•of[S II]
andII]obtain
lines
in
MUSE observations
data,
the externalpressure
Pe of3D
molecular
cloudsincreasesinseveralregionsenoughsequencestars[Ncausedby clumpy
accretion
was investigated.
Here
wesmoothed
particlehydrodyand,finally,
wetheVLTsynthetic
treating
theperform
imagesashydrodynamical
the actual
ALMA
observations.
Our models
indicatemechanismfindofresult
indisks
HTs
is expected
aﬀect
their
mass
ratio
distribution.
namicssimulations
perturbed
ato
recentclump
accretion
event.
These
simulations
further
exploredbyradiativetoexceedPi.weThis
leads
us
tobyconclude
that
we
are
observing
the expansionof areanionizedoverpressurizedcocoonand
that
that
a
planetwithaminimum
mass
of
⇠
1.4
M
orbitingatadistance
of
⇠
9
10
au
can
explainthemorphology
location
Jup
SFN #353 8-14 片岡transfer
calculations
to clouds
quantify
thethatobservational
appearanceof suchdisks.
was
shown
that
the
densitywaves
inthepathways
disks thethat
compresses
molecular
leadtocollapse.
SomeItjet-impacted
clouds,nonetheless,nearof the observed
dust
ring atandBand
7 could
and Band4. their
We canreproducethelowspectral
index
(⇠ 2)
observed
wheredust ringof jetindividually
reproducing
theclump.
data.
In
our several
best-fitmodel,
CRs
provide
of 13
the
dense
gas
heating
atlayers.
the radio
were
formedat havethefallof theAfterrevolutions
theycantoabouttransform
into
spiralsandring
structures.
Their
12 1/3rd
theclearedincreasedPianddecreased
Pe.
They
are
likelyundergoevaporation
of
their
outer
Part
of theisdetected.
Our
synthetic
imagesreproducethemorphology
of
the
CO
and
CO
observedchannelmaps
where
the cloudA
giant
planetshapingthediskaround
the
very
low
mass
star
CIDA
1
lobes,
emphasizing
the
role
of
this
often
neglected
mechanisminheatingthegas
andpotentiallygenerating
outflows.
Thegas
imagesinmillimeter
wavelengths
arevery
similartothoseobserved
with
Atacama
Large
Millimeter/submillimeterArrayinevaporated
layerscould
mass load theoutflowan
thanksto rampressurefrom co-spatial
ionizedgas
flows.
Theinobservedpressure
absorption
allowedadetection.
Applying
empirical
relation
betweenplanet
mass
and
gap
width
the
dust,
we
predictaP.
Curone,A.
F.
Izquierdo,
L.
Testi,
G.
Lodato,S.
Facchini,A.
Natta,
P.
Pinilla,N.
T.
Kurtovic,C.
Toci,temperatureanddensityindicate
that
the
jet
passageleads
toanincrease
of
about
1
order
of
magnitudeintheinternalpressuresomeprotoplanetarydisks.
We
assumethatclumpyaccretion
may
be
the
sourceofsuchstructures.
changes thus suggest that both star formation
andsuppression could simultaneously occur.
5Ourenhancement
6 suggest
3 themaximum
planet
mass
of
⇠
4
8
M
.
resultspresenceofof
massive planet
orbiting
CIDA
1, thuschallenging
Jup
Pi of
molecularM.
clouds(with Pi/k
8*10M.
upLombardi,
to 7*10 K cmC. ),F.irrespective
theaSanchis,excitation
mechanism.
the fluxes
M.
Benisty,
Tazzari,
F. fromBorsa,
Manara,E.
L. Ricci
FFrom(Abridged)
Exoplanetaryourofus
planetformationaroundVLMstars.aroundof [Sunderstanding
II] hasand provided[N II] lines
inwith
VLTexciting
MUSE data,
the externalpressure
Pe of verymolecular
clouds(VLM)
increases
in several
regions enough and Proxima
researchdiscoveriesof planets
low massstars(e.g., TRAPPIST-1

The
Great
PlanetaryTheftandcaptureregions
to exceed
Pi. This
result leadsHeist:
us to conclude
that
we areobservingin
thestar-forming
expansion of an ionized
overpressurized cocoon that

•

•

•

•

•

•

Clumpyaccretion
inRichard
pre-main-sequenceasa sourceofperturbations
incircumCentauri).
However,current
theoreticalmodels Sascha
strive toP.stars
explainplanetformationinteractionsin these
conditions
and regions
do notpredict theEmmaC.
Daﬀern-Powell,
J.
Parker,Quanz
F
Gravitationalinstar-forming
compresses molecular clouds and that could lead to their collapse. Some jet-impacted clouds, nonetheless, near pathways thatstellardisks
developmentof
giant planets.
Recenthigh-resolution
observations
from
ALMA
ofparticular,
the disk aaroundCIDA
1, a VLM star inarecapableofdisrupting
anddestroying
planetarysystems,aswell
ascreating
new
ones.
In
planetcanbestolen,thejetclearedhave
increasedPianddecreased
Pe.
They
are
likelytoundergoevaporation
of
their
outer
layers.
Partofthe outflows
Linkingpressure
gradients
withthestabilityofmolecular
cloudsingalactic
Tatiana
V. Demidova,
VladimirP.theGrininF Theof perturbationsin the circumstellarof pre-mainTaurus, show
substructureshinting atpresenceof a development
massive planet.
We aim to reproduce
the dust ringdisksof CIDA1, observed

