Star Formation NewsletterNo. 362 31-46
高橋実道（鹿児島大学/NAOJ）

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system,thebetweenRAMSES
andPLUTO
regardingmanyof the collapse
properties
and fragmentation
methodmakes
it possible
to Grandrecoverthemeanpolarization
properties
but
also
to
characterize
the fraction
intrinsic offormation
inagreement
progress.
While
there
isnot
now
evidence
that
Earth-sized
terrestrial
planets
orbit
the ionizing
sourcesuggestthepossibilityof onlythe‘rocketeﬀect’
scenarioin theremnant
cloud(BRC31).a significant
andmigration
in
the
Tack
model
discovered
eight
Scutifromcandidates.
NoneofMaxwell
these
were
previously
known.
Furthermore,
wedetected
17atheeclipsinga
distorted
inner
disk,
which
may
be
common,asindicatedbythesurveyoftransitional
disk
systems
at
resolution
on
the
local
dust-to-gas
mass
ratio.
We
found
that
the
smoothviscositytransitions
at
the
outer
edge
of
dead
zone
spectraldata
products
the
James
Clerk
Telescopearchive,centered
on
the
two
RMS
objectswith
7’x7’
processisgood.
Fragmentation
occurringintheinnermostregionandnumerical
choices
(use
of
sink
particles,
grid)
scatter,thus
creating
new
ways
to
characterizeISMturbulenceandthemagnetic
field
strength.
Finally,we
apply
StructureandKinematics
of
Sh2-138–A
distant
hub-filament
systemintheoutersolar-typestars,
theanticipateddusty
debrissignatureof
theirformationisrarelydetected.
Here
we
discuss
severalMasahiro
Ogihara,Hidenori
Genda,
Yasuhito
SekineFproper
The formation
andsubsequentmigrationof gasgiants could
binaries
where
two
were
previously
known.
Basedonthemotions
provided
by
the
Gaia
EDR3
catalogue,
we
of
⇠0.1
arcsec.
canbecomeRossbyunstableandform
vortices.
Asinglelarge-scalevortexdevelops
if
the
dust
content
of
the
disc
is
field
of
view
each,
were
utilisedforthepurpose.
The
13CO(3-2)
channelmapoftheregionshowsthemolecular
haveacrucialimpactwhen
similarbutsmoothinitialconditionsareemployedmorecrucialthan
thecode’schoiceourmethodtoanexisting
data
set
of
starlight
polarization
with
known
line-of-sightdecomposition,
demonstrating
Galactic
plane
ways
in
which
our
current
ideas
about
terrestrial
planetformation
imply
transportmechanisms
capableoferasingthesignificantly
aﬀect
themembershipmaterial
mixingin ParSecs
the Solar
System.
Instars.
thisstudy,
weuse N-bodysimulations
to ofinvestigate
Extension
of
HOPS
Out
to
500
(eHOPS).
I.
Identification
andModeling
calculatedtheclusterprobabilities
for91
variableFor
61
variables,aprobability
higher
than
80%
well
coupledtothegas,
however,
multiple
small-scalevortices
ensue
for
the
case
of
less
coupled
dust.
As
both
type
cloud
to
have
filamentary
extensions
directed
away
from
the
massive
star,
which
also
seems
to
be
at
the
edge
of
a
on
the
system’soutcome,multipleorcentrally-condensed.
Kshitiz
Mallick,
LokeshDewangan,
Devendra
Ojha,
Tapas
Baug,
Igor
Zinchenko
F
We
presentamolecularagreement
withprevious
resultsandanimproved
quantificationof
uncertainties
incloud
properties.
anticipateddebrisAMoleculartenuousgasClouds
disk
may
be25regenerated
via"takeout"theliberationofplanetary
how
much
water
is signature.
transported
into
regionof protostar:theterrestrial
formation
duringthegrowthandmigration
Disk
fragmentation
aroundathemassive
aplanetcomparisonof (i.e.,twothree-dimensional
Protostars
intheAquilawasdetermined,
which
makes
them
clustermembers.
Only
variableswithaprobability
less
than
20%
were
regardedcavitylikestructure.
Multiplemolecular
cloud
protrusions
into
thissuﬃcient
cavitystructure
hostterrestrial
localbypeaks
ofsolidemission.
of vorticesaretrappedatthe dead
zone
outer
edge,
they
providetime
forinvestigate
dust
growth.
The
content
line
study
of
the
Sh2-138(IRAS
22308+5812)
hub-filament
system
with
an
aim
to
its
structureandatmospheresingiant
impacts)or"delivery"(i.e.,
byasteroids
andcomets
flung
into
the
planetregion)atphasesofJupiter
in
the
Grand
Tack
model.
We
found
that
Jupiter’s
growthwasaccompanied
significant
mass
Surveyof H↵emission-linestarsA.inGutermuth,
the star-forming
regionJ.IC
5070
codes
Riwaj
Pokhrel,S. Thomas
Megeath, Robert
Elise Furlan, William
Fischer,Samuel Federman,
tobenon-members.
