Star Formation Seminar
News Letter No. 252, December 2013
From "Time Monitoring of Radio Jets andMagnetospheres in the Nearby Young Stellar Cluster RCoronae Australis” Liu et al.
To "Star Formation in Orion’s L1630 Cloud: an
Infrared and Multi-epoch X-ray Study” Principe et al.

Time Monitoring of Radio Jets and Magnetospheres in theNearby Young Stellar Cluster R Coronae Australis
Hauyu Baobab Liu (ASIAA) et al. ApJ, 780, 155 (2014)	

Karl G. Jansky Very Large Array 8–10 GHz 	(λ = 3.0–3.7 cm) monitoring observations	IRS7W, IRS7E: 近赤外線で最も赤く、電波で明るい。相対変動は小さい	

ClassI/II では 3.5cm の明るさと降着率の間に相関」	

Evidence of a discontinuous disk structure around the Herbig
Ae star HD 139 614
A. Matter (Max-Planck, Bonn) et al. A&A, 561, A26 (2014)

MIDI	

干渉計

モデル

✏r : Emissivity parameter

Resolved Imaging of the HR 8799 Debris Disk with HerschelBrenda C. Matthews (Hertzberg) et al. ApJ, 780, 97 (2014)A5V	

d = 39.3 pc	

multi planets	

r = 15, 24, 	38, 68 AU	

20 - 50 Myr

1. Warm inner disk, 2. Planetesimal belt (100-310AU), 3 External Halo (〜2000AU)

Fig. 6	Model fit

Fig. 3 Dust Temperature derived from SPIRE

Fig. 4 SED

波長ごとに	モデルを作成

星および内側の	円盤は「点源」

1. Warm inner disk, 2. Planetesimal belt (100-310AU), 3 External Halo (〜2000AU)

Signatures of infall
motions in the images ofthe molecular emissionof the G31.41+0.31 hotmolecular core	

J.M. Mayen-Gijon(IAA, Granada) et al. 	

MNRAS, 437, pp.
3766-3775 (2014)
Ultracompact H  II(UCHII) region
G31.41+0.31

Overlay of the integrated intensity (zero-order moment; contours) andthe intensity-weighted mean velocity (first-order moment; colourscale) maps of the ammonia (2,2), (3,3), (4,4), (5,5) and (6,6) main line
towards G31 HMC. Contour levels are 25, 30, 45, 60, 75, 90, 105, 120,135, 150, 165, 180, 195 and 210 mJy beam−1 km s−1.

VLA

Fig. 3 方位角方向に平均した強度分布

Observed intensity as a function of angular offset from the centre of G31.41 HMC, for different pairsof blueshifted (solid blue line) and redshifted (dotted red line) channel maps.

Mayen-Gijon J M et al. MNRAS 2014;437:3766-3775© 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society

HH 1050: a bipolar outflow in L 988 cloud	

T.A. Movsessian and T.Yu. Magakian (Byurakan)	

Astrophysics
An optical collimated outflow HH 1050 (L 988a) is studied.
With the usage of the 2.6 m telescope observations and thedata from catalogues and surveys, including the Hubble
telescope archive, its morphology is discussed and the bipolar
nature of the outflow is confirmed by spectral data. The
specific feature of the HH 1050 outflow is its propagation inthe wide cone with 30-40◦ opening angle, as well as thepresence of both moving condensations and shocked cloudlets.
The source of the flow should be one of the components ofte flr you(ngoul) 0.2 -0.2 ( lDynamical evolution of star forming regions	

Richard J. Parker (ETH Zurich) et al.	

MNRAS, 438, pp. 620-638 (2014)

Q = m̄/s̄

MST: minimum spanning treem̄ : mean edge distance of the minimum spanning tree	s̄ : normalized correlation length
hlaverage i+ 5/6 /lsubset⇤MSR =lsubset 1/6 /lsubset
h`aveage i ±average

MSR: mean separation ratio〜1 no segragation 	> 1 mass segragation	

< 1 inverese mass segragation

˜ subset⌃⌃LDR =˜ all⌃Fig. 1 subvirial (bound)Fig. 2 superbvirial (unbound)Fig. 6 Q vs ΣMST

Fig. 7 Q vs ΣLDR

The Atomic and Molecular Content of Disks Around
Very Low-mass Stars and Brown Dwarfs	

I. Pascucci (LPL, Arizona) et al. ApJ, 779, 178 (2013)

[NeII]H2

まとめ• [NeII] 12.8 μm はBD Diskの表面(T=5,000-10,000 K)から	

• H S(2), S(1) はBD Disk の warm 表面 (T =500 K)	

• C H /HCN の強度よび 柱密度の比は BD のほうが高い
222傾向	

SDC13 infrared dark clouds: Longitudinally collapsing
filaments?	

N. Peretto (Cardi) et al. A&A, 516, A83 (2014)

N2H

Kinematics of the ionized-to-neutral interfaces inMonoceros R2	

P. Pilleri (Los Alamos) et al. A&Ap, 561, A69 (2014)

CH+ 1-0 color	

[CII] black	

C18O while

化学モデル	と整合

Star Formation in Orion’s L1630 Cloud: an Infrared andMulti-epoch X-ray Study	

David Principe (Rochester) et al. ApJS	

X-rays among 52/87 YSOs 5/19 Class 0/I, 15/26 Class II	

11/21 transition, 21/21 ClassIII	Class 0/I only in hard band Class II, III detected also in soft band	

X-ray variability in timescale of years Class 0/I highly variable