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
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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
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at HighAngularResolution
Project (DSHARP):5, 6
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7
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Viviana V. Guzmán,
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Astronomy & Astrophysics manuscript no. 34556corr
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32

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33

Zentrumfür Astronomie,
Heidelberg
UeberleStr. 2, 69120
Heidelberg, Germany
Water
delivery by
pebbleUniversity,
accretionAlbert
to rockyplanetsin habitablec ESO 2019
Astronomy & Astrophysics manuscript no. paper
3 Department of 1
1,2
3,4
1⋆
Physics
andAstronomy,
Rice
University,
6100
Main
Street,Houston,TX
77005,
UnitedStatesofAmerica
Harvard-Smithsonian
Centerfor
Astrophysics,
60
GardenStreet,Cambridge,
MA02138,
UnitedStatesofAmericaA.
P.
Buccino,M.
Flores, C. I. Mar
R.
V.
Ibañez
Bustos†,zones
inevolving
disks
January 11, 2019
2 Departamento de Astronomı́a, Universidad de Chile, Camino El Observatorio 1515, Las Condes, Santiago, Chile
4 DepartamentodeAstronomı́a,
Universidad
de Chile,El
1515,
Las Condes,
Santiago, Chile5
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2 and Satoshi
2
Shigeru
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Flores,C.
I.
MartinezR.
V.
Ibañez
Bustos†,D.
Maizel,SergioMessina
and
P.
J.
D.
Mauas
The
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AngularResolution
Project(DSHARP)IX
3 Department
5 JointofALMA
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and Astronomy,
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1 Instituto
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2 Departamento de Fı́sica. FCEyN-Universidad de Buenos Aires, Buenos, Argentina.
dey Fı́sica
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7 Department of5Physics
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2
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4States ofDepartmentofPhysics
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Rice
University,
6100
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Street,Houston,TX
77005,
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Universityof
Nevada,Las
Vegas,
4505
S.
Maryland
Pkwy,
Las
Vegas,
NV,
89154,
USA
Andrea Isella,Jane
Huang,
Sean
M.
Andrews,
CornelisP.
Dullemond,
TilmanBirnstiel,How
planetary
growthoutperforms
migration
2 Departamento
de Fı́sica. FCEyN-Universidad
de Buenos Aires, Buenos,
Argentina.
6
3 Instituto de Ciencias
5
5
6,
7
8
9
10,Universidad
8 Institute
Astronómicas,
de la Tierra
y11
del Espacio (ICATE-CONICET),
San Juan, Argen
UnidadInternacional
Franco-Chilenade Astronomı́a,
CNRS/INSU
UMI
3386,
Departamentode Astronomı́a,de
Draft
versionDecember
12,
2018
Shangjia
Zhang,
Zhaohuan
Zhu,
Viviana
V.
Guzm
án,
Laura
M.
P
érez,
Xue-Ning
Bai,
MyriamBenisty,
forMixta
Advanced
Study
andTsinghuaCenterfor
Astrophysics,
Tsinghua
University,
Beijing
100084,China
DRAFT: February 5, 2019
3 Instituto
1 ,in
2 El
2Juan, Argentina.
de Ciencias
Astronómicas,
de laTierray del6 Ida
Espacio(ICATE-CONICET),San
122Chile,
CaminoObservatorio
1515,
Las J.
Condes,Santiago,
ChileExactas, Fı́sicas y Naturales, Universidad Nacional de San Juan, San Juan, Arge
Typeset using LATEX
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style
AASTeX62
AndersJohansen
Shigeru,andRamon
Brasser
4 Facultad
9 Unidad Mixta
dedeCiencias
John
M.
Carpenter,
Luca
Ricci,
andDavid
WilnerInternacional
Franco-ChilenadeAstronomı́a,
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 ChileClassical
T-Tauristars
with
VPHAS+:
II:
NGC
6383
in
Chile,
CaminoEl
Observatorio
1515,
Las
Condes,Santiago,
INAF-Catania
AstrophysicalObservatory, via S. Sofia 78, 95123, Catania, Italy
11
45 Context.
DepartmentofPhysics
andAstronomy,
Rice
University
6100
Main
Street,MS-108,
Houston,TX
77005,USA
Lund
Observatory,
DepartmentofAstronomy
andTheoretical
Physics,
Lund
University,
Box
43,
221
00
Lund,
Sweden,
The
ocean
mass
of
the
Earth
is
only
2.3
⇥
10
of
the
whole
planetmass.
Even
including
water
in
the
interior,
thewater
8 Institute
INAF-Catania
AstrophysicalObservatory,via
S. Sofia
78, 95123, Catania,
Italy for Astrophysics, Tsinghua University, Beijing 100084, China
for
Advanced
Study
andTsinghuaCenter
?
10
3
2
IPAG,
38000
Francefraction
would be atUniv.
most 10 Grenoble
10 . AncientAlpes,
Mars may CNRS,
have had a similar
or slightly
smallerGrenoble,
water fraction. Whatcontrolled thee-mail: anders@astro.lu.se
2 Harvard-Smithsonian
Sh
2-012
†
Centerfor
Astrophysics,
60
GardenStreet,Cambridge,
MA02138, USA2
9 University
amount
of
water
in
these
planets
has
not
been
clear,
althoughseveralmodelshave
been
proposed.
Itisimportanttoclarify
thecontrol
Earth-Life
Science
Institute(ELSI),
Tokyo
InstituteofTechnology,
Meguro,Tokyo,
152-8550,
Japan
Observatory,
FacultyofPhysics,
Ludwig-Maximilians-Universität
München,Scheinerstr.
1,
81679 Munich,Germany
11 University Observatory, Faculty of Physics, Ludwig-Maximilians-Universität München, Scheinerstr.
1,
81679
Munich,Germany
3 Zentrummechanism
to discuss water delivery
to rocky planetsin habitable zones
in exoplanetarysystems,
well69120
as that to Earth
Mars in2018
LastandupdatedMay 2thfr Astronomie,
Heidelberg
University,
AlbertUeberleStr.as 2,
Heidelberg,
GermanyLastupdated
2018
May
2th
10
our
solar
system.
Joint
ALMA
Observatory,atAvenida
Alonso deCórdova 3107,
Vitacura,
Santiago, Chile
The
Disk
Substructures
HighUniversity,
AngularResolution
Project(DSHARP):12
4 University
DepartmentofAstronomy,
Van
Vleck
Observatory,
Wesleyan
96
Foss
Hill
Drive,
Middletown,
CT 06459,
USA
Aims. Faculty
We considerof
water
delivery to planetsbyicy pebbles after the snowline inwardly passes
planetary orbits.
We derive the water
1,2
Observatory,
Physics,
Ludwig-Maximilians-Universität
München,Scheinerstr.
1,
81679
Munich,Germany
ABSTRACT
11 Instituto
c ESO
V.
M.
Kalari‡Astronomy&
Astrophysics
manuscript
no.
p
2019
de
Astrofı́sica,
Pontificia
Universidad
CatólicadeChile,
Av.
VicuñaMackenna
4860,
7820436
Macul, Santiago, Chilemassfraction
(
f
)
of
the
final
planetasafunctionofdiskparameters
anddiscusstheparametersthat
reproduce
a
small
value
of
IV.
Characterizing
substructuresandinteractions
indisks
aroundmultiplestarsystems.
water
13 Department
1 Gemini
5 Department
of 12
Physics
andAstronomy,
California
State
University
Northridge,
18111
Nordho↵Street,Northridge,CA91130,
USA
Observatory,
Operations
Center,c/o
AURA,
Casilla603, 4505
La Serena,
Chile
January
2019of Physics
andAstronomy,of
Nevada,Las
Vegas,S.
Maryland
Pkwy,
Las
Vegas,
NV,
89154,
USA
fwater15,
comparable
to thatSouthern
inferredUniversity
forthe Earth andancient
Mars.
2 Gemini-CONICYT,
Planetary migration
is a major
challengeforplanetformation
theories.
The
speed
of
Type
I migration
is proportional
to
the
mass
of Drive, Middletown,
Department
ofWe
Astronomy,
Van
Vleck
Observatory,
Wesleyan
University,
96
Foss
Hill
CT 06459, USA
ABSTRACT
DepartamentodeAstronomı́a,
Universidad
deChile,
Casilla36-D
Santiago,
Chile
ABSTRACT
Methods.
calculated
thegrowthoficy
dust
grainstopebblesandthepebbleradial
drift
with
a
1D
model,
bysimultaneously
6 Joint
1 Observatory, Avenida
1 Alonso de Córdova 1,
2, 3
4
4
5
ALMA
Vitacura,
Santiago,
a 13
protoplanet,
while
the final
decadegrowth andofM.
adissipation
pebble-accreting
planetarycore
takes placeata ratethat
scales withthe mass
Nicol
ás
T.
Kurtovic,
LauraPérez,
Benisty,
Zhaohuan
Zhu,
Zhang,
Jane
Huang,
solvingthesnowlineof
migrationof a gasMyriam
disk.
With theobtained
pebble3107,
mass
flux,
we calculated
accretionof Shangjia
icyChile
Departmentof ThisPhysics
andAstronomy,
California
State
Northridge,
18111
Nordho↵Street,Northridge,CA91130,toUSA
Mgrowth
stars
are
ideal
targets
to ofsearchplanets.
usu- from
MSourcestars are ideal
search for Earth-like planets. Hopebbles
ontoresults
planetsin
after
thesnowlinepassagetoevaluate
fwatertheLines
planets.
5planetary
6for
7
8 in
to thetwo-thirds power.
tracks(i.e.,
theevolution
ofUniversity
aEarth-likeprotoplanet’s
massHowever,versusitsthey
distance
7
Extremely
High
Excitation
SiO
in Disk-Outflow
SystemOrion
I 9 targets