The
integrated
emissionmapofthe
regionconstructed
from
only
those
emissionclumpsdetected
above
5
level
in
collected
bythevortices
canexceedseveralhundredEarthmasses,while
thedust-to-gas
densityratio
withinoften
kinematics.
ArchivalCOmolecular
line
data
from
the
Canadian
Galactic
Plane
Survey(CO(J=1-0))
for
the
wider
transport,
and thata substantial
amountofActively
water(about10protoplanetary
times
Earth’s
ocean
mass
for
the
initialplanetesimal
aThe
level
to
removethewarmdebris.
The
powerfulstellarwindfroma Thomasyoung
star
canemission
also
act,
its indeliveredJohn
J.suﬃcient
Tobin,
AmeliaM.
Stutz,
Lee
Hartmann,
Mayra
Osorio,Dan
M.
Watson,Stanke,P. (Abridged)
Manoj,
NeelamPanwar,
Jessy
Jose,
Rishi
C
F
accretingyoung
stellarobjects
show
H↵
line
their
Raphaël
Mignon-Risse,
André
Oliva,
Matthias
González,
Rolf
Kuiper,BenoîtCommerçon
F
Most
A
CCD
Searchfor
Variable
Stars
in
the
Open
Cluster
NGC
6611
ALMA
view
of
MP
Mus
(PDS
66):
a
disk
with
no
visiblegaps
theposition-position-velocity
space
aﬃrms
the
same.
MSX
sources
were
found
distributed
along
the
cavityboundary
exceeds
unity.
Thus,
suchvorticesfunctionasplanetarynurseries
withinthedisc,providing
ideal
sites
for
formationthetransitionaldiskaroundSY
Cha.
Our
high-resolution
observations
clearly
revealedtheinnercavityandthecentralregion(50arcminx50arcmin)
and
the
James
Clerk
Maxwell
Telescope(CO(3-2),
13CO(3-2),
and
C18O(3-2))
fortheMayankNarang,PrabhaniAtnagulov,
Nolan
Habel,
Wafa
Zakri
F
We
presenta
Spitzer/Herschelfocusedsurveydistribution
based
on
the
minimum-masssolar
nebula)wastransported
intotheterrestrial
planetregion.
The
total
wind
momentumproducing
a
drag
that
removeswarm
debris.
If
suchprocesses
areeﬃcient,
terrestrial
planetsmayspectra.
We
present
theresultsofsurveyforH↵emission-line
stars
in
the
star-forming
region
IC
5070
taken
with
massivestars
arelocatedinmultiplesystems.
The
modelingofdisk
fragmentation,apossiblemechanism
leadingtoG.
Michalska,Z.
Kołaczkowski,
R.
Leiton,O.
Szewczyk,
K.
Kinemuchi,
V.,
M.
KalariF
We
present
theresults
down
to
4
au
scaleswherethegasforhas
thebeen
compressed.
Spectralextraction
atthese
positionsyieldedhighMachnumbersandlowof
planetesimals
andeventuallyplanetarysystems.
point
source
the
first
time.
The
radialprofile
of
the
ring
can
be
approximatedbyabrightnarrowring
superimposed
centralportion(5arcminx5arcmin)
have
been
utilised.
AnalysisoftheCO(1-0)spectrafortheextendedregioninof
theAquilamolecular
clouds
(d
⇠
436
pc)
as
part
of
the
eHOPS
(extension
of
HOPS
Out
to
500
ParSecs)
censusSpiralStructureandMassiveStar
formation
inthe
Hub-Filament-System
G326.27-0.49
amountdeliveredincreasedfurtherduringJupiter’s
migration
phase(totaling
about
10-40
times
Earth’soceanmass),
assembleinconspicuously,
withlittlepublicity
andhooplaaccompanying
theirbirth.
Alternatively,therarityofwarm
2-m
Himalyan
Chandra
Telescope.
Based
onN.
the
H↵
slitless
spectroscopy
data,
we
identified
131Carpenter,emission-linestars
instellarmultiplicity,reliesonparallel3D
simulation
codes
whose
agreement
remainstobeevaluated.
Using
the
Cartesian
of
the
U
BV
I
variability
survey
in
the
young
open
cluster
NGC
6611
based
on
observations
obtainedduring34
nightsÁ.
Ribas,
E.
Macías,P.
Weber,
S.
Pérez,
Cuello,R.
Dong,
A.
Aguayo,C.
Cáceres,
J.
W.
R.
F.
C
ratiosofthermaltonon-thermalpressure,suggestingaWyrowski,
dominanceofsupersonicandnon-thermal
motioninthecloud.
important
step
forwardinreconstructing
themagnetizedinterstellar
medium(ISM)
in
3D
withindusty
regions.
Weonafainterwide
ring.
Furthermore,
we
found
that
there
iscolumn
a veryweak
azimuthal
asymmetryindust
continuum
emission.
ofnearbyprotostars.
For
every
sourcedetectedinthe
Herschel/PACS
bands,theeHOPS-Aquila
catalog
contains
1conjunction
with
the
hub
and
filament
identification
using
density
map
and
the
getsf
tool,
respectively,
reveals
Bhaswati
Mookerjea,
V.
S.