where
it is
directly
exchanged
betweenpassingstars during
anpressureinteraction;orcaptured,
wheregasa planet
first
ejectedfromits
evaporated
layers could
mass
load
the outflow
thanks
toF.
ram
from
co-spatial
ionizedflows. isTheobserved
pressureK.
M.
Dasyra,G.
F.
Paraschos,T.
Bisbas,Combes,J.
A.
Fernandez-Ontiveros
F
The
jets
launchedby actively
12smoothed particle13
sequencestars
causedbyclumpyaccretionwasinvestigated.
Here
we
perform
3Dhydrodynamicalhydrodyinthedustcontinuum
emission
in
ALMA
Band
7
(0.9
mm)
and
Band
4
(2.1
mm),
along
with
its
CO
(J=3-2)andCO(J=3-2)birth
systemandis free-floatingfor
a formation
period of time,
before being
captured bycould
a passingstar. We perform
sets of direct N-bodychangesthussuggest
that
both
star
enhancement
andsuppression
simultaneously
occur.
accretingblack holes
are capableof launching
severalofaccretionthe massive(millionorbillion solarmass)molecular
outflows
observed
namicssimulationsofdisks
perturbed
byarecentclump
event.
These
simulations
arefurther
exploredbyradiative
simulationsof young,
substructured
star-forming
regions,by
andfollow
their evolution
10withMyr inorder to determine
howseek
manychannelmaps,
assuming
the structuresare shapedtheinteractionof the fordisk
a massiveplanet. We
to retrieve thein galaxies.
These
outflows
could
suppressor enhance
starformation
in galaxies.
To investigate
the stabilityof thecloudscapabletransfer
calculations
toquantify
theobservational
appearanceofsuch
disks.
It
was
shown
that
the
density
waves
in
disks
planetsarestolenandcaptured,and
theirrespective
orbitalproperties.
We
show
that
in
high
density
star-forming
regions,
mass and position of the putative planet. We model the protoplanetary disk with a set of hydrodynamical simulations, varying
to
form
stars
in
outflows,
wemodeledCOseveral
and
HCO+
ALMA
data
oftransformthegalaxyIC5063,inwhich
black-holejets impact
Clumpyaccretioninpre-main-sequence
stars
as
a
sourceof
perturbations
incircumstolen
andcapturedplanetshavedistinct
properties.
The
semimajor
axis
distributionofcapturedplanetsissignificantly
skewedwere
formed
at
the
fall
of
the
clump.
After
revolutions
they
can
into
spiralsandring
structures.
Their
the mass and locations of the embedded planet. We compute the dust and gas emission using radiative transfer simulations,stellardisksmolecular
clouds.
Usingradiative
codetothat
self-consistently
performs
astrochemical
and thermalbalancecalculations
towider
orbitscompared
toa thesemimajor
distributionof observed
stolenplanetsandplanets
that
are
still
orbiting
theirparentimagesinmillimeter
wavelengths
are transfer
veryaxis
similarthose
with
Atacama
Large
Millimeter/submillimeter
Array
in
and,
finally,weobtainthesynthetic
observations
treating
theimagesastheactualALMA
observations.
Ourmodelsindicate
TatianaV.
Demidova,
VladimirGrinin F
Thedevelopmentof perturbationsin andthecircumstellar
disks
pre-mainstar(preserved
planets).
However,the P.
eccentricity
andinclination
distributionsofcapturedandstolen planets
areofsimilar,
but
based
on
the
availablegasheatingsources,
we
found
that
mechanicalheating
cosmicray(CR)heating
areandfully
capablesome
protoplanetarydisks.
We
assumethatclumpyaccretion
may
be
the
sourceofsuchstructures.
thataplanetwithaminimum
mass
of
⇠
1.4
M
orbitingatadistance
of
⇠
9
10
au
can
explainthemorphology
locationJup
stars
causedtobytheclumpyaccretion
investigated.
Here we of
perform
3D hydrodynamicalsmoothed
particle hydrodyinsequence
turn very
diﬀerent
inclination
and waseccentricity
distributions
preserved
planets. In low-density
star-forming
regionsofthediﬀerences
observed
dust
ring
at
Bandbut
7 by
and
Band
4. principle,
Weaccretion
can reproduce
the low
spectralindex(⇠ exoplanets
2) observed
where
the dust ring
namicssimulationsofdisks
perturbed
a recent
event.to Thesesimulations
arefurther
exploredbyhaveradiative
these
are
not
as distinct
could
still, clumpin
be useddeterminewhetherobserved
likely12
13
Curvedjetmotion.
I.
Orbiting
andprecessing
jetstransfer
calculations
toquantify
theobservational
appearanceofsuch
disks.
It
was
shown
that
the
densitychannel
waves
inmapsthe disks
isdetected.
Our
synthetic
imagesreproducethemorphology
of
the
CO
and
CO
observed
where
the cloudformedGreat
in situ orPlanetary
have been stolenor captured.
We andfind thatthe initialdegreeofspatialandkinematic
substructure
inaThe
Heist:
Theft
captureinstar-forming
regions
4can transform
Christian
Fendt,
Melis
Yardimci
F
Astrophysical
jets
are
often
observed
asbentinto
or
curvedstructures.
We
also
know
were
formed
at
the
fall
of
the
clump.
After
severalrevolutions
theyspiralsandring
structures.
Theirthatabsorption
allowedadetection.
Applying
anempirical
relation
betweenplanet
mass
and
gap
width
in
the
dust,
predict astar-forming
regionisasimportantafactoras
thestellardensityindetermining
whetheraplanetarysystemwillbealtered,Emma C. Daﬀern-Powell, Richard J. Parker, Sascha P. Quanz F Gravitational interactions in star-formingwe
regions
thediﬀerent
jet sourcesmay
be binaryinnature,mayleadtoa regular,
periodicmotionof orbiting
the jet nozzle,
anorbitalimagesin captured
millimeter
wavelengths
arevery
similartowhichthose
observed
with
Atacama
Large
Millimeter/submillimeterArray
in challenging
maximum
planet
mass
of
⇠
4
8
M
.
Our
resultssuggestthepresenceofamassiveplanetCIDA
1,
thus
disrupted,
orstolen.
Jup
arecapableof disrupting
anddestroying
planetarysystems,
assimulations
wellassource
creating
newones. In particular,a planetcanbe stolen,
motionorprecession.
Here,
we
present
theresults
of
2D
(M)HD
in
order
to
investigate
howaprecessing
ororbiting
some
protoplanetarydisks.
We
assumethatclumpyaccretion
may
be
the
of
such
structures.
our understandingof planet formation
aroundstars
VLMduringstars.an interaction; or captured, where a planet is first ejected from its
where
it
is
directly
exchanged
betweenpassing
jet nozzle aﬀects the propagation of a high-speed jet. We have performed a parameter study of systems with diﬀerent precession
birthsystemandis free-floating
a andperiodof time,before fieldbeing
capturedWe
byfinda passingstar.kinds
We perform
N-body
The
young
stars
inseparations,the forGalactic
Centerangles,orbitalperiods
ordiﬀerent
magnetic
strengths.
that theseof nozzlessets
leadoftodirect
curvedThe
Great
Planetary
Heist:
Theftandcapturein theirstar-forming
regions
simulations
ofvon
young,
substructured
star-forming
regions,
andthatfollow
evolution
forWe
10 findMyrin orderTim
todetermine
how many
Sebastiano
Fellenberg,
StefanGillessen,
Julia
Stadler,
Michi
Bauböck,
Reinhard
Genzel,deZeeuw,
jetpropagation
which
isdetermined
by
the
main
parameters
definethejetnozzle.
C-shapedjets
fromorbiting
Linkingpressure
gradients
withthestabilityofmolecular
cloudsingalactic
outflows
Emma
C.
Daﬀern-Powell,
RichardJ.
Parker,SaschaP.
Quanz
F
Gravitational
interactions
instar-forming
regions
planetsarestolenandcaptured,and
theirrespective
orbitalproperties.
We
show
that
in
high
density
star-forming
regions,
OliverPau Amaro
Seoane,Antonia
Drescher,Frank
MaryamThomasFelix
nozzles Pfuhl,
and S-shaped
jets fromprecessing
nozzles.
Over longtime Eisenhauer,
and long distances,the Habibi,
initially curved
jet Ott,
motionbores
K.
Dasyra,G.planets
F. andParaschos,T.
Bisbas,F.The
Combes,A. Fernandez-Ontiveros
F
Thecanjets
launchedby actively
areM.
capableof disrupting
destroying
planetarysystems,aswell as J.
creating
new ones.
In
particular,
aplanets
planetbestolen, skewed
stolenandcapturedhave
distinct
properties.
semimajor
axis
distributionofcapturedissignificantly
Widmann,
Alice
Young
F
We
present
a
large
⇠
30”
⇥
30”
spectroscopic
surveyoftheGalactic
Centerusing
the
SINFONIa broad channel into the ambient gas that is filled with high-speed jet material which lateral motion is damped, however. A
where
it
is
directly
exchanged
betweenpassingstars
duringinteraction;orcaptured,a solarplanetis first
ejectedfromits
accreting
black
holes
are capableof launching
severalofanthemassive(millionorofwhere
billionmass)
molecular
outflows
observed
IFU
at
the
VLT.
Combiningobservations
of
the
last
two
decadeswecompilespectraover
2800
stars.
Using
the
Bracketto
wider
orbitscomparedtothesemimajor
axis
distributionofstolenplanetsandplanets
that
are
still
orbiting
theirstrong (longitudinal) magnetic field can damp the jet curvature that is enforced by either precession of orbital motion of theparent
birthsystemTheseand is outflows
free-floating
for asuppress
period of ortime,
before being
captured byina passingstar.
Weperform setsof stability
direct N-bodyingalaxies.
could
enhancestarformation
galaxies.
To
investigate
theofsimilar,
clouds but
capableabsorption
lines
weidentify
195
youngstars,
extending
the
list
of
known
young
stars
by
79.
In
order
to
explorethe angularjet (preserved
sources. Weplanets).
have investigatedbalance andacrossthe jet andambient medium
and foundtheplanets
lateralmagnetic
star
However,thetheforceeccentricity
inclination
distributionsof captured
and thatstolenaresimulationsof young,
substructured
star-forming
regions,
and follow
theirdata
evolution
for galaxy
10 Myr inorder toin
determine
how many jets impact
to
form
stars
in
outflows,
wemodeled
CO
and
HCO+
ALMA
of
the
IC5063,which
black-hole
momentum
distribution
of
the
young
stars,
we
introduceanisotropic
clusterprior.
This
prior
reproducesanisotropic
cluster
in isregions
pressureandgaspressure
gradients
are almost
balanced,butthatjetsa lack of gas
pressureplanets.
on the concaveside of thecurvature
in
turn
very
diﬀerenttotheinclination
andeccentricity
distributions
preservedIn
low-density
star-forming
Curvedjetmotion.
I.
Orbiting
andprecessing
planets are stolen and captured, and their respective orbital properties. We show that in high density star-forming regions,molecular
clouds.
Usinga radiativetransfercode
that
self-consistently
performs
astrochemical
andthermalbalancecalculationsamathematically
exact
way,
which
weFbuttest
throughnumerical
simulations.
Werole.
calculatetheposterior
angularmomentumspaceleadingtothelateralmotion.
Magnetic
tension
does
not
play
a
significant
Our
resultsareobtainedincode
units,
butwethese
diﬀerences
are
not
as
distinct
could
still,
inprinciple,
be
used
to
determinewhetherobserved
exoplanets
havelikelyChristian
Fendt,
Melis
Yardimci
Astrophysical
jets
are
often
observed
asbentorcurvedstructures.
We
also
know
that
stolen and captured planets have distinct properties. The semimajor axis distribution of captured planets is significantly skewed
asfunction
ofjetprojected
separation
from
Sgr
A*.
Wefound
find
that
the
observed
young
starand
distribution
is jetsubstantiallydiﬀerent
based
on
the
availablegasheatingsources,wethatmechanicalheating
cosmicray(CR)heating
are fully incapableprovidescaling
relations
such
that
our
resultsmay
beappliedtoyoungstars,
micro-quasars,
symbiotic
stars
or
AGN.
formed
in
situ
or
have
been
stolenor
captured.
We
find
that
the
initialdegreeofspatialandkinematic
substructureathediﬀerent
sourcesmay
bebinaryinnature,
which
may
lead
to
a
regular,periodicmotionofthenozzle,an
to wider orbits compared to the semimajor axis distribution of stolen planets and planets that are still orbiting theirorbital
parentfrom anorisotropic
cluster.
We
identify
thepreviously
reportedfeatureof theinclockwise
disk
and findthat
its angularor
momentummotionprecession.
Here,
we
present
theresultsof2D(M)HDsimulationsorder
toinvestigate
howaprecessing
orbiting
star-forming
regionisasimportantafactoras
thestellardensityindetermining
whetheraplanetarysystemwillbut
be altered,star (preserved planets). However, the eccentricity and inclination distributions of captured and stolen planets are similar,
changes
asaﬀects
functionof separationof fromthe black
hole,
and
thus
confirma warp of study
the clockwise
disk(p diﬀerent⇠ 99.2%).
At large
jetnozzlethepropagationahigh-speed
jet.
We
have
performedaparameterofsystemswithprecession
in
turn
very
diﬀerenttotheinclination
andeccentricity
distributionsofpreserved
planets.
In
low-density
star-forming
regions
disrupted,
capturedor stolen.
Interplay
between
Young
Stars
and
Molecular
CloudsintheOphiuchusStar-forming
separations,discoverthree prominent
overdensities
of angularmomentum.
One that
overdensity
has ofbeenreportedpreviously,
4 to determine
angles,orbitalweperiods
or separations,andcould
diﬀerent
field bestrengths.
We findthese kinds
nozzleslead havetocurvedthese diﬀerences
are not
as distinct but
still,magnetic
in principle,
usedwhetherobserved
exoplanets
likelyComplexthepropagation
counter-clockwise disk.
The other two
arenew.parameters
Determining
thedefine
likelythe
membersof these
we find thatmany asjet
is determined
main
that
jet nozzle.
We structures,
findfromasorbiting
formed in situ whichor havebeen stolen byor thecaptured.
We find thatthe initialdegreeof spatial
and C-shaped
kinematicjets
substructure
in aAashishGupta,
Wen-Ping
Chen
F
We
present
spatialandkinematiccorrelation
betweentheyoungstellarpopulation
75% of stars
can be associatedwith
one of thesefeatures.
Stars belonging
to thedistances,warped clockwise-disk
show a jet
topmotion
heavy K-band
nozzlesand S-shaped
fromtheprecessing
nozzles.
Overtime inand
longtheainitiallycurved
bores
The
young
stars
Galactic
star-forming
regionisjetsas inimportanta factoras theCenter
stellarlong
densitydetermining
whetherplanetarysystem willbe altered,and the cloud
clumpsin theThefeatures
stellar dosampleof known areyoung
objects
at various
luminosity
function,whilestarsOphiuchus
belonging star-forming
to the larger region.
separation
not. consists
Our observations
in goodagreementA giant planet shaping the disk around the very low
mass star CIDA 1