36
37

SR] 22 Jan 201938
39

01.01433v1 [astro-ph.SR] 5 Jan 201935

1901.01433v1 [astro-ph.SR] 5 Jan 2019v2 [astro-ph.EP] 3 Feb 2019

2018
10
Jan
2019
[astro-ph.SR] 15 Jan 201934

Instituto de Sean
Astrofı́sica,
Pontificia
Universidad
CatólicadeChile,
Av.
VicuñaMackenna
4860,
7820436
Chile
ABSTRACTM.
Andrews,
CornelisP.
Dullemond,
AndreaIsella,Xue-Ning
Bai, Macul,
John Santiago,
M. Carpenter,
Results.
We findhorizontal
that fwateris(migration-dominated)
regulated
by
the
total
mass
(M
)
of
icy
dust
materials
preserved
in
the
outer
disk
regionsatthetimingres
the star) that become
increasinglywithrisingmassoftheprotoplanet.
It
has
been
shown
recently
ally have high levels of magnetic
which could
aﬀect their habitability
16 (tDecember
2014
9, 10M activity,
11
5
ally have high levels of magnetic activity, which could aﬀect
8 Departamento
=
t
)
of
the
snowlinepassageoftheplanetary
orbit.
Becausedecaysrapidlyafter
thepebbleformation
front
reaches
the
snow
res
Viviana
V.
Guzm
án,
Luca
Ricci,andDavid
J.
Wilnerde
Astronomı́a,
Universidad
deChile,
CaminoEl
Observatorio
1515,
Las
Condes,Santiago,
Chile
that
the
migration
torqueonaprotoplanetisreducedproportionaltotherelativeheight
of
the
gas
gap
carvedby
thegrowingplanet.
The
Disk
Substructures
AngularResolution
Project
used
ALMA
to
map
disk outer edge (at t = attp↵ ), High
fwater andis1,2
sensitivetothe ratiothe
tsnowdetection/tp↵ , which
determinedbythe diskparameters.
We findtsnow/tp↵< 10 the 1.255 millimeter
make
diﬃcult
ofis exoplanets
orbitingaroundthem.
Unfor3,4
5
ABSTRACT
Here
we
show
from
1-D
simulationsofplanet-discinteraction
that
the
mass
at
which
a
planetcarvesa50%
gap
is
approximately
2.3
9 Institute for Advanced
and make diﬃcult the detection of exoplanets orbiting arou
KyoungKim, Tomoya
Hirota, Masahiro
N.
Machida, YukoMatsushita, Kazuhitoor > Mi10 ispotential
important.
By evaluating
Mcombining
we deriveananalyticalformula ofand
fwaterthat ALMA
reproduces
the numericalresults.
Study
andTsinghuaCenterfor
Astrophysics,
Tsinghua
University,
Beijing
100084, China
res analytically,
Theof
MATISSEobservations:1times the pebble
isolation
mass. Using
Our
of
the
pebbleisolation
mass
1-D
match
4results
2 a systematic
continuumofWe
protoplanetary
disks
at
a
spatialresolution
5
au.
We
present
analysis
tunately,
long-term
variability
offrom
dM
stars
has
been
extensively
studied,Departamento
de measurements
Astronomı́a,
Universidad
deChile,
CaminoEl
Observatorio
1515,
Chile
Conclusions.
the analyticalformula,
we
find
that
fwater ofa rockyplanetnearsimulations
1of
aunot
is⇠
similartothe published
Earth,
i.e.,
⇠3-D
10
10 Las
,1,8
in Condes, Santiago,
ABSTRACT
63,7
10 Unidad relatively
3
presentananalysis
ALMA
1.25
millimeter
continuum
observationsof spiral
structuresintunately,
long-term
variabilityof dM stars has not been ext
7 & Mareki
Mixta Internacional
CNRS/INSU
UMI
3386,
DepartamentodeAstronomı́a,
UniversidaddeMotogi,
Naoko
MatsumotoHonmawell, except
atveryFranco-Chilena
lowviscosities(↵30-50< de
10auAstronomı́a,
) of
where
thedisk
3-D
pebbleisolationmass
is8 significantly
higher,possibly
due
disks
with
an
initial
disk
size
of
and
an
initialmass
accretion
rate
of
⇠
(10
10
)M
/r
for
disk
depletion
timescale2
Constraining
thestructureoftheinnermostregion
in
due
to
their
low intrinsic
brightness.
Forthethisreason,in1999
westartedthe to gas No
UnidadMixta
Internacional
Franco-ChilenadeAstronomı́a,
CNRS/INSU
UMIdominant
3386
of annular
substructures
in
the
18
single-disk
systemstargetedinthissurvey.
archito gap edge instabilities
that
are
not
captured
in
1-D.
The
pebbleisolation
mass
demarkstransitionfrompebbleaccretion
of
⇠
a
few
M
years.
Because
these
disks
may
be
medianorslightlycompact/massive
disks,
ourresultssuggest
that
the
water
fraction
Chile,
CaminoEl
Observatorio
1515,
Las
Condes,Santiago,
Chile
three
protoplanetary
disks
from
Disk
SubstructuresatHigh
AngularResolution
The brightness. For this reason, in 199
This
paperthepresents
optical(ugriH↵)–infrared(JHKs,3.6–8.0µm)
photometry,and dueProject.
to their low intrinsic
3HKαof rockyplanetsin habitableplanets
zones
may
often
be
similar
to
that
of
the
Earth
if
icy
pebbleaccretionisresponsible
for
water
delivery.
accretion.
Gas
accretiontoform
gas-gianttherefore
takes
place
over
a
few
astronomicalunitsof
migration
afterreaching
project,
which systematicallyobserves
the spectraof aGrenoble,large
number
Univ.
Grenoble
Alpes,
CNRS,
IPAG,
38000
France.
tectureemergesfrom
thissample;instead,remarkably
diversemorphologies
areobserved.
Annularprotoplanetary
discs
11 Univ.
Gaia
astrometryof
55
Classical
T-Tauristars(CTTS)
inthestar-forming
regionSh
2Grenoble
Alpes,
CNRS,
IPAG,
38000
Grenoble,
Francedisks
around
Elias
27,
IM
Lup,
and
WaOph
6
were
observedataresolution
of
⇠
40
60
mas
(⇠
6
7
mikyoung.kim@nao.ac.jp
first
the pebble isolation
mass and,shortly
after, the
50% gap
mass. Our
results
demonstrate how planetary growth can outperform
HKα
project,
which
systematicallyobserves the spectra o
Key words.
Planetsand satellites:
formation,
Accretion,
Accretiondisks
4 Department
012,
and
it’s
centralcluster
NGC
6383.
The
samplewas
identified
basedonphotoofstars,
inparticulardMstars,
attheComplejo
Astronómico
El
LeoncitoofPhysics
andAstronomy,
Universityof
Nevada,Las
Vegas,
4505
S.
Maryland
Pkwy,
Las
Vegas,
NV,
89154,
USA
12 Department
substructuresanyradiusmillimeter
continuum
emissionisdetected
andmigration,
both during
coreoccur
accretionand virtuallyduringgas accretion,even
when thewhere
StokesNorthridge,
numberof the pebbles
isNordho↵
small, St ⇠ 0.01,
and Northridge,of Physics
andAstronomy,
California
State
University
18111
Street,CA
91130,USA Gasau).canAll
threeatdisks
featurem=
2
spiralpatterns
inconjunction
withannularsubstructures.
S. Wolf,
and R. Brunngräber
metric J.
H↵Kobus,emissionline widths,
and has a median age of 2.8±1.6 Myr, with a mass40

