The Star Formation Newsletter#301, 22-28
島和宏

#22 The evolution of young Hii regions
I. Continuum emission and internal dynamics

http://arxiv.org/pdf/1712.04735(< 0.01 pc)
ALMAで 9つの hyper- and ultra-compact HII regionsを観測-> 質量降着による大質量原始星進化の最終段階

を調べる(もしくは大質量星の pre-main-sequence 段階)
Red MSX Source (RMS) Survey が見つけた600個のHii regionのうち- ATCA & VLA でcompact (r<5”)- bolometric luminositiesが10^4 Lsun より大きいもの- 距離が3 ~ 5.5 kpc 以内に位置しているもの(expanding / rotating / infalling)
Hii regionでガス (ionised & molecular gas) の動きがどうなっているか？
-> high-resolution(~0.5”)で観測 (ALMA Band 6)- radio recombination line H29α
- molecular emission (CS, CH3CCH)- 256GHz continuum emission

G309.89+00.40

13:50:35.54

G330.28+00.49
G332.77 00.01
G336.98 00.18
G337.63 00.08
G337.84 00.37
G339.11+00.15

16:03:43.28
16:17:31.13
16:36:12.42
16:38:19.02
16:40:26.68
16:42:59.58

61:40:21.4
57.6
0.69
Targets near G335 (6 regions)
51:51:45.6
93.5
0.71
50:32:35.7
95.6
0.62
47:37:57.5
75.1
0.63
47:4:50.7
56.5
0.61
47:7:13.1
40.4
0.62
45:49:43.6
78.2
1.68

0.62

6.17

0.15

0.53
0.46
0.47
0.46
0.47
1.11

87.19
87.62
90.00
90.00
89.07
84.79

0.13
0.18
0.13
0.12
0.18
0.51

Table 2: Summary of radio properties of the Hii regions and their host molecular clumps. The luminosity in Column 7 is that of theHii region, and the final column gives the radio derived spectral index. For the targets which were not detected in all of the ATCA
and VLA wavebands in Urquhart et al. (2007, 2009), no spectral index (↵) was determined.
Source NameRA
(J2000)G302.02+00.25 12:43:31.49
G302.49 00.03 12:47:31.76
G309.89+00.40 13:50:35.54
G330.28+00.49 16:03:43.26
G332.77 00.01 16:17:31.13
G337.63 00.08 16:38:19.02
G337.84 00.37 16:40:26.68
G336.98 00.18 16:36:12.43
G339.11+00.15 16:42:59.58(a)Integrated Flux at 6 cm

Dec.
(J2000)62:36:13.7
62:53:59.6
61:40:21.4
51:51:45.9
50:32:35.7
47:04:51.0
47:07:13.1
47:37:58.0
45:49:43.6

Distance(kpc)
4.26±0.98
3.39±0.40
5.41±1.27
5.45±0.56
5.67±0.57
3.82±0.43
2.98±0.47
4.67±0.41
4.96±0.40

Log[Mclump ]
(M )
2.76
2.61
3.12
2.95
3.22
2.88
2.55
2.51
2.93

Table 3: Spectral Setup of the observed regions. The primarytargetted species of each spectral window are listed, with thenote that spectral windows 1 and 2 were combined to get thefull CH3 CN (J=12-11) k-ladder.
SPW
1

Freq
Species(GHz)
257.403 CH3 CN

N. Chan
3840

Vel. BW(km/s)
545.8

Vel. Res.
(km/s)
0.284

Log[LBol ]
(L )
4.16
3.75
4.40
4.13
4.16
4.01
4.59
4.43
4.24

Radio Size
(00 )
2.24
2.07
1.79
2.00
1.14
2.20
3.32
1.47
1.98

Flux(a) 6 cm
(mJy)
59.5
23.4
1.2
44.9
24.6
31
11.1
18
42.9

↵
0.03
0.03
···
0.08
···
0.01
0.63
0.52
0.04

and their implications are presented in follow-up papers. In thiswork, we focus on the continuum emission, ionised gas observed
within the Hii regions, and some of the small scale molecularemission (in CS and CH3 CCH) surrounding the Hii regions to
put the analysis of the ionised gas into context. Full analysis of
the molecular environments and the chemistry of these regions
is left to future work (e.g. Klaassen et al. in prep, van der Tak et
al. in prep).