fi

P. Curone, A. F. Izquierdo, L. Testi, G. Lodato, S. Facchini, A. Natta, P. Pinilla, N. T.
Kurtovic, C. Toci, M. Benisty, M. Tazzari, F. Borsa, M. Lombardi, C. F. Manara, E.
Sanchis, L. Ricci ⋆ (Abridged) Exoplanetary research has provided us with exciting
discoveries of planets around very low mass (VLM) stars (e.g., TRAPPIST-1 andProxima Centauri). However, current theoretical models strive to explain planet
formation in these conditions and do not predict the development of giant planets.
Recent high-resolution observations from ALMA of the disk around CIDA 1, a VLM
star in Taurus, show substructures hinting at the presence of a massive planet. We aim
to reproduce the dust ring of CIDA 1, observed in the dust continuum emission in
ALMA Band 7 (0.9 mm) and Band 4 (2.1 mm), along with its 12CO (J=3-2) and13CO (J=3-2) channel maps, assuming the structures are shaped by the interaction of
the disk with a massive planet. We seek to retrieve the mass and position of theputative planet. We model the protoplanetary disk with a set of hydrodynamical
simulations, varying the mass and locations of the embedded planet. We compute thedust and gas emission using radiative transfer simulations, and, nally, we obtain thesynthetic observations treating the images as the actual ALMA observations. Ourmodels indicate that a planet with a minimum mass of ∼ 1.4 MJup orbiting at a
distance of ∼ 9 − 10 au can explain the morphology and location of the observed dust
ring at Band 7 and Band 4. We can reproduce the low spectral index (∼ 2) observed
where the dust ring is detected. Our synthetic images reproduce the morphology of the
12CO and 13CO observed channel maps where the cloud absorption allowed a
detection. Applying an empirical relation between planet mass and gap width in thedust, we predict a maximum planet mass of ∼ 4 − 8 MJup . Our results suggest thepresence of a massive planet orbiting CIDA 1, thus challenging our understanding ofplanet formation around VLM stars.

・CIDA1というTaurus領域にある
VLM (very low mass star)周りの原始惑星系円盤をALMA観測した。
・波長はB7(0.9mm)とB4(2.1mm)で、ダスト連続波と12CO(3-2)及び13CO(3-2)
・1.4MJupの惑星が約9-10auの距離を周回することで説明できる・スペクトル指数はおよそ2
・結論：VLMの周りでも惑星が形成される。

• 背景：超小質量星周りでのガス惑星形成の困難
A&A 649, A122 (2021)• ここではとりあえず0.3Msun以下の質量の星をVLM(very low mass star)と呼ぶことにする。

• 例えばTRAPPIST-1は 0.085 M⊙ の中心星が7個の岩石惑星を持っている。
• 褐色矮星周りの惑星も確認されている（25Mjupの星の周りに5Mjupの惑星
Morales et al. 2019）
Fig. 2. Moment 0 and moment 1 of the 12 CO and 13 CO. The upper right bar corresponds to 10 au size. The dashed circles (projected with the same
• 惑星形成の観点から言うと、惑星形成材料の枯渇が指摘されてきた。岩石惑
00
00
12
13

inclination and PA as CIDA
1, Table 3) are 1.0 and 0.6 in size from the center for the
CO and CO, respectively. The details of the images are
星はなんとか可能そうだがcore
accretionによるガス惑星については考えら
Fig. 1. ALMA Band 7 (0.9 mm) and Band 4 (2.1 mm) continuum images of the CIDA 1 disk. The synthesized beam is shown in the lower left
corner of each image. The details of the images are summarized in Table 2.
summarized2.
れていない(?
MiguelinetTable
al. 2020)
Table 2. Summary of the ALMA images in Fig. 1.

• ガス円盤の重力不安定で作るしかないか？
• 天体 CIDA1• Pinilla et al. 2021: Band 7 (0.9 mm) and Band 4 (2.1 mm) at aresolution of ~ 0.050

0.034 (~ 7

5 au).

