SMA Observations of Class 0 Protostars: A High-Angular Resolution Survey of
http://arxiv.org/pdf/1304.0436
Protostellar Binary Systems
Xuepeng Chen1,2, H ́ector G. Arce2, Qizhou Zhang3, Tyler L. Bourke3, Ralf Launhardt4, Jes K. Jørgensen5, Chin-FeiLee6, Jonathan B. Foster7, Michael M. Dunham2, Jaime E. Pineda8,9 and Thomas Henning4(観測と結果)33個のClass 0 原始星のサーベイ
SMA (1.3mm & 850µm), median空間分解
能2”.521/33 →連星または複数連星
50AU-5000AU
single/binaries/3/4 → 12天体/14/5/2
連星間距離と星周物質質量に相関なし– 69 –

SourceName

Other (or short)
Namea

AssociationRegion

Distance
[pc]

Lbol
[L ]

Tbol
[K]

Menv
[M ]

Class

Referencesb

L1448 IRS2
L1448 N
L1448 CPER 065
NGC 1333 IRAS 2A
NGC 1333 IRAS 2B
NGC 1333 SVS 13
NGC 1333 IRAS 4A
NGC 1333 IRAS 4B
IRAS 03282+3035
Per B1-c
Per B1-b
HH 211-MM
IC 348 MMS
CB 17 IRS
IRAM 04191+1522
L1521F-IRS
L1527 IRS
HH 114 MMS
OMC 3 MM 6
NGC 2024-FIR 5
HH 212-MM
HH 25 MMS
CG 30
B228
VLA 1623
Oph MMS 126
IRAS 16293–2422
L483
L723 VLA2
B335
L1157
L1251 B IRS1

IRAS 03222+3034
IRAS 03225+3034
L1448-mm
Per-Bolo 30
IRAS 2A
IRAS 2B
SVS 13
IRAS 4A
IRAS 4B
IRAS 03282
B1-c
B1-b

Perseus
Perseus
Perseus
Perseus
Perseus
Perseus
Perseus
Perseus
Perseus
Perseus
Perseus
Perseus
Perseus
Perseus
Isolated
TaurusTaurusTaurus
Orion
Orion
Orion
Orion
Orion
Isolated
Lupus
Ophuichus
Ophuichus
Ophuichus
Isolated
Isolated
Isolated
Isolated
Isolated

240
240
240
240
240
240
240
240
240
240
240
240
240
240
250
140
140
140
440
440
440
440
440
200
130
120
120120200
300
250
325
300

1.7-4.1
4.3-17
4.4-6.3
0.03-0.22
19-23
19-23
7-33
4.2-8.5
1.6-7.6
0.7-1.2
1.8-3.7
1.2-2.5
1.5-4.5
0.5-1.9
0.6
0.12-0.28
0.1-0.36
1.9-2.2
< 25
< 60
10
7.7-14
6.0-7.2
10-17
0.9-1.2
0.4-1.2
0.25
6.9-149-13
3-3.3
3.0-3.1
5.8-11
 10

43-63
53-90
49-69
31-37
50-69
50-69
30-180
34-51
36-54
33-60
53-76
< 25
24-31
49-59
> 55
18-36
20
36-60
40-84
30-72
20
< 56
34-41
74-11748-61< 5935
41-54
50-54
47-50
28-45
42-60
83-87