elivery by pebble accretion to rocky planets in habitable
Water delivery by pebble accretion to rocky planets in habitablezones in evolving
disks disks
34
zones in evolving

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
cienceInstitute, Tokyo
Instituteof Technology, Meguro-ku, Tokyo 152-8550, Japanが内側に移動し、惑星の水の起源として、惑星形成後snowline
87
Department of Earth and Planetary Sciences, Tokyo Institute of Technology, Meguro-ku, Tokyo 152-8551, Japan
1) Ṁg,0 = 3 ⇥ 10 , 10 M /y,@elsi.jp
of Earth
Planetary Sciences,
Tokyo Institute of Technology, Meguro-ku, Tokyo 152-8551, Japan98
icyandpebble
が降着するシナリオを考える。
DRAFT: 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
uary 5, 2019
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.
di↵
←~α
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
pebbleABSTRACTamount 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
2
2 andYamamura2
Ida1 , Takeru
Satoshi Okuzumi
Shigeru Ida1 , Takeru Shigeru
Yamamura
Satoshi2 andOkuzumi1

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

Water Fraction

solarissystem.
ocean mass of the ourEarthonly 2.3 ⇥ 10 4 of the whole planet mass. Even including water in the interior, the water
Aims.2 We consider water delivery to planets by icy pebbles after the snowline inwardly passes planetary orbits. We derive the water3
be at most 10
10 fraction. Ancienthaveashada similar
slightlyand
smallerwater
fraction.
What controlledmass( fwaterMars) of the may
final planet
a functionof diskor
parameters
discuss theparametersthat reproduce
a small value the
of
g,0
di↵
g,0
pe
fwaternot
comparable
to that althoughinferred for the
Earth andancient haveMars. been proposed.青：snowline
er in these planets has
been clear,severalmodels
It is important to clarify the control
Methods.
We calculatedof icyzones
dust grains
to pebbles and thepebble radial
drift witha 1D tomodel,
by simultaneously
discuss water delivery
to rockyplanets thein growth
habitable
in exoplanetarysystems,
as wellas thatEarthand Mars insolving 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m.
pebbles onto planets after the snowline passage to evaluate fwater of the planets.
g,di↵
We findis regulatedby themass (Mresinwardly) of icy dustpasses
materialsplanetarypreserved in orbits.
the outer We
disk regions
the timing
緑：円盤半径sider water deliveryResults.
to planets
bythaticyfwater
pebbles
after
thetotalsnowline
deriveatthewater(t = tsnow ) of the snowline passage of the planetary orbit. Because Mres decays rapidly after the pebble formation front reaches the6
fwater ) of the final planet
asafunctionofdiskparameters
anddiscusstheparametersthat
reproduce
a
small
value
of
disk 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↵ < 10
ble to that inferred forandByancientMars.
or >the10 isEarthimportant.
evaluating
Mres analytically, we derive an analytical formula of fwater that reproduces the numerical results.
Conclusions.
analyticalformula, weandfind thatplanetnearwith
1 au isasimilar
to the Earth,i.e.,⇠ 10 4 10 2 , inwater of a rocky
calculated the growthof icy Using
dust thegrainsto pebbles
the fpebble
radialdrift
1D
model,
bysimultaneously
disks 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 timescaleowline migration anddissipation of a gas disk. With the obtained pebble mass flux, we calculated accretion of icyof ⇠ a few M years. Because these disks may be median or slightly compact/massive disks, our results suggest that the water fraction
lanets after the snowline
evaluateof theplanets.
of rockypassage
planets in tohabitable
zones fmay
be similar
to that of the Earth if icy pebble accretion is responsible for water delivery.
wateroftennd that fwater is regulatedby the total(Mformation,
dust materials
preserved in・pebble
the outer disk regionsat the timingres ) of icy
は内側から外側に向かって形成が進む（pebble
形成半径）
Key words.
and mass
Accretiondisks
aursatellites:
au Accretion,
rsnow,vis
1. Time evolution ofrd,0
the =30transition
radiusPlanets
rvis/irr (Eq.
5;
red=100
lines),
snowlinersnow = max(r, rsnow,irr) au(Eqs. 6 and 7; blued,0d,0=300
hedisksnowlinepassageof(green
the lines),
planetary
orbit.
Becausedecaysafter disk
theevolution
pebble formation front reaches theres36;s),characteristic
radius t˜rd,0and pebble
formation
front rp↵M(Eq.
magenta rapidly
lines) for various
4 yr
5 yr
6 yr
t
=4x10
t
=2x10
t
=1x10
pﬀ
pﬀ
pﬀ
r
in
units
of
au
and
Ṁ
in
units
of
M
/y
are
labeledintheindividual
panels.
The
otherparameters
emeters.
(at t The= tparameters,),fissensitive
to
the
ratio
t
/t
,
which
is
determined
by
the
disk
parameters. We 形成半径が円盤半径を超えるとpebble
find tsnow /tp↵ < 10
d,0
g,0
p↵
water
snow p↵・pebble量が減少（tpﬀ）
9
6
Yamamura,
Water
delivery by icy pebbles
10 panels, i.e., Ṁpe = 10 Ida,
10 and tOkuzumi:
10
he
same
for
the
four
M
/y
=
10
y.
di↵
1. Introduction
be anthat
actualhabitat. Onthe
the numericalother hand, toomuch waterortant. By evaluating
Mres analytically,
we derive an analyticalformulaableof tofwater
reproduces
results.
10
10
10
2of nutriplanet without
continents,
where
the4 supply
10
10
Using the analyticalformula, we findthat fwater of a rocky10 planet near creates
1 au isasimilartotheEarth,
i.e.,
⇠
10
10
, in
・惑星に水が供給されるのはsnowline
が内側に移動した後 (tsnow)
ents
may
not
be
as
e↵ectiveasintheEarth.
The
oceansof the101010planets
are being
discovered
habitableryos with the massesEarth-sizeand semimajoraxes identicalto Venus,
The infilteringfactorzones
is given(HZs)by87
nitial
disk
size
of
30-50
au
and
an
initialdisk
massaccretion
rate
of
⇠
(10
10
)M
/r
for
disk
depletion
timescale
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
Earth
Earth
/rdisks,Mpl>
ears. velocity
Because
these
disks
may
be10mediancompact/massive
ourresultssuggestthe water
fractionwater
Mplanetary↵ sur- hgoceansStr coexist. thatelative
is given= (3/2)b
regime”).
⇤set ⌦ (”Hill>andcontinents
to
The mantle
may preserve
bital
waterorcanslightly
exist
on
the
>
Mars radius, in which liquid
Mars
Mars
10
10
>
0.017
・惑星の水の量はt/tsnow
pﬀ 〜10の前後で大きく変化
>
Venus
Venus
Venus
2
>
stitutingthis into 10Eq.zones
(24),
>
M
0.02
0.1
0.1M
1au
10
in
the
transition
zone
with
a
comparable
amountofocean(e.g.,
10
10s in habitable
may
often
be
similar
to
that
of
the
Earth
if
icy
pebbleaccretionisresponsible
for
water
delivery.
>face if0.1H2 O exists
there.
However,
as long
as equilibrium
tem>
>
0.01
1
5 10 0.01
0.1
5 10 0.01
0.1
1
5 10
>1

