Star Formation News Letter#298 1-5
⿇⽣有佑(ASIAA)We consider a non-magnetized, self-gravitating disk in theshearing box approximation. Accordingly, the disk is modeled
locally on a small radial-azimuthal patch of the disk,
transformed from global cylindrical coordinates (r, θ, f) to
local Cartesian coordinates (x, y, z) co-rotating with the disk
(Goldreich & Lynden-Bell 1965). These assumptions allow for
the modeling of the local properties of the disk while following
the evolution of fragments that form when using periodic
boundary conditions. Using this model, the relevant conservation equations are shown in Equations (3)–(5) with terms for
the Coriolis effect 2W ´ u and centrifugal force qWvx yˆ as wellas heating H and cooling terms C in the energy equation.

The fragmentation criteria in local vertically stratified self-gravitating disk simulations
Hans Baehr, Hubert Klahr, and Kaitlin M. Kratter

¶r
¶r
- qWx
+
¶t
¶y

· (ru) = fD (r)(3 )the most natural extension of that work and our res
The fragmentation criteria in local vertically stratified self-gravitating
disk simulations
their ﬁndings in this regard.
Hans Baehr, Hubert
Klahr,H.and
M.thatKratterの続きRecent work has focused on
numerical effecr =2/3
WithKaitlin
this, we ﬁnd
for an overdensity in our
frag

inﬂuence on non-convergence. Klee et al. (2017)
numerical oversteepening could be responsible foestimation of overdense peaks resulting in fra
Through our use of sixth-order hyperdiffusion,
expect oversteepening to be a signiﬁcant factor.
R3(2017) ﬁnd that dissipation of angular mowhich, for a protoplanetary disk around a solar-mass star,
SPH methods removes shear support from region
results in a densities of 1.2 ´ 10-10g cm-3 at 50 au andﬂow velocities and as this depends on resolution, fr
1.5×10−11 g cm−3 at 100 au. Comparing this with our
becomes easier with increasing resolution.
simulations and with the Roche density in Figure 7, we see that
While our results strongly suggest converge
this density threshold more adequately delineates between
lowest resolution fragmentation is suppressed duThe
AstrophysicalJournal,848:40(10pp),
2017
October
10Klahr, & Kratterfragments and non-fragments. A disk with the temperatures as
cient resolution for both 2D and 3DBaehr,
models,sim
results of Turk et al. (2012), which found th
in these simulations will have an aspect ratio H/R≈0.11 at 50
velocity ﬂuctuations suppressed the formation of
au and H/R≈0.16 at 100 au. With these densities and aspectmagnetic dynamos when the Jeans length is not reratios, we approximate threshold fragment masses of 5 MJ andleast 64 grid cells. At higher resolutions, the result
15 MJ at 50 and 100 au, respectively.
standard fragmentation scenario, with clear fragm
Applying the density threshold to our low-resolutionβ=2 and a lack of fragmentation evident at β=simulations, which failed to form sustained fragments as can
The β cooling prescription is not a true substitute
be seen in Figure 8, simulations with very short cooling times
cooling, only a simple parametrization of the(β = 1, 0.5) surpass this threshold. If the maximum density of aphysics. The use of a ﬁxed background term may ha
fragment can surpass this critical density for more than an orbit,
on convergence (Rice et al. 2012), thus one must be
it can be considered a fragment even if it is subsequently
convergence is not lost if this term is remov
disrupted. Thus, this threshold may provide a useful sink cell
Kratter 2016). However, as simulations using β
formation criterion for simulations with resolution too low tobackground irradiation converge, it supports our un
fragment.
Figure 9. Left: map of surface density from a low-resolution (N = 256 ) 3D run with efﬁcient cooling β=2. With such a short cooling timescale, this setup is
expected to fragment, but instead shows sheared self-gravitatingof
ﬁlaments
of gravitoturbulence. Right: map of surface density from a 2D simulation, which
thetypicalphysics.
similar to the 3D case fails to fragment, but is slightly clumpier due to the stronger self-gravity. The simulation shown on the right is the same as the models fromsimulations to withstand tidal disruption, as is shown in• 分裂の評価は２DではRoche⾯密Figure 7, it must satisfy
度だが、３DなのでpressureM
modified Hill条件。
r h . 25.57 * ,
(28)

3

3

Baehr & Klahr (2015), but scaled down to mimic the size and resolution of the 3D runs presented in this paper.

