Star Formation NewsletterNo. 314 31-40
高橋実道（工学院大学）

Draft version January 16, 2019
Typeset using LATEX twocolumn style in AASTeX62

31

The Disk Substructures at High Angular Resolution Project (DSHARP):
II. Characteristics of Annular Substructures MNRAS 000, 1–?? (2018)

Preprint 8 January 2019

Compiled using MNRAS

1
1
2
3
4
Jane Huang,
Sean
M.
Andrews,
CornelisP.
Dullemond,
AndreaIsella,Laura
M.
Pérez,MNRAS 000, 1–?? (2018)
Preprint 8 January 2019using MNRASL TEX style file v3.0
The Disk 1Substructures
at HighAngularResolution
Project (DSHARP):5, 6
7 Compiled
7
8
9, 10
Viviana V. Guzmán,
Karin
I.
Öberg,Zhaohuan
Zhu,
Shangjia
Zhang,
Xue-Ning
Bai,
MyriamBenisty,c ESO 2019
Astronomy & Astrophysics manuscript no. 34556corr
III. SpiralContinuum of the EliasRicci,
27, IM
112019 Structures in the Millimeter13 Lup, and WaOph
3 6 DisksFebruary 5,
long-term
activity
Tilman Birnstiel,
John M. Carpenter,5 A. Meredith Hughes,12 Luca First
Erik Weaver,and study of AU Microsco
1
1
1
2
David
J.
WilnerJane Huang, Sean M. Andrews, Laura M. Pérez, Zhaohuan Zhu,3 Cornelis P. Dullemond,4 Andrea Isella,5First
long-term
activity
study
of
AU
Microscopii:apossiblechromosphericcycle.
6, 7
8
9
10
10, 11MyriamBenisty,
Xue-Ning
Bai,
TilmanBirnstiel,John
M.
Carpenter,
Viviana
V.
Guzm
án,
1 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, United States of America
12
1
13
1
3
A.
Meredith
Hughes,Karin
I.
Öberg,
Luca
Ricci,DavidJ.
Wilner,andShangjiaZhang
2
possible chromospheric cycle.

32

A

33

Zentrumfür Astronomie,
Heidelberg
UeberleStr. 2, 69120
Heidelberg, Germany
Water
delivery by
pebbleUniversity,
accretionAlbert
to rockyplanetsin habitable
3 Department of 1
1⋆
Physics
and Astronomy,
Rice
University,
610060Main
Street,Houston,TX
UnitedStatesof A.
America
Harvard-Smithsonian
Centerfor
Astrophysics,
GardenStreet,Cambridge,
MAIbañez02138,
UnitedStatesofP.America
Buccino1,2, M. Flores3,4, C. I. Mar
R.77005,
V.
Bustos†,zones
in evolving
disks
2 Departamento de Astronomı́a, Universidad de Chile, Camino El Observatorio 1515, Las Condes, Santiago, Chile
4 Departamento
Universidad
de Chile,El
1515,
Las Condes,
Santiago, Chile5
1,2 Camino
3,4 Observatorio
3
1⋆
2
Shigeru, Takeru
Yamamura
and Satoshi
Okuzumi1
1,2
P.1Buccino, M. 2Flores, C.
I. Martinez
R.deV.Astronomı́a,
Ibañez Bustos†, A. Ida
D.
Maizel,SergioMessina
and
P.
J.
D.
Mauas
3 Department
5 JointofALMA
PhysicsObservatory,
and Astronomy,
University
Nevada,Las3107,
Vegas,
4505 S. Santiago,
Maryland Pkwy,
AvenidaAlonsoofde
Córdova
Vitacura,
Chile Las Vegas, NV, 89154, USA
1
51,2
1 Instituto de Astronomı́a y Fı́sica del Espacio (CONICET-UBA), C.C. 67 Sucursal 28, C1428EHA-Bue
D.1 Earth-Life
Maizel, Sergio
Messina
P. J. D.
Mauas
Science
Institute,Tokyo Instituteandof Technology,
Meguro-ku,
Tokyo 152-8550, Japan
4 Zentrum
6 Instituto de Astrofı́sica,für
Astronomie,
Heidelberg
University,
AlbertUeberleStr.
2, 69120
Heidelberg,
Germany Chile
Pontificia
Universidad Católica de Chile, Av. Vicuña Mackenna 4860,
7820436
Macul, Santiago,e-mail:ida@elsi.jp
1 Instituto
2
2 Departamento de Fı́sica. FCEyN-Universidad de Buenos Aires, Buenos, Argentina.
de Astronomı́ay Fı́sicadel Espacio(CONICET-UBA),
C.C.
67 Sucursal
28, C1428EHA-Buenos
Aires,
Argentina.
Departmentof Earth andPlanetary
Sciences,Tokyo InstituteofTechnology,
Meguro-ku,
Tokyo
152-8551,
JapanHouston,
7 Department of5Physics
DepartmentofPhysics
andAstronomy,
Rice
University,
6100
Main
Street,States ofAmericaand Astronomy, University of Nevada, Las Vegas, 4505 S. Maryland Pkwy,TX
Las77005,
Vegas,UnitedNV, 89154,
USA
2 Departamento de Fı́sica. FCEyN-Universidad de Buenos Aires, Buenos, Argentina.
6 Unidad Mixta
3 Instituto de Ciencias Astronómicas, de la Tierra y del Espacio (ICATE-CONICET), San Juan, Argen
8 InstituteInternacional
Franco-Chilenade Astronomı́a,
CNRS/INSU
UMIUniversity,
3386,
Departamentode Astronomı́a,
Universidad defor Advanced
Study
and
TsinghuaCenterfor
Astrophysics,
TsinghuaBeijing
100084,China
DRAFT:
February5,
2019
3 Instituto de Ciencias Astronómicas, de la Tierra y del Espacio (ICATE-CONICET), San Juan, Argentina.
Camino El Observatorio 1515, Las Condes,4 Facultad
Santiago,
ChileExactas, Fı́sicas y Naturales, Universidad Nacional de San Juan, San Juan, Arge
9 Unidad Mixta Internacional Franco-Chilena Chile,dedeCienciasdeAstronomı́a,
CNRS/INSU
UMI
3386,
Departamento
Astronomı́a, Universidad de
ABSTRACT
4 Facultad de Ciencias Exactas, Fı́sicas7y Naturales, Universidad
Nacionalde SanJuan, San
Juan, Argentina.
Univ.
Grenoble
Alpes,
CNRS,
IPAG,
38000
Grenoble,
France5 ChileChile, Camino El Observatorio
1515,
Las
Condes,Santiago,
INAF-Catania Astrophysical Observatory, via S. Sofia 78, 95123, Catania, Italy
5 Context.
The oceanmass of Observatory,
the Earth is only
2.3Sofia⇥ 1078,4 ofthe wholeplanetmass. Even including water in the interior, the water
8 Institute
INAF-Catania
Astrophysicalvia
S.
95123,
Catania,
Italy
for
Advanced
Study
andTsinghuaCenterfor38000
Astrophysics,
Tsinghua
University, Beijing 100084, China
10
3
2
IPAG,
Francefraction would be atUniv.
most 10 Grenoble
10 . AncientAlpes,
Mars may CNRS,
have had a similar
or slightly
smallerGrenoble,
water fraction. Whatcontrolled the
9 Universityamountof water in theseFaculty
planets has not
beenclear, althoughseveral models have been proposed. It is importantMünchen,
to clarify the control
Observatory,ofPhysics,
Ludwig-Maximilians-Universität
Scheinerstr.
1,
81679 Munich,Germany
11 University Observatory,
FacultyofPhysics,
Ludwig-Maximilians-Universität
München,Scheinerstr.
1,
81679
Munich,Germany
mechanism to discuss water delivery to rocky planets in habitable zones in exoplanetary systems, as well as that to Earth
Mars in2018 May 2th
LastandupdatedLast
updated
2018
May
2th
10
our solar system. Joint ALMA Observatory, Avenida Alonso de Córdova 3107, Vitacura, Santiago, Chile
12 Department of Astronomy,
Vanwater
Vleck
Observatory,
Wesleyan
University,
Fossorbits.
HillWeDrive,
Middletown, CT 06459, USA
Aims. We considerdeliveryto planets by icy pebbles
after the snowline
inwardly passes96
planetaryderive the water11de Astrofı́sica,
Pontificia
Católicade Chile,
Av. that
Vicuñamass
fraction ( fwater ) of the
final planet as Universidad
a function of disk parametersand discuss
the parameters
reproduceMackenna
a small value of 4860, 7820436 Macul, Santiago, Chile
13 Department of Instituto
Physics
andAstronomy,
California
State
University
Northridge,
18111
Nordho↵Street, Northridge, CA 91130, USA
fwater comparable to that inferred for the Earth and ancient Mars.
12 Department
Van
Vleck
Observatory,
University,
96byFoss
Hill Drive, Middletown,
CT 06459, USA
ABSTRACTABSTRACT
Methods.of
WeAstronomy,
calculated the growthof icydust grains
to pebbles and theWesleyan
pebble radial driftwith a 1D model,
simultaneously
the snowline migration and dissipation of a gas disk. With the obtained pebble mass flux, we calculated accretion of icy
13 DepartmentsolvingofPhysics
Astronomy,
California
State
Northridge,
18111
CA targets
91130,toUSA
M stars
are ideal
targets
to ofsearchforUniversity
Earth-like planets.
However, theyusu- Nordho↵ Street, Northridge,
M stars are ideal
search for Earth-like planets. Hopebbles onto planetsand
after thesnowlinepassagetoevaluate
fwaterthe planets.

36
37
38
39

01.01433v1 [astro-ph.SR] 5 Jan 201935
1901.01433v1 [astro-ph.SR] 5 Jan 2019[astro-ph.SR] 15 Jan 201934

ABSTRACT
ally have high levels of magnetic activity, which could aﬀect(t = t ) of the snowline passage of the planetary orbit. Because M decays rapidly after the pebble formation front reaches the
The Disk Substructures
AngularResolution
Projectused
ALMA
disk outer edge (at t = att ), Highfis sensitivetothe ratiothet detection/t , whichofis exoplanets
determinedbythe diskparameters.
We findt to/t map< 10 the 1.25 millimeter
andmake
diﬃcult
orbitingaroundthem.
UnforABSTRACT
and make diﬃcult the detection of exoplanets orbiting arouor > 10 is important. By evaluating M analytically, we derive an analytical formula of fthat reproduces the numerical results.
continuum ofWe
protoplanetary
disks
at
a
spatialresolution
of
⇠
5
au.
We
presentasystematic
analysis
tunately,
long-termof dM stars has
notbeen
extensively
studied,Conclusions. Using the analyticalformula,we
findthat variabilityfpresent an analysis of ALMA 1.25 millimeter continuum observations of spiralstructuresintunately,
long-term variabilityof dM stars has not been ext
due18
to their
low intrinsic brightness.
For thisreason, in 1999
westartedtheof annular
substructuresinthesingle-disk
systemstargetedinthissurvey.
No
dominantarchi40three
protoplanetary disks from the Disk Substructures at High Angular ResolutiondueProject.
The brightness. For this reason, in 199
to their low intrinsic
HKα project,which systematicallyobserves
the spectramorphologies
of a large number are observed. Annular
tecture emerges
from
this
sample;instead,remarkably
diversedisks around Elias 27,of IM
Lup,
and
WaOph
6
were
observedataresolution
of
⇠
40
60
mas
(⇠
6
7
HKα
project,
which
systematicallyobserves the spectra ostars,
inparticulardMstars,
attheComplejo
Astronómico
El
Leoncito
substructures
virtuallyany
where
millimeter
continuum withemissionis detected
andau).can
Alloccurthreeatdisks
featurem radius= 2 spiralpatterns
in conjunction
annularsubstructures.
Gas
Results. We find that fwater is regulatedby thetotal
massof(Mmagnetic
materials
preserved
the outerregions at the timingres ) of icy dust
ally havehighlevelsactivity,
which
could inaﬀect
theirdisk
habitability
snow

res

p↵

water

snow

res

p↵

water

water

snow

p↵

34

Water delivery by pebble accretion to rocky planets in habitablezones in evolving disks

As we explained in section 2.1, theEarth-Life Science Institute, Tokyo Institute of Technology, Meguro-ku, Tokyo 152-8550, Japan
パラメータ
calculatedbytheseparameters.
Wepee-mail: ida@elsi.jp
惑星の水の起源として、惑星形成後snowline
が内側に移動し、
87Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Meguro-ku,
Tokyo 152-8551, Japan
1) Ṁg,0 = 3 ⇥ 10 , 10 M /y,98icy pebble
DRAFT:が降着するシナリオを考える。
February 5, 20192) Ṁpe = 10 , 10 M /y,
ABSTRACT drift を考慮。円盤進化と同時に計算。
3) rd,0 = 30, 100, 300 au,
1Dモデルでicy pebble の形成とradial
6
6
Context. The ocean mass of the Earth is only 2.3 ⇥ 10 of the whole planet mass. Even including water in the interior, the water
4)
t
=
10
,
3
⇥
10
y. ←~αdi↵fraction would be at most
10
10 . Ancient Mars may have had a similar or slightly smaller water fraction. Whatcontrolled the は岩石：氷=1:1
惑星のmigration
は無視。初期は惑星は完全に岩石、icy
pebbleamount of water in these planets has not been clear, although several models have been proposed. It is important to clarify the control
The initial total gas disk mass is gmechanism to discuss water delivery to rocky planets in habitable zones in exoplanetary systems, as well as that to Earth and Mars in
Shigeru Ida1 , Takeru Yamamura2 and Satoshi Okuzumi2

1

Ida, Yamamura, Okuzumi: Water delivery by icy pebbles

arXiv:1901.04611v2 [astro-ph.EP] 3 Feb 2019

2

4

3

2

Ida, Yamamura, Okuzumi: Water delivery by icy pebbles

our solar system.
Aims. We consider water delivery to planets by icy pebbles after the snowline inwardly passes planetary orbits. We derive the watermass fraction ( fwater ) of the final planet as a function of disk parameters and discuss the parameters that reproduce a small value offwater comparable to that inferred for the Earth and ancient Mars.
青：snowline
Methods. We calculated the growth of icy dust grains to pebbles and the pebble radial drift with a 1D model, by simultaneously
solving the snowline migration and dissipation of a gas disk. With the obtained pebble
mass flux, we calculated accretion of icy
赤：粘性加熱/輻射加熱境界
pebbles onto planets after the snowline passage to evaluate fwater of the planets.
Results. We find that fwater is regulated by the total mass (Mres ) of icy dust materials 緑：円盤半径
preserved in the outer disk regions at the timing(t = tsnow ) of the snowline passage of the planetary orbit. Because Mres decays rapidly after the pebble formation front reaches thedisk outer edge (at t = tp↵ ), fwater is sensitive to the ratio tsnow /tp↵ , which is determinedマゼンダ：pebble
by the disk parameters. We find 形成半径
tsnow /tp↵ < 10or > 10 is important. By evaluating Mres analytically, we derive an analytical formula of fwater that reproduces the numerical results.
Conclusions. Using the analytical formula, we find that fwater of a rocky planet near 1 au is similar to the Earth, i.e., ⇠ 10 4 10 2 , indisks with an initial disk size of 30-50 au and an initial disk mass accretion rate of ⇠ (10 8 10 7 )M /r for disk depletion timescaleof ⇠ a few M years. Because these disks may be median or slightly compact/massive disks, our results suggest that the water fractionof rocky planets in habitable zones may often be similar to that of the Earth if icy pebble accretion is responsible for water delivery.