• inner ringと、20auにリングが見えた。0.5Mjupの惑星で再現できるとされ
た。

• 本研究

Band

[mm]

7

0.9

4

2.1

Fpeak
[Jy beam 1 ]Ftotal[Jy][Jy beam ]7.9 ⇥ 10 4

3.1 ⇥ 10 2

1.7 ⇥ 10 5

1.4 ⇥ 10 4

5.1 ⇥ 10 3

(using the inclination and position angle report in Table 3). For
this figure, each profile is normalized to the peak of the ring andthe images are previously restored with the same beam before
deprojection (0.0500 ⇥ 0.03400 ). For the deprojection, we use theinclination (inc) and position angle (PA) from Table 3, which are
obtained from the visibility analysis explained in Sect. 3.2. The
error bars include the standard deviation of each elliptical bin
divided by the square root of the number of beams spanning fullazimuthal angle at each radial bin. In this figure, it is possible
to see that emission at both wavelengths peaks at the ring location (20 au) and there is a very bright inner disk. The 12 CO peakintensity map also shows a cavity that remains unresolved with asize of ⇠7 au along the major axis of the disk. Another interesting result from the 12 CO peak intensity map is that this emission
is more extended than the dust continuum emission, as found in
Kurtovic et al. (2021). The analysis of the 12 CO and 13 CO will
be presented in a future paper by Curone et al. (in prep.).
We calculate the optical depth of the peak of the continuum
ring, assuming ⌧ = ln[1 T brightness /T physical ], with T brightness andT physical being the brightness and physical temperature respectively. We obtain the brightness temperature from the full
black-body Planck function. We used a radially constant physical temperature of 20 K and we find that the optical depth
at the peak is ⌧peak,B7 = 0.48 and ⌧peak,B4 = 0.28 for Band 71

5.7 ⇥ 10 6

Beam[mas ⇥ mas]
54 ⇥ 3450 ⇥ 34

the dust disk mass. These values for the optical depths fall inthe same range as reported by the DSHARP sample (Dullemondet al. 2018) for more massive disks. One potential explanation
for this range of the optical depth inside the ring is planetesimalformation in this region (Stammler et al. 2019).
Under the assumption of optically thin emission, we calcu2
late the dust disk mass as Mdust ' ⌫dB⌫F(T⌫ ) , where d is the distanceto the source, F⌫ is the total flux at a given wavelength, andB⌫ is the blackbody surface brightness at a given temperature(Hildebrand 1983). Taking a mass absorption coefficient (⌫ ) at
a given frequency as ⌫ = 2.3 cm2 g 1 ⇥ (⌫/230 GHz)0.4 (which
is typical for a population of large millimeter grains, Beckwith
et al. 1990; Andrews et al. 2013, which is compatible within 2
with the spectral index we infer for CIDA 1 as shown later), anda dust temperature of 20.0 K or 14.7 K, the dust disk mass is
7.4 MEarth or 12.0 MEarth , respectively, when taking the total flux
from the image in Band 7. For Band 4, the dust disk mass is 7.8
MEarth or 11.4 MEarth for 20 or 14.7 K, respectively. Therefore,
the inferred dust disk mass is consistent between the two wavelengths with a large uncertainty that depends on the assumed
temperature. In addition, ⌫ is a very unknown quantity in protoplanetary disks, and for direct comparison we take the same⌫ assumed to calculate the dust disk mass of large populationsof protoplanetary disks (e.g., Pascucci et al. 2016). Recent work

Fig. 3. Azimuthally averaged radial intensity profiles of the deprojected continuum images (lineal scale on the left and logarithmic scale in thecenter) at each wavelength. Each profile is normalized to the peak. The profiles are obtained from images that are restored with the same beamal. 2021がgap shapeを理論モデルから作っていたが、本研究で• Pinilla et (50mas ⇥ 34 mas). The error bars include the standard deviation of each elliptical bin divided by the square root of the number of beams spanning
は流体計算で作る。それで画像を再現できるか考えてみる。
the full azimuthal angle at each radial bin. The right panel shows the radial profile of the spectral index taking into account the errors on the radialintensity profiles in addition to 10% of the error due to flux calibration.

• Pinilla et al. 2021

P. Curone et al.: A giant planet around CIDA 1• 手法

P. Curone et al.: A giant planet around CIDA 1

This paper is organized as follows: in Sect. 2, we describe thenumerical simulations and procedures used to obtain the final
synthetic observations. In Sect. 3 we present the results on themodeling of the dust and gas emission, comparing them to the
ALMA observations of CIDA 1. Section 4 is devoted to the discussion of our findings: we analyze the simulated spectral index
and optical depth, evaluate whether planet-induced perturbations
could be detected in the gas line emission, and constrain the minimum and maximum mass of the putative planet. We also compare our modeling with previous mass estimates of the planet andinvestigate its possible origin. Finally, in Sect. 5, we summarize
our results.

• SPH codeのPHANTOM (Price et al. 2018)を利用Table 1. Initial parameters used for the simulations with Phantom. Each
entry is commented in the main text.

Parameters

Value

NSPH
106
M? [M ]
0.2
R? acc [au]1
Rin [au]1
Rout [au]100
Rc [au]
80
p
1.5
q
0.3
H(Rin )/Rin
0.08
hydrodynamical model for the radiative transfer simulation,
by extrapolating and interpolating the dust densities↵for
2. Methods
5 ⇥ 10 3SSpanel: starting from dust density values obtained with SPH
simulation(red dots), we simulation
perform a linear fit for log
⇢d
↵AV
0.36
2.1. Gas
and dust hydrodynamical
wo smallest simulated grain sizes to obtain densities for grains down to 5 nm (blue line). Then, we use a cubic spline
hhi/H
0.14
Wefitperforma set10of dustfive hydrodynamical
simulations
thebetween
Mgas [M ]1.5 ⇥ 10 3
ing log ⇢d values (orange line). Right panel: with the linear
we obtain
densities related
to grainwith
sizes
Smoothed Particle Hydrodynamics (SPH) code Phantom (Price
Mdust /Mgas
10 2
eft of the vertical gray dashed line), while with the cubic
splineinterpolation
weobtain50
densities
for
grain
sizes
et al. 2018b). This code has been extensively used for the mod5
a
[cm]
[a
=
1.6
⇥
10
, amax = 0.1, N = 11]dmin(to the right of the vertical gray dashed line).
eling of protoplanetary disks, with the intent of reproducing the⇠
3.5
observed structures in both the dust and gas emission (e.g., Dip⇢0 [g cm 3 ]2ierro et al. 2015, Ragusa et al. 2017, Pinte et al. 2018, Priceet al. in2018a,
Cuelloet al.
2019, Ubeira
Gabellini etfor
al. 2019,
insic consequence of the artificial vis- is illustrated
Fig.
3.
We
repeatthis
operation
every
SPH
RP acc [au]1/4 of Hill radius
Toci
et
al.
2020a,
Veronesi
et
al.
2020,
Toci
et
al.
2020b).
SPH
dP,0 [au]10.0
n Phantom is that ↵SS / hhi / ⇢ 1/3 particle andobtainandin thetotal
60 dustdensity spatial
distributions,formulation,
Phantom
implementationin particular,inMP,0 [MJup ]0.1, 0.5, 1.0, 1.5, 2.0
cludesexact
conservationof
mass,
momentum,andangularmoe disk viscosity increases wherever the 10 for grain sizes between 5 nm and 0.37 µm and 50 related tomentum,along0.37
with aµm
self-consistentcomputation of the stellar
to & Price 2010). A local increase in grain sizes
betweenand 1 mm.
and planet accretion rates and migrations (Price et al. 2018b).
rter viscous timescale and, therefore, a
WhileWeinuse
SPH
the informationis contained
inetpoint
particles,
the one-fluid(Laibe & Price
2014; Ballabio
al. 2018)
Appendix A). The gas in the disk is in vertical hydrostatic equimultigrain(Hutchison
et al. 2018)onalgorithm,
whichfordiscretizes
ar momentum in the disk. This descrip- Polaris needs
librium, which leads to the following aspect ratio
data
to be sampled
a 3D grid
the radiative
the disk with a single set of SPH particles, each containing inations: if the embedded planet is massive transfer simulations.
the spatial
distributionof physformation of gasTo
andmaintain
dust with di↵erent
grain sizes.
This method!1/2 qn the disk, in that region, the viscosity ical properties
as
close
as
possibletothesimulation
outputwe
is suitable for treating dust grains not fully decoupled from the H(R)cs (R)
H(Rin ) R==,
(3)
brings to a faster depletion of the inner use a Voronoi
gas. Such
condition
is fulfilled
if the midplane
numbergrid.
Given
a distributionof NStokes
points,a Voronoi
R
3K (R)Rin
Rin
St / ⇢0 ad /⌃g < 1, where ⇢0 is the dust grain intrinsic density, ad
he central star.