2017)

Deuterated methanol on Solar System scale around the HH212 protostar
E. Bianchi, C. Codella, C. Ceccarelli, V. Taquet, S. Cabrit, F. Bacciotti, R. Bachiller, E. Chapillon, F.
Gueth, A. Gusdorf, B. Lefloch, S. Leurini, L. Podio, K. L. J. Rygl, B. Tabone and M. Tafalla

A&A 606, L7 (2017)• prestellarでダスト上のCがD化分⼦にà原始星期に放出、つまり歴史を保存。
• さらに円盤形成のショックでも変化するので原始星の惑星形成領域を⾒たい。
observations are then crucial to measure the D/H ratio within
A.1. Examples of line profiles in T scale (not corrected for the
50–100 au from the protostar, that is, in the region hosting them dilution):
species and transitionsClassare reported. The0,
verticaldashed•
HH212,
Orion
(450
pc),
分⼦円盤(M*=0.2-0.3
R~60
protoplanetary discs. Mo,
Dust grains
and icesAU)。
may also be a↵ected
stands for the systemic V velocity (+1.7 km s , Lee et al. 2014).
by the accretion shock near the centrifugal barrier, therefore weand blue curves are for the Gaussian fit. In the spectrum of theBand
7,doublet
メタノール,
Cycle 1, 0.43 km/s,
0.4“; Cycle 4, 0.87 km/s, 0.15”
le 1•(1 –0ALMA,)A CH OH transition,a CH DOH
containdo not know the deuterium fractionation at small scales.
the (5 –5 )e1 and the (5 –5 )e1 transitions is also shown (see13CH
e A.1).
4 spectraOH
the (7 –6)A CH OH and the (8 DOHが12本、E–
The HH212 star-forming region in Orion (d = 450 pc) is an• In Cycle
5本、CH2
up=17-438 K、円盤形成領域で初検出。
SO transitions are also3
shown.
B

1

LSR

1,1

0,0

4,2

3,2

13

3

2

4,1

3,3

1,7

1,6

3

2,6

2

ideal laboratory for studying the jet-disc system. The HH212mm Class 0 protostar is driving a bright, extended, and bipolar molecular jet extensively observed using IRAM-NOEMA,
SMA, and ALMA (e.g. Lee et al. 2006, 2007, 2008,22015, 2016,2017a,b;Codella16‒2 et al. 2007; Cabrit et al. 2007, 2012). A molec17
ular disc was revealed2in HCO+ , C17 O, and SO emission, using
the first ALMA cycles with‒2
angular resolutions of ⇠000. 6. Velocity gradients have been detected along the equatorial plane consistent with a rotating disc around a 0.2–0.3 M protostar (Leeet al. 2014; Codella et al. 2014; Podio et al. 2015). A disc witha radius
60 au has indeed been imaged by Lee et al. (2017a),
A&A
606, L7of(2017)
who observed the dust continuum emission at 850 µm. Finally,
Codella et al. (2016) and Leurini et al. (2016) suggested that
HDO and CH3 OH emission is likely associated with outflowing
gas, and possibly with a disc wind. To conclude, the HH212 region is the unique Class 0 protostellar region where a bright jet,a compact rotating disc, and signatures of a disc wind have been
revealed. In this Letter, we exploit ALMA Band 7 observations
with an angular resolution down to 000. 15 to obtain the first measurement of methanol deuteration in the disc formation region.