M

= 2t

( Ṁ

t
= 0.06
10 y

0

0

0

-1

-1

-1

-2

-2

-2

-3

-3

-3

-4

-4

-4

-5

-5

-5

-6

-6

-6

-7

-7

-7

ter Fraction[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
>
core
could have H equivalent to 2% by weight of H2 O
lanetsandsatellites:
formation,
Accretion,
Accretion
disks
yond
the
HZs,
becausethegaspressureof protoplanetary
disks
✓yr
◆(M)
>
6
5the
1/2 7; blue>
1. Timetevolutionofthetransition
radius
r
(Eq.
5;
red
lines),
snowline
r
=
max(r
,
r
)
(Eqs.
6
and
M
t
=1x10
snow
snow,vissnow,irr>
snow =1x10 yr! (M) vis/irr tsnow >10 tpﬀ
snow
M
St
r
pl
⇤
>
>
(M)
ofThe
the
Earthdisk(Nomura1/3 of>0.040
isradiusmanyordersmagnitude
lower
than
that
of10 planetaryatmo-lines)
6 front
79>s), disk characteristict˜rd,0(greenlines),
andpebbleformation(Eq.
36;
variousevolutionet al. 2014). However, the original waterM>
Fig. 3. Timeevolutionofwater
fractionforthemodels
with
t
=
10
y,
Ṁg,0 =rp↵
M /y,andmagentaṀ/y. forleft, center,pldi↵pe = 10 M0.1M
>
M
0.1
1au
1/3
4
2
>
6results
6 Earth,>⇡sphere2Strshowr.of(27)
fraction
of
the
Earth
would
still
be
very
small
(⇠
10
10
),
and
the
condensation
temperatureisconsiderably
lower
andbset
right
panel
the
rd.0and= 30au,100au,
and 300au,
respectively.
The blue,red,
andgreen lines1x10
representthe:meters. The parameters,
units
of
au
Ṁ
in
units
of
M
/y
are
labeledintheindividual
panels.
The
otherparameters2.5x10yr(E)yr(E)
d,0 in
g,0
[M
>
M
;
2D],
3M
pl
2D3D
<106 tcall
pﬀ(V)Mars and Venus
analogs, ⇤respectively. 9
10 that
10 O in a solid/liquideven with the possibleH
he same for the four thanpanels,i.e.,atṀ1peatm.
= 10Hereafter,
M /y andwetdi↵simply= 10 y.
2(29)water reservoir in the interior because nei6
6
10
10
5x10
yr For(V)the Earth, a volatile
2x10yr(V) Onat ⇠ther stellar
irradiation
1 au(Machida
& Abe
2010)
nor giant
phase“water.”supplybyablethe (21).
gas
capturewhere
we10used
Eq.
to
be
an
actualhabitat.
the
other
hand,
too
much
water
10
We
take
into
account
thedecreaseindust
surfacedensity
impacts(Genda
&
Abe
2005)
can
vaporizethemajorityof
thefrom the disk is ruled out because observed10values of rare-Earthryos with the masses and10semimajor axes identical to Venus, The
filteringfactorisgiven
bycreatesplanetwithout
whereof thedue
to pebble
accretion
onto
the planets.
After10
10 flux
water
fromthe continents,
gravitational
potential
Earth.supply
We note ofthatnutriit is
he numerical simulations,
we areusetooa morefor- toandelements
low ingeneral
the Earthbe pebble
consistentwiththea disk
0

0

-1

-1

-2

-2

-3

-3

-4

-4

!

Ṁ )