Veena,
Rolf
Guesten,F.
Akhil
LasradoF
Hub-filament
systems(HFSs)
are
which
was
less
dependent
onsimulation
parameters.
In
addition,atthesestages,terrestrial
planets
were
not
fully
excesses
may
imply
that
terrestrial
planets
typically
form
early,
emerging
fully
formedfromthenebular
phase
⇠
0.29
squaredegrees
area
of
the
IC
5070
region.
Using
Gaia
Early
Data
Release3,
weestimatedthemeanproper
AMR
code
RAMSES,
wecomparedisk
fragmentationinEspaillat,
a centrally-condensed
protostellar
systemto the F
study
of
Oliva
12found
13 CO
18 of
Dent,
I.
de
Gregorio-Monsalvo,G.
Duchêne,C.
C.
P.
Riviere-Marichalar,
M.
VillenaveWepresent
spanning
one
year.
In
total,
we95
variablestars.
Most
these
stars
are
classified
asperiodicandirregular
Investigatingthemorphology
andgas
kinematics
of
Sh2-112
regionFor
gas Therefore,
emissions,wewhichdetected
CO(2
1),
CO(2
1)the
and
C
O(2
1),
from
which
we
estimated
the
total
gas
mass atdevelopa modelinwaterthepolarization
signalfromthemagnetized
and
dusty
ISM
isreddeningbythinlayers
850µm
SEDs
assembledfrom
2MASS,
Spitzer,
Herschel,
WISE,
andJCMT/SCUBA-2
data.
Using
adescribednewlydeveloped
awithout
complexstructurewiththespectralextractionforcentralposition
displaying
multiplevelocity
components.
potentialsites
offormationofstarclusters
and
high
mass
stars.
To
understand
the
HFSs
and
to
provideobservationalgrown.
suppliedduringthese
earlystagescouldinteractwithmetalliciron
duringthecoreformation
motionandparallaxoftheemission-linestars.
Wealso
estimatedthemeandistanceandtowardtheregionundergoinglate-stage
giant
impacts.
Ineithercase,
theobservable
signpostsofterrestrial
planetformation&
Kuiper(2020)
performed
on
a
grid
in
spherical
coordinates
using
PLUTO.
Two
RAMSESruns
areconsidered
andDirectimaging
discoveryofasuper-Jovian
aroundthe
young
Sun-like
star
AF
Leporis4
4
ALMA
multiwavelength
observations
oftheprotoplanetarydiskaroundthenearby(d⇠100
pc)
young
solar
analogMP
pre-mainsequence(PMS)
stars.
The
analysis
of
the
JHK
2MASS
photometryandfour-colour
IRAC
photometry
Kshitiz
Mallick,
Saurabh
Sharma,LokeshDewangan,
Devendra
Ojha,
NeelamPanwar,
Tapas
Baug
F be
We
S
settheof criteria,
weclassify
objects
by
their
SEDs
as
protostars,
pre-mssequencestars
withdisks,
andgalaxies.
Ainferred
total
of
disk
to
be
2.2
⇥
10
M
,
assuming
a
CO/H
ratio
of
10
.
The
observations
showed
that
the
gas
is
present
variousdistances.
Ourmodeling
makes
itpossible
to
infer
the
mean
polarization(amplitude
andorientation)induced
2
Based
on
the
Herschel70
micronwarm
dust
emission,
one
of
the
filaments
intheextendedregionwastoconstraints
oncurrent
theoriesthat
attempttoexplainstar
formation
globally,wereport
a
study
of
the
regionassociatedofprotoplanets
and/orgrowing
Earth.
Since
hydrogeninwatermoleculescandissolve
into
theircores,
this
could
using
the
emission-linestars,
thatare⇠ previously
833
pcof
and
⇠2
mag,
respectively.
ByLate-stage
examiningthelocations
ofE.
these
stars
appearmore
challenging
todetectthan
assumed.
We
discuss
observational
tests
of
these
ideas.
give
qualitatively
distinct
pictures.
When
allowing
forunlimitedsinkparticlecreation,gas
fragmentation
leads
to
aLea
Takeout
andDelivery:ErasingtheDusty
SignatureofTerrestrial
PlanetRobert
J.
De
Rosa,
Eric
L.
Nielsen,
Zahed
Wahhaj,Jean-Baptise
Ruﬃo,
Paul
G.
Kalas,
Anne
Peck,
12
Mus
(PDS
66).
These
observations
at
0.89
mm,
1.3
mm,
and
2.2
mm
have
angularresolutionsof⇠
1",
0.05",
and0.25",
revealed
165
Class
II
young
stellarsources,
20
which
are
irregular
variables
and
one
is
an
eclipsingbinary.
These
present
a
study
of
the
molecular
cloudin
Sh2-112
massivestarforming
region
using
the
3-2
transition
of
CO
isoof
172
protostars
are
found
in
Aquila,tightly
concentratedinthemolecular
filaments
that
threadtheclouds.
Ofthese,
insidethedustcavity.
The
analysisofthevelocity
structure
of
the
CO(2
1)
emissionline
revealedthatthevelocitybyindividual
dusty
cloudsandtoaccountfortheturbulence-induced
scatterinagenericway.