• 13CH3OH過去のCH3OHでLTE回転温度、柱密度(CH DOHも)。
• 13CH3OH: (6.5±2.1)x10 cm , CH DOH: (1.1±0.2)x10 cm‒2。
Fig. 1. Left panel: HH212 protostellar system as observed by ALMA• 12C/13C=70とし、D/H=(2.4±0.4)x10
Band 7 (Codella et al. 2014). Blue and red contours plot the blue- andredshifted SiO(8–7) jet overlaid on the continuum at 0.9 mm (black con• IRAM, Perseus, Class 0ではD/H~0.5
tours). Positions are with respect to the coordinates reported in Sect. 2.
The filled ellipse shows the synthesised beam (HPBW): 0 . 61 ⇥ 0 . 45.
• Tdust~12 K in Perseus, >16 K in Orion。Orionのホットコアでも他より1桁低い。
Central panels: zoom-in of the central region as observed by ALMA-

A.2. Rotation diagrams for 13 CH3 OH (upper panel) and CH2 DOH
wer panel). An emitting region size of 000. 19 is assumed (see text).
parameters Nu , gu , and Eup are the column density, the degener-

•
•
•
•

2. Observations
HH212 was observed in Band 7 with ALMA using 34 12 m antennas between 15 June and 19 July 2014 during the Cycle 10000Band 7 Cycle 1: 13 CH3 OH(130,13 –121,12 )E and CH2 DOH(90,9 –81,8 )e0
integrated over ±4 km s 1 with respect to the vsys = +1.7 km s 1 , (black
contours and grey scale). First contours and steps are 5 for 13 CH3 OH
2 beam 1 km s 1 ) and CH2 DOH (35 mJy
2 beam 1 km s 1 ). The(15 mJy
130000
HPBWs are 0 . 52 ⇥ 0 . 34 (PA = 64 ) for CH3 OH and 000. 54 ⇥ 000. 35(PA = 65 ) for CH2 DOH. Right panel: zoom-in of the central region,as observed by ALMA-Band 7 Cycle 4, showing the 13 CH3 OH(121,11 –
120,12 )A emission integrated over 10 km s 1 around vsys (black contours
and grey scale). First contours and steps are 5 (20 mJy beam 1 km s 1 )and 3 , respectively. The HPBW is 000. 15 ⇥ 000. 12 (PA = 88 ).

CH DOHの北成分はSO のblue。
⾚、⻘、マゼンタとも90x45 AU。
±1 km/sの勾配はジェットと逆。
r~0.1“は円盤半径に近いので降着衝撃波か。
3. Results and discussion
3.1. Line spectra and maps

LkCa 15
TW HyaUX Tau A
V4046 Sgr

167
140
63
77

3.9
0.3
1.4
<0.1

0.25
0.04
0.27
<0.04

16.7
8.3
5.3
1.4

K3
K6
K2
K5

2.0
1.5
1.0
2.4
1.7

0.69
0.43
0.09
0.35
0.26

2.9
3.3
11.1
6.7
6.3

K4
M2
K7
K0
K7

No
No
No
No

Espaillat et al. (2010); Andrews & Williams (2005)
Torres et al. (2006); Weintraub, Sandell & Duncan (1989)
Herbig (1977); Andrews & Williams (2005)
Quast et al. (2000); Rosenfeld et al. (2013)

Chemical enrichment of the planet forming region as probed by accretion
Richard A. Booth and Cathie J. Clarke

EG Cha
TWA 7
V1086 Tau
V396 Aur
V397 Aur

Weak T Tauri stars
Mamajek et al. (1999)
Torres et al. (2006)
Herbig & Bell (1988)
Herbig & Bell (1988)
Steffen et al. (2001)

a The 1.3 mm flux has been renormalized to mJy at a distance of 140 pc.
bThe Si:N, Si:C and C:N hot gas line flux ratios are from Ardila et al. (2013).
c The 1.3 mm flux has been extrapolated from the 880 µm flux.

d The 1.3 mm flux has been estimated by extrapolating the far-infrared SED.
e The line profiles of the sources marked ‘Yes’ may be affected by outflows.