Key words.
and 5;
satellites:
formation,
Accretion
disks
1. Time evolution of the transition
radiusPlanets
rvis/irr (Eq.
red lines),
snowline Accretion,
rsnow = max(rsnow,vis , rsnow,irr ) (Eqs. 6 and 7; blues), disk characteristic radius t˜rd,0 (green lines), and pebble formation front rp↵ (Eq. 36; magenta lines) for various disk evolution
meters. The parameters, rd,0 in units of au and Ṁg,0 in units of M /y are labeled in the individual panels. The other parameters
9
6 delivery by icy pebbles
Water
100 panels, i.e., Ṁpe = 10 Ida,
100 and tOkuzumi:
100
he same for the four/ydi↵ = 10 y.
1. Introduction M Yamamura,able to be an actual habitat. On the other hand, too much water
10-1

10-1

10-1

10-2

10-2

10-2

-3

-3

-3

-4

-4

-4

-5

-5

-5

-6

-6

-6

-7

-7

-7

Water Fraction

creates a planet without continents, where the supply of nutrients may not be as e↵ective as in the Earth. The oceans of the10
10 to Venus,
Earth-size
planets
are being
discovered
habitableryos with the masses
and semimajoraxes identical
The infilteringfactor10zones
is given(HZs)
by
10
10
Earth
only! ✓0.023%
by weight and this amount enablesh, and Mars (eccentricities
are set to be zero).
In10thesecases,
inexoplanetarysystems.
These
HZs
are
definedasa8!range of◆ or! 1 comprise
!1/2
◆
10
10
10 1 ✓
1/2
1/2>
Earthby v = (3/2)bset ⌦ (”Hill regime”).
Earth
Earth
/r
Mpl
>
Mplanetary↵ sur- hgoceansStr coexist. The mantle may preserve water
elative velocity is given⇤>
and continents
tobital
water can exist
onthe>Mars radius, in which liquid
Mars
10
10
10
>
0.017
>
Venus
>
stituting this into 10Eq.Venus(24), if H O exists there.
>
M 10 10 2tem- 0.02
0.1
0.1M
in thetransitionzone 1au
with a comparable amount of ocean (e.g.,
10 However, as long
>
face
as
equilibrium
2
>
>
0.01
0.1
1
5 10 0.01
0.1
1
5 10 0.01
0.1
1
5 10
>
[Mpl <&MKarato>
2D3D ; 3D]2003; Hirschmann 2006; Fei et al. 2017),>
Bercovici
peratureTimeis [Myr]
concerned, H2 O ice grainscondense
only well be-Time [Myr]<Time [Myr]fflt ' >>! 2/3! 1/3 while
!2/3
>
the
could have H equivalent to 2% by weight of H2 O
yond
the
HZs,
becausethegaspressureof protoplanetarydisks✓ core◆ and>
1/2 7; blue>
1. Time evolution of the transition radius rvis/irr (Eq. 5; red lines), snowline
r
=
max(r
,
r
)
(Eqs.
6
M
snow
snow,vissnow,irr
>
M
St
r
pl
⇤
>
!1/3 of>
Earthdisk(Nomura
>
0.040
many
ordersmagnitude
lower
than
that
planetary
atmo-lines)offorthe>s), disk characteristicis
radiust˜rd,0(greenlines),
andpebbleformation
front
rof
36; magenta
variousevolutionet al. 2014). However, the original waterp↵ (Eq.
M
>
pl
>
M
0.1
0.1M
1au
1/3
4
2
>
bset ⇡sphere
2Strd,0 inr.condensation(27) of M /y>fraction
of
the
Earth
would
still
be
very
small
(⇠
10
10
),
and
the
temperatureisconsiderably
lower:
meters. The parameters,
units
of
au
and
Ṁ
in
units
are
labeledintheindividual
panels.
The
otherparametersg,0[Mpl > M2D3D ; 2D],
3M⇤
9
that
he same for the four thanpanels,i.e.,atṀ1peatm.
= 10Hereafter,
M /y andwetdi↵simply= 106 y.call H2 O in a solid/liquid even with the possible(29)water reservoir in the interior because neiphase “water.” For the Earth, a volatile
supplyby Eq.
the (21).
gas capture ther stellar irradiation at ⇠ 1 au (Machida & Abe 2010) nor giant
where
we used
We takeinto ofaccount
the decreasein dust(Genda
surface &density
impacts
Abe 2005) can vaporize the majority of thefrom the disk is ruled out because observed
valuesrare-Earthryos with the masses and semimajor axes identical to Venus, The
filteringfactorisgiven
byflux due
to pebble
accretion
onto
the planets.
After
water
from
the gravitational
potential of Earth. We note that it is
he numerical simulations,
we areusetooa morefor- toandelements
low ingeneral
the Earthbe pebble
consistentwiththe diskMg,0 = 2tdi↵ ( Ṁg,0tdi↵= 0.06106 y!

Ṁpe )

Ṁg,3⇥1

which ranges from 0.06M to 0.6M
Because we start with relatively large
is relatively large. As we show in sdisks tend to produce dry planets, whi
produce water-rich planets.
The initial dust surface density dby 0.01 ⌃g,0 . With the gas disk evoluti
culate the pebble growth from the du
The dust disk is depleted by the forpebbles.

Ida, Yamamura,Okuzumi:Water delivery
by icypebbles
10
10
herwise.
We cancombinethetwolimits in Eq. (41) by a
10
10
formulaas10
水の割合の近似式 10

1

10

0

0

-1

-1

-2

-2

-3

10

-3

fflt (Mpl,0 ) 10
1
fwater
'
M .
10
10
Earth
Earth res
Mars 2 Mpl,0 + fflt (Mpl,0 )MMars
10
10 res
5

10

10-4

-4

-5

-5

-6

-6

10

-7

Venus

0.01

0.1

1

5

10

10

-7

(42)

Venus

0.01

0.1

1

5

10

ure 7, fwater,sim
obtainedby our simulations is
ﬂux
ﬂt : pebble
Time[Myr]のうち、惑星に降着する割合
Timecompared[Myr]q. (42)Mwith
thesimulatedM.
This
figure
shows
that
res
res : t=tsnow で円盤に残っているpebble mass)fraction
reproduces
the
very
Both
thecenter,
nu-andfor the models
withnumericalrd.0 = 100au, tdi↵results= 106 y andṀini =well.
10 7 M /y.
The left,
Ida, Yamamura, Okuzumi: Water delivery by icy pebbles
998/y, 3 ⇥Eq.
10 M
/y, and
10 M /y,respectively.
pe = 10 MandlṀresults
(42)
show
f
for fwater ⌧ 1/2.
water / Mres 近似式パラメータ依存性
近似式とモデル計算の比較
y dust mass Mres depends sensitively on the disk pars, Ṁg,0 , Ṁpe , tdi↵ , and rd,0 . On the other hand, fflt in 2D
pendent of thesepdisk parameters, while that in 3D deonly weakly (/ rd,0 /tdi↵ ). In the case of Mpl ⌧ Mpl,0 ,' ( fflt /Mpl,0 )Mres . As we discussed, fflt /Mpl,0 is almost
nt, so that fwater should be almost proportional to Mres for⌧ Mpl,0 .
cause the analytical solution given by Eq. (42) reproduces
merical results, we next derive an analytical formula fordust mass Mres at the snowline passage as地球を説明するには
follows. Fromrd = 30-50 au、 Mdot g,0 = 10-8 -10-7 Msun/yr, the snowline passes the planet orbit at apl when

一般的or
少しコンパクトな円盤
nd icy dust mass preserved in the outer disk at the snowline passage Mres →obtainedby our simulations.
lation results for the Earth analogs with di↵erent values of Ṁg,0 , Ṁpe , tdi↵ , and rd,0 (section 2.4). The
太陽のような星の周りのハビタブルゾーン内の惑星は地球と同程度の水を
ytical solution
given by Eq. (42).
g,snow' Ṁ✓ a ◆9/4 M ! 3/4 ✓ ↵ ◆1/2 持っていそう。
pl⇤8= 2 ⇥ 10
M
/y.
(43)
2

tion of planetesimals contributes significantly to the growth from
2. Analytical pebble accretion growth tracks
planetesimal sizes to protoplanets with masses 0.001 0.01 ME
36 How planetary growth outperforms migration
due to the low rates of pebble accretion in the Bondi regime
In this sectionAnders
we derivefor
2 the growth
Johansen1analytical, Shigeru Ida2 , expressions
and Ramon Brasser
while pebble accretion in the Hill regime dominates the furthe
track of a protoplanet growing by pebble accretion. We then growth. Therefore we start our protoplanets at M = 0.01 M
0E
Lund Observatory, Department of Astronomy and Theoretical Physics, Lund University, Box 43, 221 00 Lund, Sweden,
use
thisexpression
toderivethelocationwherethegrowthtrack
e-mail:anders@astro.lu.se
惑星のmigration は惑星形成の最大の問題の一つ。migrationandrate
は惑星の質量に依存
ignorethecontributionofplanetesimalaccretion
to
the
cor
Earth-Life
Science Institute(ELSI), Tokyo
Institute of Technology,
crosses
the pebble
isolation
mass. Meguro, Tokyo, 152-8550, Japan
growthrate,
althoughtheinclusionofplanetesimalaccretion
一方、pebble accretion によりmigration中でも惑星の質量は変化しうる
could give a boost to the accretion rate, depending on the mi
ABSTRACT
1Dモデルを用いて惑星の軌道と質量の進化を計算
grationspeed of the protoplanet (Tanaka & Ida, 1999).
Planetary2.1.
migration
is a major accretion
challenge for planet formation theories. The speed of Type I migration is proportional to the massofPebblea protoplanet, while the final decade of growth of a pebble-accreting planetary core takes place at a rate that scales with the mass
簡単のため、Stokes
numberとalphato thetwo-thirds power. This results in planetary
growth tracks (i.e.,
the evolution は時間、空間で一定を仮定
of a protoplanet’s mass versus its distance fromthe star)To
that become
increasingly
horizontal (migration-dominated)withgrowth
rising mass ofthe protoplanet.
It has beenshown recently
derivetheanalytical
shape
of
the
track
of
a
solid
prothat the migration torque on a protoplanet is reduced proportional to the relative height of the gas gap carved by the growing planet.
2.2. Type I migration
Here wetoplanet,show from 1-D wesimulations
planet-discinteraction thatgrowth
the mass at whichcarvesa 50% gapaccreis approximately 2.3
useoftheprotoplanet
ratea planetfrompebbletimes the pebble isolation mass. Our measurements of the pebble isolation mass from 1-D simulations match published 3-D resultsin the2-DHill regime&pebbleKlahr,
LambrechtsForrelativelytion
well, except
at very
low viscosities(↵ < 10 )(Ormel
where the 3-D
isolation2010;
mass is significantly
higher, possibly
due Type I migration we use the standard scaling law,
to gap edge instabilities that are not captured in 1-D. The pebble isolation mass demarks the transition from pebble accretion to gas&GasJohansen,
2012;
etthereforeal., 2016),
accretion.
accretion to form
gas-giantIda
planets
takes place over a few astronomical units of migration after reaching✓◆
2
2
first the pebble isolation mass and, shortly after, the 50% gap mass. Our results demonstrate how planetary growth can outperform
⌃
r
M g
H
migration, both during core accretion and during gas accretion, even when the Stokes number of the pebbles is small, St ⇠ 0.01,
and
ṙ
=
k
v
.
(3
mig
K
the pebble-to-gas flux ratio in!the
M? M? r2/3protoplanetary disc is in the nominal range of 0.01–0.02. We find that planetary growth is very rapid
in the first million yearsStof the protoplanetary disc and that the probability for forming gas-giant planets increases with the initial sizeof the protoplanetarydi↵usion.
Ṁ = 2 disc and with decreasing⌦R2H ⌃turbulent(1)p.
Here ṙ is the migration speed of the protoplanet, kmig is a con
0.1
Key words. planet-disk
interactions, planets and satellites: formation, planets and satellites: gaseous planets
stant prefactor that depends on the gradients of surface density
andtemperature,
M
is
the
mass
of
the
central
star,
⌃
is
th
?
g
ntroduction
by a positivefrom the accretion heat
Here M is the mass of the protoplanet,
Stcorotation= ⌦⌧torquethe Stokes
f is resultingof the protoplanet (Benı́tez-Llambay et al., 2015) orgas
fromsurface
thedensity,
H/r
is
the
disc
aspect
ratio
and
v
is
th
K
numberthe many
pebbles
inofequation⌦ is the& Pessah, 2018).
formationof planets ofinvolves
distinct (defined
steps in the laterscattering(large) pebbles16),(Benı́tez-Llambay
Keplerian
speed
at
the
positionoftheplanet.
Fortheprefacto
wth from dust and ice particles to full planetary system (a Migration can even stall entirely if the turbulent viscosityistooKeplerianthe location
theprotoplanet,
⌧
is
the
f
isation thatwas pioneeredfrequency
50 years ago by at
Safronov,
1969). weakof
to di↵use away the gas density enhancement thatkformswe
in- follow here a fit to 3-D numerical simulations found in
mig
competition
betweentime
radial of
migrationand growth(proportional
is nev- terior of thefrictionthe pebble
toplanetary
the particle
size2002;
whenorbit (Rafikov,
Li et al., 2009; Fungeless a general theme in planet formation. The formation & Lee,
D’Angelo&
Lubow(2010),
1/32018).
pebbles are small), R = [M/(3M )] r is the Hill radius of the12

3

planetesimals, for example, has to overcome
H the radial drift ? A more direct way to overcome Type I migration is simply
sed by thehead-wind of theMslower
movinggas onthefor the planetarycore
to theincrease
its massvery rapidly. The acprotoplanet,
is
the
mass
of
the
centralstar,risradialloca?
= 2(1.36 + 0.62 + 0.43⇣) ,(4wing particles (Weidenschilling, 1977; Brauer et al., 2008). cretion rate of pebbles is potentially high enough forkthemigprototionin of
the bumps
planetandin ⌃
is the gas
pebbledensity.theSignificant
pping pebbles
pressure
formedthep turbulent
planetsurface
growth to outperform
nominal rate of Type I migrationw (Lyra et al., 2008; Johansen et al., 2009a; Bai, 2015) or by (Lambrechts & Johansen, 2014; Ormel et al., 2017; Johansen &e↵ortisetcurrently
being
put into
how pebble ac- where and ⇣ are the negative logarithmic derivatives of the surbedded planets(Lyraal., 2009) or throughrun-away
pile- understanding
Lambrechts, 2017). Bitsch et al. (2015b) demonstrated that procaused bycretionthe friction depends
on the gas (Youdin
Goodman,2005;
on &theeccentricity
and inclination of the pro-7

8

Johansen, Ida, Brasser: How planetary growth outperforms migration

1.0
0.8

1000.00

0.6

100.000.4

αv=10−4αv=10−3αv=10−20.2
0.01

M [ME]