0.6-1.4
1.5-4.5
0.7-1.9
0.4-2.1
1.0-2.8
1.0-2.8
1.3-3.3
2.7-7.8
1.4-3.7
0.4-1.0
2.1-182.8-26
0.5-3.0
1.8-10<40.5
0.7-4.8
0.4-0.9
1.4-2.8
6-12
8.2-15
0.3-1.2
0.5-1.2
1.1-2.3
0.3-0.4
0.2-0.5
0.51
1.2-2.8
0.3-1.8
0.6-1.6
0.7-1.2
0.5-2.6
2.0-2.100/I00000/I
0000/I
0000/I
000/I
000000/I
00000/I
0000/I1, 2, 3, 41, 2, 3, 4
1, 2, 3, 4
3, 4
1, 2, 3, 4
1, 2, 3, 4
1, 2, 3, 4
1, 2, 3, 4
1, 2, 3, 4
1, 2, 3, 4
3, 4, 5, 6
3, 5, 7
1, 2, 3, 4
3, 4
8
1, 2, 9, 10
11, 12, 13
1, 2, 14
1, 2
1, 2
1, 2
1, 2
1, 2
1, 2
2, 14
1, 2, 4
4
1, 2, 4
1, 2, 141, 14
1, 2, 14
1, 2, 14
2, 15, 16

L1389
IRAM 04191
L1521F/MC 27
IRAS 04368+2557

BHR 12IRAS 15398–3359
IRAS 16253–2429
IRAS 16293
IRAS 18148–0440IRAS 19156+1906
IRAS 19345+0727
IRAS 20386+6751
IRAS 22376+7455

A Mechanism of Exciting Planetary Inclination and Eccentricity through a ResidualGas Disk
http://arxiv.org/pdf/1303.6736
Yuan-Yuan Chen, Hui-Gen Liu, Gang Zhao, and Ji-Lin Zhou

(背景)少なくとも8つ程度の逆行Hot Jupiterが見つかっている。
→その形成メカニズムは？（HJのinclinationを上げたい）→外側にもう1天体いて古在効果を起こしても難しい→3番目の天体(high inclination>39.2°)があると一番内側のHot Jupiterのinclinationをあげる(この論文)
2つの惑星+外側にガスが残っていたら内側のHJのiを上げれる(外のガスがvertical secular resonanceで惑星のiをあげる)(結果) parameter studyi

図：色)最終的にiFig. 6.—
With different a2,0 and m2 , the lefttion of the outer planet (filled color contour)

evolution (y coordinations of the star in Figu
例:a massive planet (10MJ) at 30AU with 6o inclined
to a massive disk (50MJ ) can finally enter the Kozailocations of the inner planet when Itot,max = 4

resonance with an inner Jupiter around the snowlinetions of the star in Figure 3a). The right pan

al. 2012; Longmore et al. 2013;
With both stronger backgroundthe temperature
structure of the Galactic Centre cloud G0.253+0.016
gher On
cosmic-rayfluxes comparedhttp://arxiv.org/pdf/1303.1978
Paul C. Clark1, star
Simonformation
C. O. Glover1,isSarah E. Ragan2, Rahul Shetty1 and Ralf Klessen1
neighborhood,higher volume and column densi(目的と手法)
a standard
giant molecular cloud). 銀河中心にある分子雲G0.253+0.016を想定したchemistry入りSPHシミュレーション。
is G0.253+0.016 (also referred toRadiation Field(ISRF)及びcosmic ray ionization rate(CRIR)の2
hichパラメータのうちInterstellar
displays both extremely highnsities,
yet very little sign of star
つを振って観測を良く再現するモデルを探した。
l. 1981; Lis et al. 1994; Longmore
実際の観測特徴：ダスト温度は19K(中心),27K(edge), ガス温度は~65-70K(kinetic)
he current
lack of star formation,s in this object are thought to be
red for the formation of massiveore et al. 2012).
vestigate the influence of the exon the thermodynamics of dense
clouds, in an attempt to better
conditions for star formation in
ne. We adopt values for the internd the cosmic ray ionisation rategher than those measured in solar
ar clouds. For more fundamental
mass, dimensions, and turbulent
he clouds, we take the values ford by Longmore et al. (2012). In
clouds in the GC, the apparent
n G0.253+0.016 makes it an ideal
the e↵ects of the environmental