Accretion and chemical evolution

Figure 1. Flux ratios of Si, N and C normalized to the WTT sample mean against the flux at 1.3 mm normalized to the distance of Taurus (140 pc). The 1σ
deviations of the WTT sample are shown by the black dashed lines. Filled circles denote full discs, while large hollow symbols refer to sources with known
large cavities. Triangles denote upper limits. The sources with line profiles that may be affected by outflows are marked with stars. The spectral type of the
2. theBindingenergies and volume mixing ratios of chemical species adopted (from Madhusudhan, Amin & Kennedy 2014;sources is shown by point colour: M-stars are in magenta, F and G stars in cyan and K stars in black. Note that for the cavity source VTable
4046 Sgr,normalized
Booth
et
al.
2017).
Si/N ratio (0.03) lies below the bottom of the figure.

oaded from https://academic.oup.com/mnras/article-abstract/473/1/757/4157283
stitute of Earth Sciences, Academia Sinica user
November 2017

Species (X)N2473, 757–764 (2018)
MNRAS
CO
CH4
CO2
NH3
H2 O
Carbon grains
Silicates

Tbind (K)aCase 1b : X/H

Case 2c : X/H

770
850
1300
2575
2965
5700
–
–

0.5 × (N/H−NH3 /H)
0.45 (1 + fCO2 ) × C/H
0.45 (1 − fCO2 ) × C/H
0.1 × C/H
0.07 × N/HO/H – (3 × Si/H + CO/H + 2 × CO2 /H)
0
Si/H

0.5 × (N/H−NH3 /H)
0.65 × C/H
00.15 × C/H
0.07 × N/HO/H – (3 × Si/H + CO/H + 2 × CO2 /H)
0.2 × C/H
Si/H

a We use binding energies Collings et al. (2004), Garrod & Herbst (2006), Martı́n-Doménech et al. (2014) and Fayolle et al. (2016).

Chemical enrichment of the planet forming region as probed by accretion
Richard A. Booth and Cathie J. Clarke

762

R. A. Booth and C. J. Clarkeの続きNew binaries in the ε Cha association
Cesar Briceno and Andrei Tokovinin

New binaries in the ε Cha association
Cesar Briceno and Andrei Tokovininの続き

Figure 3. Images of six newly resolved binaries with faint companions displayed on an arbitrary negative scale. The separation is indicat
each image, the companions are marked by arrows. Cha-13 and TYC 9238-612-1 are average images in closed AO loop, the rest are SAA