Gap height

etary growth outperforms migration

10
Mp [ME]

10.00
1.00
0.10

Miso, Mgap [ME]100

Miso 1−D
Miso 3−D (B+18)
Mgap 1−D
Mgap 2−D (K+18)

10

0.01
0.1

0.0010αv

10.0
r [AU]

1
0.00011.0

0.0100Fig. 3. The results of 1-D simulations of an accretion disc with
an embedded planet whose torque on the gas is based on theparametrisations of D’Angelo & Lubow (2010). The top panel
shows the equilibrium relative gap height as a function of the

100.0

39

Extremely High Excitation SiO Lines in Disk-Outflow System in Orion Source I

Extremely High Excitation SiO Lines in Disk-Outflow System in Orion Source I

3,4 , Masahiro N. Machida5 , Yuko Matsushita5 , Kazuhito
Mi Kyoung Kim1,2 , Tomoya
Hirota1,2 , Tomoya Hirota3,4 , Masahiro N. Machida5 , Yuko Matsushita5 , Kazuhito
Mi Kyoung KimMotogi
6 , Naoko Matsumoto3,7 & Mareki Honma1,8Orion Source I.07208v1 [astro-ph.GA] 22 Jan 20191901.07208v1 [astro-ph.GA] 22 Jan 2019

Motogi6 , Naoko Matsumoto3,7 & Mareki Honma1,8
mikyoung.kim@nao.ac.jp

mikyoung.kim@nao.ac.jp
ABSTRACT

high-mass protostar candidate,ABSTRACT
光度 >10^4 Lsun, 距離~420
We present high-resolution images of the submillimeter SiO line emissions of• envelope に埋もれているため、可視や近赤より電波、sub-mm で詳細な観測
a massivestellarobject Orion images
Source Iof using
the Atacama Large
We youngpresent
high-resolution
the submillimeter
SiO Millimeline emissions of• bipolar
outﬂow~ 1000au,atedge
disk
ter/Submillimeter
Array(ALMA)
band
We
detected
GHz SiOLarge
v=4 Millimea massive
youngstellarobjectOrion8.on
SourceI usingthethe464Atacama
J=11-10line in Source Array
I, whichis the firstdetectionof theSiO v=4
line
in GHzstar- SiO v=4
ter/Submillimeter(ALMA)
at
band
8.
We
detectedthe464• SiO maserが観測される ~100 au29: rotating outﬂow
forming regions, together with the 465 GHz SiO v=2 J=11-10 and the 428 GHz SiO
J=11-10 line in Source I, which is the first29 detection of the SiO v=4 line in star• H2O,
CO などのline：5-9Msunのケプラー回転と整合的
v=2 J=10-9
lines with a resolutionof 50 AU.
The 29 SiO v=2 J=11-10 and SiO v=4
•

•
•

•
•

forming regions, together with the 465 GHz SiO v=2 J=11-10 and the 428 GHz SiO
J=11-10 lines have compact structures with the diameter of29
<80 AU. The spatial and
v=2 J=10-9 lines with a resolution of 50 AU. The SiO v=2 J=11-10 and SiO v=4
velocity distribution suggest that the line emissions are associated with the base of the
J=11-10lines
have ofcompact
structures
withtheof J=10-9<80 →H2,
AU.emission
TheCOで観測される爆発的なoutﬂow
spatial and
固有運動から、500年前にmassiveと diameterinteraction
outflow
and thesurfacethe edge-on
disk. star
In contrast,
SiO v=2
velocity
distributionthat theofline
emissions are associatedwiththe base of theshows
a bipolar
structure suggest
in the direction
northeast-southwest
low-velocity
outflow
このシナリオでは、M=20Msun
andthe Thesurfaceof theIn contrast,
SiO v=2
J=10-9 emission
withoutflow⇠200 AU
scale.
emission
lineedge-on
exhibits disk.
a velocity
gradient along
the direction
showsbipolar structure
the directionof ring
northeast-southwest
low-velocityof thedisk aelongation.
With theinassumptionof thestructure with Keplerian
ro- outflow
with
⇠200
AU
scale.
The
emissionline
exhibitsavelocity
gradientalong
the
directiontation,weestimated
the
lower
limit
of
the
central
mass
to
be
7
M
and
the
radiusofSource I の円盤、アウトフローについての高分解能観測が必要
12 AU<
r <26of thediskAU.
elongation. With the assumption of the ring structure with Keplerian ro励起温度3600-7000Kのラインから、内側のdynamics
を調べる
tation, we estimated theのSiO
lower limitof the central mass to be 7 M and theradius of1
12VLBIAU<
r <26 AU.
Mizusawa
Observatory,
National Astronomical Observatory of Japan, Hoshigaoka 2-12, Mizusawa-ku, Oshu,

Iwate 023-0861, Japan
2

Korea
Astronomy and Space Science Institute, Hwaam-dong 61-1, Yuseong-gu, Daejeon, 305-348, Republic of1
Mizusawa VLBI Observatory, National Astronomical Observatory of Japan, Hoshigaoka 2-12, Mizusawa-ku, Oshu,
Korea

Iwate 023-0861, Japan

3

Mizusawa VLBI Observatory, National Astronomical Observatory of Japan, Osawa 2-21-1, Mitaka, Tokyo 181-

–8–

SiO v=4

p-v diagram
SiO v=4– 10 –

Centroids of each velocity channel
緑線：M=7Msun のケプラー回転
他：リングモデル M=5Msun, 13-23 au
M=7Msun, 12-26 au
M=10Msun, 6-30 au
M=15Msun, 16-30 au

実線：ケプラー回転

Fig. 4.— (a) The position-velocity diagram of the SiO v=4 J=11-10 emission. The Keplerianvelocity
curves for 10M (grey)
and 15M
破線：半径5,60 au
での(black) are overlaid. The dashed lines show the velocity
urves at 5 AU and 60 AU. The dotted horizontal line represents the systemic velocity of 6 km s 1 .
回転速度b) The position-velocity
diagram using the centroids of each velocity channel of the SiO v=1 and 2
J=1-0 SiO maser emission (grey cross), the v=4 J=11-10 (orange) and 29 SiO v=2 J=11-10 (blue)
mission. The solid line indicates the position-velocity diagram of the ring model with parameters
この観測からは先行研究の軽い方の中心星質量を支持
of M = 7M , rin =12 AU, rout =26 AU. Also, we overlaid the model curves with M = 5M withAU, rout =23 AU, M = 10M with rin =6
AU, rと見るべき？
分解能などの問題でlower
limit
in =13out =30 AU, and M = 15M with rin =16 AU,
out =30 AU. The dashed green line represents the Keplerian rotation curve with M = 7M . The
horizontal dashed line marks the adopted systemic velocity of 6 km s 1 .

SiO v=4より、M=7Msunモデルがもっとも合う。
M=5Msun だと高速度成分（図の右上）が合わない

星形成領域でのSiO v=4の初検出より高い分解能で観測できれば円盤やoutﬂow のより内側を見ることができる

Figure 4 (b) presents the results of the fitting to the velocity centroids of the SiO v=4 J=1110 emission. We also display the rotation curves with the central mass of 5, 10, and 15M . The

nidad Mixta Internacional Franco-Chilena de Astronomı́a, CNRS/INSU UMI 3386, Departamento de Astronomı́a, Universidad deChile, Camino El Observatorio 1515, Las Condes, Santiago, Chile
10 Univ.
The
Disk
Substructures
at HighAngularResolution
Project (DSHARP):
Grenoble
Alpes, Angular
CNRS,
IPAG,
38000 Grenoble,
FranceThe Disk Substructures
at High
Resolution
Project(DSHARP):
1 University Observatory, Faculty of Physics, Ludwig-Maximilians-Universität
II. Characteristics
Annular
SubstructuresMünchen,Scheinerstr. 1, 81679 Munich, Germany
II. Characteristics
of AnnularofSubstructures
12 Department of Astronomy, Van Vleck Observatory, Wesleyan University, 96 Foss Hill Drive, Middletown, CT 06459, USA
1
1
2
3
4
Andrea1Jane Huang, Sean M.
1 Andrews, Cornelis P. Dullemond,2
3 Isella, Laura M. 4Pérez,
Jane Huang,
Sean
Andrews,
Cornelis
P. Dullemond,
AndreaIsella,Laura
M. PCAérez,
Departmentof Physics
andM.
Astronomy,
California
State1 University
Northridge,
18111 Nordho↵
Street,Northridge,
91130, USA
5, 6
7
7
8

31

9, 10
Viviana5,V.
Guzm
án,
Karin
I.
Öberg,Zhaohuan
Zhu,
Shangjia
Zhang,
Xue-Ning
Bai,
MyriamBenisty,
1
7
7
8
9, 10
V. Guzmán, 6 Karin I. Öberg,
Zhaohuan
Zhu,
Shangjia
Zhang,
Xue-Ning
Bai,
MyriamBenisty,
11
5
12
13
3
TilmanBirnstiel,John
M.
Carpenter,
A.
Meredith
Hughes,
Luca
Ricci,Erik
Weaver,
and
11
5
12
13
3
lman Birnstiel, John M. Carpenter, A. Meredith
Hughes,Erik
Weaver,and
1Luca Ricci,
ABSTRACTDavid J.
1 Wilner

David J. Wilner
The Disk
Substructures at High Angular Resolution Project used ALMA to map the 1.25 millimeter
1 Harvard-Smithsonian
Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, United States of America
continuum of protoplanetarydisks at a 60
spatialresolutionof ⇠ 5 au.MA
We02138,
presenta systematic
analysis
Harvard-Smithsonian
Centerfor
Astrophysics,
GardenStreet,Cambridge,
UnitedStatesof2
Zentrum für Astronomie, Heidelberg University, Albert Ueberle Str. 2, 69120 Heidelberg, America
Germanyof 2annular
substructuresinHeidelberg
the 18 single-disk
systemstargeted
in2, thissurvey.
No dominantarchiZentrum
für Astronomie,
University,
AlbertUeberleStr.
69120
Heidelberg,
Germany
3 Departmentof Physics and Astronomy, Rice University, 6100 Main Street, Houston, TX 77005, United States of America
tectureemerges
this sample;
instead, remarkably
diversemorphologies
are Unitedobserved.
Annular
4 Departamento
artmentof Physics
andfrom
Astronomy,
Rice
University,
6100
Main
Street,Houston,TX
77005,
StatesAmericade Astronomı́a, Universidad de Chile, Camino El Observatorio 1515, Las Condes, ofSantiago,
Chilesubstructures
can occuratvirtually de
anyChile,
radiuswhereElmillimeter
continuum
emission
isSantiago,
detectedChileand
4 Departamento
5 Joint
de Astronomı́a,
Universidad
CaminoObservatorio
1515,
Las
Condes,
ALMA Observatory, Avenida Alonso de Córdova 3107, Vitacura, Santiago, Chile
range
in5 Joint
widthsfromObservatory,
a few au toAvenida
tens of Alonsoau. Intensity
ratiosbetweengapsSantiago,
and adjacentrings range
6 Instituto
ALMA
deCórdova
3107,
Vitacura,
Chilede Astrofı́sica, Pontificia Universidad Católica de Chile, Av. Vicuña Mackenna 4860, 7820436 Macul, Santiago, Chilefromnear-unity to just a few percent. In a minority of cases, annular substructures co-exist with other7 Departmentof Physics
and Astronomy,
Universityof Nevada,
Las Vegas,
4505 4860,
S. Maryland
Pkwy,
Las Santiago,
Vegas, NV,Chile89154, USA
to de Astrofı́sica, Pontificia
Universidad
Católicade Chile,
Av. VicuñaMackenna
7820436
Macul,
types of substructures,
including spiral arms (3/18) and crescent-like azimuthal asymmetries (2/18).
8 Institute for Advanced
Study and
TsinghuaLas
Centerfor Astrophysics,
Tsinghua
University,
Beijingment of Physics and Astronomy, Universityof Nevada,
Vegas,
4505 S. Maryland
Pkwy,
Las Vegas,
NV,100084,
89154, China
USA
No
clear trend is observed between the positions of the substructures and stellar host properties. In
9 Unidad
8 InstituteMixta Internacional
Franco-Chilenade Astronomı́a,
CNRS/INSU
UMI
3386, Departamentode Astronomı́a,
Universidad defor
Advanced
Study
andTsinghuaCenterfor
Astrophysics,
Tsinghua
University,
Beijing
100084,China
particular, the absence of an Chile,obviousassociation
with stellar
hostCondes,
luminosity(andhence the disk
CaminoEl Observatorio
1515, Las
Santiago,
Chile
MixtathermalInternacional
Franco-Chilena
de 10
Astronomı́a,
CNRS/INSU
UMIpreferentially
3386, Departamentode Astronomı́a,
Universidad de
structure)suggests that
substructures
do
not
occur
near
major
molecular
snowGrenoble Alpes,
IPAG,Santiago,
38000 Grenoble,
Chile, Camino ElUniv.
Observatorio
1515, CNRS,
Las Condes,
Chile Francelines.
AnnularObservatory,
substructures
like
those
observed
in
DSHARP
have
long
been
hypothesized
to
be
due
11 University
FacultyofPhysics,
Ludwig-Maximilians-Universität
München,Scheinerstr.
1,
81679
Munich, Germany
10 Univ. Grenoble Alpes, CNRS, IPAG, 38000 Grenoble, France
to planet-disk
interactions.
A few
exhibit characteristics
particularly
suggestiveof Middletown,
this scenario,
12 Departmentof Astronomy,
Van disks
Vleck Observatory,
Wesleyan University,
96 Foss
Hill Drive,
CT 06459, USA
sity Observatory,
FacultyofPhysics,
Ludwig-Maximilians-Universität
München,Scheinerstr.
1,
81679
Munich,Germany
including
substructuresinpossiblemean-motion
resonanceand“doublegap”
featuresreminiscentof
13 Departmentof Physics and Astronomy, California State University Northridge, 18111 Nordho↵ Street, Northridge, CA 91130, USA
artment
of Astronomy,simulations
Van Vleck Observatory,
University,
96 Foss
Drive, Middletown,hydrodynamicalof multiple Wesleyangaps opened
by a planet
in aHill
low-viscosity
disk. CT 06459, USA

ent of Physics and Astronomy, California State University Northridge, 18111 Nordho↵ Street, Northridge, CA 91130, USA

ABSTRACT
Keywords: protoplanetary disks—ISM: dust—techniques: high angular resolution
DSHARPのリング構造について
The Disk Substructures at High Angular Resolution Project used ALMA to map the 1.25 millimeter
ABSTRACT
continuum of protoplanetary disks at a spatial resolution of ⇠ 5 au. We present a systematic analysis
1. INTRODUCTION
variations
inALMA
properties
are thought
to millimeterbe closely tied to<10
au,
コントラスト~数%-oder
1
Theリング幅
Disk SubstructuresatHigh
AngularResolution
Project
used
to
map
the
1.25
of annular substructures in the 18 single-disk systems targeted in this survey. No dominant archidi↵erencesin where
and whenplanets formedin the proontinuumof tecture
protoplanetarydisksremarkable
at asample;
spatialresolutionof ⇠ 5 au.
We presenta systematic
analysis
xoplanet surveys
have
uncovereddiveremerges
from
this
instead,remarkably
diversemorphologies
are observed.
Annularspiralarm
付随が3/18,
三日月状構造付随が2/18
toplanetarydisks
orbiting
young
stars (e.g.,archiÖberg et al.
inthemasses,radii,
andcompositionofexoplanets,
annularsubstructures
in
the
18
single-disk
systemstargetedinthissurvey.
No
dominant
substructures can occur at virtually any radius where millimeter continuum emission is detected and2011b; Mordasini et al. 2012; Lee & Chiang 2016). Rewell
as
in
the
overallarchitecturesof
exoplanetary
cture emerges
fromthis sample;
observed.
Annularrange
in widths
from a instead,few au toremarkably
tens of au. diverse
Intensitymorphologies
ratios betweenaregaps
and adjacentrings range
リング半径と中心星光度等に相関なし
惑星起源を示唆するものも見つかる
cent discoveriesof complex features in protoplanetarytems(e.g.,
Howardetal.
2010;
Borucki
et
al.
2011;
to just a any
few percent.
In a minorityof cases,annularemission
substructures
co-existandwith otherubstructuresfrom
can near-unity
occur at virtually
radius where
millimeter
continuum
is detecteddisks, such as annular substructures, spiral arms, andnn&
Fabrycky2015;
Fultonetal.
2017).
These
wide
types
of substructures,
includingarms ratios(3/18) between
and crescent-likenge in widths
froma few au to tensof au.spiral
Intensity
gaps andazimuthal
adjacentasymmetries
rings range (2/18).