H29αintegrated intensity(moment zero)

256GHz continuum
red: 5GHz
core: yellow

intensity weighted
velocity(moment one)“bulls-eye”-> infallingclumpiness
Jenas Length~2000 AU
(100K, 10^7/cc)< core separation

RRLs
H29α spectra
fit by Gaussian(no Lorentzian)

33Msun(@20K)

CS
no emission-> destroyed

VLSR = -37.1 km/s
Line Width = 11.4 km/s-> ne < 5x10^7 /cc(upper limit)
Fig. 1: Continuum, H29↵, and CS emission from G302.02. The top left panel shows the 256 GHz continuum in colour scale inwhich the 5 GHz emission is shown in red contours; the red contours in the other images represent this same 5 GHz emission forsimilar (to within 3 sigma of each other at 24.1 and 23.9 mJy/beam for the full and 12 m only data, respectively), however in the 12
m only dataset, we recover only 80% of the flux present in the full (i.e. including ACA) dataset.
Figure A.2 shows how the amplitude of the emission varies as a function of uv distance. Of note here is the overlapping uv
distances of the three configurations and generally consistent fluxes between configurations. The data are sampled well enough inthe overlap region to allow for proper combination of the datasets.
Appendix A.3: H29↵ emission

H29↵ was detected in most of our sources and on small enough scales to not require the use of ACA data. It was only detected in
the stand-alone ACA data for G302.02, which is the target with the brightest and most extended H29a emission. However, as shownin Figure A.3, the 12 m array data recover all the flux so it was not necessary to combine this data with the ACA data.
Table A.2: Clump positions, Areas, Derived Fluxes, Masses, and Column Densities
ID Number

1
2
3
ID Number
4
5
6
7
8
9
10
11
12
13
1
2
3
4
5
6
7
8
9
10

Peak RAPeak DEC
Area
Flux
Clump Mass (M )2(h:m:s)(d:m:s)(arcsec ) (mJy) (20 K) (50 K) (100 K)
A&A
no. EYH_Internal
3
G302.02 (1.00e+07
cm proofs:, 70.0manuscriptK)
12:43:31.50 -62:36:13.36
4.63
62.08
25.37
8.37
3.94
Table
A.2:
continued.
12:43:31.54 -62:36:17.68
13.45
81.48
33.29
10.99
5.17
12:43:30.71 -62:36:19.92
5.22
23.92
9.77
3.23
1.52
Peak RAPeak DEC
Area
Flux
Mass (M 0.29)
12:43:29.87-62:36:22.00
0.94
4.57
1.87Clump0.62(h:m:s)(d:m:s)(arcsec(20K) (50K) (100
12:43:32.33-62:36:16.80
0.75 2 ) (mJy)
3.01
1.23
0.41
0.19K)
12:43:30.92 -62:36:21.12
1.5
6.01
2.46
0.81
0.38
12:43:32.17 -62:36:18.32
1.39
5.57
2.28
0.75
0.35
12:43:30.41 -62:36:18.72
0.38
1.29
0.53
0.17
0.08
12:43:30.36 -62:36:21.28
0.3
0.83
0.34
0.11
0.05
12:43:31.23 -62:36:20.40
0.16
0.43
0.17
0.06
0.03
12:43:30.30 -62:36:22.08
0.09
0.23
0.09
0.03
0.01
12:43:32.52 -62:36:15.60
0.2
0.52
0.21
0.07
0.03
12:43:31.89 -62:36:14.40
0.11
0.27
0.11
0.04
0.02
3
G302.48 (1.00e+07 cm , 70.0 K)
12:47:31.80 -62:54:0.84
4.31
93.89
24.3
8.02
3.77
12:47:31.76 -62:54:3.32
6.84
73.15
18.93
6.25
2.94
12:47:31.97 -62:54:0.92
2.74
27.3
7.06
2.33
1.1
12:47:32.59 -62:53:57.72
1.5
8.32
2.15
0.71
0.33
12:47:31.31 -62:53:57.00
0.14
0.47
0.12
0.04
0.02
12:47:32.01 -62:53:59.32
0.2
0.62
0.16
0.05
0.02
12:47:32.44 -62:54:1.56
0.49
1.47
0.38
0.13
0.06
12:47:32.70 -62:53:59.96
0.13
0.4
0.1
0.03
0.02
12:47:31.35 -62:53:52.76
0.17
0.51
0.13
0.04
0.02
12:47:31.21 -62:53:54.28
0.17
0.46
0.12
0.04
0.02