• 適当な粘性降着ガス円盤をおき、ガスの0.01倍のダストを起き、手を話す。ダストサイズは固定(0.16µm-1mm)。

• 内側はsinkになっていて、1au以内は見えない。
よってinnder diskは議論しない• （SPHなので）乱流αは密度が低いところで高くなる•が、結果に影響しない(?)

P. Curone et al.: A giant

A&A proofs: manuscript no. aanda

0.1

0.2

0.3

gas

t=40270 yrs

2×10-5 4×10-5 6×10-5 8×10-5

2.2 μm dust
5×10-3

0.4

0.01

0.015

5×10-6

1×10-5

1.5×10-5

0.16 μm dust
5×10-5 1×10-4 1.5×10-4 2×10-4

0.01

0.02

2×10-5

1×10-5 2×10-5 3×10-5 4×10-5

0.37 μm dust

0.90 μm dust

2×10-4 4×10-4 6×10-4 8×10-4

5.2 μm dust
0.02

1×10-512 μm dust
0.03

0.02

0.04

2×10-3

4×10-330 μm dust
0.06

0.02

0.04

0.06

0.08

20 au

72 μm dust

0.17 mm dust

0.42 mm dust

1.0 mm dust

Fig. 3. Refinement of the hydrodynamical model for the radiative transfe
a single SPH particle. Left panel: starting from dust density values obtai
各ダストサイズごとの結果を持ってきて、各グリッドに
values •associatedwith the two smallest simulated grain sizes to obtain deninterpolationon the remaining log ⇢d values (orange line). Right panel: wit
2.1.2. Properties of the central star and the embedded planet the gas outside of its orbit, which attracts nearby dust and interて適当に密度分布を内挿・外挿してダスト分布を得る。
cepts dust migrating from the outer regions towards the central
5 nm and 0.37 µm (to the left of the vertical gray dashed line), while wit
例：惑星質量が1.5Mjupの場合。
The central star and theplanet are modeled as sink particles, star. The faster motion of larger grains (from ⇠ 0.1 to 1 mm)
which are free to migrate and accrete gas and dust (see Ap- results in ring-shaped dust distributions, whereas smaller grains
between
0.37
µm
and
1
mm
(to
the
right
of
the
verticalgraydashedline).
driftする
pendix B). The stellar 大きなダストはより早くradial
mass of CIDA 1 is known to be in the present wider
radial profiles of their density, because they have
• （別ダストサイズのシミュレーションの結果をどう
range ⇠ 0.1 0.2 M (Pinilla et al. 2021). Kurtovic et al. (2021) a slower radial drift being more coupled to the gas.
estimate a mass of ⇠ 0.19
M using the Pascucci et al. (2016)
ので細いリングを作るのが見て取れる
After this first suite of simulations, we aim at better conmergeしているのかよくわからず…）
method with the distance of 137.5 pc (Pinilla et al. 2021). In our straining the minimum and maximum planet mass able to reproFig. 2. Face-on gas and dust surface density, in units of g cm 2 , from the Phantom simulation with initial planet mass of 1.5 MJup , and final planet
mass of 2.0 MJup after ⇡ 4 ⇥ 104 yrs (⇡ 560 planet orbits). Gas density is displayed in the top left corner, while the remaining panels present thesurface density for the simulated 11 dust grain sizes. The bigger central green dot represents the star, while the smaller green dot indicates theplanet position. Images were produced using the tool Splash (Price 2007).

Furthermore, an intrinsic consequence of the artificial viscosity implementation in Phantom is that ↵ / hhi / ⇢ 1/3(in 3D), meaning that the disk viscosity increases wherever thedecreases (Lodato & Price 2010). A local increase in
and d density=

simulations, we adopt a stellar mass M? = 0.2 M . The star ac- duce the observed dust emission by running additional simulacretion radius is R? acc = 1 au and defines a region where in- tions. In these cases, the embedded planet is placed at di↵erent
coming SPH particles are considered accreted onto the star. The initial radial distances from the star to find the best match withSS
planet accretion radius is chosen to be RP acc = 1/4 RH , where RH the peak intensity of the observed ring. The minimum mass ofis the planet Hill radius,片岡注：ダストの破壊・成長の物理を入れずに移流のみでサイズ分布を表現しているので、結果の議論に注意が必要
defined as
the planet is discussed in Sect. 4.4, where we present the results
RH =

1 MP

!1/3

dP ,

(4)

of two simulations: the first with MP,0 = 0.5 MJup
P,0
12.0 au, the second with MP,0 = 1.0 MJup and dP,0 = 11.0 au. The

P. Curone et al.: A giant planet around CIDA 1

A&A proofs: manuscript no. aanda

Fig. 4. Band 7 (0.9 mm, top panels) and Band 4 (2.1 mm bottom panels) comparison between dust continuum images from the ALMA observationand our synthetic observations obtained from the simulation with final planet mass of 2.0 MJup after 4 ⇥ 104 yrs, along with their residuals. The
synthesized beam (0.05000 ⇥ 0.03400 for Band 7, 0.04800 ⇥ 0.03200 for Band 4, FWHM) is shown in the bottom left corner of each image. The
contours in the residuals represent the 5 and 5 flux levels, respectively for Band 7 and Band 4.

is able to generally reproduce the morphology and the intensity that these last three cases also share consistent estimates of theof the observed emission from the ring. As expected, our syn- total dust mass needed to match the observed flux, ⇠ 7⇥10 6 M ,thetic images 2.0Mjup,
do not present the4e4yearsの結果を観測的可視化。
inner disk, which persists in with a dust-to-gas mass ratio of ⇠ 9 ⇥ 10 3 .
the residuals. Moreover, we note that the residuals at both bands
Results for the dust emission from the simulations aftershow some areas, located in the region of the ring and the gap, a longer evolution time of 8 ⇥ 104 yrs are presented in Apabove the 5 value or below the 5 value. Slight shifts in the pendix D. The synthetic profiles for simulations with a minimum
0.1
to could
4.0MJupを振ったが、2.0Mjupが最も良かった
simulated image
centroids
not eliminate these di↵erences. planet mass of 2.0 MJup still show a good agreement with the obSuch inequalities between our model and the observations might servations in Band 7 (which we take as reference, Appendix C).
be caused by an imperfect estimate of the disk inclination and However, the simulated profiles in Band 4 have a slightly lower
position angle that we assumed in the simulations or by some••Fig. 5. Comparison between radial profiles of azimuthally averaged intensities from the observations, simulations and corresponding residuals,
after the simulations have evolved for 4 ⇥ 104 yrs. Left-hand panels show results in Band 7, while right-hand panels refer to Band 4. Each row
contains the intensity profiles from the same simulation with a specific final planet mass, ranging from 0.2 MJup (top row) to 2.5 MJup (bottom row).
The distance of the planet from the central star is indicated by the brown vertical dash-dotted line. The mean FWHMs of the synthesized beam inBand 7 and Band 4 are shown as horizontal bars in the top row panels. The radial intensity profiles are obtained by deprojecting the disk, using thedisk inclination angle i = 37.5 , and dividing it into overlapping annuli, whose width corresponds to the averaged synthesized beam diameter. For
each bin, uncertainties are calculated by taking the intensity standard deviation for each pixel in the annulus and dividing it by the square root of
the number of synthesized beams contained in the area of the annulus.
Article number, page 8 of 22

contour levels plots. The uncertainty in the observation intensity profile is the 1 noise level (1.2 mJy beam ).

Fig. 10. Left and central panels: azimuthally averaged radial profiles of the optical depth along the line of sight and the intensities from thefull-resolution (i.e., not convoluted with the synthesized beam) dust emission image of the simulation with final planet mass of 2.0 MJup after
4 ⇥ 104 yrs, at Band 7 and Band 4. The brown vertical dash-dotted line indicates the location of the planet, while the horizontal gray dotted line
marks the optical depth ⌧ = 1 level. The region where the emission is optically thick (optical depth ⌧1) is shown in beige. Right panel:azimuthally averaged radial profiles of the spectral index from the ALMA observation and our simulation with final planet mass of 2.0 MJup after
4 ⇥ 104 yrs. Values are obtained using Eq. 5 with the synthetic image intensity profiles in Fig. 5. Uncertainties include the original error in theintensity profiles and a 10% flux error due to calibration. As a reference, the distance of the planet from the central star is indicated by the brown
vertical dash-dotted line and the position of the peak intensity is displayed by the blue vertical dotted line. The beige-shaded area marks the radii
where the full-resolution simulated emission is optically thick (⌧ 1) in both Band 7 and Band 4.