9 University Observatory, Faculty of Physics, Ludwig-Maximilians-Universität München, Scheinerstr. 1, 81679 Munich, Germany
10 Joint ALMA Observatory, Avenida Alonso de Córdova 3107, Vitacura, Santiago, Chile

The Disk Substructures at High Angular Resolution Project (DSHARP):
32
DepartmentIII.
of Astronomy,
Van VleckinObservatory,
Wesleyan
University, 96
Drive,CT WaOph
06459, USA
Spiral Structures
the Millimeter
Continuumof Fossthe HillElias
27, Middletown,
IM Lup, and
6 Disks

11 Instituto de Astrofı́sica, Pontificia Universidad Católica de Chile, Av. Vicuña Mackenna 4860, 7820436 Macul, Santiago, Chile
12

13 Department of Physics and Astronomy, California State University Northridge, 18111 Nordho↵ Street, Northridge, CA 91130, USA

Jane Huang,1 Sean M. Andrews,1 Laura M. Pérez,2 Zhaohuan Zhu,3 Cornelis P. Dullemond,4 Andrea Isella,59
1010, 11Myriam Benisty,6, 7 Xue-Ning Bai,8 Tilman
Birnstiel,John
M.
Carpenter,
Viviana
V.
Guzm
án,
ABSTRACT
12
A. Meredith Hughes, Karin I. Öberg,1 Luca Ricci,13 David J. Wilner,1 and Shangjia Zhang3
We present an analysis of ALMA 1.25 millimeter continuum observations of spiral structures inthree 1protoplanetarydisksCenterfrom forthe Astrophysics,
Disk Substructures
atStreet,High Cambridge,
Angular Resolution
Theof America
Harvard-Smithsonian
60 Garden
MA 02138,Project.
United States
2 Departamento
disks around
Elias 27,deIM
Lup, and Universidad
WaOph 6 wereobserved
at aElresolutionof ⇠1515,
40 Las60 mas(⇠ 6Santiago,
7
Astronomı́a,de Chile,
CaminoObservatorio
Condes,Chile
3au).
All threedisks featurem = 2 spiralpatterns
in conjunction
annularsubstructures.
Gas NV, 89154, USA
Departmentof Physics
and Astronomy,
Universityof Nevada,
Las Vegas, with4505 S.
MarylandPkwy, Las Vegas,
12
kinematics establishedby Astronomie,
CO J = Heidelberg
2 1 observations
that thespiral arms
are
4 Zentrum für
University,indicate
Albert Ueberle
Str.continuum
2, 69120 Heidelberg,
Germany
trailing.
The arm-interarm
intensity contrasts are modest, typically less than 3. The Elias 27 spiral
5 Departmentof Physics and Astronomy, Rice University, 6100 Main Street, Houston, TX 77005, United States of America
pattern extends throughout much of the disk, and the arms intersect the gap at R ⇠ 69 au. The
6 UnidadMixta Internacional Franco-Chilena de Astronomı́a, CNRS/INSU UMI 3386, Departamento de Astronomı́a, Universidad despiral pattern in the IM LupChile,
disk isCamino
particularlycomplex—it
aboutSantiago,
halfway Chile
radially throughEl Observatorio
1515,extends
Las Condes,
the disk, exhibiting pitch angle
variations
with radius and interarm features that may be part of ring
7 Univ.
Grenoble Alpes, CNRS, IPAG, 38000 Grenoble, France
substructures
spiral arm branches. Spiral arms also extend most of the way through the WaOph
8 Instituteorfor
Advanced Study and Tsinghua Center for Astrophysics, Tsinghua University, Beijing 100084, China
disk, but the source overall is much more compact than the other two disks. We discuss possible
96
University Observatory, Faculty of Physics, Ludwig-Maximilians-Universität München, Scheinerstr. 1, 81679 Munich, Germany
origins for the spiralstructures, including gravitational instability and density waves induced by a
10 Joint ALMA Observatory, Avenida Alonso de Córdova 3107, Vitacura, Santiago, Chile
stellarorplanetarycompanion.
Unlikethemillimeter
continuum
counterparts
of
many
of
the
disks
11 Instituto de Astrofı́sica, Pontificia Universidad Católica de Chile, Av. Vicuña Mackenna 4860, 7820436 Macul, Santiago, Chile
with spiral arms detected in scattered light, these three sources do not feature high-contrast crescent12 Department of Astronomy, Van Vleck Observatory, Wesleyan University, 96 Foss Hill Drive, Middletown, CT 06459, USA
like asymmetries or large (R > 20 au) emission cavities. This di↵erence may point to multiple spiral
13 Department of Physics and Astronomy, California State University Northridge, 18111 Nordho↵ Street, Northridge, CA 91130, USA
formation mechanisms operating in disks.

ABSTRACT
Keywords: protoplanetary disks—ISM: dust—techniques:
high angular resolution

We present an analysis of ALMA 1.25 millimeter continuum observations of spiral structures in
INTRODUCTION
tary companion(e.g., AngularGoldreichResolution& TremaineProject.
1979; LinThethree1. protoplanetarydisks from the Disk Substructures
at High& Papaloizou
Tanaka et ofal.⇠2002),
gravitational
disks
27, IMkey
Lup,
andtoWaOph
6 wereobserved 1986;
at a resolution
40 60
mas (⇠ 6 7
Spiral arms
are aroundthought Elias
to provide
clues
the
instability(e.g.,au). Allofthreedisks featurem although= 2 spiral patterns
in conjunction
with annular substructures. Gas
ynamical evolution
protoplanetarydisks,
12kinematics
establishedby mechanisms
CO J = 2is 1 observations indicate that the continuum spiral arms are
he precise natureof spiral
formation
ighly debated.
Proposed
for intensity
inducing spitrailing.
Themechanisms
arm-interarm
contrasts are modest, typically less than 3. The Elias 27 spiralal features include
by a stellar
or planepatternperturbations
extends throughout
muchof the disk, and the arms intersect the gap at R ⇠ 69 au. Theysical Observatory, via S. Sofia 78, 95123, Catania, Italy

possible chromospheric cycle.
33 First long-term activity study of AU Microscopii: a possible chromospheric cycle.
1,21⋆
chromospheric, M. Flores3,4, C. I. Martinez3
R. V. possible
Ibañez Bustos†, A. P. Buccinocycle.
1

5

R. V. Ibañez Bustos1⋆†, A. P. Buccino1,2, M. Flores3,4, C. I. Martinez3

1,2

arXiv:1901.01433v1 [astro-ph.SR] 5 Jan 2019

D. Maizel , Sergio Messina and P. J. D. Mauas
ABSTRACT
1,2
3,4
3
1⋆
1 Instituto
A. P. Buccino, M.
Flores, C. I. Martinez
R.de V.
Ibañez
Bustos†, (CONICET-UBA),
Astronomı́ay Fı́sicadel Espacio
C.C. 67
Sucursal
28, C1428EHA-Buenos
Aires, Argentina.
D. Maizel1, Sergio Messina 5 and P. J. D. Mauas1,2
M2 Departamentostars
to search
planets.
deidealFı́sica.
de Buenos
1 targets
5 forAires,
1,2 However, they usu- 1
D.are
Maizel, FCEyN-Universidad
Sergio Messina
andEarth-like
P. Buenos,
J. D. Argentina.
Mauas
Instituto de Astronomı́a y Fı́sica del Espacio (CONICET-UBA), C.C. 67 Sucursal 28, C1428EHA-Buenos Aires, Arge

arXiv:1901.01433v1 [astro-ph.SR] 5 Jan 2019arXiv:1901.01433v1 [astro-ph.SR] 5 Jan 2019hFirst long-term activity study of AU Microscopii: a

M star は地球型惑星探しのよいターゲット。

3 Instituto de Ciencias Astronómicas, de la Tierra y del Espacio (ICATE-CONICET), San Juan, Argentina.
1 Instituto de Astronomı́a y Fı́sica del Espacio (CONICET-UBA), C.C. 67 Sucursal 28, C1428EHA-Buenos Aires, Argentina.
2

ally have high levels of magnetic activity, which could aﬀect their habitability

Departamento de Fı́sica. FCEyN-Universidad de Buenos Aires, Buenos, Argentina.

磁気活動がハビタブルゾーンに影響、観測を困難に。
and make diﬃcult the detection of exoplanets orbiting around them. Unfor4 Facultad de Ciencias Exactas, Fı́sicas y Naturales, Universidad Nacional de San Juan, San Juan, Argentina.
2 Departamento de Fı́sica. FCEyN-Universidad de Buenos Aires, Buenos, Argentina.

5 INAF-Catania Astrophysical Observatory, via S. Sofia 78, 95123, Catania, Italy
3 Instituto de Ciencias Astronómicas, de la Tierra y del Espacio (ICATE-CONICET), San Juan, Argentina.

tunately,
long-termdM stars
hasNacional
not been
extensively
studied,4 Facultadde Cienciasvariability
Exactas, Fı́sicas yof
Naturales,
Universidad
de San Juan,
San Juan, Argentina.
Last updated
2018 May 2thAstrophysical Observatory, via S. Sofia 78, 95123, Catania, Italy
INAF-Catania
due
to 5their
low intrinsic brightness. For this reason, in 1999 we started the

3 Instituto de Ciencias Astronómicas, de la Tierra y del Espacio (ICATE-CONICET), San Juan, Argentina.

変光についての理解が不十分。

4 Facultad de Ciencias Exactas, Fı́sicas y Naturales, Universidad Nacional de San Juan, San Juan, Argentina.
5 INAF-Catania Astrophysical Observatory, via S. Sofia 78, 95123, Catania, Italy

2004-2016までのスペクトルを観測

HKα project, which systematically observes the spectra of a large number Last
updated 2018 May 2th→変光周期5年、自転~4.85day
Last updated 2018 May 2th

ABSTRACTof stars, in particular M
dMstars, at the Complejo Astronómico El Leoncitostars are ideal targets to search for Earth-like planets. However, they usu-

変光の起源はαΩダイナモの可能性

ally havehigh levels
magnetic activity,
which could
aﬀect
their habitability(CASLEO). In this work,
weABSTRACT
study
theof long-term
activityof theyoung
activeABSTRACTand makediﬃcult
the detection
exoplanets
orbitingplanets.
aroundHowever,them. UnforM stars
are ideal
targets toof
searchfor Earth-likethey usu-

M stars are ideal targets to search for Earth-like planets. However, theytunately,of dM stars
haswhich
not been
allylong-term
have highvariability
levels of magnetic
activity,
couldextensively
aﬀect theirstudied,habitability

ally have high levels of magnetic activity, which could aﬀect their habitab

dM1 star AU Microscopii. We analyze the Mount Wilson index S derived fromCASLEO spectra obtained
2004 and2016,Forwhich
we complement
withtheandthedetectionof exoplanets
orbitingthem.
Unfordue tobetween
theirmakelow diﬃcult
intrinsic
brightness.
this reason,in 1999aroundwe started
tunately,which
long-term
variability observesof dM stars
not beenHKαproject,
systematicallythehasspectraof aextensively
large
the S-index derived fromHARPS,FEROS
and UVES
publicspectra.
We numberalsostudied,dueintoparticular
their low dM
intrinsic
For this Astronómico
reason, in 1999
started theof stars,stars,brightness.
at the Complejo
Elwe
Leoncitoand make diﬃcult the detection of exoplanets orbiting around them. Un

tunately, long-term variability of dM stars has not been extensively studanalyze the simultaneous photometriccounterpart provided by the ASAS pubHKα project, which systematically observes the spectra of a large number

due to their low intrinsic brightness. For this reason, in 1999 we startedof AUstars,
in2000particularstars,theat Mountthe ourComplejo
Astronómico
El from
Leoncito
lic database for this star
and
2009,
and
ownindex
photometry.
dM1between
star
Microscopii.
WedM
analyze
WilsonS derived

HKα project, which systematically observes the spectra of a large num(CASLEO).
In this work,
we study
the 2016,
long-term
activityof the young
activeCASLEO
spectra obtained
between2004 andwhich
we complement
with
In both totally independent time series, we detect a possible activity cycle
dM1 star
AU Microscopii.
WeFEROSanalyzeand
the Mountindex S derived
the S-index
derivedfrom HARPS,UVES Wilson
public spectra.
We alsofromof stars, in particular dM stars, at the Complejo Astronómico El Leon

(CASLEO). In this work, we study the long-term activity of the young active(CASLEO). In this work, we study the long-term activity of the young acof period ∼ 5 years. We
alsoa obtained
preciserotation
period
for
this
star
CASLEO
spectrabetween2004 and2016, which
complement
analyzethederived
simultaneous
photometriccounterpart
provided
by we
the
ASAS
pub-with

dM1 star AU Microscopii. We analyze the Mount Wilson index S derived f

the S-index derived from HARPS, FEROS and UVES public spectra. We also

CASLEO spectra obtained between 2004 and 2016, which we complement w

lic databasefor this
between 2000
and 2009,
and ourown photometry.
Prot = 4.85 days, consistent
withthestarliterature.
This
activitycycle
reflects

analyze the simultaneous photometric counterpart provided by the ASAS pubIn both totally independent time series, we detect a possible activity cyclethat an αΩ dynamo could be
operatingin starthisbetween
star. 2000 and 2009, and our own photometry.
lic databasefor thisof period ∼ 5 years. We also derived a precise rotation period for this star
In both totally independent time series, we detect a possible activity cycle

the S-index derived from HARPS, FEROS and UVES public spectra. We

analyze the simultaneous photometric counterpart provided by the ASAS p

elivery by pebble accretion to rocky planets in habitable
Water delivery by pebble accretion to rocky planets in habitable
DRAFT: February
5, 2019 in evolving disks
34
zones
zones in evolving disks
2 and Satoshi Okuzumi2
Shigeru Ida1 , Takeru Yamamura
1
2
2
ABSTRACT
Shigeru Ida , Takeru Yamamura and Satoshi Okuzumi
1