Log(Column Density)(20 K) (50 K) (100 K)
24.41
23.93
23.6
23.79
23.31
22.98
23.77
23.29
22.96
Log(Column
23.62
23.14 Density)
22.81
(20
K) (50K) (100
K)
23.45
22.97
22.64
23.43
22.95
22.62
Articlenumber,page
19 of 25
23.41
22.92
22.6
23.32
22.84
22.51
23.18
22.7
22.37
23.12
22.64
22.31
23.09
22.61
22.28
23.07
22.59
22.26
23.04
22.56
22.23
24.69
24.21
24.14
23.68
23.28
23.21
23.18
23.15
23.14
23.11

24.21
23.73
23.65
23.2
22.79
22.72
22.7
22.67
22.66
22.63

23.88
23.4
23.33
22.87
22.47
22.4
22.37
22.34
22.33
22.3

#23 Stellar mass spectrum within massive collapsing clumps
I. Influence of the initial conditions
https://arxiv.org/pdf/1711.00316
B1++, 4 AU

IMF の傾きは何が決めるか-> density と turbulence を変化させてシミュレーションした (RAMSES + sink)
1000 Msun のコア
0.75 pc (~10^4 /cc)
0.084 pc (~10^7 /cc)
M=7
M = 22
A&A proofs: manuscript no. 31522corr
A1++, 9 AU

A1+, 19 AUC1+, 2 AU

Γ~0thermal support dominant
B1++, 4 AU

Γ ~ -3/4

turbulent dispersionD1,
dominant
2 AU
B1+, 8 AU#24 THE TOP-SCOPE SURVEY OF PLANCK GALACTIC COLD CLUMPS:SURVEY OVERVIEW AND RESULTS OF AN EXEMPLAR SOURCE, PGCC
G26.53+0.17
http://adsabs.harvard.edu/pdf/2017arXiv171104382L(< 14K)
TOP-SCOPE: Plank Galactic Cloud Clumps (PGCCs) の low temperature dust を観測-> 星形成の初期段階~2000 clumps with 12CO(1-0) & 13CO(1-0)~1000 clumps with 850μm continuum emissions

G26.53+0.17 (G26)
a filamentary infrared dark cloud

12CO(1-0) channel map
The TOP-SCOPE survey
The TOP-SCOPE survey

23

11

spatial filters (see section 6.2 in Appendix A for details).
R1 with a spatial filter of 20000 is very efficient to
identify dense clumps/cores and is used for creating
dense core/clump catalogues in our first data release to
the team. However, here we fit the SEDs with datasets
obtained from two other data reduction methods (R2,
R4 ), which use larger spatial filters (300 00 and 600 00 )and thus can recover more flux. We applied two sets of
SED fits (S1 and S2 ) using di↵erent datasets.
(1) S1: Herschel 160-500 µm data and SCUBA-2
850 µm data in the R2 data reduction (see section
6.2 in Appendix A) were used. The extended emission
larger than 30000 in the Herschel and SCUBA-2 maps
was filtered out.
(2) S2: Herschel 160-500 µm data and SCUBA-2
850 µm data in the R4 data reduction (see section
Figure 4. Spitzer/IRAC three color (3.6 µm in blue, 4.5
Spizer/IRAC
three
color
µm in green, and 8 µm in red) composite image of PGCC
6.2 in Appendix A) were used. The extended emission
Figure 14. Channel maps of J=1-0
of CO (gray scale images), CO (black contours), and C O (blue contours).
00 transitions
G26.53+0.71.
The yellow
contours represent
SCUBAyellow:
SCUBA-2
850μmthecontinuum
black:
13CO,
blue:andC18O,
red:contour
850μm
largerthan
600
Herschel
SCUBA-2
The
contour levels
for COare fromin
10% theto 90% insteps of 10% of thepeak intensity(8.2 K). Themaps
levels for CO are
1213