• 低いスペクトル指数（α=2.0）もよく再現された。

low , i.e., < 1, meaning that ↵B7, B4 < 3, could be indicative of
the presence of grains with size & 0.1 mm, suggesting that grain
Having •dust
emission data at two di↵erent wavelengths
allows growth in the disk may have occurred (Draine 2006). Protoplan20-30auはモデルでopticallythinなので、ここからダストの情報を得られるのではないか
us to compare the observed and simulated spectral index. Given etary disks around VLM stars or brown dwarfs with low spectral
4.2. Spectral index and optical depth

fl

fl

fi

fi

Interplay between Young Stars and Molecular Clouds in theOphiuchus Star-forming Complex
Aashish Gupta, Wen-Ping Chen ⋆ We present spatial andkinematic correlation between the young stellar population andthe cloud clumps in the Ophiuchus star-forming region. The stellar
sample consists of known young objects at various evolutionary
stages, taken from the literature, some of which are diagnosed
with Gaia EDR3 parallax and proper-motion measurements. The
molecular gas is traced by the 850 μm Submillimetre CommonUser Bolometer Array-2 image, reaching ∼2.3 mJy beam−1, thedeepest so far for the region, stacked from the James Clerk
Maxwell Telescope/Transient program aiming to detect
submillimeter outburst events. Our analysis indicates that themore evolved sources, namely the class II and III young stars, arelocated further away from clouds than class I and at-spectrum
sources that have ample circumstellar matter and are closely
associated with natal clouds. Particularly the class II and III
population is found to exhibit a structured spatial distribution
indicative of passage of shock fronts from the nearby Sco-Cen OB
association thereby compressing clouds to trigger star formation,with the latest starbirth episode occurring now in the densest
cloud laments. The young stars at all evolutionary stages sharesimilar kinematics. This suggests that the stellar patterns trace therelics of parental cloud laments that now have been dispersed.

・Ophiuchus領域の若い天体のクラスターとしての性質を調べた。
・ClassII/IIIのような年老いた天体は、ClassIや at
よりもクラウドから離れた場所にある・Class II/III はSco-Cen OB associationからのショックフロントの通過して雲が圧縮された構造と見られる（・stellar patternは今はもう消えてしまったフィ
ラメントの痕跡と言えるか）3

al, 163:233 (10pp), 2022 May

Gupta & Chen

!23°

FCRAO COMPLETE 13CO$ Oph

!23°30"# (J2000)

L1704

!24°

L1729

% Sco
L1689N!24°30"HD 147889

L1712

!25°

L1689S

22 Sco!25°30"16h44m16h40m16h36m16h32m! (J2000)

16h28m16h24m16h20mFigure 2.
A map of 13 CO integrated intensity in the Ophiuchus cloud complex
taken from the COMPLETE survey (Ridge et al. 2006). The major clouds are labeledwith their Lynds designations as are four B stars from the Upper Scorpius subgroupof the Sco-Cen OB association.

Wilking 2008
cloud L1688. Dark streamers trail to the northeast (L1709) and the southeast (L1689).
detailed
due to dust derived from star counts has been presented bymore sensitive than the JCMT GouldThe
Belt Survey
data extinction(PattleCambrésy (1999) and Lombardi, Lada, & Alves (2008) and the corresponding column
et al. 2015).

BA2 850 μm emission map of L1688. The red polygons show the clump boundaries as identiﬁed by the FellWalker algorithm. Prominentashed line denotes the string of small clumps, as discussed in Section 3.

measurements across a range of waves to infer the star formation history in the

L1688

L1709

13

163:233 (10pp), 2022 May

Gupta & Chen

・JCMT/SCUBA-2でとったデータを使った。450 µm 9.8arcsec, 850µm
14.6arcsecの性能。(Herczeg et al. 2017; Johnstone et al. 2018
)感度 2.3 mJy/beam
・Clumpを同定。108個同定。noiseは10mJy/beamとした。
・YSOはthere are 23 class I, 28 at-spectrum, 92 class II, and 36 class III
sources. There are 59 sources without classi cation.
・合計256個のソースに対して、Gaia EDR3の対応天体があったのは99天体。
・今回は動力学をしりたいんで、proper motionを調べる。84天体について
proper motionがわかった。

・それはそれとして、各天体のSEDは自分たちでデータを持ってきて再解析。225µmの赤外線の傾きを調べた。(1) α 0.3 (class 0 to I); (2) ­ 0.3 α < 0.3( at-spectrum sources); (3) ­ 1.6α<­0.3 (classII); (4)α<­1.6 (classIII).
・At the end, our YSO sample consists of 30 Class 0/I sources, 56 at850 μm emission map of L1688. The red polygons show the clump boundaries as identiﬁed by the FellWalker algorithm. Prominent
ed line denotes the string of small clumps, as discussed in Section 3.
spectrum sources, 110 Class II sources, and 58 Class III sources, ofasurements across a range of wavemore sensitive than the JCMT Gould Belt Survey
data~21%(Pattle of the sources had no classi cation prior to our analysis.
which
JCMT/SCUBA 850 µm

fl

−1

fi

fl

udy include submillimeter emission
ecular clouds, and a sample of young
collected from the literature. We are
the spatial distribution and kinematicsfi

ata and Analysis

et al. 2015).
We identiﬁed enhanced submillimeter substructure, or“clumps” using the STARLINK implementation of the FellWalker algorithm (Berry 2015), which traces boundaries ofclumps by following paths from low-valued to high-valued
pixels in an iterative manner. Polygonal clump boundaries are
identiﬁed and their peak ﬂuxes and total ﬂuxes are estimated. For
our analysis, the key parameter for clump detection, the “noise,”flinfer the star formation history in theonomical Journal, 163:233 (10pp), 2022 May• YSOと、一番近い分子雲クランプの距離を測り、Gupta & Chen

histgram を作った。

• Class Iと atは割と分子雲クランプに近い。

The Astronomical Journal, 163:233 (10pp), 2022 May

Gupta

Figure 4. Projected distances from the nearest 850 μm emission clumps of YSOs at different evolutionary phases. The solid color bars show the distributio
YSOs of different classes. The black lines show the distribution for the sample of Dunham et al. (2015).

• 赤い線は進化した星をつないだもの
We now present the motion of the YSOs relative toare class III young stars with no corresponding submilimeteremission, thereby to our knowledge not recognized before.
Spatial distribution of YSOs and of the 850 μm emission outlined by the contours. The YSOs (class I marked by blue circles, ﬂat-spectrum
by purple
To theother side of the main cloud ﬁlaments (A-C-E-F),
lass II by green triangles, class III by red crosses, and unclassiﬁed sources by yellow symbols) are not randomly distributed. Instead, theybetween
appear to Oph-B
follow and Oph-F additional stellar patterns appear topatterns. Inner purple dashed line denotes the string of small clumps, as discussed in Section 3 and illustrated in Figure 1. Outer red dasheddenotesstandline
out,
approximately in the NS of NE-SW direction. It is
volved sources, as discussed in Section 3.1.
not clear whether these are parts of the cloud streamers or of thesouthwest YSO loops which are physically closer in 3d to the
OB stars.
3.1. Stellar Spatial Distribution
without dereddening. The conclusion that less evolved
Such YSOs,
organized patterns could not have been the outcome ofeither with our sample or with that of Dunham et al.
(2015),
are from common sites of formation. In order torandomejectionbased on available kinematic data, as discuss
Section 2.2.1. The peculiar motion of YSOs, i.e., themotion of individual sources subtracted by the medianmotion, is shown in Figure 6. Using these relative velo
we inspected the kinematic distribution for different
of YSOs.
Figure 7 presents the tangential velocity distributi
YSOs at different evolutionary stages. Lacking proper-m
data for highly embedded sources, we combined Cla• 西と南西（右と右下）にOB星があるので、ここからのショックフロントの通過面ではないか？

fl3 displays the spatial distribution of the YSOs with

s K function of the class II and III objects in our sample (in red) is clearly different from that of central 95 percentile interval (the shaded grayion of a randomly distributed simulated sample.