Ṁ
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

Johansen & Lambrechts (2017)(12)demonstrated
that thecontributes
accretion ofplanetesimals
significantly
to thegrowthfrombarrier(Okuzumi
et al., 2012),
while CO
ice
(and
lik
Ṁg = 2⇡rur ⌃g ,2
2. Analytical pebble accretion
growth tracks
tionofplanetesimals
contributes
significantly
tothegrowthfromplanetesimalsizes
toprotoplanetswithmasses
0.001
0.01
M
Et
as
well)
appearstohavesticking
properties
similarow
planetary
growthoutperforms
migrationplanetary
growthoutperforms
migrationṀp = How2⇡rv
n growth
tracks36
r ⌃p .
duetothe0.001
low ratesof 2016a,b).
pebbleaccretionin theBondi
regimeplanetesimal sizes to protoplanets (13)withmasses0.01
ME,(Musiolik
et
al.,
The
CO
ice
line
sits
at
2
In thissectionwederiveanalyticalexpressions
forthegrowth1222Anders1 Johansen, Shigeru
Ida, andRamonBrasser
Brasser ofwhileature
pebbleaccretion
in
the
Hill
regimedominates
thefurtheAnders Johansen, Shigeru
Ida2 ,to
and
Ramon
due
the
low
rates
pebble accretion
intheofBondi
regime,approximately 70 K at solar abundances, co
track
of of
a protoplanetaccretion.
then growth. Therefore
The
ratio
the
densitiesbyofpebble
pebbles
to gas isWethenl expressionsforthesurface
growthgrowing
wefurtherstart our protoplanets at M0 = 0.01 ME
while
pebbleaccretiontheHillregimedominates
theLund Observatory, Department of Astronomy and Theoretical
Physics,
Lund University,
Box 43, 221in
00 Lund,Sweden,
ing
to
the
2–4
AU
regioninthelatestages
of
prot
use
this
expression
toderivethelocationwherethegrowthtrack
yDepartment
pebbleaccretion.
Wethene-mail:anders@astro.lu.seof Astronomy and Theoretical
Physics,
LundTherefore
University, Boxwe
43, start
221 00 ourLund,protoplanets
Sweden,
惑星のmigration
は惑星形成の最大の問題の一つ。migration
rate
は惑星の質量に依存
and
ignorethecontributionofplanetesimalaccretion
to
the
cor
growth.
at
M
=
0.01
M
0
E
Earth-Life
Science(ELSI),
Institute of Technology,⌃crosses
ṀInstitutepebbleisolation
mass. Meguro,
urTokyo⇠ Tokyo, 152-8550, Japandiscevolution(Bitschetal.,2015a;
Madhusudhanetpwherepthe growthro.lu.secationthetrack
growthrate,
althoughtheinclusionofplanetesimalaccretion
andignorethecontributionofplanetesimalaccretion
to
the
core
=
=
.
(14)
一方、pebble
accretion
によりmigration中でも惑星の質量は変化しうる
Institute(ELSI), Tokyo Instituteof Technology,
Meguro, Tokyo, 152-8550, Japan
Hence,
we
expectthat
the growthofpebbles islimited
⌃g
+
1
could
give
a
boost
to
the
accretion
rate,
dependingonthe miṀg 2St v + ur (2/3)(St/↵)ABSTRACT
growthrate,
althoughtheinclusionofplanetesimalaccretion
1Dモデルを用いて惑星の軌道と質量の進化を計算
ing
orfragmentationintheaccretion
regionofthecogration
speed
of
the
protoplanet(Tanaka&Ida,
1999).
Planetary2.1.
migration
is
a
major
challengeforplanetformation
theories.
The
speed
of
Type
I
migrationis
proportional
to
the
mass
of
Pebble accretion ABSTRACT
could
give
a
boost
to
the
accretion
rate,
dependingonthemia protoplanet,
while
the
final decade of
growthof a pebble-accreting
planetary ascore intakesIda
place ata ratethat
scales with the mass gas giants. Ices of CO and CO may, in turn, underHere
wedefined
the
ratio
of
the
fluxesetal.
(2016),
2
簡単のため、Stokes
numberとalphato thetwo-thirds power. This results in planetary
growthgration
tracks (i.e.,theevolution は時間、空間で一定を仮定
of a theprotoplanet’s
mass versus its (Tanaka
distance from & Ida, 1999).
speedofprotoplanetstar)Tothatbecomeincreasingly
horizontal(migration-dominated)withrisingof
mass
of
the
protoplanet.
Itishasbeen
shown recently
Johansen, Ida,
Brasser: How
planetary growth outperforms
migration
ation
form
longerrefractoryorganic
molecules(Muñ
derivetheanalytical
shape
of
the
growth
track
of
a
solid
pros athemajorchallengeforplanetformation
theories.
The
speed
Type
I
migration
proportional
to
the
mass
of
that 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
migrationṀptheHerefinal
decadeof ofathepebble-accreting
planetary
takes
place
ata 50%a ratethat
scales withmass
wetoplanet,show
fromof
1-Dgrowth
simulations
planet-discinteraction thatthe mass atcore
which
a planet
carvesgapaccreis approximately
2.3 theweuse
protoplanet
growthrate
frompebbleSchutte,2003).
We
ignorehere
thepossibility
that
su
⇠
=
.
(15)
をパラメータとして与える
the results
pebbleisolationmass.
Ourmeasurementsof thepebblemass offromsimulations match
resultse times
growth
track
of
a
solid
prower.
This
in planetary
growthtracks(i.e.,
theisolation
evolutiona 1-D
protoplanet’s
masspublishedversus3-D
its
distance from
1000.00
ing the2-D
Hill regime(Ormel&pebbleKlahr,
2010;
Lambrechts
Type
I migration
For
I migration
weuse
the standard
scalingthe
relativelytion
well,Ṁ
exceptat very
low viscosities(↵ < 10 )2.2.
where
the
3-D
isolationmass
is significantly
higher,possibly
due Type
molecules
could
bestickyandfacilitate
formation
M law,
α =0.0001
increasingly
horizontal(migration-dominated)withrisingmassoftheprotoplanet.
It
has
been
shown
recently
owth
rate
from
pebbleaccreto gap edge
instabilities
thatare not captured
in 1-D. The pebble isolation mass demarks the transition from pebble accretion to gas&
Johansen,2012;
Ida
etthereforeal.,to2016),
100.00que
on a protoplanet
isformreducedproportional
theof the gasunits
gapofcarved
byafter
thereachinggrowinglarger
planet. than millimeters in size (Lodders, 2004).
accretion.
Gas accretion to
gas-giantplanets
takesrelative
place overheighta few astronomical
migration✓◆
2
2&
Klahr,
2010;
Lambrechts
For
Type
I
migration
we
use
the
standard
scalinglaw,
thepebbleisolation
mass
and,shortly
after,
the
50%
gap
mass.
Our
results
demonstratehowplanetary
growthcanoutperform⌃r-Dfirstsimulationsofplanet-discinteraction
that
the
mass
at
which
a
planetcarvesa50%
gap
is
approximately
2.3
M g
H
We
will
show
below
in
Sections
2.5
and
2.6
that
⇠
is
a
key
papebbleaccretion
migration
migration,
bothduringcore accretion andduringgas accretion,even whenthefrom
Stokes1-D
numberof the pebblesmatchis small,publishedSt ⇠ 0.01,
and
ṙ
=
k
v
.
(3
ation
mass.
Our
measurementsofthepebbleisolationmass
simulations
3-D
resultsmig
K
10.00, the pebble-to-gas
fluxthatratio in!determines
theprotoplanetary
disctheis in thenominal rangeof protoplanet’s