Earth-Life Science Institute, Tokyo Institute of Technology, Meguro-ku, Tokyo 152-8550, Japan4e-mail: ida@elsi.jp
2
Departmentof Earthof
andTechnology,
Planetary Sciences,Meguro-ku,
Tokyo Institute of Tokyo
Technology,
Meguro-ku, Tokyo
152-8551, Japanience Institute, Tokyo
Institute152-8550,
Japanof the whole planet mass. Even including water in the interior, the water3
2
fraction
would
be
at
most
10
10
. Ancient Mars may have had a similar or slightly smaller water fraction. What controlled theelsi.jp
DRAFT:
February
2019 planets has not been clear, although several models have been proposed. It is important to clarify the control
ofwater
in 5,thesef Earth amountand Planetary
Sciences,Tokyo Institute of Technology, Meguro-ku, Tokyo 152-8551, Japanmechanism to discuss water delivery to rocky
planets in habitable zones in exoplanetary systems, as well as that to Earth and Mars in
ABSTRACT
our solarContext.
system.
The ocean mass of the Earth is only 2.3 ⇥ 10 of the whole planet mass. Even including water in the interior, the waterry 5, 2019
fraction
would be at most
10 delivery
10 . AncienttoMars
may have had
a similar
or slightly smaller
water
fraction.
What controlled
theAims. We
considerwater
planetsbyicy
pebblesafter
thesnowline
inwardlypasses planetary orbits. We derive the wateramount of water in these planets has not been clear, although several models have been proposed. It is important to clarify the control
mechanism(todiscuss) water
deliveryto rockyplanets in ashabitable
zones in exoplanetarysystems,
as well as that to andEarth andMars in the parameters that reproduce a small value ofmass fraction
fwaterof thefinal
planeta functionof disk
parameters
discuss
our solar system.
ABSTRACT
fwater comparable
towater
thatdelivery
inferred
the
Earth
and
ancient
Aims. We consider
to planetsfor
by icypebbles
after thesnowline
inwardly Mars.
passes planetary orbits. We derive the watermass fraction ( f) of the final planet as a function of disk parameters and discuss the parameters that reproduce a small value of
Methods.
We
calculatedof icydust mass.
grainsEvento pebbles
theinpebble
radialthedriftwith a 1D model, by simultaneously
4growthcomparable
to that2.3
inferred
for theEarth
and ancientMars.
cean mass of thef Earthis only⇥the10of thewhole
planetincludingand
water
the interior,water
Methods.
the growth of icyand
dust grains
to pebbles andof
the pebble
radialdrift witha 1D model,bysimultaneously
2 We calculated
solvingsnowlinemigration
dissipation
a
gas
disk.
With
the
obtained
pebble mass flux, we calculated accretion of icy
be at most
10 3 the10.
Ancient
Mars
may
have
had
a
similarorslightly
smallerwater
fraction.
solving the snowline migration and dissipation of a gas disk. With the obtained pebble mass flux, we calculated accretionWhat
of icy controlled thepebblesonto
planets clear,after
the snowline
passageto evaluate
fof thepebblesplanets
after
the snowline
passagetoplanets.
evaluate
fwater ofIt theplanets.to clarify the control
in theseplanets onto
has
not
been
althoughseveralmodelshave
been
proposed.
isimportant
Results. We find that f
is regulated by the total mass (M ) of icy dust materials preserved in the outer disk regions at the timing
iscuss water
deliveryrocky
planets
inisofhabitablein exoplanetarysystems,well
asfront
thatto Earthand Mars in
Results.
We
fwaterregulated
byBecause
the
total
mass
ofasicy
dust
materials
in the outer disk regions at the timing(t =t to)findofthe thatsnowlinepassagethe planetary zones
orbit.
M decaysrapidly(Mafterresthe) pebble
formation
reaches
the preserved
outer edge (at t = t ), f
is sensitive to the ratio t /t , which is determined by the disk parameters. We find t /t < 10m.
(t = tsnowdisk)
ofthesnowlinepassageof wethederive
planetary
orbit.of fBecause
Mres
decaysresults.
rapidly after the pebble formation front reaches theor > 10 is important. By evaluating
M analytically,an analytical formulathat reproduces
the numericalider water
deliverytoplanetsbyicy
pebblestheinwardlyplanetary
orbits.
We
derivethewaterConclusions.
Using
the
analyticalformula,after
we findthat fsnowlineof toa rockyplanetnear 1t aupasses
is similartothe Earth, i.e.,⇠determined
10
10 , in
disk
outer
edge
(at
t
=
t
),
f
is
sensitive
the
ratio
/t
,
which
is
by
the
disk parameters. We find tsnow /tp↵ < 10p↵of 30-50
watersnow 10p↵)M /r for disk depletion timescale
disks with an initial disk size
au and an initial disk mass accretion rate of ⇠ (10the>final
asyears.
a function
ofdisks
disk
andcompact/massive
discuss
parametersthata smallvaluethatof reproduces the numerical results.
water ) ofor
ofplanet⇠important.
a few M
Becausemay parameters
be medianslightlydisks,
our results
thatreproduce
the water
fraction
10 is
By these
evaluating
Mres oranalytically,
wethe
derivean suggest
analyticalformulaof fwater
rocky
planetsin habitablezones may often
be similar to that of the Earth if icy pebble accretion is responsible for water delivery.
e to that inferredoffor
the
Earth
and ancient
Mars.
4
2
Conclusions.
Using
the
analyticalformula,
we
find
that
f
of
a
rocky
planetnear
1
auissimilartothe
Earth,
i.e.,
⇠
10
10
,
in
water
Key words.
Planetsdustand satellites:
Accretion,
Accretion
calculated the growthof icygrainsformation,
to pebbles
andthe diskspebble radial drift with a 1D model, by simultaneously
8
7
disks
with
an
initial
disk
size
of
30-50
au
and
an
initialdisk
massaccretion
rate
of
⇠
(10
10
wline migration and dissipation of a gas disk. With the obtained pebble mass flux, we calculated accretion of icy )M /r for disk depletion timescaleof the⇠ 1.asnowline
few
M
years.
Because
these
disks
may
be
medianorslightlycompact/massive
disks,
ourresultssuggest
that
the
water
fractionanets after
passagetoevaluatefoftheplanets.
water
Introduction
able to be an actual habitat. On the other hand, too much water
rocky
planetsbyinthehabitablesimilartowithoutthatcontinents,ofthe outerEarthicypebbleaccretion
createsa planet
where disk
theifsupplyof nutrid that fof
is regulated
total masszones(Mres )mayof icyoften
dust bematerials
preserved
in theregions
at thetiming is responsible for water delivery.
water

arXiv:1901.04611v2 [astro-ph.EP] 3 Feb 2019

Context. The ocean mass of the Earth is only 2.3 ⇥ 10

4

3

2

water

water

water

water

res

snow

res

p↵

water

snow

p↵

res

snow

water

water

8

4

p↵

2

7

ents may not be as e↵ective as in the Earth. The oceans of the
Earth-size ofplanetsarebeing discoveredin habitable
zones
(HZs)
e snowline passage
theplanetary
orbit.
BecauseM
decaysrapidlyonly
after
the pebble formation front reaches theresor- Earth comprise
0.023% by weight and this amount enables
inexoplanetarysystems.
These
HZs
are
defined
as
a
range
of
words.
Planetstoandsatellites:
formation,
Accretion,
disks(at t = tKey
is sensitive
the
ratio
tsnowon/tthe, whichsuris determinedbyAccretion
theto disk
parameters.
findwater
tsnow /tp↵ < 10
oceans and continents
coexist.
The mantle mayWe
preserve
in which liquidwater
can existp↵ ), fbitalwaterradius,p↵planetary
face if H2 O
there. However, as long as equilibrium tem- in the transition zone with a comparable amount of ocean (e.g.,
rtant. By evaluating
Mexists
res analytically, we derive an analytical formula of fwater that reproduces the numerical results.
perature is concerned, H2 O ice grains condense only well be- Bercovici & Karato 2003; Hirschmann 2006; Fei et al. 2017),4
2
Using the analyticalformula,
we
find
that
f
of
a
rocky
planetnear
1
auissimilartothe
Earth,
i.e.,
⇠
10
10
, in
water
yond the HZs, because the gas pressure of protoplanetary disks while the core could have H equivalent to 2% by weight of H2 O
7of theofEarthal. 2014).
the original
water timescalemanyordersauof magnitude
lower thanthat massof planetaryatmo- rate
itial disk sizeisof
30-50
and an initial
disk
accretion⇠ (Nomura(10 8 et10
)M However,/r for disk
depletion4very small(⇠ 10an
10 2 ),
sphere and the condensation temperature is considerably lower fraction of the Earth would still be
1.
Introduction
able
to
be
actualhabitat.
On
the
other
hand,
too
much
water
ars. Becausethan
these
disks
may
be
medianorslightlycompact/massive
disks,
ourresultssuggest
that
the
water
fractionthat at 1 atm. Hereafter, we simply call H2 O in a solid/liquid even with the possible water reservoir in the interior because neiin habitable phasezones
mayForoften
be similar
to thatof gasthecapture
Earth ifthericy
pebbleaccretioniscreates
responsible
fornorwater
delivery. continents, where the supply of nutristellar
irradiation
at ⇠ 1 au (Machida& Abea2010)
giantwithoutplanet“water.”the Earth,a volatile supply
by the

惑星の水の起源は？ペブルアクリーションで惑星に持ち込む水の質量を見積もる
地球のような惑星を説明するには、
半径30-50 au、accretion rate ~10^-8~-7Msun/yrの円盤が良いents may not be as e↵ective as in the Earth. The oceans of thefrom the disk is ruled out because observed values of rare-Earthelements formation,
are too low in the
Earth to be consistent
withdisks
the disk
nets and satellites:
Accretion,
Accretion

impacts (Genda & Abe 2005) can vaporize the majority of thewater from the gravitational potential of Earth. We note that it isEarth-size planets are being discovered in habitable zones (HZs)

E

11 Univ. Grenoble Alpes, CNRS, IPAG, 38000 Grenoble, France

Department of Physics and Astronomy, California State University Northridge, 18111 Nordho↵ Street, Northridge, CA 91130, USA

35

The Disk
Substructures
High
AngularResolution
Project(DSHARP) - IX
The Disk
Substructures atat
High
AngularResolution
Project (DSHARP)- IX
A highdefinition
definition studyof theplanetformingdisk.ApJL
A highstudy
ofHDthe163296
163296planetforming(Accepted
7HD
December
2018,
in disk.
press.)

1
4
Andrea Isella,Jane Huang,22 Sean M. Andrews,2 Cornelis
P. Dullemond,3 Tilman Birnstiel,
1
2
3
4
5
5
6, 7
8
9
10, 11 Birnstiel,
AndreaIsella,Jane
Huang,
Sean
M.
Andrews,
CornelisP.
Dullemond,
TilmanShangjia Zhang, Zhaohuan Zhu, Viviana V. Guzmán,
Laura M. Pérez, Xue-Ning Bai, Myriam Benisty,
8
2
John5 M.
Carpenter,
Ricci,David J.
Wilner
jia Zhang,5 Zhaohuan Zhu,
Viviana
V.6 Luca
Guzmán,126, 7andLaura
M.
Pérez,Xue-Ning Bai,9 Myriam Benisty,10, 11

ABSTRACT6122
M.Astronomy,
Carpenter,
Luca
David
J.TXWilner
Department of John
Physics andRice University
6100Ricci,
Main Street,andMS-108,
Houston,
77005, USA
ALMA observations
ofprotoplanetarydisks
acquired
by
the
Disk
SubstructureatHigh
AngularHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
1 Department of Physics and Astronomy, Rice University 6100 Main Street, MS-108, Houston, TX 77005, USA
Resolution
Project(DSHARP)
resolvethe Str.
dust
andgas Germany
emission on angular scales as small as 3
Zentrumfr Astronomie,
Heidelberg University,
Albert Ueberle
2, 69120
Heidelberg,
2 Harvard-Smithsonian
University
Observatory, Faculty of Physics,
Ludwig-Maximilians-Universität
München, Street,
Scheinerstr.
1, 81679 Munich,Centerfor
Astrophysics,
60 Garden
Cambridge,
MAGermany
02138, USA
astronomical
units,o↵ering
anunprecedented
detailed
view
of
the
environment
where planets form.
DepartmentofPhysics
andAstronomy,
Universityof
Nevada,Las
Vegas,
4505
S.
Maryland
Pkwy,
Las
Vegas,
NV,
89154,
USA
3 Zentrum fr Astronomie, Heidelberg University, Albert Ueberle Str. 2, 69120 Heidelberg, Germany
In this article,
present
anddiscussof Santiago,
the HD
Jointwe
ALMA
Observatory,
AvenidaAlonso deobservations
Córdova 3107, Vitacura,
Chile163296 protoplanetary disk that imaged
versity Observatory,
Facultyof Physics,
Ludwig-Maximilians-Universität
München,
81679 Munich, Germany
Instituto de Astrofı́sica,
Pontificia
Universidad
Católica de12
Chile, Av. Vicuña Mackenna 4860,
7820436 Scheinerstr.
Macul, Santiago, 1,
Chile
the
1.25
mm
dust
continuum
and
CO
J=2-1
rotationalline
emissionata spatial resolution of 4 andDepartamentodeAstronomı́a,
Universidad
deChile,
CaminoEl
Observatorio
1515,
Las
Condes,Santiago,Chileartment of Physics and Astronomy, University of Nevada, Las Vegas, 4505 S. Maryland Pkwy, Las Vegas, NV, 89154, USA
Institutefor Advanced StudyTheand Tsinghua
Center for Astrophysics,
Tsinghua University,
Chinaus to characterize the previously
10 au,
continuum
observations
resolveBeijing
and100084,
allow
6respectively.
ALMA
Observatory,
AvenidaCNRS/INSU
Alonso deCórdova
3107, Vitacura,Santiago,
Chile
Unidad Mixta Joint
Internacional
Franco-Chilenade Astronomı́a,UMI
3386, Departamentode Astronomı́a,
Universidad
dediscovered
dust
rings
at
radii
of
67
and
100
au.
They
also
revealnewsmall scale structures, such
Camino El Observatorio
1515,
Las Condes,
Santiago, Chile
ituto de Astrofı́sica, PontificiaChile,
Universidad
Católica deChile,
Av. VicuñaMackenna 4860, 7820436 Macul, Santiago, Chile
Univ.
Grenoble
Alpes, CNRS,
IPAG,at
38000
Grenoble,
Franceas a darkdegap
at
10
au,
a
bright
ring
15
au,
a
dust crescent
at a radiusofChile55 au, and several
8 Departamento
Astronomı́a,
Universidad
deChile,
CaminoEl
Observatorio
1515,
Las
Condes,Santiago,
Department of Physics and Astronomy, California State University Northridge, 18111 Nordho↵ Street, Northridge, CA 91130, USA
9 Institutefainter
asymmetries.
Theforobservationsof the University,
CO and Beijing
dust 100084,
emission
inform about thefor azimuthal
Advanced Studyand Tsinghua Center
Astrophysics, Tsinghua
China
7and
December
2018,
ApJL
press.)
verticalstructureof the(Accepted
disk
allow
us
toin directly
constrain
the dedust
extinction
opticaldedepth atd MixtaInternacional
Franco-Chilenade Astronomı́a,
CNRS/INSU
UMI 3386,
Departamento
Astronomı́a,
Universidad
Camino El Observatorio
1515,asymmetries
Las Condes, Santiago,
the dust rings. Chile,
Furthermore,
theABSTRACT
observedin theChile
dust continuum emission corroborate
11 Univ. Grenoble Alpes, CNRS, IPAG, 38000 Grenoble, France
to thehypothesis
the complex
structure
HD 163296
is the result of the gravitational
ALMA
observations thatof protoplanetarydisks acquiredby the of
DisktheSubstructure
at High disk
Angulartment of Physics
andProject
Astronomy,
California
State
University
Northridge,
18111scales
Nordho↵Street,Northridge, CA 91130, USA
Resolution(DSHARP)
resolve
the
dust
and
gas
emissiononangular
as
small
as
3
interaction
with yet unseen planets.
astronomical units, o↵ering an unprecedented detailed view of the environment where planets form.
1

