SMA Observations of Class 0 Protostars: A High-Angular Resolution Survey of
http://arxiv.org/pdf/1304.0436
Protostellar Binary Systems
Chen1,2, H ́ector G. Arce2, Qizhou Zhang3, Tyler L. Bourke3, Ralf Launhardt4, Jes K. Jørgensen5, Chin-Fei
70 Xuepeng–Lee6, Jonathan B. Foster7, Michael M. Dunham2, Jaime E. Pineda8,9 and Thomas Henning4(観測と結果)(議論)

33個のClass 0 原始星のサーベイ
SMA (1.3mm & 850µm), median空間分解

MF (multiplicity frequency)=0.64 ± 0.08
→class I 天体の値の2倍程度(図)能2”.5→原始星進化と一緒にbinary具合も進化し21/33 →連星または複数連星ている？

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(天体のリストを次ページ)– 69 –

Source
Name

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

240240240240240240240
240240240240240
240
240
250
140
140
140
440
440
440
440
440
200
130
120
120
120
200
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
2036-60
40-84
30-72
20
< 56
34-41
74-117
48-61
< 59
35
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<4
0.5
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, 4
1, 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, 22, 14
1, 2, 4
4
1, 2, 4
1, 2, 141, 14
1, 2, 14
1, 2, 14
2, 15, 16L1389
IRAM 04191
L1521F/MC 27
IRAS 04368+2557

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

A Mechanism of Exciting Planetary Inclination and Eccentricity through a Residual
Gas 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)

図：色)最終的にiが40°に達した結Fig. 6.—
With different a2,0 and m2 , the left

果を出した系の外側惑星の初期ition ofthe outer planet (filled color contour)(結果) parameter study
縦：外側惑星の質量 横：外側惑星evolution (y coordinations of the star in Figu
例:a massive planet (10MJ) at 30AU with 6o inclinedの位置
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-ray
fluxes 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(結果とか)et al. 2012).
vestigate
the influence of the exISRFは太陽近傍の1000倍強くないと
on the thermodynamics of dense
合わないclouds,in an attempt to better
conditions
forformation in−14star
CRIRは10s−1(高い)ne. We adopt values for the internd →coolingがCO
the cosmic ray dominantではなく、ionisation rategher than those measured in solar
neutral O が効いてる。
ar clouds.
For more fundamental
mass,
dimensions, and turbulent
理由：宇宙線電離が強い→Heが電離he clouds, we take the values ford by→次の反応でCOが減る。
Longmore et al. (2012). In+ +O+He
cloudsin +thethe apparent
Fig. 1.— Column density, and mean gas and dust temperatures
CO+He
→CGC,
in our fiducial cloud setup (simulation ‘1’ in Table 1), with then G0.253+0.016 makes it an ideal
ISRF set at 1000 G0 , and the CRIR at 3 ⇥ 10 14 s 1 .
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,Filter
D. Lafreni ́eExp.
re2, time
R. Doyon2, A.
Riedel4,UT Date
Comments
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 adaptiveTAopmm
W
aroJ
aspstw
intaw
fothR2fr
poD
n0tho
re1o(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 ̈rnberger1
nonvariable stars
amplitude < 0.2 mag
amplitude < 0.5 mag
amplitude < 1 mag
amplitude > 1 mag
main sequence
30 Av reddening
0.3 mag excess line4

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

0012H-KFig. 3. JHK color–color diagram for 977 stars with K < 15 mag.
Nonvariable sources with combined errors <0.15 mag are shown ingray, the 136 variable sources with complete JHK data sets have colored symbols. The color codes for the K-variability are the following: amplitudes ≤0.2 mag red, ≤0.5 mag yellow, ≤1 mag green, and>1 mag magenta. The curve denotes the main sequence from M4 to B0(Ducati et al. 2001), the dashed lines correspond to reddening paths for
AV = 30 mag, and the dotted line marks the limit for K-excess sources.