2 850 µm continuum emission with filtering out scales of

13

18

13

from 10% to 90% in steps of 10% of the peak intensity (3.0 K). The yellow circles mark the central massive clump. The yellow

(K)HCO+ J=1-0

13CO(2-1)PV図

H2 CO 21,2

(K)

(K)

(km s

) (km s) (km s3.56 0.74 15.70 11.69 19.60

48.98

1.04

0.15

49.07

0.93

0.06

The TOP-SCOPE survey

11,1 2.21 0.79 15.44 12.03 19.54

enough energy themselves to drive the envelope
ansion.
he virial mass of the clump MM6 considering turbuRV2vir
support can be derived as M
=
210(
)(
)
1
M
pc km scLaren et al. 1988; Zhang et al. 2015), wheres the radius (1.15 pc) and V is the linewidth
2 km s 1 ) of C18 O (1-0). The virial mass is
00 M , which is much smaller than the clump mass
100 Msun ), indicating that the whole clump may bein collapse. Therefore, the expansion revealed by
O+ J=1-0 and H2 CO 21,2 11,1 lines should be very
lized.
gure 22 shows a cartoon to describe the PGCC
based on the results from the present data. Our
ngs of G26 are: (i) The G26 filament may be
med due to large-scale compression flows evidenced
the temperature and velocity gradients across its
l cloud; (ii) Sub-filaments in G26 have di↵erent
cities and may interact with each other; (iii) The
ral massive clump where massive stars are forming
Figuregreen:
16.
diagrams of 13CO(2-1) Theline
still accrete
gasPosition-Velocity
along
sub-filaments;(iv)
systemvelocity,
49
km/s
emission. The contour levels are from 10% to 90% in steps ofsive clump
inthewholemayemission
bestill in global collapse
peak
10% of red:peakvalue (5.3
K). The green dashed vertical line
e its inner
seems velocity
to beofundergoingmarkspartthe systemic
49 km s 1 . Theexpansion
blueshifted)25

al. (2013) found that the CO abundance is strongly(anti-)correlated to other physical parameters (e.g., dust
temperature, dust emissivity spectral index, column
density, volume density, and luminosity-to-mass ratio),suggesting that the gaseous CO abundance can beused as an evolutionary tracer for molecular clouds.
Similarly, Giannetti et al. (2014) also found that lessevolved ATLASGAL-selected high-mass clumps seem
to show larger values for the CO depletion than theirmore evolved counterparts, and CO depletion increases
for denser sources. However, both studies in Liu etal.
(2013); Giannetti et al.
(2014) used singlepointing molecular CO data, which limited the accurate
determination of CO depletion in molecular clouds.
The molecular CO mapping survey data in the TOP
survey are more suitable for investigating how COabundances or CO depletion varies inside individual
molecular clouds and changes in di↵erent kinds ofmolecular clouds.
The upper panel of Figure 17 presents the spectra of13
CO (1-0), 13 CO (2-1) and C18 O (1-0) at the continuum
13
peak
for G26.22.
The This
CO cartoon(2-1) and shows
C18 O (1-0)
Figuretheemission
environment of PG
have aシリンダー
spatial distribution similar to that of the SCUBAG26.53+0.17. The main gas filament is shown in gre
2 850 µm continuum as shown in the lower panel ofThe17.SCUBA-2 filament is shown in yellow. Other sm
Figure18 ~6200 Msun,
are
shown
in red,and blue. PG~12pc,(500
Msun/pc)
Csub-filaments
O (1-0) emission
is opticallythin
in G26green,(see Table
locatedin afollowing
parent Liu
cloudwith veloc
2). G26.53+0.17
We derived C18 Oiscolumn
densities
etal. and(2013)
by assuming thatthe excitation
temperature
gradients
alongtemperature
theturbulent
east-west directi
isothermal,
non-magnetized18of CTheO (1-0)equalsclump
to the dust
temperature.
C18 O may be still
centralMM6(dashed The
ellipse)18
abundance
wasinnerderivedpartby comparing
the C
O
C 18 O ) its
collapse(Xwhile(color filled
ellipse)is undergo
column densities with the H2 column density map fromexpansion due to outflow feedback from the protostars. T
the SED fits with Herschel data and Planck+SCUBA-2
zoomed-in
the central
clump
is shown in the upp
data.
The C18 Opicturecolumnofdensity
map and
H2 column