• 青がGaiaデータ。Class IIとIIIは速度分散は同じくらい。ClassIと atは精度が悪いが同程度の速さで動いていることと無矛盾• →YSOの集団は空間的に一緒に動いている
The Astronomical Journal, 163:233 (10pp), 2022 May

Gupta & Chen

Figure 7. Distributions of relative speeds for YSOs of different classes. The blue bars represent the Gaia EDR3 measurements, whereas the orange bars denote theless-precise ground-based measurements (Monet et al. 2003; Ducourant et al. 2017).

flmotions of YSOs, i.e., the proper motion relative to the mean motion. Symbols for different stellar classes are the same as in Figure 3. Each arrow marks
the otherchain of class III sources that are more
er motion, with the length proportional to the speed. The blue arrows represent Gaia measurements, whereas the maroon arrows earlier
are for epoch
valuesonfrom−1
4
evolvedor 3.5depletedof 6¢ in× 10 much
yr. of the circumstellar disks and2.1). The scale reference on the top right marks 10 mas yr , which, in accord with the coordinate axes, corresponds to a motion
interstellar cloud.
White et al. (2015), using the C18O J = 3–2 emission,

This increase of stellar velocity can be the consequence ofdynamical evolution of the young cluster. Simulations ofdynamics of young embedded clusters (e.g., Proszkow et al.
2009) demonstrate that as a system evolves from a subvirial

Clumpy accretion in pre-main-sequence stars as a source of
perturbations in circum- stellar disks
Tatiana V. Demidova, Vladimir P. Grinin ⋆ The developmentof perturbations in the circumstellar disks of pre-mainsequence stars caused by clumpy accretion was investigated.
Here we perform 3D hydrodynamical smoothed particle
hydrody- namics simulations of disks perturbed by a recent
clump accretion event. These simulations are further
explored by radiative transfer calculations to quantify theobservational appearance of such disks. It was shown thatthe density waves in the disks were formed at the fall of theclump. After several revolutions they can transform intospirals and ring structures. Their images in millimeter
wavelengths are very similar to those observed with
Atacama Large Millimeter/submillimeter Array in some
protoplanetary disks. We assume that clumpy accretion may
be the source of such structures.

• 3D SPH計算で、
clumpが降着した際の星周円盤に摂動を与えた結果どうなるかをみた。

• 観測的可視化の結果、ALMAでよく見えるリングなどを再
現できた。

4

Demidova & Grinin

Figure 2. The average value of the z coordinate of the particles in the cells of R, φ. The model parameters are K = 3,

I = 30◦ and L = 0.8. The time in years is in the upper right corner of the pictures.

Table 1. The models parameters
L

I

K

R

dR

φ

Remnant mass

Lifetime
Figure 2. The average value of the z coordinate of the particles in the cells of R, φ. The model parameters are

Float

DegreesNumberAU

AU

Degrees

Jupiter mass

Sructures

(1)

(2)

(3)

(4)

(5)

(6)

(7)

(8)

◦

I = 30 and L = 0.8. The time in years is in the upper right corner of the pictures.
yrs(9)
Table 1. The models parameters

0.8
0.8
0.8
0.8
0.8
1
1
1
1
1
1
1.2
1.2
1.2
1.2
1.2
0.8
1
1.2

5
10
20
30
10
5
10
20
30
5
5
5
10
20
30
30
30
30
30

3
3
3
3
5
3
3
3
3
5
10
3
3
3
3
1
3
3
3

20
20
20
20
20
20
20
20
20
20
20
20
20
20
20
20
10
10
10

5
5
5
5
5
5
5
5
5
5
5
5
5
5
5
5
2
2
2

30
30
30
30
30
30
30
30
30
30
30
30
30
30
30
30
30
30
30

0.11
0.11
0.11
0.11
0.19
0.11
0.11
0.11
0.11
0.19
0.38
0.11
0.11
0.11
0.11
0.04
0.04
0.04
0.04

Arc, One-hand spiral, Horseshoe
Arc, One-hand spiral, Horseshoe
Arc, Faint two-arm spiral, Horseshoe
Arc, Faint two-arm spiral, Horseshoe
Arc, One-hand spiral, Horseshoe
Arc, One-arm spiral, Multi Rings, Ring
Arc, One-arm spiral, Ring
Arc, One-arm spiral, Faint two-arm spiralArc, One-arm spiral, Faint two-arm spiralArc, One-arm spiral, Multi Rings, Ring
Arc, One-arm spiral, Multi Rings, Ring
Arc, One-arm spiral, Multi Rings, Ring
Arc, Bright two-arm spiralArc, Bright two-arm spiralArc, Bright two-arm spiral, Asymmetric ring
Arc, Bright two-arm spiral
Arc
Arc
Arc, Faint two-arm spiral, Multi Rings

> 600
L
I
K
R
dR
φ
Remnant mass
Lif
> 600
Float Degrees Number AU AU Degrees
Jupiter mass
Sructures
> 600
(1)
(2)
(3)
(4) (5)
(6)
(7)
(8)
> 600
0.8
5
3
20
5
30
0.11
Arc, One-hand spiral, Horseshoe
>
> 600
0.8
10
3
20
5
30
0.11
Arc, One-hand spiral, Horseshoe>∼ 1000
0.8
20
3
20
5
30
0.11
Arc, Faint two-arm spiral, Horseshoe
>
0.8
30
3
20
5
30
0.11
Arc, Faint two-arm spiral, Horseshoe
>
> 600
0.8
10
5
20
5
30
0.19
Arc, One-hand spiral, Horseshoe
>
> 600
L:
初期clumpがケプラー速度の何倍で動
1
5
3
20
5
30
0.11
Arc, One-arm spiral, Multi Rings, Ring
∼
> 600
1
10
3
20
5
30
0.11
Arc, One-arm spiral, Ring>
いているか。
1
20
3
20
5
30
0.11
Arc, One-arm spiral, Faint two-arm spiral
>
> 600
1
30
3
20
5
30
0.11
Arc, One-arm spiral, Faint two-arm spiral
>
> 600
1
5
5
20
5
30
0.19
Arc, One-arm spiral, Multi Rings, Ring
>
1
5
10
20
5
30
0.38
Arc, One-arm spiral, Multi Rings, Ring
>
> 600
I:
クランプの初期速度ベクトルの赤道面
1.2
5
3
20
5
30
0.11
Arc, One-arm spiral, Multi Rings, Ring
>
> 600
1.2
10
3
20
5
30
0.11
Arc, Bright two-arm spiral
>
からの角度
1.2
20
3
20
5
30
0.11
Arc, Bright two-arm spiral
>
> 600
1.2
30
3
20
5
30
0.11
Arc, Bright two-arm spiral, Asymmetric ring ∼∼ 2000
1.2
30
1
20
5
30
0.04
Arc, Bright two-arm spiral
>
> 600
0.8
30
3
10
2
30
0.04
Arc
∼
K:クランプは初期に周囲のK倍の密度を
1
30
3
10
2
30
0.04
Arc
∼
∼ 100
1.2
30
3
10
2
30
0.04
Arc, Faint two-arm spiral, Multi Rings∼
持つものとして投入する。
∼ 100
Note—The column of “Structures” lists the types of observed asymmetries in the order of their appearance in the disk
The column of “Lifetimes” is a long-lived structures lifetime.
∼ 450

•
•
•

Note—The column of “Structures” lists the types of observed asymmetries in the order of their appearance in the disk images.
The column of “Lifetimes” is a long-lived structures lifetime.

• R,dR,φの範囲に密度をボコッとふやす。

For the models discussed here, the initial position of the disturbing remnant of the clump was set equal to R
AU with a step of dR = 5 AU. Calculations have shown that the parameter L, which characterizes the kineticof the falling clump, has the greatest influence on the type of disturbance in the disk. Therefore, we will sequ

Clumpy accretion in p-m-s stars as a source of perturbations in circumstellar disks5• サブケプラーの摂動（L<1）だとarc、
渦、スパイラルにすぐ変わる。(~125年)• ケプラー速度の摂動(L=1)

Figure 5. The images at wavelength 1 mm. The color shows the flux of radiation (Fν ) multiplied by R2 in conventional

units. The model parameters are K = 3, I = 10◦ and L = 0.8. The time in years is in the upper right corner of the
Figure 3. The surface density multiplied by the distance from the center of mass (ΣR). The model parameters are
pictures.
K = 3, I = 10◦ and L = 0.8. The time in years is in the upper right corner of the pictures.

Clumpy accretion in p-m-s stars as a source of perturbations in circumstellar disks

7

だと、arc, one-handspiral, その後500年くらいでringっぽくなる
Figure 8. The same as in Fig. 5 for model parameters K = 3, L = 1 after 600 years.◦ The angle of I is in the upper
6. The same as in Fig. 3 for model parameters K = 3, I = 10 and L = 1.
right corner of theFigure
pictures.