Fig
RC20030wiing

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

2422.8-3423 in detail.
observationsof thecircumstellar
around PDS 66 and CRBR
ble 4.Mid-infrared
Most of them
are taken fromprevious
studiesdisksof CRBR
2422.83423
s. Forthe grain
size distribution we use the commonly
C. Gr ̈afe and S. Wolf
N distribution
by Mathis et al. (1977) and we fix the Table 5. Constraints on the inner-d
原始惑星系円盤２つを中間赤外線で観測
heightat 100 AU at a typical value of 10 AU (e.g., of the observed objects
望遠鏡：VISIR/VLT対象天体・波長：PDS66（Nband）と2012;
Sauter et al. 2009; Pinte et al. 2008).
Using the=CRBR
3(β −2422.8-3423(N,Q-band)0.5), which results from viscous accretion
TargetRin [AU]
kuraPDS&66Sunyaev 1973), and the given surface density
PDS 66< 15.0+0.5−0.5= α − β, the parameters α and β amountto 2.25~13Myrと年老いているが円盤がある。5× 10−9M⊙
yr−1降着
+0.5
<10.5
−1.0
espectively.
Theinnerdisk
radiusisusedasvariable
CRBR
2422.8-3423
CRBR 2422.8-3423
http://arxiv.org/pdf/1303.3417

ρ Ophiuchus, class I, 降着やアウトフローは見えていない. ice–w us a comparison with the observations, the simNotes. The uncertainties in the innerが受かっている
ges, that are constructed using the radiative transfer by the uncertainty in the disk inclinati
結論：innderdisk Wolf
hole の半径に制限(内側に穴があるとした(Wolfet al. 1999;2003),
areconvolved
withtheC. Gräfe et al.: Mid-infrared observations of the circumstellar disks around PDS 66 and CRBR 2422.8-3423
ing
standard star observations.
Following the method
ら、その穴の半径のupperlimitを決めた)
n § 4.1 a residual flux profile is determined for every
For both objects, the differenmage. If the disk is spatially resolved in the observa- star flux profiles is below the dete
reproduce the residual flux profile with the described icant extension of the star-disk syvarying the inner disk radius and thus determine the left and Fig. 5, left). Using ourhole radius of the object. For disks that could not be which inner-disk hole radius wesolved our model allows us to estimate an upper limit icant extension of the star-disk s-disk hole radius.
per limit to the inner-disk hole rato be smaller than 15.0+0.5−0.5 AU anCRBR 2422.8-3423, respectively
dopted modelFig.
parameters.
4. Left: Observed residual flux of PDS 66 including the determined detection threshold. Right: Modeled residual flux for several
inner-disk hole radii including the detection threshold.

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

観測領域:10 pc-long L1495/B213 complex in Taurus
観測波長:C18O(1–0), N2H+(1–0), and SO(JN=32–21) with the 14-m FCRAO telescope, + dust
continuum observations using APEX (870 μm) andIRAM 30m (1200 μm).
N2H+から19個のコアを同定
C18OのPosition-Position-Velocity spaceで３次元的なフィラメント構造を同定する手段を開発(FIVe:
Friends In Velocity).
結果、35のフィラメント構造を同定
長さ0.5pc, 単位長さ辺りの質量は温度10Kのcriticalline massくらいA. Hacar et al.: Hierarchical core formation in L1495/B213

Fig. 8. Central panel: FCRAO integrated intensity maps of the B211-B213 region in C18 O(1–0) (grey scale and black contours)
and N2 H+ (1–0) (red contours). Left and right panels: Spectra from selected positions illustrating the complex velocity structure ofthe emission. The blue spectra correspond to C18 O(2–1) and the red spectra correspond to the isolated (F1 F = 01–12) component of
N2 H+ (1–0) (multiplied by 3) observed simultaneously with the IRAM 30m telescope. Note the presence of 5 di↵erent C18 O peaks
in panel number 3.

4000

3000

2000

10000Δδ−1000

Δα (arcsec)

6.0
5.5
5.0
4.5Vlsr (km s−1)

6.5

7.0

7.5c) Step 3: Association−3000
4000300020001000

Δα (arcsec)

0−1000−2000−1000Δδ

secra(0c)1000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