nMedian RangeDp-value p-sig.
#25
fingerprints
of hot Jupiter planet formation
8.0 Chemical
4.1/100.32 0.03
0.31
42.7
12.5/95
0.16 0.64
0.13
http://arxiv.org/pdf/1712.01035
2.4
0.1/110.28 0.09
0.03
1.07
0.83/1.41
0.09 0.99
0.20
Hot Jupiterがどうやって出来たか
5656
5025/6704
0.19 0.41
0.13
9 -7.49-73.53/29.03 0.25 0.15
0.12-> in situ
formation
v.s.0.37
migration
7.61
6.6/8.57
0.24
0.05); 45 (G); 31 (K)D); 7 (R)Cool Jupiter もしくは Hot Jupiter を持つ

約100個の星の化学組成を詳しく分析

Fig. 4. [Fe/H] cumulative frequencies.

-> Hot Jupiter を持つ星は metallicity が高い(low metallicity で Hot Jupiter を持つ星はない)
Cool Jupiter と Hot Jupiter は形成プロセスが違う(Cool Jupiter が migration してきたわけでない)もしくは metallicity に依存するような
migration のモデルが必要#26 Shifting of the resonance location for planets embedded in circumstellar disks
http://arxiv.org/pdf/1712.04178

F. Marzari: Resonance shiftingourmodels the planets are also in apsidal resonance and the frediscポテンシャルを含めて2つの惑星の軌道共鳴を計算
350
quency of the apsidal longitude of the outer planet matches thatof the inner one. As a consequence, the secular system responds
300
in a unitary way to the disk perturbations.
6350

4250

Fraction of cases

No disk 2Pl
1 MMSN
1Pl+Disk
5 MMSN
2Pl+Disk

5300

Per. Long
Fractionof (deg)
cases

Crit. Arg. (deg)F. Marzari: Resonance shifting

200
3
150
2
100
1

50

0 0

07.9

8
1000

8.1
2000 8.2 30008.3
Semimajor
Timeaxis(yr)(au)

8.4
4000

8.5
5000

250

20200

No disk
1 MMSN
5 MMSN

150
16
100

12 50
8

0

0

0.4

0.8
Time (Myr)

1.2

Fig. 4. 4 Time evolution of the σ1 critical argument of the 2:1
resonance during the dissipation of the disk. The libration slowly
turns into
0 circulation (for both σ1 and σ2 ) as the density of the
8.15 leading
8.2 to8.25
8.3up of
8.35
8.4
8.45
8.5
gas declines
the breakthe resonance.
The initialvalue of Σ is equal to Σ1MMS
Semimajor
axis (au)N.

Fraction of cases

120
Fig. 5.
3. Evolution
Distribution
the ofinitialsemimajor
axes of ϖ
theinouter
withoftime
the pericenter
longitude
three
disk
Shift in the location of the resonance: Nosuper-Earths
planet ofmodels
a massive(mIn
m2 planets= 1MShave) trapped
in 5.3.
1 =J the
diﬀerent
as inpairFig.1.
this1Mcase
five and
木星と土星の2:1共鳴
2つのスーパーアース(地球質量の5倍)の2:1共鳴
1 MMSNa 2:1 Earthresonance
forrespectively,
diﬀerent valuesof innerthe diskΣ.
100 consider two planets whose masses
5 MMSN
threemasses,and theonegashas density
a semimaHere weare five and threeForhigherdensities
theresonant
regionisshiftedinwards.
The
jor discの質量を5倍にすると内側に移動
axis of 1 au. The disk potential causes a negative precession times->-> thediscの質量を5倍にすると外側に移動
Earth mass, respectively, with the more massive planet
volumeof thealsomutual
reducedand the sizeof thewhich adds
up phaseto thatspace
due toisthegravitational
perturba80 orbit. They are supposed to be trapped in resonancein the innerresonance
regionshrinks.
Thisisrevealedbythesmallerareaoftions of the planets. As a consequence, the circulation rate of during their type-I migration or formation process, like insidetheisGaussian
the histogram.
ϖ
negativecurvein thefitting
full modelwith two planets and the disk out growth.
60
Their masses are not large enough to open a gap
potential (red line), contrary to what
happensformassiveplanin the disk and for this reason we adopt for the disk potential
discの質量と惑星の質量に依存
ets within
a diskIt is alsooffastercomparedto thatobserved
There isalso gap.
a shrinking
the volume
in thephase
space Eq. 4 with40 both planets embedded in the disk. The precession
5
in
a
pure
three-bodyproblem
(blue
line)
and
for
a
singleplanetwhere stable resonant systems (at east over 1 × 10 yr) can be rate of the apsidal longitude due to the disk potential on a single(blackline).
planet is negative (black line in Fig. 5) and concordant with thefound forincreasing Σ. This reduction is 98% for Σ = Σ