We
presentalikelihood
associatedwithactivestar
formation,
and
is
host
to
a
Bolocam
1.1
mm
clump
of
1606
Msun.
Integrated
intensitymap
with
G326.27-0.49
using
infrared
data
of
dust
continuum
andnewly
obtained
observationsonmolecular
tracersusing
explainthedensity
deficitobservedinthecurrent
Earthcore.
Notably,
Jupiter
could
play
an
importantroleasyoungainthecolor-magnitude
diagrams
constructed
using
Gaia
and
PanSTARRS1
data,
we
found
that
a
majorityoftheH↵
multiplestellarsystemwhose
multiplicity
isaﬀected
by
the
grid
when
triggeringfragmentation
andbynumericallyPlanetarynurseries:
vortices
formedatsmoothviscositytransition
Formation
A.
Hirsch,WilliamRobersonF(abridged)
Expandingthesampleofdirectly
imagedcompanions
tonearby,respectively,
and
probe
the
dust
and
gas
in
the
systemwith
unprecedented
detailandsensitivity.
The
disk
appears
classifications,complemented
by
UKIDSS
photometry
and
riH↵
VPHAS
photometry,
were
tofor
identify
7113CO(3-2)(42%) areClass
0 protostars,
54 JHK
(31%)
are
Class
Iwhichprotostars,
43(25%)
areparallax.
flat-spectrum
protostars,
and used
4space,(2%)
topologues
CO,
13CO,
and
C18O;
supplemented
in
part
by
CGPS
HI
line
emission
and
MSX
data.
Sh2-112isan
isdistortedatthelocation
of
the
dust
inner
disk,
may
be
owing
to
warping
of
the
disk
or
radialgas
flow
withinfunctionthat
explicitly
accounts
foruncertainties
inpolarization
andWe
developaframework
reconofemission,constructedfromclumpsdetectedatabove
5sigmainposition-position-velocity
revealsthe
APEX
telescope.
We
use
the
spectroscopic
observations
toidentify
velocity-coherent
structures(filaments
and”barrier”
inexplaining
thedichotomyoftheisotopic
compositions
betweennoncarbonaceous(NC)
andcarbonaceousemittersareyounglow-mass(<
1.50M) stars.
We
also
comparedourcatalog
ofexpected
emission-line
stars
with
the
available
assistedmergers.
On
the
other
hand,
using
a
unique,central,fixedsinkparticle,acentrally-condensed
systemforms,
Zs.
Regaly,K.
Kadam,
D.
Tarczay-Nehez
F
ExcitationofRossbywave
instability
anddevelopmentofalarge-scale
Joan
R.
Najita,Scott
J.
KenyonF
The
formationofplanets
like
Earth
is
to
concludewithaseries
of
stars
that
are
amenabletodetailed
astrometricandspectroscopic
studiesiscriticalforthecontinued
development
and
are
Class
II
sources.
Ten
of
the
Class
protostars
are
young
PACS
BrightRed
Sourcessimilartothosediscoveredinsmooth
down
to
the
4
au
resolution
of
the
1.3
mm
observations,incontrast
with
most
disks
observed
atcomparable
24
candidates
forclassical
T
Tauri
stars
and
30
weak-linedT
Tauristars.
In
addition
tothePMS
variables,
we
optically
visibleregionpowered
by
an
O8V
type
massive
star
BD
+45
3216,
and
hosts
two
Red
MSX
Surveysourcesthecavity
of
the
dust
disk.
High-resolution
observations
of
SY
Cha
showedthat
thissystemiscomposed
of
a
ring
and
Early
water
deliverytoterrestrial
planetregions
duringthestagesofJupiter’s
formation
structingthemagnetizedISM
throughthemaximizationofthelog-likelihood
usinganestedsampling
method.
We
threefilamentary
structures(labelled
W-f,
SW-f,
and
SE-f)
in
the
centralportion.
Velocity
gradients
observedinclumps)
and
study
their
properties
ataresolution
of
0.4
pc.
The
regioncontains
two
mainvelocity
components:
first
(CC)
meteorites.
This
study’s
results
show
that
Jupiter’s
growthnecessitatessomemixingofNC
andCCmaterials.
+0.11
young
stellarcatalogs
and
found
that
most
of
them
are
Class
II/
flat
spectrumsourceswiththespectraltype
rangingsimilartothatreportedin
PLUTO.
The
RAMSES-PLUTO
comparison
isperformedwiththelatter:agreement
vortex
at
the
outer
dead
zone
edge
of
protoplanetary
discs
is
one
of
the
leadingtheoriesthat
explains
horseshoe-likelate-stage
giant
impacts
thatgeneratewarm
dusty
debris,themostanticipatedvisiblesignpostofterrestrial
planetOrion.
We
compare
the
SEDs
to
a
grid
of
radiative
transfermodelstoconstraintheluminosities,
envelope
densities,
validation
oftheoriesof
theirevolutionandatmosphericprocesses.
The
recentreleaseoftheGaia
astrometriccatalogue
spatialscales.