P. Delorme et al.: Direct imaging of a 12-14 MJu

Direct imaging discovery of 12-14 Jupiter mass object
a youngbinaryobservations
systemTable 1. orbiting
Summary of theNACO (VLT-UT4)
of 2M0103AB (RA=01:03:35.63; Dec=-55:15:56.1).
of very low-mass stars
P. Delorme1, J. Gagn ́e2, J.H. Girard3, A.M. Lagrange1, G. Chauvin1, M-E.
Naud2,FilterD. Lafreni ́eExp.
re2, time
R. Doyon2, A.
Riedel4,UT DateComments
http://arxiv.org/pdf/1303.4525
L032⇥200⇥0.2=1280s
Seeing:M. Bonnefoy5, and L. Malo2
2012-11-25
2002-10-28

KSHJH

8⇥20=160s
8⇥20=160s
4⇥5=20s
5⇥10⇥2=100s0.700 -0.800
Airmass:
1.16-1.25
Archive data

直接撮像で惑星発見。
中心星：2MASS J01033563-5515561AB :M5型連星、距離47.2pc, ~30Myr, 連星距離12 AU
惑星：12-14Mj, 中心星から84AUの距離
観測：NACO survey, L‘バンド+JHK follow
up

Fig. 1. 2MASS0103(AB)b in November 2012, with NACO
in L0 band. The green arrow shows the position of the companion in 2002. The light-blue circle identifies the expected
position of the companion if it had been a backgroundsource.
ESO archive NACO H-band images of 2M0103, obtainedin October 2002 (run 70.D-0444(A)). These early images
were acquired in field tracking and with poor adaptive

TAopmmW
aroJ
aspstw
intaw
fothR2
fr
po
D
n0
tho
re
1o(TWo1fa
inisthNear-infrared variability in the star-forming region RCW 38
A&A 553, A48Mathias D ̈orr1, Rolf Chini1,2, Martin Haas1, Roland Lemke1 and Dieter Nu ̈rnberger14

赤外線変光観測。
3ヶ月NIRでRCW 38領域をモニターし3た。

Armazones,Chile)(結果)
139天体が10%以上の光度変動。

J-H

望遠鏡：80cm IRIS(Cerro21

そのうち47%はXやMIRの対応天体有り。
→NIRは変動天体を見つけるのに良いツールである。
cf) RCW 38
大質量星形成領域, 1.7kpc

0012

H-K

Disk-Related Bursts and Fades in Young Stars

http://arxiv.org/pdf/1303.3629

Krzysztof Findeisen1, Lynne Hillenbrand1, Eran Ofek2, David Levitan1, Branimir Sesar1, Russ Laher3 andJason Surace3

Palomar Transient Factoryというサーベイ結果。
波長帯：R-band(red)dayスケールから年スケールまで
14/186天体がバースト、29/186天体が減光。

Magnetically Active Stars in Taurus-Auriga: Photometric Variability and Basic
Physical Parameters
http://arxiv.org/pdf/1303.3037
K.N. Grankin1

ROSATでみたWTTSのX線光度変化
サンプル：28個のWTTSと60個のWTTS候補星
22/28のWTTSと39/60のWTTSの光度が周期的変動
周期；0.5-10日

Mid-infrared observations of the circumstellar disks around PDS 66 and CRBR
2422.8- 3423
C. Gr ̈afe and S. Wolf

http://arxiv.org/pdf/1303.3417

C. Gräfe et al.: Mid-infrared observations of the circumstellar disks around PDS 66 and CRBR 2422.8-3423

Cores, filaments, and bundles: hierarchical core formationin the L1495/B213
A. Hacar et al.: Hierarchical core formation in L1495/B213
http://arxiv.org/pdf/1303.2118
Taurus region
A. Hacar1,2, M. Tafalla1, J. Kauffmann3, and A. Kov ́acs4

A. Hacar et al.: Hierarchical core formation in L1495/B213

Assessing molecular line diagnostics of triggered star formation using synthetic obser- vations
http://arxiv.org/pdf/1303.1322
Thomas J. Haworth1, Tim J. Harries1, David M. Acreman1, and David A. Rundle2