イメージ

The Astronomical Journal, 154:195 (9pp), 2017 November

Briceño & Tokovinin

パワースペクトルTransitional Disk (TD). Murphy et al. (2フリンジか伸びで検出。
is variable in Cha-13, though the line pwide, with a 10% width of ~170 km s-1
accretion rate of ~10-11 M: yr-1. These
resemble those of other TDs, like
新しく⾒つかった連星(Espaillat et al. 2008). In addition toは10個。
(2013) ﬁnd a number of other emission
The Astronomical Journal, 154:195 (9pp), 2017 November
Briceño & Tokovinin
Cha-13, like He I, [N II]l6548 6583, [SFigure4.
Power
spectraofthree
resolvedclosebinaries
displayedontheTable 3others, leading them to suggest the gap• εChaの中⼼にある同名の三重連星。
Detection Limits for Unresolved Targets
logarithmic scale. The separation is indicated in the lower left corner; theby jet/outﬂow activity. Our discovery
inserts in the lower right corners show the central fragments
the ACFs.
• of外は反時計、内は時計回り。
Name
rmin
Dm (0. 15)
Dm (1 )
∼90 au raises the alternative interpretatio
(″)
(mag)
(mag)
related to the binarypair。
nature of the syst
• つながれたｘと□がouterHD 82879
0.04
1.6
5.1
1200 au , a companion can truncate th
in 2000. The subsystem Ba,Bb was also unresolved at SOAR in
CP-68 1388
0.04
2.2
4.8
A-Bはサブシステム(a,b)のせいでよ
TYC 9414-191-1
0.04
1.6
4.3
2014 and 2015, although at DJ = 0.3 mag it •shouldbe easily
separations of few tens of au, the di
RX J1123.2-7924
0.04
1.9
3.4
detectable. It is possible that the pair Ba,Bb becamecloser (itsfrom the inside (Manoj et al. 201
2MJ11432669-78...
0.10
0.9
2.2
ろよろしている。
Figure 3. Images of six newly resolved binaries
with faint companions displayed on 0.04
an arbitrary negative scale.1.7
The separation is indicated4.0
in the lower left corner of
RX J1147.7-7842
estimatedperiodis∼70years).
The
pair
AB
moved
very
littleChamaeleon I, Daemgen et al. (2016each image, the companions are marked by arrows. Cha-13 and TYC 9238-612-1 are average images in closed AO loop, the rest are SAA images with or without AO.
RX J1149.8-7850
0.04
2.1
4.3
•
サブはあと数年で周期が決まる。
its discovery in 1994; its estimated period is ∼400 years.
statistically signiﬁcant difference in
RX J1150.4-7704
0.04
1.8 Murphy et al. (2013)
4.6 also ﬁnd thatsinceTransitional Disk (TD).
Hα
2MJ11550485-79...
0.10
1.7 though the line proﬁle
3.3 itself is not very
is variable in Cha-13,
It is not a member of the association, but deﬁnitely a young
between single and binary systems;
consistent with a low
wide, with a 10% width
T Cha
0.04
2.4 of ~170 km s , 5.1
object;Murphyetal.
(2013)
attribute
it
to
the
Cha
I
group.
Itissystems with separations 1100 au show
accretion
rate
of
.
These
characteristics
closely~
10M
yr
RX J1158.5-7754B
0.04
2.0
4.2
•
連星率はG0か⼩質量では0.1
perspeciﬁcallyresemble those of other TDs, like CVSO-224 in OrionCXOUJ115908
0.10
2.2
2.3
of accretion activity. More
(Espaillat et al. 2008). In addition to Hα, Murphy etnot
al. featured in the Gaia DR1, so its true membership is still
HD 104237E
0.04
1.6of other emission lines
4.6 in their spectra of(2013) ﬁnd a number
TDs shows that close to 38% can b
difﬁcult to ascertain.
decade separation。矮星と同程度。
2MJ12005517-78...
0.04
1.4
II]l6548 6583, [S II2.6]l6716 6731, amongCha-13, like 2017年の⾃⼰相関
He I, [NFigure 4. Power spectra of three resolved close binaries displayed on theothers, leading them0.7
to suggest the gap may
HD 104467
0.04
6.1 have been cleared 11186-7936.
interactions between a close binary co
2MASS J11183572-7935548 (Cha 13,
logarithmic scale. The separation is indicated in the lower left corner; theby jet/outﬂow activity.
of a companion at•
A,
B型は全て。0.6
per decade
USNOB-120144-78...
0.10
2.0 Our discovery 2.9
inserts in the lower right corners show thecentral fragments of the ACFs.
∼90 au raises the alternative interpretation that the TD statusiswhile the remaining
proportion are likely
I=12.22
mag, M4.5) is a new 0 92 binary. Murphy et al.
CXOUJ120152-78...
0.10
2.0
3.2
related to the binary nature of the system. At separations of
RXJ1202.8-7718
0.04
2.5
4.5
(2013)
suspected
RV
variability,
which
might
mean
that
it
is
like
disk
photoevaporation,
grain grseparation。
1200 au , a companion can truncate the outer disk, while atin 2000. The subsystem Ba,Bb was also unresolved at SOAR in
J1204.6-7731
0.04
2.3tens of au, the disk
4.5could be truncated= 0.3
2014 and 2015, although at DJ RX
mag it should be easily
separations of few
triple, because thearcsec
new wide pair has a period of ∼2 kyr. In
interactions (Ruíz-Rodríguez et al. 20
detectable. It is possible that the2MJ12074597
pair Ba,Bb became closer (itsfrom the inside 2.5(Manoj et al. 2011).
0.10
3.6 Indeed, studying
estimated period is ∼70 years). The
pair
AB
moved
very
littleChamaeleon
I,
Daemgenetal.
(2016)
ﬁnd
that
there
is
a
Figure5.
Tentative
orbitsofthetriplesystem
òCha
with
axis
scale
in
their Spitzer
study
ofouter
Chamaeleon,
Manoj et al. (2011) classify
accretion activity and excess infrared
RX J1207.7-7953
0.04
2.6
3.9
since its discovery in 1994; its estimated period is ∼400 years.
statistically signiﬁcant difference in the (イラストnotaccretor arcseconds.
fraction
Only a fragmentof theorbit is forplotted; publication)
its wavy trajectory
yet
ready
RX J1216.8-7753
0.04
2.4 binary systems; in
4.6 particular, binary
It is not a member of the association,
but deﬁnitely a young
between single and
this
as
a
Weak-lined
T
Tauri
star
based
originate in one or two circumprimary
reﬂects
thestarwobblecausedby the inner subsystem.
Crossesandsquareson the modest Hα
RX J1219.7-7403
0.04
1.8 1100 au show a4.2
low ∼6% incidence
object; Murphy et al. (2013) attributeit to the Cha I group. It issystems with separations
connected to the orbit by dotted lines denote the measurements of the outerequivalent width of 11 Å reported in literature low
circumbinary disk? Has the gap in this Tof accretion activity.
a recent study ofemission24
not featured in the Gaia DR1, so
its true membership is still
2MJ12210499-71..
0.04
1.7More speciﬁcally, 5.1
-1