The
dust
disk
has
a
radius
of
60±5
au,
a
dust
mass
of
0.14
M
,
and
a
mm
spectralindex<2
discovered
eight
Scuti
candidates.
None
of
these
were
previously
known.
Furthermore,
wedetected17
eclipsing
Jup
G083.7962+03.3058
andG083.7071+03.2817
classified
asHII
regionandyoungstellarobject,respectively.
Reduced0.06
adistorted
inner
disk,
which
may
be
common,asindicatedbythesurveyoftransitional
disk
systemsataresolution
andmigration
in
the
Grand
Tack
model
test
our
Bayesian
inversion
methodonmock
datatakingintoaccount
realistic
uncertainties
from
Gaia
and
as
expected
13CO(3-2)
position-velocity
slicespoint
tolongitudinal
gas
flow
along
the
filaments
into
thecentralregion.
Filaments
component
shows
four
filaments
between
-63
and
-55
km/s
forminga spiralstructure
converging
inafindshub,
thesecond20
from
K
to
M.
Based
on
the
propermotion/parallax
valuesandlocationsonthecolor-magnitude
diagrams,
about
between
the
two
codes
is
found
regardingthefirstrotationally-supported
disk
formation,
thepresenceofanaccretionbrightness
distributionintransition
discs.
Formationofsuchvorticesrequiresarelatively
sharp
viscositytransition.
andenvelope
massesoftheprotostars.
A
comparison
oftheeHOPS-Aquila
to
the
HOPS
protostars
in
Orion
that
formation
inprogress.
While
there
is
now
evidence
that
Earth-sized
terrestrial
planetsorbitasignificant
fraction
of
in
the
inner
30
au,
suggesting
optically
thickemissionfromgrainswithhighalbedointhisregion.
Severalmolecular
allowsustoeﬃciently
searchfortheseelusivecompanions
bytargeting
those
stars
that
exhibittheastrometricreflexbinaries
where
two
were
previously
known.
Basedonthepropermotions
provided
by
the
Gaia
EDR3
catalogue,
wespectraldata
products
from
the
James
Clerk
Maxwell
Telescopearchive,centered
on
the
two
RMS
objects
with
7’x7’
of
⇠0.1
arcsec.
Masahiro
Ogihara,Hidenori
Genda,
Yasuhito
SekineF
The
formationandsubsequentmigrationofgas
giants
could
for
the
opticalpolarization
surveyPASIPHAE
accordingtothecurrently
plannedobservingstrategy.
Wedemonstrate
W-f,
SW-f,
and
SE-f
were
calculatedtohave
observed
line
masses
of
32,
33.5,
and
50
Msun/pc,
respectively.
Thefilamentarycomponent
at
-72
km/s
harborsamassiveyoung
stellarobjectpossiblyinteracts
with
the
hub.
The
emission-line
stars
are
flaggedasnon-members.
The
relative
propermotionoftheemission-line
stars
with
respect
totheprotostellar
luminosity
functions
in
the
two
star-forming
regionsarestatisticallyindistinguishable,
thebolometric
shock
onto
it,
the
first
fragmentation
phase.
Gaseousfragments
form
and
their
properties
areinagreement
between
Detailed
modelling,
however,
indicatesthat
viscositytransitions
at
the
outer
edge
of
the
dead
zone
is
relatively
smooth.
solar-typestars,
theanticipateddusty
debrissignatureof
theirformationisrarelydetected.
Here
we
discuss
several
gas
lines
are
also
detected
extendingupto130±15au,
similartosmall
grainstracedbyscatteredlightobservations.
motioninducedbyanorbiting
companion.
The
nearby
(27
pc),
young
(24
Myr)
star
AF
Leporis
(AF
Lep)
was
calculatedtheclustermembershipprobabilities
for91
variablestars.
For
61
variables,aprobability
higher
than
80%
ALMA
Band
6
high-resolution
observationsofthetransitionaldiskaround
SY
Cha
field
of
view
each,
were
utilisedforthepurpose.
The
13CO(3-2)
channelmapoftheregionshowsthemolecularsignificantly
aﬀect
the
material
mixinginthe
Solar
System.
In
thisstudy,
weuse
N-bodysimulations
toinvestigatethat
ourmethodiseﬀectiveatrecovering
the
cloud
properties
as
soon
as
the
polarizationinduced
by
a
cloud
to
its
cloud
was
found
to
be
dominatedbysupersonicandnon-thermal
motions,
with
high
Mach
numbers
(>3)
and
low
clumpsharbouring
the
three
main
YSOs
regionaremassive(187-535
Msun),
have
luminosities
consistentwithtemperatures/envelope
massesofeHOPS-Aquila
protostars
areshiftedtocoolertemperatures/higher
masses,andthetheionizing
sourcesuggestthepossibilityofthe‘rocketeﬀect’
scenario
intheremnant
cloud
(BRC
31).
In
this
study,
we
present
2D
global,non-isothermal,
gas-dust
coupledhydrodynamic
simulations
toinvestigate
thetwocodes.