0.01–0.02. We✓find thatplanetary
growthtrackis very rapid
rametershapeofagrowthBothpebbleaccretion
(in
the
Hill
regime)
and
r
3
M
M
r
2/3
◆
2
?
?
2
t in
at thevery
lowviscosities
(↵
<
10
)
where
the
3-D
pebbleisolationmass
issignificantly
higher,possiblydue
first million yearsStof the protoplanetary disc and that the probability forM
forming
gas-giantplanets increases with the initial size⌃rHg
2 turbulent
ofthattheandprotoplanetary
disc and withdecreasingdi↵usion.
ies
are
not
captured
in
1-D.
The
isolation
the transition
accretion
to gas on the Stokes
the
total
migrationthedemarks
protoplanet
beforereachdepend
number of the pebbles rather th
1.00
Ṁ
=
2
⌦R
⌃ppebble.distance(1)ṙ = of
kmass
vfrom
(3)
planetary growth outperformsHmigrationmig
K . pebble
Here
ṙ
is
the
migration
speed
of
the
protoplanet,
k
is
a
con
mig
0.1
ion
towords.
formplanet-disk
gas-giantplanets planets
thereforetakes place
over
aM
few
astronomicalunitsof
migration
afterreaching
MrKey
interactions,and satellites:
formation,planetsandsatellites:
gaseousplanets?and ?solid components ofing
thepebbleisolation
mass.
The
gas
physicalsizes.
The
pebbleStokesnumberiscalculate(α, St, ξ)=0.01,0.01,0.01
ion mass and, shortly after, the 50% gap mass. Our results demonstrate how planetary growth canstantprefactor
thatdependsonthegradientsofsurfacedensity(α, St, ξ)=0.01,0.01,0.02
0.10outperform(1)M(r),(α, St, ξ)=0.001,0.001,0.01
tion forandtheduring
growthtrack
glacore accretion
gas accretion,
even
when
the
Stokesnumberofthepebblesissmall,
St
⇠
0.01,
and
Here
ṙ
is
the
migration
speed
of
the
protoplanet,kisacon(α, St, ξ)=0.001,0.001,0.02
andtemperature,
M
is
the
mass
of
the
central
star,
⌃
is
th
mig
?
g
ntroduction
by of
a positive
torqueresultingfrom theaccretion
heatrapid
M is the discmass
protoplanet,
Stcorotation= We⌦⌧findtheplanetary
Stokesratio inHere
the protoplanetaryis inofthethenominalrange
0.01–0.02.
growthis very
0.01
f isthatoftheprotoplanet(Benı́tez-Llambay
etal., the
2015)
orgas
from
the sizestantprefactor
thatdepends
ongradientsofsurfacedensitysurfacedensity,
H/r
is
the
disc
aspect
ratio
and
v
is
th
K
0.1
1.0
10.0
100.0
dM
Ṁ
ars
of
the
protoplanetary
disc
and
that
the
probability
forforming
gas-giantplanetsincreaseswiththeinitialnumberthe many
pebbles
inofequation⌦ is the& Pessah, 2018).
formationof planets ofinvolves
distinct (defined
steps in the laterscattering(large) pebbles16),(Benı́tez-Llambayr [AU]=
discfrom
anddustwithanddecreasing
turbulentdi↵usion.
Keplerian
speed
at
the
positionoftheplanet.
Fortheprefactowth
ice particles
to full planetarysystem(a temperature,
and
M
is
the
mass
of
the
central
star,
⌃
is
the
?
g
Migration
can
even
stall
entirelyiftheturbulentviscosity
is
too
dr
ṙ
Keplerianthe location
theprotoplanet,
⌧
is
the
16)
anet,
St
⌦⌧f frequency
istheagoStokesfisation that
was=pioneered
50 years
by at
Safronov,
1969). weakof
to di↵useaway thegasdensityenhancement
thatkaspectformswein- ratio
follow
here
a
fit
to
3-D
numerical
simulations
found
in
gas
surfacedensity,
H/r
is
the
disc
and
v
is
the
2/3
2/3
mig
惑星の質量、軌道の進化トラック
isk
interactions,planetsandsatellites:
formation,planetsandsatellites:
gaseousplanets
K
competition
betweenradialmigrationandgrowthisnevfriction
time
of
the
pebble(proportionaltotheparticlesize
when⇠ is the 2(St/0.1)
Mthe
terior ofplanetaryal., 2009;
Fungtracks of planetary cores for four combinations of the accretion viscosity ↵, the pebble Stokes numbterinequation
16),⌦
Fig.Li
1. etAnalytical
growth? (3M? ) orbit (Rafikov, 2002;
eless a general theme
in planet formation. The formation
D’Angelo&(2010),=
1/32018).
(set toof
be equal
toplanet.
↵) and the ratio
ofLubow
radialpebble-to-gas
flux rates ⇠. Protoplanets are started at either 5 AU or 25 AU and& Lee,
Keplerian
speed
at
the
position
the
For
the
prefactor⇣
pebblesaresmall),
R=[M/(3M
)]
r
is
the
Hill
radiusofthe2for example,
has to ⌧overcome? Gc
成長とともに惑星は急速に落下
nplanetesimals,of the protoplanet,(2/3)(St/↵)+the1radial driftkmig
a starting
mass of
M . The pebble isolation mass is indicated for two values of the turbulent viscosity ↵ , assumed here t
f is HtheAU
A moredirectway
toovercomeTypeI
migrationis 0.01
simplys1
sed by thehead-wind of theMslower
movinggas onthekwefollow
here
a
fit
to
3-D
numerical
simulations
found
in
0.1
times
the accretion
viscosity↵. The proportionality
betweenthe migration rate and the mass results in all growth tracks tur
mig
for
the
planetarycore
toincrease
its
mass
very
rapidly.
The
acprotoplanet,
is
the
mass
of
the
central
star,
r
is
the
radialloca?
onalparticles
to theparticlek=2(1.36
+
0.62
,
(4
wing
(Weidenschilling,
1977;
Brauer et al., 2008).
nearlyhorizontal
beforereaching
theirmaximalmass +
at r 0.43⇣)= 0.
⇣ size
1/3 whenmig
byapositive
corotation
torqueresultingfrom
theaccretion
heat
cretionrateofpebblesispotentiallyhighenoughfortheproto⇥r bumps
M formed. in ⌃(19)
D’Angelo&
Lubow(2010),
1/3pebbles
tion
of
the
planetandisthepebblesurfacedensity.
Significant
ppingin
pressure
theturbulentgaspplanetgrowth to outperformthe nominal rateet
of TypeI migration
)]
r
is
the
Hill
radius
of
the
of
the
protoplanet(Benı́tez-Llambay
al.,
2015)
or from the
w
(Lyra
et
al.,
2008;
Johansenetal.,2009a;
Bai,
2015)
or
by
(Lambrechts & Johansen,
2014;pebble
Ormel et al.,ts
involves
many
distinct
steps
in
the
We2017;
finallyJohansen
obtainthe&shapeofthe⇣growth
track, r(M),from accretion
rate of equation(7), as the latter may
bedrivenbye↵ort
iscurrently
being
put
into
understandinghowacwhereandarethenegativelogarithmic
derivatives
of
the
sur
scatteringof(large)pebbles(Benı́tez-Llambay&
Pessah,2018).
The
solution
is
found
by
separationofvariables,
beddedplanets
(Lyra
et
al.,
2009)
or
throughrun-away
pileentral
star,
r
is
the
radialloca(21), that prowinds at a weak level of actual turbulence (Bai & Stone, 2
Lambrechts,2017).
Bitsch et+al.0.43⇣)(2015b)equation
demonstratedk=2(1.36+0.62,(4)ecausedparticlestofullplanetarysystem(amig
bycretion
the friction depends
on the gas (Youdin
Goodman,2005;
on &theeccentricityof theproMigrationandcan inclinationeven stall entirely
if theturbulent viscosity is too
1
2