2

3

4

5

6

7

8

9

10

11

12

In this article, we present and discuss observations of the HD 163296 protoplanetary disk that imaged
7 December
2018,
ApJL
press.)
the 1.25 mm dust continuum (Acceptedand 12 CO J=2-1
rotational line
emission
at ainspatialresolution of 4 andKeywords:
protoplanetaryplanet-disk
interactions,submillimeter:planetary systems
10 au, respectively.
The continuumdisks,observations
resolve and allow
us to characterize
the previously
discovered dust rings at radii of 67 and 100 au.ABSTRACT
They also reveal new small scale structures, suchas a dark gap at 10 au, a bright ring at 15 au, a dust crescent at a radius of 55 au, and several
1. INTRODUCTION
informabout
responsible for the formation
azimuthal
asymmetries.
The observations
the CO andby
dust
emission
about thethe processes
ALMAfainterobservationsof protoplanetarydisksofacquiredtheDisk inform
Substructure
at High Angularvertical structure of the disk and allow us to directly constrain the dust extinction
optical depth atofplanets.
Resolution
Project(DSHARP)
resolve
the
dust
and
gas
emissiononangular scales as small as 3
n recenttheyears,
millimeter-wave
interferometersanddust rings.
Furthermore, the observed
asymmetries in the
dust continuum emission corroborate
circumstellar
disksform.
observed at a spatial resounits,o↵eringan unprecedented
detailed
viewis theof result
theSeveral
environment
where planets
to thehypothesisthat thecomplexstructureof the HD
163296 diskof the gravitational
arastronomical
infraredhighcontrast
camerashave imaged
nearbyinteraction
yet unseen
In this article,
wewithpresent
andplanets.
discuss observations of the HD 163296
protoplanetarydisk
thatreveal
imagedring-like features in the
lutionbetterthan
50
au
toplanetary systems at unprecendented
angular res12
the 1.25 Keywords:
mm dustprotoplanetarycontinuumdisks,
andplanet-disk
CO J=2-1
rotationalline emission
at a ofspatialresolutionof 4dust
and particles, as well as ofemission
small
and
large
interactions,submillimeter:planetarysystemstion in both continuum and line emission (e.g., An-

DSHARPのHD163296について
分解能ダスト~4 au, 12CO J=2-1 ~10 au
リング構造 15, 67, 100 au, gap構造 10 au 三日月状構造 55 au
構造としてunseen planet を支持

10 au, respectively. The continuum observations resolve and allow
to characterize
the previously
theusmoleculargas (Andrews
et al. 2011b,a; Boehler et al.

ws et al. 2016; ALMA Partnership et al. 2015; Isella

2Earth-Life Science Institute (ELSI), Tokyo Institute of Technology, Meguro, Tokyo, 152-8550, JapanHow
planetary
growthoutperforms
migrationHow
planetary
growthoutperforms
migration
36
ABSTRACT
1 , Shigeru Ida
2 , and Ramon Brasser2
12AndersJohansenAnders Johansen , Shigeru Ida , and Ramon Brasser2

Planetary
migration
is a major
challenge
forLundplanetformation
The speed of Type I migration is proportional to the mass of
Lund
Observatory, Departmentof Astronomy
and Theoretical
Physics,
University,
Box 43, 221theories.
00 Lund, Sweden,
anders@astro.lu.seaprotoplanet,
while andthe Theoretical
final decadeof growthof a pebble-accreting
planetarycore takes place at a rate that scales with the massy,e-mail:
DepartmentofAstronomy
Physics,
Lund
University,
Box
43,
221
00
Lund,
Sweden,2
Earth-Life Science Institute (ELSI), Tokyo Institute of Technology, Meguro, Tokyo, 152-8550, Japan1

to the two-thirds power. This results in planetary growth tracks (i.e., the evolution of a protoplanet’s mass versus its distance fromstro.lu.se
ce Institute(ELSI),
Instituteof Technology,
Meguro,(migration-dominated)Tokyo, 152-8550, Japan with rising mass of the protoplanet. It has been shown recently
the star)
thatTokyo
becomeincreasingly
horizontal
ABSTRACTthat the migration torque on a protoplanet is reduced proportional to the relative height of the gas gap carved by the growing planet.
Planetary migration is a major challenge for planet formation theories. The speed of Type I migration is proportional to the mass ofHere wesimulationsof planet-discthemass
a planet carves a 50% gap is approximately 2.3
a protoplanet,
whileshow
the finalfrom
decade1-Dof growthof a pebble-accreting
planetary coreinteraction
takes place at a thatrate thatscaleswith atthe whichmass
ABSTRACT
to thetimes
two-thirds
power.
This resultsin planetary
growthOur
tracksmeasurements(i.e., the evolution of ofa protoplanet’s
mass versus
its distancefromfrom 1-D simulations match published 3-D resultsthepebbleisolation
mass.
the pebble
isolation
mass
the star) that become increasingly horizontal (migration-dominated) with rising mass of the3protoplanet. It has been shown recently
relatively
well,
exceptvery low
viscosities(↵height<of10
thebyis3-D
pebblen thatis athemajor
challenge
planetatisformation
theories.
The
speed
Type
Iwheremigration
proportional
to the massmassof is significantly higher, possibly due
migration
torqueon aforprotoplanet
reducedproportional
to therelativeof the)gas
gap carved
thegrowingplanet.isolation
we
show
from
1-Dof
simulations
interactionthat themass ata planet
a 50%
gap
is approximately
2.3
leHeretheto
final
growthofofplanet-discathat
pebble-accreting
planetary
core
takes
place
atisolationa ratethatmassscaleswith the mass
gapdecadeedge
instabilitiesarenot captured
inwhich
1-D.
Thecarvespebbledemarks
the transition from pebble accretion to gas
times thepebbleisolation
mass.
Our measurementsof the pebble
isolation
mass fromof
1-Da simulations
match published3-D results
power.
This
resultsinplanetary
growthtracks(i.e.,
theevolution
protoplanet’s
mass
versusitsfew
distancefromaccretion.
thereforetakes placeastronomical
units of migration after reaching
relatively
well, exceptGas
at veryaccretion
low viscositiesto(↵ form
< 10 3 ) gas-giant
where the 3-D planets
pebble isolation
mass is significantly
higher, overpossiblyadue
meto increasingly
horizontal(migration-dominated)with rising
massofprotoplanet.
Itaccretion
has
been
shown
recently how planetary growth can outperform
gapfirst
edge instabilities
that arenotcapturedmass
in 1-D. and,The pebble
isolation
mass demarks
thethetransition
from pebble
to gasthepebbleisolationshortly
after,
the
50%
gap
mass.
Our
results
demonstrateaccretion.
accretion to form
gas-giant planets
therefore takes
placeover a few
astronomical
migration
torqueonGasa protoplanetis reduced
proportional
to therelativeheightof the units
gas ofgap
carvedafter
byreaching
the growing planet.
migration,
both
core
andmassduringgas aaccretion,
even
when
the
Stokes numberof the pebbles is small, St ⇠ 0.01, andthepebble isolation
massduring
and, shortly
after, accretionthe 50% gap mass.
Our
results demonstrate
how planetary
growthcan outperform
m first1-D
simulationsofplanet-discinteraction
that
the
at
which
planetcarvesa50%
gap
is
approximately
2.3
migration,
both during core accretion
andduringingastheaccretion,even when the Stokes
numberofthe nominal
pebbles is small,St ⇠ 0.01,
andthepebble-to-gas
flux
ratio
protoplanetary
disc
is
in
the
range
of
0.01–0.02.
We find that planetary growth is very rapid
solationmass. Ourmeasurementsof theisolationfrom We
1-Dfindsimulations
matchis publishedthe pebble-to-gas
flux ratio
in the protoplanetary
disc pebble
is in the nominal
rangemassof 0.01–0.02.
that planetary growthvery rapid 3-D results
3 and
the
first
millionyears
theprotoplanetary
andthatmass
the probability
forming
gas-giantin thefirstmillionyears
of the protoplanetarythat thethe
probability
fordiscforming
gas-giantplanets
with thefor
initialsize possibly
cept
atin
very
low
viscosities(↵ < of10disc) where3-D pebble
isolation
isincreases
significantly
higher,due planets increases with the initial sizeof the protoplanetary disc and with decreasing turbulent di↵usion.
ilities
thattheareprotoplanetary
not captured in 1-D.
isolation mass
demarksdi↵usion.
the transition from pebble accretion to gasofdisc The
andpebble
with decreasing
turbulent

Key words.
planet-disk
interactions,planetsand satellites:
formation,satellites:
gaseous planets
cretionto formgas-giantplanets
therefore
takesplaceplanets
over anda few
astronomical
units of migration after reachingplanet-disk
and satellites:
planetsandgaseous planets
olationKey
masswords.
and, shortly
after, theinteractions,
50% gap mass.planets
Our results
demonstrateformation,
how planetary
growthcansatellites:
outperform
ring core accretion and during gas accretion, even when the Stokes number of the pebbles is small, St ⇠ 0.01, andntroduction
by a positive corotation torque resulting from the accretion heat
flux ratio in the protoplanetary disc is in the nominal range
0.01–0.02.
We find that etplanetaryof the ofprotoplanet(Benı́tez-Llambayal., 2015)growthor from isthevery rapid
formationof protoplanetaryplanets involves many
distinctin the scattering
yearsof thedisc and
thatsteps
the probability
for forming
planets increases
with2018).
the initial sizeof (large)gas-giant
pebbles (Benı́tez-Llambay& Pessah,wthfrom anddust withand iceparticles toturbulent
full planetarysystem (a Migration can even stall entirely if theby
turbulentviscosity iscorotation
too
ary
disc
decreasingdi↵usion.
. Introduction
a positive
torque resulting from the accretion heatType I migration : 惑星massに依存、ペブルアクリーションで変化
惑星が重いほどmigration がよく効く
isation that was pioneered 50 years ago by Safronov, 1969). weak to di↵use away the gas density enhancement that forms inof the
protoplanet(Benı́tez-Llambay
et al., 2015) ormass
from thecompetition
between radialmigrationand growthis nev- terior
１D計算から、50％のgas
gapを開ける質量~2.3xpebbleisolationof theplanetaryorbit(Rafikov, planets
2002;
Li et al.,2009; Fungt-diskinteractions,planetsand satellites:
formation,planetsandsatellites:
gaseouseless formationa general themeof
in planet
formation.
The formationThe
planets
involves
many&distinct
Lee, 2018). steps in the
scattering of (large) pebbles (Benı́tez-Llambay & Pessah, 2018).
planetesimals, for example, has to overcome the radial drift
A more direct system
way to overcome
Type I migration is simply
rowth
from
dust
and
ice
particlestofullplanetary(ased bypebble
the head-wind of isolation
the slower moving gasmasson the for the
Migrationeven stall entirely if the turbulent
viscosity is too
到達から数au
落ちた時で、50%gap
形成の直後。
planetary core to increase its mass
very rapidly.can
The acwing particles (Weidenschilling,
1977; Brauer50
et al.,
2008).ago
ealisationthat was pioneered
yearsbySafronov,
1969).
cretionrateofpebblesispotentiallyhighenoughforthe protoweaktodi↵usethe heatgas density enhancement that forms inbyapositive
corotation
torqueresultingfrom
theaway
accretion
pping pebbles in pressure bumps formed in the turbulent gas planet growth to outperform the nominal rate of Type I migration
The
competition
betweenradialmigration
growthisnevw (Lyraet al., 2008; Johansen
et al., 2009a;
Bai, 2015)
or byof (Lambrechts
theandprotoplanet(Benı́tez-Llambayet theal., planetary
2015)
oforbitthe(Rafikov, 2002; Li et al., 2009; Fung
ガス惑星は大きな円盤、乱流が弱い円盤でできやすい。
& Johansen, 2014; Ormelterior
et al., 2017;
Johansen& or fromnets involves
distinct
stepsrun-awayin thepilebedded
planets (Lyramany
et al., 2009)or throughrtheless a general theme in planet formation.
The
formation
Lambrechts,2017).
Bitschet al. (2015b)
that proscatteringof(large)pebbles(Benı́tez-Llambay& Pessah, 2018).
&demonstrated
Lee, 2018).

caused by the friction on the gas (Youdin & Goodman, 2005;

37

Classical T-Tauri stars with VPHAS+: II: NGC 6383 in?
Sh 2-012T-Tauri†
Classical
stars with VPHAS+: II: NGC 6383 inarXiv:1901.07511v1[astro-ph.SR] 22
22 Janiv:1901.07511v1[astro-ph.SR]
Jan20192019