Asaminor
diﬀerence,fragments
dynamics
causesthedisk
structuretobe
sub-Keplerian
in
RAMSES
ways
in
which
our
current
ideas
about
terrestrial
planetformation
imply
transportmechanisms
capableoferasingtheComparingthefluxesofdiﬀerentCOisotopologues
withprevious
modelsyields
a
gas
mass
of
0.1
1M
,
implying
targeted
becauseofits
astrometricacceleration,
consistentwithawide-orbit
planetarycompanion
detectable
with
Ryuta
Orihara,Munetake
Momose,Takayuki
Muto,
Jun
Hashimoto,
Hauyu
BaobabLiu,
Takashi
Tsukwasdetermined,
which
makes
them
clustermembers.
Only
25
variableswithaprobability
less
than
20%
were
regarded
Jup
6
3
cloud
to
have
filamentary
extensions
directed
away
from
the
massive
star,
which
also
seems
to
be
at
the
edge
of
a
thermaltonon-thermalpressure
ratio(0.01-0.1).
backgroundstars
higher
than
⇠
0.1%
for
the
adoptedsurveyexposure
time
and
level
of
systematic
uncertainty.
Our
how
much
water
is
transported
into
the
regionoftheterrestrial
planetformation
duringthegrowthandmigration
B-typestars,
havecentraldensities
of
10
cm
and
drive
large
outflows.
Majorityofthevelocity-coherent
clumpseHOPS-Aquila
protostars
do
not
show
the
declineinluminosity
withevolution
foundinOrion.
We
briefly
discuss
SurveyH↵emission-line
stars
in
the
star-forming
regionIC
5070
ofvortexexcitationsmoothviscositytransitions.
Ourmodels
are
based
on
ahost
recently
postulated
scenario,
whereasitTomoyuki
isof
found
to
be1-10.
Keplerianandmeasurereachesquiescence
PLUTO.
We
attribute
thisdiscrepancy
toderive
theof
centralstar
anticipateddebrissignature.
Aatmoleculartenuous
gas
disk
may
be in
regenerated
via"takeout"(i.e.,
theliberation
planetaryapossibility
gas
to
dust
ratio
of
We
also
a
dynamical
stellarmass
ofM=1.30±0.08
M
and
an
age
ofthe
high-contrast
imaging.
We
used
the
SPHERE
instrument
on
the
VLT
to
searchfor
faintsubstellar
companions
inagoshi,
Kudo,
Sanemichi
Takahashi,
Yi
Yang,
Yasuhiro
Hasegawa,
Ruobing
Dong,
MihokoKonishi,tobenon-members.
dyncavitylikestructure.
Multiple
cloud
protrusions
into
this
cavitystructure
local
peaks
of
emission.
methodmakes
itpossibletorecover
not
only
the
mean
polarization
properties
but
also
to
characterizetheintrinsic
phasesofJupiter
in
the
Grand
Tack
model.
We
found
that
Jupiter’s
growthwasaccompaniedbysignificant
massin
the twiceregionshow
virialparameters
between2-7,
which
considering
thedetection
ofhistories,
protostars
impliescollapsetobewhether
these
diﬀerences
are
due
to
biasesbetweenthesamples,
divergingstar
formationorIn
theinfluence
ofregion)
NeelamPanwar,
Jessy
Jose,
Rishi
C
F
Activelyaccretingyoung
stellarobjectsshow
H↵
emission
line
in
their
whereintherecombinationofchargedparticlesonthesurfaceof
dust
grainsresultsin
reducedionisation
fractionbeing
lessmassivein
RAMSES
becauseofthediﬀerent
stellaraccretion
subgridmodels.
acentrally-condensed
atmospheresingiant
impacts)or"delivery"(i.e.,
byasteroids
andcomets
flung
into
the
terrestrial
planetat
7-10
Myr forthesystem.
The
survivalofobservations
large
grainsinfromanevolveddisk
without
gaps/ringsissurprising,
and
itand
is
Eiji
AkiyamaFIn
thisstudy,
wereportedtheresultsofhigh-resolution(0.14
arcsec)Atacama
Large
Millimeimmediate
vicinity
of
AF
Lep.
We
used
of
a
nearbystar
interleaved
with
those
of
AF
Lep
to
eﬃciently
4The
integrated
emissionmapofthe
regionconstructed
only
those
emissionclumpsdetected
above
5
level
in
Extension
of
HOPS
Out
to
500
ParSecs(eHOPS).
I.
Identification
andModelingofenvironment
onprotostellar
evolution.
scatter,thus
creating
new
ways
to
characterizeISMturbulenceandthemagnetic
field
strength.
Finally,we
applytransport,
and
that
a
substantial
amountofwater(about10
times
Earth’s
ocean
mass
for
the
initialplanetesimal
gradual.
We
concludethattheregionconsistsofa
networkoffilaments
throughwhich
massaccretes(10
Msun/yr)spectra.
We
present
theresults
ofobservations
surveyforH↵emission-line
stars
inalpha-parameterthestar-forming
region
IC
5070
taken
with 1
inturn
theturbulenceduetomagnetorotational
instability.
Thus,
the
for
the
disc
viscosity
depends
system,theagreement
betweenRAMSES
andPLUTO
regarding
many
of
the
collapse
properties
andfragmentationalevel
suﬃcienttoremovethewarmdebris.