3

v

M [ME]

isoEv

h tracks for a protoplanet underKanagawa
etal.
(2018)
performed
a
suite
o
r
when
iso
igrating
towards
the star, under
to measure the torque on embedded planets o
Pebbleisolationmass,
Gas
accretion,Gap
opening
2
3
!
!
2(1
⇣)
1 ⇣7
Stokes numberisaconstant
both
6
masses.
They
found
that
the
torqueiswell-des
r
r
6
7
iso
iso
4/3 isolation
4/3
7
4/3 6
・Pebble
mass:
6
7
M
=
M
=
M
1
.
(28)
6
7
ebble mid-planelayer
issuffimax
4
5
sical
Type
I
torque,
which
gives
rise
to
the
mig
iso
iso,0 rr
00
Pebbleaccretion
が続き惑星質量が増加→円盤構造が変化、Pebble
が惑星に降着せずに円盤にtrapn to take place in 2-D, and thatsion
given in equation (3), multiplied by the re・それ以降は円盤からのガス降着を考慮
stant
ratio
the radial
gas flow.
Thisofequationforms
a second order polynomial,⌃gap
ions・惑星質量が増加すると円盤にgapを形成、惑星に働くトルクが減少
to derive the!4/3radial location
=
c
.
mig
0
etary growth outperforms
migration
7
8
Johansen, Ida, Brasser: How planetary growth outperforms migration
M
⌃g
iso,0
the pebble isolation
2 mass. Our
X + X 1 = 0,(29)
strate that
undergo
1.0 Mprotoplanetsmax
1000.00
Here
c
=
k
/2
is
the
torqueprefactor,
⌃
mig
mig
0.8 towards the pebble isor growth1 ⇣1/(1 ⇣)
density
in
the
gap,
⌃
is
the
unperturbed
sug100.00
with
X
=
(r
/r
)
or
r
=
r
r
=
[1
X
]r
.
The
0.6
iso 0isolation iso0
iso0
of reaching the pebble
20.4positive solution to the polynomial is
0 (/ M ) is the natural torque scaling. The
10.00
t of the0.2starting location.
the bottom of the gap is fitted well by the epin our0.0model,1compared
to pre+4A
11.00& MacFadyen, 2013; Fung et al., 2014; Kana
1
10X=
, et al.,(30)n and migration(BitschM[M ]Fung & Chiang, 2016)2A
0.10, is the100 reduction of the migra4/3
M 1−D
where
=(B+18)(Miso,0 /Metmax) . Note that a solution
exists for all A, ⌃gap
1
0.01
3−D
planetary
gapMMA(Kanagawa
al.,
1−D
=
,
0.1all starting positions
1.0
10.0
100.0
i.e.
the
pebbleisolationmass
isreachedforM 2−D (K+18)
r [AU]⌃
1 + 0.04K
e connection
between the 50%
g
10
r
.
That
is
due
to
the
steeply
falling
pebbleisolation
mass
with
0
・黒点付きの線がガス惑星形成を説明可能な進化トラック
t al. (2018) and the pebble isodecreasing distance, in the passively
irradiatedcase.
results
Fig. 4. Numericallyintegrated
growthOur
tracks forcore accretion towhere
the pebble isolation mass followed by gas accretion. We start theに対応)
s et al. 1(2014). From numerical
protoplanets at a mass(各黒点間が0.2Myrof M = 0.01 M at t = 0.9 Myr (except
for the ↵ = St = 0.01 growth track starting from 25 AU, which we
generallydo
not apply
to the viscouslyinterior
start at t = 0.3heatedMyr) in a protoplanetary
discregionsthat evolves over a total time of 3 Myr.!The dots indicate the time for the growth track
0.00010.00100.01002 dots
✓◆
5 a time of 3, 2 and 1 Myr). Wes embedded
in
a
1-D
model
of
that
successfully
formsaJupiter
analogue(smalldots
areseparated
by
0.2
Myr,
large
indicate
・ガス惑星形成を説明するにはMHαof the protoplanetary
disc where ⇣useincreases
theaspect1
a migration modeland
where themigration
rate is ratio
reduced by multiplication with the relative gap height, following
Kanagawa et al.
= mass beyond the pebble ↵. mass. This results inthat Mgap⇡
2.3M.
Reachingv(2018). The migration rate is therefore inversely proportional toK
the planet
isolation
iso
小さいペブルSt ~0.01 M?
becomes
relatively
constant(Bitschetal.,2015a;
Ida
et
al.,
2016;
r
gas
accretion
over
a
few
astronomicalunitsof
migration.
Fig. 3. The results of 1-D simulations of an accretion disc withndan embeddedslightly
later
the
gap
transiplanet
whose
torqueonthegas
is based on the
Brasseretal.,2017).
ペブル/ガス降着率比ξ=0.01-0.02の狭い範囲(2D, 3Dシミュレーションによる検証が必要)
parametrisationsof D’Angelo & Lubow (2010). The top panel
through the Hill radius, as most of this gas is transported out This
The implies
prefactor in equation(39)thecan be migration
converted to solar units
portant
eventsinthegrowth
of
that
rate,
ṙ
=
2
shows the equilibrium
relativelimit
gap heightof theIn theA as a function
1, corresponding
torr
through
equa0 orbits andiso more complex streamlines.
again on horse-shoe
to compare with the disc accretion rate, 1.5 ⇥ 10 M yr ⇡αv=10−4αv=10−3αv=10−2

M [ME]

Gap height

Miso αv=0.0001

Miso, Mgap [ME]pE(α, St, ξ)=(0.01 , 0.01 , 0.01)(α, St, ξ)=(0.01 , 0.01 , 0.02)(α, St, ξ)=(0.001, 0.001, 0.01)(α, St, ξ)=(0.001, 0.001, 0.02)

iso
iso

gap
gap

0

E

0

0

v

3

E

1

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-

Moment 0, 1 map–8–

SiO v=2

29SiO v=2

SiO v=4
白線：連続波
灰色線：moment 0
カラー：moment 1
灰色点(左図) : maser

Fig. 2.— Moment 0 (grey contour) and moment 1 maps (color) of observed SiO lines superposed
SiO
v=2 : 北東-南西に伸びるアウトフローの根元
on the continuum map (white contour). The contour levels are 5, 10, 20, 40, and 80 times root1 and 5 mJy beam 1 ,mean-square
(RMS)
noise
levels,
and
the
RMS
noise
levels
are
3
mJy
beam
北西-南東の速度勾配 red-shift 成分の方が明るい
respectively, for 430 GHz and 460 GHz continuum maps. (a) Map of SiO v=2 J=10-9 and 430 GHz
continuum emission. The contour levels are 5,10, and 20 times RMS noise level of 26 mJy beam 1
for SiO v=2
J=10-9line.v=4
Grey dots
represent the position of SiO v=1 and 2 J=1-0 maser emission
29SiO
v=2,
SiO
: コンパクトな円盤(Kim et al. 2008). The beam sizes are 0.0900 ⇥0.0700 (grey ellipse), PA=82 and 0.0800 ⇥ 0.0700 (white
ピーク位置がダストに比べて北東にずれる→ダストが光学的に厚い、SiOは円盤表面
or outﬂow の根元から？
ellipse),
PA=-80 for SiO v=2 J=10-9 and 430 GHz continuum emission, respectively. (b) Map of
29 SiO v=2 J=11-10 and 460 GHz continuum emission. The contour levels are 5,10, 20, and 40 times
輝度温度229,349K,
ダスト温度(500-800K)より低い
1
RMS noise level of 33 mJy beam for 29 SiO v=2 J=11-10 line. The beam sizes are 0.1300 ⇥0.1100 ,PA=82 (grey ellipse) and 0.1000 ⇥0.0900 , PA=83 (white ellipse) for 29 SiO v=2 J=11-10 and 460 GHz
continuum emission, respectively. (c) Map of SiO v=4 J=11-10 and 460 GHz continuum emission.
The contour levels are 5,10, and 20 times RMS noise level of 57 mJy beam 1 for SiO v=4 J=1110 line. The beam sizes are 0.1200 ⇥0.1100 , PA=87 (grey ellipse) and 0.1000 ⇥0.0900 , PA=83 (white
ellipse) for SiO v=4 J=11-10 and 460 GHz continuum emission, respectively.

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
Substructures
at HighAngularResolution
Project (DSHARP):
The Disk
Disk Substructures
at HighAngularResolution
Project (DSHARP):
32
SpiralStructures
Structures
theContinuumof the Elias
27,Hill
IM Drive,
Lup,
6CT
Disks
DepartmentIII.
ofIII.
Astronomy,
Van Vleckinin
Observatory,
Wesleyan
University,
96
Middletown,
06459, USA
SpiraltheMillimeter
Millimeter
Continuumof FosstheElias
27,andIMWaOphLup, andWaOph
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, USA1
4
5
Jane Huang,
Sean M. Andrews,1 1Laura M. Pérez,2 Zhaohuan
Zhu,3 Cornelis
1
2
3 P. Dullemond, Andrea Isella,
45Jane Huang,
Sean
M.
Laura
M.
P
érez,
Zhaohuan
Zhu,
CornelisP.
Dullemond,
AndreaIsella,6,Andrews,
78910
10, 11Myriam Benisty,6, 7 Xue-Ning Bai, Tilman
Birnstiel, John 9M. Carpenter, Viviana V.
8
10 Guzmán,
10, 111211313MyriamBenisty,
Xue-Ning
Bai,
TilmanBirnstiel,John
M.
Carpenter,
Viviana
V.
Guzm
án,
ABSTRACT
A. Meredith Hughes, Karin I. Öberg,
Luca Ricci, David J. Wilner, and Shangjia Zhang