#27 Planetary-like spirals caused by moving shadows in transition discs
http://arxiv.org/pdf/1712.09157

原始惑星系円盤のスパイラル構造はどうやって出来たか-> 惑星がなくてもできるのではないか
shadow を考慮したシミュレーションでもスパイラルができた
The Astrophysical Journal Letters, 798:L44 (4pp), 2015 January 10
The Astrophysical Journal Letters, 823:L8 (6pp), 2016 May 20

includes a blackbody radiative cooling. The code solves theNavier–Stokes, continuity, and energy equations on a staggeredmesh in polar coordinates (r, f). For detailed description of thecode see Masset (2000) and Baruteau & Masset (2008).
2.1. Code Units and Initial Setup
The simulations were run in code units, assuming the central
star mass, M0 = Må, and r0 = 1 au, as the units of mass andlength. The code unit of time, t0, corresponds to the orbital
period at r0 divided by 2π, that is t0 = (GM r03)-1 2 . The
gravitational constant is G = 1 in code units. The temperatureunit is GMåμmp/(kBr0), with μ being the mean molecularweight (μ = 2.35 in all our simulations), mp as the proton mass,
and kB as the Boltzmann constant. We adopt two values for the
disk-to-star mass ratio, q = 0.25 and 0.05.
Figure 1.TheSchematic
view with arbitraryof theparametricmodel
computational
domain orientationin physicalunits
extends
frompresented
inSection2.
The
centralstar
isplacedattheorigin.
The
outer
disk
lies
= 400
logarithmically spaced radial
r = 10–150 Marion
au over nr etal.inclination(2015)
in the x–y plane. The angle
α is the relative
between the midplane ofequallycells.
The
grid
samples2π
inazimuthwith
nf = 800
the outer disk and the plane of the inner disk. The dust mass density
distribution
is renderedallowedintofalse
outﬂowat theof the spaced
inner disksectors.
and outerGas
diskmaterial
sections arecolor. The
gapdisk
isedges.
shown devoid of material for simplicity. The inner disk is scaled up in size andTheinitialdensity proﬁle scales with r−1:
density forbettervisualization.

Marino, Perez, & Casassus

with Rs = 148 AU and where the azimuthal contrast in surface
et al. arateThe volume densityMontesinos
density isHeating
set to c = 10.0.
follows withstandard vertical Gaussian distribution:)
2 *Σg (r, φ)zρg (r, z, φ) = √
exp −
,
(5)
2H 2
2π H
with H (r) = 20.0(r/(130 AU))1.17 . The exact value of thisflaring exponent is not well constrained.
This parametric model also includes the effect of dust
trapping, following the procedure described in Birnstiel et al.
(2013) and Pinilla et al. (2012). However, the bulk of the opacity
in the H band is driven by particles well below the sizes required
for efficient aerodynamic coupling, and so the effects of dust
trapping in the outer disk are not relevant to this report. The
runs detailed in Section 3 confirm that the outer disk is opticallythick at the H band and that the scattered light does not trace thecrescent shape seen in the submillimeter.
2.1.1. Emergent intensities