Sh 2-012?†
1,2
ABSTRACTV.
M.
Kalari‡1

1,2 Southern Operations Center, c/o AURA, Casilla 603, La Serena, Chile
Gemini Observatory,V.
M.
Kalari‡2 Gemini-CONICYT,
Departamentode Astronomı́a,
Chile,Chile
Casilla 36-D Santiago,
Chile
1 GeminiThis
paper
presents
opticalphotometry,
andObservatory,
Southern
Operations (ugriH↵)–infrared
Center,c/o AURA, Universidad
Casilla 603,(JHKs,3.6–8.0µm)
Lade
Serena,2 Gemini-CONICYT, Departamento de Astronomı́a, Universidad de Chile, Casilla 36-D Santiago, Chile
Gaia astrometry of 55 Classical T-Tauri stars (CTTS) in the star-forming region Sh 2012, andit’s centralcluster NGC 6383. The sample was identified based on photo16 December
2014
December 2014
metric16H↵emission line widths, and has a median age of 2.8±1.6 Myr, with a mass
range between 0.3–1 M . 94% of CTTS with near-infrared cross-matches fall on the
ABSTRACTABSTRACTnear-infrared T-Tauri locus, with all stars having mid-infrared photometry exhibiting
This paper
presents(ugriH↵)–infrared(JHKs,3.6–8.0µm)
photometry,evidence for accreting circumstellar
CTTS
are foundconcentrated
around andthe photometry, andThisdiscs.
paper opticalpresents
optical(ugriH↵)–infrared(JHKs,3.6–8.0µm)
Gaia astrometryof 55 ClassicalstarsT-Tauri(CTTS) stars
in the (CTTS)
star-forming
Sh 2Gaia astrometryof 55T-Tauri
Classical
in region
thestar-forming
region Sh 2central cluster NGC 6383, andtowards
thebrightrims
located
at
the
edges
of
Sh
2-012.
012, and it’s central cluster NGC 6383. The sample was identified based on photo012,
andages,
it’sline
centralNGC
samplewas
identified
metricH↵ emission
widths,cluster
and hasof
a medianageTheofburst2.8±1.6Myr,witha mass based on photoStars across the region have
similarsuggestivea 6383.
singleofstarformawidths,
has a medianage offall
2.8±1.6
range metricbetween H↵
0.3–1emission
M . 94% lineof CTTS
with andnear-infrared
cross-matcheson the Myr, with a masstion. Mass accretion rates (near-infraredṀacc) estimated
via
H↵
and
u-bandline near-infraredintensities
show
a
range
betweenlocus,
0.3–1
M
94% having
of
CTTS
with
cross-matches
fall on the
T-Tauriwithall. stars
mid-infrared
photometry exhibiting
for accretingstudies,circumstellar
discs.
CTTS
are
found
concentrated
thescatter (0.3 dex) similar to evidence
spectroscopic
indicating
suitabilityof aroundH↵ phonear-infrared
T-Tauri
locus,
withall thestars
havingmid-infrared
photometry
exhibiting
centralevidence
cluster NGC
6383,
and towards
the bright rims
locatedat theedgesof Shconcentrated
2-012.
foraccretingcircumstellar
discs.
CTTS
are
found
around thetometry to estimate Ṁacc .Stars
Examiningthevariation
of
Ṁ
with
stellarmass(M),
across the region have similar ages, suggestiveacc of a single burst of star forma⇤central cluster NGC 6383, and towards
the bright rims located at theedges of Sh 2-012.
tion.
Mass
accretion
rates
(
Ṁ
)
estimated
via
H↵
and
u-bandline
intensities
show
a
acc
we find a smaller interceptscatterin theṀ
-M
relationthan
oft-quoted
in theof literature,Stars
acrosstheregionhave
similarages, suggestive
aofsingle
burst of star formaacc⇤(0.3 dex) similar to spectroscopic
studies,
indicating
the suitabilityH↵ phoproviding evidence to discriminate
betweentheories
protoplanetary
disc
tion.
Mass
accretion
rates (Ṁ) estimatedvia
H↵ stellar
and u-band
line
intensities show aacc
tometry
to estimateṀacccompeting. Examiningthevariation
ofof
Ṁacc
with
mass (M⇤ ),(0.3dex) similar
toaccspectroscopic
studies,
indicating
the suitability of H↵ phowe findscattera smaller
intercept
in the Ṁ
-M⇤ relation thanoft-quoted
in the literature,
evolution.
providingevidence
discriminate
betweencompetingtheoriesof protoplanetary
disc stellar mass (M⇤ ),tometry
to toestimate
Ṁacc. Examiningthevariationof Ṁacc withevolution.
accretion, accretion
discs, stars: pre-main sequence, stars: variables:

Key words:
we find a smaller intercept in the Ṁacc -M⇤ relation than oft-quoted in the literature,words:
accretion,accretion
discs,
stars:
pre-mainsequence,
variables:
55個のCTTS
星形成領域Sh
T Tauri, open clustersの可視、近赤の観測
andKeyassociations:individual:
Sh 2-012,
NGCcompeting6383 stars:
providingevidence
to discriminate
betweentheoriesof2-012,
protoplanetary中心のNGC6383
disc
T Tauri, open clusters and associations: individual: Sh 2-012, NGC 6383

evolution.

2.8 1.6 Myr, 0.3-1KeyMsun
words: accretion, accretion discs, stars: pre-main sequence, stars: variables:
T Tauri, open clusters and associations: individual: Sh 2-012, NGC 6383
ほとんどのCTTSがクラスターNGC6383に集中、Sh2-012のedgeにbrightrim
as it controls the evolution of protoplanetary discs and theplanetary systems within (Alexander et al. 2014). Currently,
Hαからmass
accretionrate(Hartmannの推定、質量との関係を得る
1 INTRODUCTION
as itetcontrols
the evolution
discs and thef pre-main
sequence(PMS) evoluviscous evolution
al. 1998;
Balbus of&protoplanetary
Hawley1

INTRODUCTION

as it controls the evolution of protoplanetary discs and theplanetary systems within (Alexander et al. 2014). Currently,
In the current paradigm of pre-main sequence (PMS) evoluviscous evolution (Hartmann et al. 1998; Balbus & Hawleytion, optically visible, PMS stars, i.e. Classical T-Tauri stars1998) acting in conjunction with sources of ionisation (for
(CTTS) accrete gas from their circumstellar disc via a stellar
e.g. gamma-rays in Gammie (1999), or as summarised inmagnetosphere (Koenigl 1991; Calvet & Hartmann 1992),
Gorti et al. (2015);
Ercolano& Pascucci(2017)
from interplanetarysystems
within(Alexander
et al. 2014). Currently,
S stars, i.e. Classical1998)
actingviain conjunction
withUV-radiation,
sources ofor X-rays)
ionisation(forfacilitated T-Tauriin part by stars
removal of angularmomentumnal photoevaporation,
are considIn the current paradigm of pre-main sequence (PMS) evoluviscous evolution (Hartmann et al. 1998; Balbus & Hawley
outflows. This accretion processes results in a combination
ered the chief accretion drivers. Hydrodynamic turbulence7 Department of Physics and Astronomy, Rice University 6100 Main Street, MS-108, Houston, TX 77005, USA
8 Institute for Advanced Study and Tsinghua Center for Astrophysics, Tsinghua University, Beijing 100084, China

The Disk Substructures at High Angular Resolution Project (DSHARP):
The Disk Substructures at High Angular Resolution Project (DSHARP):
IV. IV.
Characterizing
substructuresinteractions
disks
aroundmultiplestar systems.
10 Instituto de Astrofı́sica,
Pontificia
Universidad
Católica de Chile,
Av.
VicuñaMackenna
4860,
7820436
Macul,
Santiago,
Chile
Characterizing
substructures
andandinteractions
in disksinaroundmultiplestarsystems.

38

9 Joint ALMA Observatory, Avenida Alonso de Córdova 3107, Vitacura, Santiago, Chile

Department of Physics and Astronomy,
California State 1University
Northridge,1,18111
Nordho↵Street, 4Northridge, 4CA 91130,
USA
1 1
1
1,
2, 3
2, 3
4

T. Kurtovic,Laura
Laura M.
M. PP
érez,
Benisty,
ZhaohuanZhu, Shangjia
JaneZhang,
Huang,54 Jane Huang,5NicolNicolás T.ásKurtovic,érez,Myriam
MyriamBenisty,
ZhaohuanZhu, Zhang,
Shangjia
78
9
5 5 Cornelis P. Dullemond,6 Andrea
6
7
8
9
Sean
M.
Andrews,
Isella,Xue-Ning
Bai,
John
M.
Carpenter,
Sean M. Andrews, Cornelis P. Dullemond,
AndreaIsella,Xue-Ning
Bai,
John
M.
Carpenter,
ABSTRACTViviana V. Guzmán,9, 10 9,
Luca
Ricci,11 and 11
David J. Wilner510Viviana V. Guzmán,Luca Ricci, and David J. Wilner51812.04536v1 [astro-ph.SR] 11 Dec 2018

To characterize
the substructures induced in protoplanetary disks by the interaction between stars in
1 Departamento de Astronomı́a, Universidad de Chile, Camino El Observatorio 1515, Las Condes, Santiago, Chile
12
1 Departamento
multiplesystems, we study
the
1.25
mm
continuum
and
the
CO(J
= 2El Observatorio
1) spectral line1515,
emissiondeAstronomı́a,
Universidad
de Chile, deCaminoLas ofCondes, Santiago, Chile
2 UnidadMixta Internacional
Franco-Chilena
Astronomı́a,
CNRS/INSU UMI 3386
the triple systems HT
Lup andAS
205,
at scales of ⇡CNRS,
5 au, aspart ofde
the“Disk Substructures
at High
2 Unidad3 Univ.
Mixta
Internacional
Astronomı́a,
CNRS/INSU
UMI 3386
Grenoble Alpes,Franco-Chilena
IPAG, 38000
Grenoble, France.
AngularResolution
Project”(DSHARP).
In theofcontinuum
emission,
weS. findtwo symmetricspiralNV, 89154, USA
4 Department
3 Univ. Universityof Physics
and Astronomy,
Nevada,Las
Vegas,
4505
Maryland
Pkwy,
Las
Vegas,
Grenoble Alpes, CNRS, IPAG, 38000 Grenoble, France.
5
arms in the disk aroundAS 205 N, withpitchof 14 ,60while
theStreet,southerncomponent
AS 205S,
Harvard-Smithsonian
Centerfor angle
Astrophysics,
GardenCambridge,
MA 02138,
USA
4 Department of Physics
and Astronomy, University of Nevada, Las Vegas, 4505 S. Maryland Pkwy, Las Vegas, NV, 89154, USA
6 Zentrum
itself a spectroscopic
binary,is surrounded
by a University,
compact inneranda 2,brightat a radiusoffr̈ Astronomie,
Heidelberg
Albert disk
UeberleStr.
69120ring
Heidelberg,
Germany
5Center Rice
fortidalAstrophysics,
60withGardenStreet,Cambridge,
MA 02138, USA
34 au. The 712Department
COHarvard-Smithsonianline exhibits
clear
interactions,spiralMS-108,
arms, extended
arc-likeof Physics
andsignatures
Astronomy, ofUniversity
6100 Main
Street,Houston, TX
77005, USA
6 Zentrum fr̈ Astronomie, Heidelberg University, Albert Ueberle Str. 2, 69120 Heidelberg, Germany
Institute
Advanced
Study
and Tsinghua
CenterAstrophysics,
Tsinghua University,
100084,emission, 8andhighforvelocitygas,possibleevidenceof aforrecent
close encounter
between Beijing
the disks
in China
9 Joint ALMA Observatory, Avenida Alonso de Córdova 3107, Vitacura, Santiago, Chile
DepartmentofPhysics
and Astronomy,
University 6100
Main Street,
MS-108,
Houston, TX 77005, USA
the AS7205
system, asthesefeaturesare predictedRiceby hydrodynamic
simulationsof fly-by
encounters.
108
Instituto
de system,
Astrofı́sica,
Universidad
CatólicadeChile,
VicuñaMackenna
4860,
Macul,
Santiago,100084,
Chile
In theHT LupwePontificia
detectcontinuum
emission
from
allAv.
threecomponents.
The 7820436
primary
disk, Beijing
Institutefor
Advanced
Study
and Tsinghua
Centerfor
Astrophysics,
Tsinghua
University,
China
11 Department of Physics and Astronomy, California State University Northridge, 18111 Nordho↵ Street, Northridge, CA 91130, USA
9 Joint
HT Lup A, also shows
two-armed
spiralstructurewith dea pitchangle3107,
of 4 ,Vitacura,
while HT Santiago,
Lup B
ALMA symmetricObservatory,
AvenidaAlonsoCórdova
Chileand C, locatedat 25 andPontificia
434 au in projected
separation
from
HT LupAv.
A, arebarelyresolved with
⇠ 7820436
5
10 Institutode Astrofı́sica,
Universidad
CatólicadeChile,
VicuñaMackenna
4860,
Macul, Santiago, Chile
ABSTRACTand ⇠ 10 au in diameter, respectively. The gas kinematics for the closest pair indicates a di↵erent
1 Departmentof Physics and Astronomy, California State University Northridge, 18111 Nordho↵ Street, Northridge, CA 91130, USA
To characterize
substructuresinducedin protoplanetaryby therotationinteraction
betweensense of rotationfor eachthedisk,which could
be explainedby either disks
a counterof thetwo stars in
multiple systems,
we studyplanes,
the 1.25
theof12theseCO(Jdisks= 2 with
1) spectral
line90emission ofdisks in di↵erent,
close to parallel,ormm
by acontinuum
projectionande↵ect
a close to
ABSTRACT
the triple
systems
HT Lup and AS 205, at scales of⇡ 5 au, as part of the “Disk Substructures at Highmisalignment
betweenthem.
Resolution Project” (DSHARP). In the continuum emission, we find two symmetric spiral
ToAngular
characterize
the substructures induced in protoplanetary disks by the interaction between stars inarms
in the disk aroundAS 205N, withpitch ISM:
angledust,of 14techniques:, while thesouthern
Keywords:
protoplanetarydisks, stars:
binaries(close),angularcomponent
resolution AS 205 S,
12highmultiplewe study
1.25 mm bycontinuumCO(J= 2 ring1)atspectralline emission of
itself systems,
a spectroscopic
binary,theis surrounded
a compact andinnerthedisk anda bright
a radius of12
the triple
systems
andASsignatures
205, at scales⇡ 5 au, as
partof arms,the “Disk
Substructures
at High
34 au. The
CO HTline Lup
exhibits
clear
of tidal ofinteractions,withspiralextendedarc-likeemission,and high Project”
velocity gas,possible evidenceof acontinuum
recentthatclosemostencounterbetweenthetwodisks
in
1. INTRODUCTION
may
Given
stars live
or appeartohave
AngularResolution(DSHARP).
In form.
theemission,wefindsymmetric
spiralthe
205disk
system,as thesefeaturespredictedbyhydrodynamic
simulationsoffly-by (Raghavan
encounters.
been formed
inofbinaryor
multiple
arms
inAS
the
around205 N,are
with
pitch
angle
14 , while
the systems
southerncomponent AS 205 S,
n the earlystagesofstarformation,
theAS
conservation
In thethroughHT Lupthe
system,we detectcontinuum etemissionfrom
all threecomponents.
primary thatdisk,
al. 2010;
Duchêne& Kraus2013), itTheis expectedangular momentum
gravitational
collapse
itself a spectroscopic binary, is surrounded by a compact inner disk and a bright ring at a radius of
HT LupA,
alsoandshows
two-armed
symmetric
spiralstructurewith encountersa pitch angle
4 , while
LupinB
companions
or closewillofmodify
theHT
disks
ds to the34
formation
of
a
gas
dust
disk
around
the
12
au.
The
CO at
line
exhibits
clear
signaturesof stellar
tidalinteractions,withspiralarms,
extendedarc-likeandC,
located
25
and
434
au
in
projected
separation
from
HT
Lup
A,
are
barelyresolved
with⇠5
multiplesystems,when
comparedtodisks
aroundung forming star; it is here where planetary systems
emission,
velocitygas, possible
evidenceof stars.
a recentclose
and ⇠ and
10 au highin diameter,
respectively.
The single,
gaskinematics
forthe closest
pairencounter
indicates a betweendi↵erent the disks in
isolatedsenseof system,
rotation forwhich arecouldpredictedbeexplainedbyeithera beencounterrotationof ofthe
two encounters.
Nonetheless,have
detectedaroundsinglethe AS
205
as eachthesedisk,
featuresby planets
hydrodynamic
simulations
fly-byresponding author:
Nicolás
T. Kurtovic
inmultiplefrom
systems
Eggenberger
al. 2007;disks
indi↵erent,
close weto parallel,planes,or starsby aemission
projectione↵ectof (e.g.,
these
disks
with a etcloseto
90 primary disk,
In
the
HT
Lup
system,detectcontinuum
allthreecomponents.
Theokurtovic@gmail.com
Chauvin et al. 2011), mostly at separations larger than
misalignment between them.