12.04193v2 [astro-ph.SR] 15 Jan 2019

A. 1Meredith Hughes,12 Karin I. Öberg,1 Luca Ricci,13 David J. Wilner,1 and Shangjia Zhang3
We present
an analysis Centerof ALMA
1.25 millimeter
continuum
observationsof spiralin
Harvard-Smithsonian
for Astrophysics,
60 Garden Street,
Cambridge,
MA 02138, UnitedStates structuresof America
2 Departamento de Astronomı́a, Universidad de Chile, Camino El Observatorio 1515, Las Condes, Santiago, Chile
three 1protoplanetarydisksCenterfrom forthe Astrophysics,
Disk Substructures
atStreet,High Cambridge,
Angular Resolution
Theof America
Harvard-Smithsonian
60 Garden
MA 02138,Project.
United Statesof Physics
and Astronomy,
Las Vegas, at
4505
S. Maryland Pkwy,
LasNV, 89154,
USA
2 Departamento
disks3 Department
aroundElias
27,deIM
Lup, and University
WaOph of6 Nevada,wereobservedaElresolutionof ⇠1515,
40 Vegas,
60 mas(⇠ 6Santiago,
7
Astronomı́a,
Universidad
deChile,
CaminoObservatorio
Las
Condes,Chile
4 Zentrum für Astronomie, Heidelberg University, Albert Ueberle Str. 2, 69120 Heidelberg, Germany
3au).
All
three
disks featurem = 2 spiralpatterns
in conjunction
withannularsubstructures.
Gas NV, 89154, USA
Departmentof Physics
andAstronomy,
Universityof
Nevada,Las
Vegas,
4505
S.
Maryland
Pkwy,
Las
Vegas,
5 Departmentof Physics and12Astronomy, Rice University, 6100 Main Street, Houston, TX 77005, United States of America
kinematics
establishedby Astronomie,
CO J = Heidelberg
2 1 observations
indicatethat thecontinuum
spiral arms
are
4 Zentrum für
6 Unidad Mixta
University,
AlbertUeberle
Str.
2,
69120
Heidelberg,
Germany
Internacional Franco-Chilena de Astronomı́a, CNRS/INSU UMI 3386, Departamento de Astronomı́a, Universidad detrailing.
The arm-interarm
intensity
contrasts
are modest,
lessHouston,than
The77005,
EliasUnited
27 spiral
5 Department
CaminoEl
Observatorio
1515,
Las typicallyCondes,Santiago,
Chile 3. TX
of Physics and Chile,
Astronomy,
Rice
University,
6100
Main Street,States of America
7 Univ. Grenoble
pattern extends throughout muchof the Alpes,
disk, CNRS,
and thearms
the gap at R ⇠ 69 au. The
IPAG,
38000intersect
Grenoble, France
6 Unidad
Mixta
Internacional Franco-Chilena de Astronomı́a, CNRS/INSU UMI 3386, Departamento de Astronomı́a, Universidad de
8 Institute for Advanced Study and Tsinghua Center for Astrophysics, Tsinghua University, Beijing 100084, China
spiral pattern in the IM LupChile,
disk isCamino
particularlycomplex—it
extends
aboutSantiago,
halfway Chile
radially throughEl
Observatorio
1515,
Las
Condes,
University
Observatory,
FacultyofPhysics,
Ludwig-Maximilians-Universität
München,Scheinerstr.
1,may
81679beMunich,Germany
the 9disk,
exhibiting
pitch
angle
variations
withradiusandinterarmfeatures
that
part
of
ring
7 Univ.
Grenoble
Alpes,
CNRS,
IPAG,
38000
Grenoble,
France10 Joint ALMA Observatory, Avenida Alonso de Córdova 3107, Vitacura, Santiago, Chile
substructures
spiral arm branches. Spiral arms also extend most of the way through the WaOph
8 Instituteorfor
11 Instituto
Advanced
Study
and Tsinghua
Tsinghua
University,
Chinade Astrofı́sica,
Pontificia
Universidad
CatólicaCenterde Chile,for
Av.Astrophysics,
Vicuña Mackenna
4860, 7820436
Macul, Beijing
Santiago,100084,
Chile
disk,
but the source overall is much more compact than the other two disks. We discuss possible
96
12
Departmentof Astronomy,
VanofVleck
Observatory,
Wesleyan University, 96 Foss Hill
Drive, Middletown,
CT 06459,
USA Munich, Germany
University
Observatory,
Faculty
Physics,
Ludwig-Maximilians-Universität
München,Scheinerstr.
1, 81679
origins
for thespiralstructures, including
gravitational
instability
anddensitywaves
inducedby USAa
13 Department
10 Jointof Physics
and Astronomy,
California
State
University
Northridge,
18111
Nordho↵Street,Northridge,CA91130,
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, thesethree sources do not feature high-contrast crescentABSTRACT
12 Department of Astronomy, Van Vleck Observatory,
Wesleyan
University,
96may
Foss point
Hill Drive,
Middletown,
CT 06459, USA
like asymmetries
or
large
(R
>
20
au)
emissioncavities.
Thisdi↵erencetomultiplespiralpresent an analysis of ALMA 1.25 millimeter continuum observations of spiral structures in
13 Department We
of Physics andoperating
Astronomy,
California
State University Northridge, 18111 Nordho↵ Street, Northridge, CA 91130, USA
formationmechanisms
indisks.
three protoplanetary disks from the Disk Substructures at High Angular Resolution Project. The

disks around Elias 27, IM Lup, and WaOph 6 were observed at a resolution of ⇠ 40 60 mas (⇠ 6 7au).protoplanetary
All three disks disks—ISM:
feature m = 2dust—techniques:
spiral patterns
in conjunction
withresolution
annular substructures. Gas
ABSTRACT
Keywords:
highangularkinematics established by 12 CO J = 2 1 observations indicate that the continuum spiral arms areWepresentananalysis
of
ALMA
1.25
millimeter
continuum
observationsofspiralstructuresintrailing. The arm-interarm intensity contrasts are modest, typically less than 3. The Elias 27 spiral
1. protoplanetary
INTRODUCTION
tary
companion(e.g.,
Goldreich&
1979; LinThethreedisks muchfrom ofthe
Substructures
at HighAngularpattern
extends throughout
the Disk
disk, andthe arms
intersect
the gap
at R ⇠Resolution
69 Tremaine
au. The Project.
& Papaloizou
Tanakaal.⇠2002),
gravitationaldisks
aroundElias
27,IMIMLup,
and
6 wereobserved
atabout
a resolutionof40
60
mas (⇠ 6 7
spiralpattern
the
Lup
disk
is particularlycomplex—it
extends1986;
halfway etradially
throughSpiral arms
arethought
toinprovide
key
clues
toWaOphtheinstability(e.g.,
Boss that
1998;
Mayer
et substructures.
al.ring
2004; LodatoGas
disk,
exhibiting
angle
variations
with radius
and interarm
featuresmay
be partofau).theAll
diskspitch
featurem= 2 spiralpatterns
in conjunction
withannularynamical evolution
ofthree
protoplanetarydisks,
although12& Rice2004),
andpressure
duespiralto shadowsubstructuresorformation
spiral arm
branches.
also
extendmostof theway throughthe WaOph
kinematics
establishedby mechanisms
CO J =Spiral2is arms
1 observations
indicatethatthevariations
continuumarms arehe precise natureof spiral
6 disk, but the source overall is much more compact
than
the
other
two disks.
We
discuss
possibleing
fromamisaligned
inner
disk
(e.g.,
Montesinos
et al.
ighly debated.
Proposedmechanisms
forinducing
spitrailing.
The
arm-interarm
intensity
contrasts
aremodest,typically
less
than
3.
The
Elias
27
spiralorigins for the spiral structures, including gravitational
instability
anddensitywaves
inducedbya2016; Montesinos & Cuello 2018).
al features include
perturbations
byastellarorplanepattern
extends
throughout
much
of
the
disk,
the arms
intersectof thegap
at disksR ⇠ 69 au. The
stellar or planetary companion. Unlike the millimeterandcontinuum
counterparts
many
of
the
Disk spiral structures have primarily been mapped in

DSHARPの渦状腕構造について
3つ全てリング構造も持つ、m＝２の腕、trailing, コントラスト < 3三日月状構造や広いgap は持たない。
起源として惑星の密度波と重力不安定性について議論

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