUV Radiation Fields
toDIGIT: Herschel and Spitzer spectro-imaging of SMM3and SMM4 in Serpens
Star Formation News Letter 2013 August (No. 1-10)
花輪知幸

Viscous Evolution and Photoevaporation of Circumstellar
Disks due to External FUV Radiation Fields
Kassandra R. Anderson, Fred C. Adams & Nuria Calvet
ApJ 774 9 doi:10.1088/0004-637X/774/1/9
strong FUV in cluster

粘性が十分大きいな
ら、FUV により円盤全体が消失

G0 = 3000
G0 = 0 dashedLONG-TERM EVOLUTION OF PHOTOEVAPORATING
PROTOPLANETARY DISKSJaehan Bae, Lee Hartmann, Zhaohuan Zhu, Charles Gammie
ApJ, 774, A57

初期にゆっくり回転する(角運動量が少ない) コアが多ければ、光蒸発だけで 遷移円盤になる確率が20%であることを説明できる。

A non-LTE radiative transfer model to study ionizedoutflows and disks. The case of MWC349A.
A. Ba ́ez-Rubio, J. Mart ́ın-Pintado, C. Thum, and P. Planesas

A&Ap 553, A45 (16 pages)

MWC349A
電波再結合メーザー

Young stellar clusters in the Rosette molecular cloud
Argeuments against triggered star formation
L. Cambre ́sy, G. Marton, O. Feher, L. V. To ́th, and N. Schneider
A&Ap 557, A29

横軸d log( F )↵ =d log

Ks − 12µm

NGC2244 が最も古く、遠ざかるにつれ若くなると指摘されているが、反例も多い
The age of PL 03 is similar, but it is located beyond the influence of NGC2244. PL 05 is even older than these poten- tially triggered clusters, withabout 6.1 × 105 yr. Going farther, PL 06 and PL 07 are older at more than 1Myr and may even have formed at the same time as NGC 2244. Schneider
et al. (2010) and Hennemann et al. (2010) argue that PL 07 would be theyoungest cluster in the RMC, but their age classification was determined ina preliminary way and with lower quality statis- tics. We agree that there
are young protostars in this cluster, but the relevant age that determines thebeginning of the collapse is the one of the oldest population of the cluster,
not the youngest. The collapse of the more distant clusters, REFL 09,CMFT 10, and CMFT 11, are similar to PL 04 whereas they are definitely
out of reach of the OB stars in NGC 2244. We cannot rule out thepossibility that some cluster formation has been triggered by NGC 2244,
but it cannot be true for those at greater distances that are within the sameage range. The overall picture favors the Heyer et al. (2006) claim also
supported by Schneider et al. (2012) of a dynamical evolution of the wholecloud with a very minor triggering effect, if any.

CEN 34 – High-Mass YSO in M 17 or Background Post-AGB Star ?
Zhiwei Chen, Dieter Nu ̈rnberger, Rolf Chini, Yao Liu, Min Fang, and Zhibo Jiang
A&Ap 557, A51
CEN34 = B358
K(2MASS) = 7.88
B = 22.8, V18.8
class II/III vs Post AGB
λ = 8375-8770 Ålate F - mid G
luminosity class II, or I
Teff = 5250 K, log g = 2.0
CO bandhead abs.
early K giant or mid G supergiant
radial velocity
vr = −57±6 km/s (CaII/CO),−64 km/s (CO)+29.4 km/s (O stars in M17)
+20 km/s (MC)
銀河回転では説明不可能

問題点:High mass PMS in M17
M17からの脱出。
1000年でほとんど降着し、現在は星周物質がほとんどない
G Supergiant 距離は 2.5-4.5 kpc

Stellar and circumstellar properties of visual binaries in theOrion Nebula Cluster
S. Correia, G. Ducheˆne, B. Reipurth, H. Zinnecker, S. Daemgen, M. G. PetrGotzens, R. Ko ̈hler, Th. Ratzka, C. Aspin, Q. M. Konopacky, and A. M. Ghez

A&Ap 557, A63

Fig. 5
Fig. 1 K-band & L’-band
Gemini North (no rel. motion)

JHKL photometry
R5000 K-band spectroscopy

スペクトル型は決め方により異なる。

Baraffe et al. 98

Siess et al. 00

binary は coeval

Palla & Stahler 99

質量比分布は 領域によらない

ONC では mixed pair が多い傾向

Berkeley 94 and Berkeley 96: Two Young Clusters with Different
Dynamical Evolution
A. J. Delgado, A.A Djupvik, M.T. Costado and E.J. Alfaro
MNRaS doi: 10.1093/mnras/stt1311
Fig. 2Ber94

Ber963°Fig. 1 60µm (R), 25 µm (G), 12µm (B)UBVRCICHαJHKs Nordic Optical TelescopeBer94

Ber96

Fig. 5Fig. 6
Fig. 4 ZAMS, t = 1 Myr, 10 Myr
log t = 6.6, 7.0, 7.4, 8.0

Ber 94

Ber 96

MS+PostMS

PMSR

NIR excess

Cartwright & Whitworth 04
Ber 96
Ber 94Q = m̄/s̄m̄ : mean edge lengths̄ : normalized correlation length

B96 t = 10 Myr, B94 = 30 Myr
NIR excess stars are low mass ends
mass segregation
B94: warm collapse
B96: cold collapse

質量順での星Photometric Determination of the Mass Accretion Rates of PreMain Sequence Stars. IV. Recent Star Formation in NGC 602
Guido de Marchi, Giacomo Beccari & Nino Panagia
ApJ 775 A68
HSTV (F555W)
I (F814W)
Hα (N658N)

赤化補正したデータ

0.4−2.5M⊙

galaxy

Pre-main sequence stars older than 8 Myr in the Eagle Nebula
Guido De Marchi, Nino Panagia, M. G. Guarcello, and Rosaria Bonito
MNRaA (in press)

NGC6611 clusterには t > 8Myr でガス降着が盛んな円盤が付随した天体が存在する。
RWE = red stars with IRexcess
BWE = blue stars withIR excess
BVIJHK 3.6, 4.5, 5.8 and 8.0 µm
地上, 2MASS, Spitzer

DIGIT: Herschel and Spitzer spectro-imaging of SMM3 andSMM4 in Serpens
O. Dionatos, J. K. Jørgensen, J. D. Green, G. J. Herczeg, N. J.
Evans II, L. E. Kristensen, J. E. Lindberg, and E. F. van Dishoeck
A&Ap in press• 目的: 暖かい core でのCO/H 比を測る
• 励起温度 T(CO), T(H )〜300K & 1000 K, T(H O),
222T(OH)=100-200 K, r = 10”-20”•• Outflow によるJ-shockでの解離を考えれば単一励起
n(CO)/n(H2) = 10-4 (warmer) - 10-5 (hotter)
温度で多くの輝線を説明できる

Fig. 5 連続波 背景は70μm(protostar), 緑 450 μm
80, 130, 180 μmの明るい場所は oﬀset
Fig. 11CO J=18-17(black)
J=3-2
blue-shifted
red-shifted
Fig. 1 観測領域 Spitzer(□), Herschel (＋)

shock excitationin outﬂows

Fig. 6 CO SMM3

Fig. 13 blue, center, red

Fig. 7 CO SMM4

Fig. 13 blueFig. 17 warm 300 K &hot 1000 K
J shock
解離衝撃波