The
powerfulstellar
wind
from
a
young
star
can
also
act,
its
deliveredpossiblethatexisting
substructures
remainundetectedduetooptically
thickemissionat
1.3
mm.
Alternatively,small
ter/submillimeter
Array(ALMA)
of
the
225
GHz
dust
continuumandCOmolecularemissionlines
fromsubtracttheresidual
point
spreadfunction.
This
providedsensitivity
tofaintplanetary-masscompanions
withintheposition-position-velocity
space
aﬃrms
theofsame.
MSXsources
were
found
distributed
along
thenewcavityboundary
Protostars
intheAquilaMolecular
Cloudsourmethodtoanexisting
data
set
of
starlight
polarization
with
known
line-of-sightdecomposition,
demonstrating
distribution
based
on
the
minimum-masssolar
nebula)wastransported
intotheterrestrial
planetregion.
The
total
onto
the
hub.
The
hub
and
some
of
the
ends
filaments
appeartobeundergoingcollapsetoformstars.
This
SpiralStructureandMassiveStar
formation
inthe
Hub-Filament-System
G326.27-0.49
2-m
Himalyan
Chandra
Telescope.
Based
on
the
H↵
slitless
spectroscopy
data,
we
identified
131
emission-line
stars
in
on
the
local
dust-to-gas
mass
ratio.
We
found
that
the
smoothviscositytransitions
at
the
outer
edge
of
the
dead
zone
process
is good.
Fragmentation
occurringintheinnermostregionandnumerical
choices(useof(9sink
particles,
grid)
wind
momentumproducingaMegeath,dragthatremoveswarm
debris.
Ifthesesuchprocesses
areeﬃcient,
terrestrial
planetsmay
structures
may
still
remainunresolved
withthecurrent
observations.
BasedonWilliam
simplescaling
relationsforgap-opening
arcsec
(⇠30
au)
of
the
star.
We
detectedthecompanion
AF
Lep
b
at
a
separation
of
339
mas
au),
within
the
inner
where
the
gas
has
the
been
compressed.
Spectralextraction
atpositionsyieldedhighMachnumbers
and
low
Riwaj
Pokhrel,S.
ThomasRobertA.
Gutermuth,
Elise
Furlan,J.
Fischer,SamuelFederman,agreement
withprevious
resultsandanimproved
quantificationof
uncertainties
incloud
properties.
amountdeliveredincreasedfurtherduringJupiter’s
migration
phase(totaling
about
10-40
times
Earth’soceanmass),
study
identifies
atargetregionfor
futurehighresolution
observations
that
could
probe
the
link
between
the
core
and
Bhaswati
Mookerjea,
V.
S.
Veena,
Rolf
Guesten,F.
Wyrowski,
Akhil
Lasrado
F3,Hub-filament
systems(HFSs)areStarlight-polarization-based
tomographyofthemagnetizedinterstellar
medium:PASIPHAE’s⇠
0.29
squaredegrees
area
of
the
IC
5070
region.
Using
Gaia
Early
Data
ReleaseweestimatedthemeanpropercanbecomeRossbyunstableandform
vortices.
Asinglelarge-scalevortexdevelops
if
the
dust
content
of
the
disc
have
a
crucialimpactwhen
similarbutsmoothinitialconditionsareemployedmorecrucialthan
thecode’schoiceassembleinconspicuously,
withlittlepublicity
andhooplaaccompanying
theirbirth.
Alternatively,
rarityofwarm
planets
andgap
widths,
this
lack
of
substructures
placesupper
limitstothemassesofplanets
in
the
disk
as
low
as
2isedgeofitsunresolved
debrisdisk.
Themeasured
K-bandcontrast
and
the
age
of
the
star
yield
a
model-dependent
ratiosthermaltonon-thermalpressure,suggestingadominanceofsupersonicandnon-thermal
motioninthecloud.
JohnJ.
Tobin,
AmeliaM.
Stutz,
Lee
Hartmann,
Mayra
Osorio,Dan
M.
Watson,ThomasStanke,P.
Manoj,
filament
evolution.
which
was
less
dependent
onsimulation
parameters.
In
addition,atthesestages,terrestrial
planets
were
not
fully
line-of-sight
inversion
methodpotentialsites
offormationofstarclusters
and
high
mass
stars.
To
understand
the
HFSs
and
to
provideobservationalmotionandparallaxoftheemission-linestars.
Wealso
estimatedthemeandistanceandreddeningtowardtheregion+2.9
wellcoupledtothegas,
however,
multiple
small-scalevortices
ensue
for
the
case
of
less
coupled
dust.
As
both
type
on
the
system’soutcome,multipleorwithcentrally-condensed.
excesses
may
imply
that
terrestrial
planets
typically
form
veryZakri
emerging
fully
formedfromthenebular survey
phase
M
-0.06
M
at
rPrabhani>
40
au.
The lackof themm
emission
at11
radii
r early,
> 60
au
also
suggests
that
the
gap
innear-infrared
scattered
light
Jup
mass
of
4
and
6
M
,
consistentmass
derivedfrom
anorbital
fit
of
4.3
M
.