DSHARP 連星系について

・AS205N: spiral, pitch angle 14 , AS205S: ring ~34 au
12CO の観測からﬂy-by encounter が示唆される

・HLLup A: spiral, pitch angle 4 , BCの円盤は~5, ~10 au でほとんど分解できていない。
ABの円盤について、回転軸は反平行 or ~90

39

Extremely High Excitation SiO Lines in Disk-Outflow System in Orion Source I

Extremely High Excitation SiO Lines in Disk-Outflow System in Orion Source I.07208v1 [astro-ph.GA] 22 Jan 20191901.07208v1 [astro-ph.GA] 22 Jan 2019

ABSTRACT
3,4 , Masahiro N. Machida5 , Yuko Matsushita5 , Kazuhito
Mi Kyoung Kim1,2 , Tomoya
Hirota1,2 , Tomoya Hirota3,4 , Masahiro N. Machida5 , Yuko Matsushita5 , Kazuhito
Mi Kyoung KimMotogi
6 , Naoko Matsumoto3,7 & Mareki Honma1,8
6 , Naoko Matsumoto3,7 & Mareki Honma1,8MotogiWe present high-resolution images of the submillimeter SiO line emissions of
mikyoung.kim@nao.ac.jp
a massive young stellar object Orion Source I using the Atacama Large Millimemikyoung.kim@nao.ac.jp
ter/Submillimeter Array (ALMA) at band 8. We detected the 464 GHz SiO v=4
J=11-10 line in Source I, which is the firstABSTRACT
detection of the SiO v=4 line in starABSTRACT
forming regions, together with the 465 GHz 29 SiO v=2
J=11-10 and the 428 GHz SiO
29 SiO v=2 J=11-10 and SiO v=4
v=2 J=10-9 lines
witharesolution
of
50
AU.
The
We present high-resolution images of the submillimeter SiO line emissions of
J=11-10 lines
haveWecompact
structureswith
thediameter
of
<80
AU.
The
spatialanda massiveyoungstellarobjectOrion
SourceI
using
the
AtacamaLarge
present high-resolution images of the submillimeter SiO Millimeline emissions ofvelocity distribution
suggest that
the(ALMA)
line emissions
are8.associatedwith thebaseof theSiO v=4
ter/Submillimeter
Array
at
band
We
detected
the
464
GHz
a massive young stellar object Orion Source I using the Atacama Large Millimeoutflow andthe surfaceof Source
the edge-on
disk.is the
In contrast,
SiO v=2
J=10-9emission
J=11-10
line
in
I,
which
first
detection
of
the
SiO
v=4
in GHzstar- SiO v=4
ter/Submillimeter Array (ALMA) at band 8. We detected theline464
shows a bipolarstructure
the direction
northeast-southwest
low-velocity
outflow
forming
regions, in
togetherwith theof465
GHz 29 SiO v=2 J=11-10
and the428 GHz SiO
J=11-10 line in Source I, which is the first29 detection of the SiO v=4 line in starwith ⇠200 v=2
AU scale.
emission
exhibits
gradient
the direction
J=10-9The
lines
with a line
resolutionof a50velocity
AU. TheSiO alongv=2 J=11-10
and SiO v=429
forming regions, together with the 465 GHz SiO v=2 J=11-10 and the 428 GHz SiOof the diskJ=11-10
elongation.
the assumptionof thewithlinesWith
have compact
structures
withring
the structure
diameter of<80Keplerian
AU. The rospatial and
29
v=2 J=10-9 lines with a resolution of 50 AU. The SiO v=2 J=11-10 and SiO v=4
tation, we velocity
estimated
the lower suggest
limit ofthat
the thecentralto beare7M
and theradiusof of thedistribution
line massemissionsassociatedwiththe base
J=11-10lines
have ofcompact
structures
the diameterof J=10-9<80 AU.emission
The spatial and
12 AU< r <26
AU.and theoutflow
surfacethe edge-on
disk. with
In contrast,
SiO v=2
velocity
distributionthat theofline
emissions are associatedwiththe base of theshows
a bipolar
structure suggest
in the direction
northeast-southwest
low-velocity
outflow
outflow
andthe Thesurfaceof theedge-ondisk.
In contrast,
SiO v=2
J=10-9 emission
with
⇠200
AU
scale.
emissionline
exhibitsavelocity
gradientalong
the
direction
1
Mizusawa VLBI Observatory, National Astronomical Observatory of Japan, Hoshigaoka 2-12, Mizusawa-ku, Oshu,
showsbipolar structure
the directionof ring
northeast-southwest
low-velocityof thedisk aelongation.
With theinassumptionof thestructure with Keplerian
ro- outflow
Iwate 023-0861, Japan
with
⇠200
AU scale.
Thelimit
emissionline
exhibits
atovelocity
gradientalong
the
directiontation,weestimated
the
lower
of
the
central
mass
be
7
M
and
the
radiusof2
Korea Astronomy and Space Science Institute, Hwaam-dong 61-1, Yuseong-gu, Daejeon, 305-348, Republic of
12 AU<
r <26of thediskAU.
elongation. With the assumption of the ring structure with Keplerian roKorea

ALMA によるOrion Source 1 の観測、resolution =50 au
SiO v=4 J=11-10, 29SiO v=2, J=11-10, compact structure <80 au
tation, we
estimated
the lower
limit onofofthecentraltoMitaka,be 7 M
outﬂowの根元、edge
diskの表面
Mizusawa VLBI
Observatory,
National
Astronomical
Observatory
Japan,
Osawamass
2-21-1,
Tokyoand181-the radius of
12VLBIAU<
r <26 AU.
Mizusawa
Observatory,
National Astronomical Observatory of Japan, Hoshigaoka 2-12, Mizusawa-ku, Oshu,
8588, Japan
Iwate
023-0861,J=10-9,
Japan
SiO
v=2
bipolarstructure,
low Studies),
velocityoutﬂow ~200 au
Department of Astronomical Sciences, SOKENDAI(The Graduate
University for Advanced
Osawa
Korea 181-8588,
Astronomy
and Space Science Institute, Hwaam-dong 61-1, Yuseong-gu, Daejeon, 305-348, Republic of
2-21-1, Mitaka, TokyoJapan
Mizusawa VLBI
Observatory, National Astronomical Observatory of Japan, Hoshigaoka 2-12, Mizusawa-ku, Oshu,
Korea
ケプラー回転するリングを仮定すると
半径12 -26 au
023-0861,
Japan Sciences, Faculty of Sciences, Kyushu University, Ms~7Msun,
Department Iwateof Earthand Planetary
Motooka 744, Nishi-ku,
3

1

4

2

1

5

3

Mizusawa VLBI Observatory, National Astronomical Observatory of Japan, Osawa 2-21-1, Mitaka, Tokyo 181-

Institut für Theoretische Physik und Astrophysik, Christian-Albrechts-Universität zu Kiel, Leibnizstraße 15, 24118 Kiel, Germany
l of combining
MATISSE and ALMA observations:e-mail: jkobus@astrophysik.uni-kiel.de

42v1[astro-ph.SR]
14
Jan
2019
:1901.04342v1 [astro-ph.SR] 14 Jan 2019

Thestructure
potential of combining
MATISSE and ALMA
observations:ining theof the innermost
regioninConstraining the structure of the innermost region in40
protoplanetary discs
protoplanetary discs

J. Kobus, S. Wolf, and R. Brunngräber

J. Kobus, S. Wolf, and R. Brunngräber

ABSTRACT

In order to study the initial conditions of planet formation, it is crucial to obtain spatially resolved multi-wavelength observationsChristian-Albrechts-Universitätof the innermost region of zu
protoplanetary
discs.15, 24118 Kiel, Germany
hysik und Astrophysik,
Kiel, Leibnizstraßeysik.uni-kiel.de
Aims. We evaluate the advantage of combining observations with MATISSE/VLTI and ALMA to constrain the radial and verticalstructure of the dust in the innermost
region of circumstellar discs in nearby star-forming regions.
ABSTRACT
Methods. Based on a disc model with a parameterized dust density distribution, we apply 3D radiative-transfer simulations to obtain
Context. In order to study the initial conditions of planet formation, it is crucial to obtain spatially resolved multi-wavelength obseridealof theintensity
maps.
These arevations
innermost regionof protoplanetary
discs.used to derive the corresponding wavelength-dependent visibilities we would obtain with MATISSE
Aims. We evaluate the advantage
of combining observations with MATISSE/VLTI and ALMA to constrain the radial and vertical
ABSTRACT
as wellmaps
simulatedstructureof theas
dustALMA
in the innermost
regionof circumstellarwith
discs inCASA.
nearby star-forming regions.
Methods.
Based ona disc modelwitha parameterized dust
density distribution,
we apply
3D
radiative-transfer
simulations to obtain
Results.
Withintheconsideredparameter
space,
wefindthatconstraining
thedust
density
structureintheinnermost5
auaroundideal intensity
maps. These
are used to it
derivethe corresponding
wavelength-dependent
visibilities
we would obtain with MATISSE
the initial conditionsof planet
formation,is crucial
to obtain
spatially resolved
multi-wavelength
obsercentralstar
is challenging
with MATISSE alone, whereas ALMA observations with reasonable integration times allow us toasthewell asALMA maps
simulatedwith CASA.
gion of protoplanetary
discs.
Results. Within the considered parameter space, we find that constraining the dust density structure in the innermost 5 au aroundderivesignificant
constraints
on whereas
the disc
surfaceHowever,thatvantage of combining
MATISSE/VLTI
and
ALMA
todensity.
constrain
theintegration
radialweandfindverticalthecentral observations
star
is challengingwith
with MATISSE
alone,
ALMA
observations
with reasonable
times
allow
us to the estimation of the di↵erent disc parameters can bederivesignificant
constraints
on the indiscnearby
surfacedensity.
However,
weregions.
find that the estimationof the di↵erent
disc parameters canbe example, combining a 30-minute ALMA observationconsiderably
improvedbycombining
MATISSEandALMA
observations.
For
innermost regionofcircumstellar
discs
star-forming
considerably improved by combining MATISSE and ALMA observations. For 00
example, combining a 30-minute ALMA observation
model with a parameterized
density
distribution,
we apply
radiative-transfer
simulations
to obtainGHzwithan angularresolution
of3D
0.03
MATISSEobservationsin the L and M bands (with visibility accuracies of about(at(at310310
GHz with
andustangularresolutionof 0.03 ) for
MATISSEobservationsin the) Lforand M
bands (withvisibility
accuracies
of about
3 %) allows
theradial density slope
and the dust surface density profile
to be constrained
to withinobtain↵ = 0.3withand (↵) = 0.15,
e are used to derive
theallows
corresponding
wavelength-dependent
visibilities
wewould
MATISSE3%)
theradialdensity
slope
and
the
dust
surfacedensity
profiletobetoconstrained to within ↵ = 0.3 and (↵) = 0.15,
respectively. For an accuracy of ⇠ 1 % even the disc flaring can be constrained to within= 0.1. To constrain the scale heightmulated with CASA.
within5 au, M band accuraciesof 0.8% are required.
While
ALMA
is sensitive
todiscthe numberof largecan
dust grains
settled to the disc to within
respectively.
Foranaccuracy
of
⇠
1
%
even
the
flaringbeconstrained
=
0.1.
To
constrainthescaleheightto
we wefind thatthethat
impactconstrainingof the surface densityof the large
grains on thequantities is 5
small.
dered parametermidplane
space,
findthedistribution
dust density
structurein observed
the innermost
au aroundwithin5au,M
band
accuracies
of
0.8
%
are
required.
While
ALMA
is
sensitivetothenumber
of
large
dust
grainssettled
to
the
disc
Key
words.
Protoplanetary
discs–
Radiative
transfer–
Techniques:interferometric–Stars:
variables:
T
Tauri,
HerbigAe/Beging with MATISSE alone, whereas ALMA observations with reasonable integration times allow us to
midplane
weHowever,find thatwe
thefind
impactofestimation
the surface
density
distributionof thecanlarge
ts on the disc surface
density.
that theof thedi↵erent
disc parameters
be grains on the observed quantities is small.
Context.
Institut
für Theoretische Physik und Astrophysik, Christian-Albrechts-Universität zu Kiel, Leibnizstraße 15, 24118 Kiel, Germany
e-mail: jkobus@astrophysik.uni-kiel.de00

combining1.MATISSE
and ALMA observations. For example,form?
combininga migration
30-minute
ALMA
observation
IntroductionHow
does
influencetheplanetformation proKey00 words. Protoplanetary discs – Radiative transfer – Techniques: interferometric– Stars: variables: T Tauri, Herbig Ae/Be
ar resolution of 0.03 ) for MATISSE observations in the L andcess?
M bands(withbyvisibilityof about(see reviews
Morbidelliaccuracies& Raymond 2016;
Wolf et al.
The di↵erences between exoplanets and the planets in the solar 2012).
sity slope andthe dust surface density profile to be constrained to within ↵ = 0.3 and (↵) = 0.15,
system became apparent with the first detection of an exoplanet
formationmodels are theoftenscale
based heighton the minimum
cy of ⇠ 1 %evenathediscstarflaring
be constrained
within Planet= 0.1.
To constrain
toorbiting
Sun-like(Mayorcan& Queloz
1995), whichtoturnedmass solar nebula (MMSN). The MMSN is a protoplanetary disc
out
to
be
a
hot
jupiterorbiting
51
Pegasiwithasemi-majoracies of 0.8 % are required. While ALMA is sensitive to the number
ofjustlarge
dustsolid
grainssettledtothe
theplanets
disc of thecontaining
enoughmaterialtobuild
Introduction
form?
does
migration
influencetheplanetformationpro⇣ ⌘ How
axis
of 0.05 au.density
Today, morethan 3800 exoplanets(exoplanet.eu;
1.5
mpact of1.
thesurface
distribution
of
the
large
grainsontheobserved
quantities
issmall.
rg cm 2
Schneider et al. 2011) are known, showing great heterogeneity solar system and has a surface density ⌃ = 1700

VLTIとALMAの combining で円盤内縁半径と厚み方向の構造を評価
輻射輸送計算とCASAの模擬観測
cess?
(seeon reviewsby Morbidelli & Raymond 2016; Wolf et alis basedtworegarding their masses and sizes as well as their orbital separa- (Hayashi 1981). The construction of the MMSN
半径~5au でダスト密度の冪を誤差0.3,面密度の冪を誤差0.15で得られる。
ry discs –The
Radiative
transfer –between
Techniques:interferometric– Stars:
variables:inT the
Tauri,
HerbigAe/Be
exoplanets
andtheplanetsolarmain planets
assumptions:a)formation
process
tions di↵erences
and orientations. For
two decades now,the developmentof the2012).has an effi1 au

ciency of 100
and b)
the planets formed in situ. The in situ forplanet formation
modelsapparent
explaining thewith
broad varietyof planesystembecamethe first
detection
of% anexoplanet