-11

:

-1

CN rings in full protoplanetary disks around young stars as probe of disk structure
P. Cazzoletti, E. F. van Dishoeck, R. Visser, S. Facchini and S. BrudererP. Cazzoletti et al.: CN rings in full protoplanetary disk

uscript no. cazzoletti_2017

in
ite
ze.

1)
in
200
re
he
m,
ow
l.

DR
er

Table 1: Parameters of the disk models in the main grid.
Parameter
Chemistry[C]/[H][O]/[H][N]/[H][PAH]
Physical structure
hc
Rc
Mgas
flargeStellar spectrum
T e↵
Lbol
LX
Dust properties
Dust
Other parameters
Cosmic-ray ionization
rate per H2External UV flux

Range
1⇥10 43.5⇥10 4
1.6⇥10 5
10 3 ISM abundance
1
0.1, 0.2, 0.3
0.1, 0.2 rad
60 AU
10 5 , 10 4 , 10 3 , 10 2 , 10 1 M
0.99
0.24000 K + UV ( Ṁ = 10 8 M /year),
10000 K1, 10 L
1030 erg s 1
0.005-1 µm (small)
1-1000 µm (large)
5 ⇥ 10 17 s 1
G0

an input gas and dust density structure, the dust radiative trans-

CN rings in full protoplanetary disks around young stars as probe of disk structure の続き
P. Cazzoletti, E. F. van Dishoeck, R. Visser, S. Facchini and S. BrudererFig. 5: Ray-traced images of the CN emission rings in models with 10 2 M , = 0.3, hc = 0.1 disks around a T Tauri and a Herbig
star. The ring in the Herbig disk is clearly more extended than that around the T Tauri star. The images are not convolved with any
beam, and the resolution is set by the size of the cells in the spatial gridding of the disk (⇠ 2.5 AU). For the ray-tracing, the disks
are assumed to be at a distance of 150 pc.