• スーパーケプラー速度の摂動(L>1)だと、渦ができて、渦、で２本の腕のspiralになる。

Figure 4. The average value of the z coordinate of the particles in the cells of R, φ along x (left) and y (right) axes

after 600 years. The model parameters are K = 3, L = 0.8 and the angles are in the upper right corner of the pictures.

4.1.1. Sub Keplerian perturbations
In this case, when the parameter is L = 0.8, due to the differential rotation of the Keplerian disk the remnant
stretches and transform to a piece of arc reembling a cyclonic vortex and then turn into a spiral during one revolution
around the star (∼ 125 years). Since the matter of the disk is involved in its motion the spiral dips and thickening of

10

Demidova & Grinin• 1000年位するとクランプは見えなくなり、2000年位だと非軸対称リングとして見えるようになる。

• R=30auだと4e3年くらい、
R=50auだと1e4年くらい、でrelaxする
Figure 14. The same as in Fig. 13 for model with parameters K = 3, I = 30◦ , L = 1.2 at the time 2000 years.

Over time, density waves scattered and the all structure settles down to the plane of the disk. The ring of the firstmodel stretches along the radius and loses brightness mixing with the matter of the protoplanetary disk with time. It
is faintly noticeable at 1000 years after the fall of the clump (Fig. 13 left). Than it is not visible against the backgroundof the disk matter. For the second model spiral waves are still noticeable after 1000 years (Fig. 13 right), but after∼ 2000 years they completely disappear. An asymmetric ring structure can be seen on the disk by the time of 2000
years (Fig. 14).
The charateristic time of the disk dynamic relaxation after the fall of the clump also depends on the place of its fall.
For example, with R0 = 30 AU and the same clump parameters as in the previous model, the lifetime of spirals and3

Linking pressure gradients with the stability of molecular clouds in galactic out ows
K. M. Dasyra, G. F. Paraschos, T. Bisbas, F. Combes, J. A. Fernandez-Ontiveros ⋆ The jets
launched by actively accreting black holes are capable of launching several of the massive(million or billion solar mass) molecular out ows observed in galaxies. These out ows could
suppress or enhance star formation in galaxies. To investigate the stability of clouds capable toform stars in out ows, we modeled CO and HCO+ ALMA data of the galaxy IC5063, in which
black-hole jets impact molecular clouds. Using a radiative transfer code that self-consistently
performs astrochemical and thermal balance calculations based on the available gas heating
sources, we found that mechanical heating and cosmic ray (CR) heating are fully capable

fl

fl

fi

fl

fl

fl

fl

fl

fl

of individually reproducing the data. In our best- t model, CRs provide about 1/3rd of thedense gas heating at the radio lobes, emphasizing the role of this often neglected mechanism inheating the gas and potentially generating out ows. The gas temperature and density indicatethat the jet passage leads to an increase of about 1 order of magnitude in the internal pressure
Pi of molecular clouds (with Pi/k from 8*105 up to 7*106 K cm−3), irrespective of theexcitation mechanism. From the uxes of [S II] and [N II] lines in VLT MUSE data, theexternal pressure Pe of molecular clouds increases in several regions enough to exceed Pi. This
result leads us to conclude that we are observing the expansion of an ionized overpressurizedcocoon that compresses molecular clouds and that could lead to their collapse. Some jetimpacted clouds, nonetheless, near pathways that the jet cleared have increased Pi anddecreased Pe. They are likely to undergo evaporation of their outer layers. Part of theevaporated layers could mass load the out ow thanks to ram pressure from co-spatial ionizedgas ows. The observed pressure changes thus suggest that both star formation enhancement
and suppression could simultaneously occur.

Emma C. Daffern-Powell, Richard J. Parker, Sascha P. Quanz ⋆ Gravitational interactions in star-forming regions are capable ofdisrupting and destroying planetary systems, as well as creating new ones. In particular, a planet can be stolen, where it is directly
exchanged between passing stars during an interaction; or captured, where a planet is rst ejected from its birth system and is freeoating for a period of time, before being captured by a passing star. We perform sets of direct N-body simulations of young,
substructured star-forming regions, and follow their evolution for 10 Myr in order to determine how many planets are stolen andcaptured, and their respective orbital properties. We show that in high density star-forming regions, stolen and captured planets
have distinct properties. The semimajor axis distribution of captured planets is signi cantly skewed to wider orbits compared tothe semimajor axis distribution of stolen planets and planets that are still orbiting their parent star (preserved planets). However,
the eccentricity and inclination distributions of captured and stolen planets are similar, but in turn very different to the inclinationand eccentricity distributions of preserved planets. In low-density star-forming regions these differences are not as distinct but
could still, in principle, be used to determine whether observed exoplanets have likely formed in situ or have been stolen or
captured. We nd that the initial degree of spatial and kinematic substructure in a star-forming region is as important a factor as
the stellar density in determining whether a planetary system will be altered, disrupted, captured or stolen.

• N体計算で恒星遭遇における惑星の捕獲等について調べた。
• 高密度の星形成領域では、捕獲された惑星は違う性質を持つ。軌道長半径が長かったり。だが、eccentricity/fi

fiinclinationの分布に強い違いは見られなかった。

fifl

The Great Planetary Heist: Theft and capture in star-forming regions

fi

fi

Sebastiano von Fellenberg, Stefan Gillessen, Julia Stadler, Michi Bauböck, Reinhard Genzel, Tim de Zeeuw, Oliver Pfuhl, Pau Amaro
Seoane, Antonia Drescher, Frank Eisenhauer, Maryam Habibi, Thomas Ott, Felix Widmann, Alice Young ⋆ We present a large ∼ 30” ×
30” spectroscopic survey of the Galactic Center using the SINFONI IFU at the VLT. Combining observations of the last two decades
we compile spectra of over 2800 stars. Using the Bracket-γ absorption lines we identify 195 young stars, extending the list of known
young stars by 79. In order to explore the angular momentum distribution of the young stars, we introduce an isotropic cluster prior.
This prior reproduces an isotropic cluster in a mathematically exact way, which we test through numerical simulations. We calculate
the posterior angular momentum space as function of projected separation from Sgr A*. We nd that the observed young star
distribution is substantially different from an isotropic cluster. We identify the previously reported feature of the clockwise disk andnd that its angular momentum changes as function of separation from the black hole, and thus con rm a warp of the clockwise disk(p ∼ 99.2%). At large separations, we discover three prominent overdensities of angular momentum. One overdensity has beenreported previously, the counter-clockwise disk. The other two are new. Determining the likely members of these structures, we ndthat as many as 75% of stars can be associated with one of these features. Stars belonging to the warped clockwise-disk show a top
heavy K-band luminosity function, while stars belonging to the larger separation features do not. Our observations are in good
agreement with the predictions of simulations of in-situ star formation, and argue for common formation of these structures.

fifi

The young stars in the Galactic CenterCurved jet motion. I. Orbiting and precessing jets

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fi

fi

fi

fi

Christian Fendt, Melis Yardimci ⋆ Astrophysical jets are often observed as bent or curved structures. We also know that the different
jet sources may be binary in nature, which may lead to a regular, periodic motion of the jet nozzle, an orbital motion or precession.
Here, we present the results of 2D (M)HD simulations in order to investigate how a precessing or orbiting jet nozzle affects the
propagation of a high-speed jet. We have performed a parameter study of systems with different precession angles, orbital periods orseparations, and different magnetic eld strengths. We nd that these kinds of nozzles lead to curved jet propagation which isdetermined by the main parameters that de ne the jet nozzle. We nd C-shaped jets from orbiting nozzles and S-shaped jets fromprecessing nozzles. Over long time and long distances, the initially curved jet motion bores a broad channel into the ambient gas
that is lled with high-speed jet material which lateral motion is damped, however. A strong (longitudinal) magnetic eld can damp
the jet curvature that is enforced by either precession of orbital motion of the jet sources. We have investigated the force balanceacross the jet and ambient medium and found that the lateral magnetic pressure and gas pressure gradients are almost balanced, butthat a lack of gas pressure on the concave side of the curvature is leading to the lateral motion. Magnetic tension does not play asigni cant role. Our results are obtained in code units, but we provide scaling relations such that our results may be applied to youngstars, micro-quasars, symbiotic stars or AGN.