Figure 1. Initial proﬁle for the stellar heating rate per unit area Qd+(r, f ) for a
3 shadows subtend 0.5 rad or 28°. 6. The plot is in log
modelwith radmc3d
Lå = 1 Le. The
We usefor radiative transfer computations (ver−1
scale with units erg s cm−2.

sion 0.38; Dullemond et al. 2014). Scattering and polarization
for the last scattering are treated with scatteringmatrices for our
5
Figure distribution
1 shows theinshadowsdustovera timescaleof 30
orbits.
different
species,each onewitha power-law

4Montesinos & CuelloFigure 2. Snapshots taken after 20 kyrs of disc evolution, of the pressure (top) and surface density field (bottom) for models withshadows rotating at diﬀerent periods: Ts = 1 (static), 5, 10 and 20 kyr.
Table 1. Set of simulations after 20 kyrs of disc evolution with shadows, for diﬀerent shadow’s rotating frequencies.

なぜスパイラルができるか

large pressure gradientsmall pressure gradientgasshadowgas
co-rotation point-> larger pitch angle-> small pitch angle

3

Guilloteau+1999#28 Morphology of the 13CO(3-2) millimeter emission across the gas discsurrounding the triple protostar GG Tau A using ALMA observatio

http://www.raa-journal.org/docs/papers_accepted/0225.pdf

ALMA でGG Tau Aを観測

GG Tau Ab1~ 0.38 Msun

Fig.
4 Left:Line brightness distribution (Jy beam−1 ); the red curve is a Gaussian fit to t
-dust
continuum
noise
peak. Right: Doppler velocity spectrum weighted by brightness and integrated over 8×-13CO(3-2)
arcsec2 (blue); the red histogram is obtained from the original by symmetry about the orig

GG Tau Aa~ 0.6 Msun

GG Tau Ab2~ 0.3 Msun

CO(3-2) emission across the disc surrounding protostar GG Tau A

n in multiple stellar system?

9

3

13
Fig. 5 Left:
Sky
map
of
the
CO(3-2)intensity
integrated intensity.
TheDoppler
black arrowvelocity
shows the p13CO(3-2) integrated
mean
sition of the hot spot in 12 CO(6-5) (Dutrey et al. 2014) and 12 CO(3-2) (Tang et al. 201
Map in theline
disc planeof the difference between the
integrated
inten-of the mean Doppler velocity (weighted by brightness) excluding the regi
Right:Sky map
emissioned over ω at the same r. The black circles show the maxima of therotation~R
3.1
contained in the scaled-down ellipse shown in the left
panel. Invelocity
both panels< km/s
2.5 arcs
mean radial integrated intensity distribution, r=1.22 and 1.87 arcsec
black
ellipses are the best fit to the distribution of < R > in the continuum data ale corresponds to the mean value of r in the dust andmap the(1.62
arcsec).

the product of the disc thickness by the sine of the tilt angle.

0o

We estimate the thickness of the disc by comparing the value
dust disc tilt : 32°of the smearingof tilt
theinner edge of the disc map near the
gas
disc
:
35°
o
8 of the ellipse with its value nearN.T.
P.N. Diep90&o A. Dutrey et270al.,
major axis
the Phuong,minor axis.
line integrated intensity v.s. R

180o

To 95% confidence level we obtain an
upper limit of 0.24 arcsec (34 au) for
the scale height H(r) at r=1 arcsec(140 au) where the Keplerian velocity
is ~3 kms−1; at 30 K, the soundvelocity is
0.5
kms−1
and
hydrostatic equilibrium implies
H(r) = 0.5/3 = 0.17 arcsec comparedminor axis (0°, 180°)
major
axis
(90°,
270°)
with
the
0.24
arcsec obtained above.
Fig.
Line emission. Dependence
on R (left panels) and on r (ri-> 9
discの厚みを反映-> キャンセル

grated intensity averaged in 60◦ wide angular sectors centred on6th
スケールハイト:H(r) ~ 0.24
arcsec(34 au) sectors and the rightmost panel
the leftmost panel
is forminor-axis
arcsec(140 au) in the
Keplerian
3 km/scentral valuesatofr ~ω1 are
indicatedinsertsvelocity:
for eachsector.