•
•
•
•

T TauriとHerbigで半径が違う。
hcは効かない。
ψが⼤きいかUVが強いと⼤きく明るい。
粒⼦サイズを変えても半径差は数AU。

P. Cazzoletti et al.: CN rings in full protoplanetary disks around young stars as probe of disk structure

Fig. 6: Comparison between the radial CN column density profile (blue) and intensity profile (red) for the two disks shown in Fig.
= 0.2, hc = 0.1 disk surrounding a T Tauri star assuming
5. The plots show how the emission ring follows the column density. The total gas column density is also plotted in yellowf as a= 0.1 and
0.8. In these models, the higher amount of small
large
reference.
grains in the disk atmosphere lowers the intensity of the FUV
v = -2 km/s

v = -1 km/s

v = 0 km/s

v = 1 km/s

v = 2 km/s

field. Accordingly, the high CN-abundance region is moved toeven higher altitudes in the disks where G0 /ngas is similar. As aconsequence, the CN column density decreases by a factor of < 2
for the flarge = 0.8 model and by a factor of ⇠3 for the flarge = 0.1
model. However, the integrated fluxes are only ⇠20% and ⇠30%
lower, respectively, and the sizes of the rings are similar in the
flarge = 0.1, 0.8 and 0.99 models within a few AUs. The fact thatthe flux di↵erences are so small is due to the high optical depthof the CN (N = 3 2) line studied here.

幅はhcの違い。TW Hyaのフラックス、半径を再現。

3.4. Excess UV from accretion

In order to further test the impact of the UV field on the CN

Fig. 7: Simulated observations of a Mdisk = 10 2 M , hc = 0.1, = 0.2 disk around a Herbig star, inclined of 60 . The imageflux
wasand distribution, we ran an additional set of models by
14: Integrated flux of the CN (N, J)=(3-2,7/2-5/2) emission varying the excess UV due to accretion onto a T Tauri star.
simulated using the tasks simobserve and simanalyze in the CASAFig.
software.
2

δ：Cのdepletion factorSo far, the T Tauri stellar spectrum was modelled as a 4000

in a disk with Mgas = 10 M , = 0.2 and hc = 0.1 as a function of the C and O depletion. The blue dot refers to the model
where a higher gas-phase carbon abundance than oxygen is assumed. All the fluxes are normalized to the non-carbon-depleted= 1 case. The fluxes vary of less than a factor of 2.

K blackbody spectrum with a UV excess for an accretion rateof 10 8 M year 1 . The excess accretion UV is modelled asa 10000 K blackbody on a 1.65 R radius star (Kama et al.
2016). The additional accretion rates considered are 10 7 , 10 9 ,10 10 M year 1 and a non-accreting blackbody spectrum, andwe investigate the e↵ects of the di↵erent UV excess on a disk
with Mgas = 10 2 M , = 0.2 and hc = 0.1.

• CNから質量はわからない。ß少し光学的に厚く、上層だけだから。
Fig. 9, on the other hand, shows the size of the ring as afunction of M . More massive disks haveArticle
larger rings.
Thepagedif- 5 of 12
number,• CやNが少なくても、破壊源のOも少なければCNの量は変わらない。
ference between T Tauri and Herbig stars is much more evident
The integrated flux and ring size as function of accretion ratediskhere than for the flux, hinting at a strong dependence of the CN
abundance on the FUV spectrum. In particular, disks surrounding T Tauri stars show rings with sizes ranging between 10 AU
and 50 AU while Herbig disks show rings extending to more thanare plotted in Fig. 11. The observed trends presented in Fig. 11
confirm the main di↵erences seen between T Tauri and Herbig
stars. Higher accretion rates corresponding to higher UV fluxes
show higher CN integrated emission. Moreover, the radius of the