The
SED
MayankNarang,Atnagulov,
Nolan
Habel,
Wafa
F
We
presenta
Spitzer/Herschelfocused
13
Jup
Jup
1.2
grown.
Therefore,
water
suppliedduringthese
earlystagescouldinteractwithmetalliciron
duringthecoreformation
V.
Pelgrims,
G.
V.
Panopoulou,
K.
Tassis,V.
Pavlidou,A.
Basyrov,
D.
Blinov,E.
Gjerløw,S.
Kiehlmann,N.
constraints
oncurrent
theoriesthat
attempttoexplainstar
formation
globally,wereportaofstudyof disk.
theregionassociated
using
the
emission-linestars,
are
⇠the
833
pc
and
⇠2
mag,
respectively.
By
examiningthelocationsofsolid
these
stars
of
vorticesaretrapped
at
the
dead
zone
outer
edge,
they
providesuﬃcient
time
for
dust
growth.
The
content
without
undergoinglate-stage
giant
impacts.
Ineithercase,
theobservable
signposts
terrestrial
planetformation
between30-80
auislikely
not
a
gap
in
disk
density,butashadowcastbyapuﬀed-up
inner
The
ALMA
view
of
MP
Mus
(PDS
66):
a
protoplanetary
disk
with
no
visiblegapsofplanetisconsistentwithanobjectatthe
L–T
spectral
type
transition,butunder-luminouswithrespect
totheAquilamolecular
clouds
(d
⇠
436
pc)
as
part
of
the
eHOPS
(extension
of
HOPS
Out
to
500
ParSecs)
censusMandarakas,
A.
Papadaki,R.
Skalidis,A.
Tsouros,R.
M.
Anche,H.
K.
Eriksen,T.
Ghosh,J.
A.
Kypriotakis,
S.
ofprotoplanets
and/orgrowing
Earth.
Since
hydrogeninwatermoleculescandissolve
into
theircores,
this
could
with
G326.27-0.49
using
infrareddata
ofpreviously
dustthecontinuum
andnewly
obtained
observationsonmolecular
tracersinthecolor-magnitude
diagrams
constructed
using
Gaia
and
PanSTARRS1
data,
we foundthata majority
ofPlanet
theusing
H↵
Takeout
andDelivery:Erasing
Dusty
SignatureofLate-stage
Terrestrial
collected
bythevortices
canexceedseveralhundredEarthmasses,while
thedust-to-gas
densityratio
withinoften
appearmore
challenging
todetectthan
assumed.
We
discuss
observational
tests
of
these
ideas.
down
to4
au
scalesfield-gravity
objects.
AFVariableLepbsourcejoinsStars
adetected
growing
numberofRamaprakash,
substellar
companions
imagedaroundstarsFin theyoung
ofnearbyprotostars.
For
every
in
the
Herschel/PACS
bands,theeHOPS-Aquila
catalog
contains
1- aMaharana,E.
Ntormousi,
T.
J.
Pearson,S.
B.
Potter,
A.
N.
A.
C.
S.
Readhead,
I.
K.
Wehus
A
CCD
Search
for
in
the
Open
ClusterNGC
6611
explainthedensity
deficitobservedinthecurrent
Earthcore.
Notably,
Jupiter
could
play
an
important
role
as
the
APEX
We
use
observations
to identify
velocity-coherent
structures(filaments
andF.
emitters
aretelescope.
young
low-mass(<the
1.5spectroscopic
MPérez,) stars.
We
also compared
ourcatalogofemission-line
stars
with
the
available
Formationexceeds
unity.
Thus,
suchvorticesfunctionasplanetarynurseries
withinthedisc,providing
ideal
sites
for
formation
Á.
Ribas,
E.
Macías,P.
Weber,S.
N.
Cuello,R.
Dong,
A.
Aguayo,C.
Cáceres,J.
Carpenter,
W.
R.
850
µmmoving
SEDs
assembledfrom
2MASS,
Spitzer,
Herschel,and
JCMT/SCUBA-2
data.
Using
amagnetic
newly
developed
Picgroup.
With
aon
mass
ofof
between3inand7 WISE,MK.
itoccupies
anoncarbonaceous
gap
inKalari
thisisochronalsequence
betweenWe
present
thefirstBayesianmethodfor
tomographic
decompositionoftheplane-of-sky
orientationoftheJup ,Kinemuchi,G.
Michalska,Z.
Kołaczkowski,
R.
Leiton,O.
Szewczyk,
V.,
M.
F
We
present
theresults
Empirical
constraints
turbulence
proto-planetary
discs”barrier”
inexplaining
thedichotomy
theisotopic
compositions
between(NC)andcarbonaceous
youngstellarcatalogs
and
found
that
offormation
them
Class
II/ flat
spectrumwiththespectraltype
rangingclumps)
and
study
their
properties
atFamost
resolution
ofare
0.4of
pc.
The
regioncontains
two mainvelocity
components:
first
Joan
R.
Najita,Scott
J.
KenyonTheplanets
likeRiviere-Marichalar,Earthis sources
expected
toM.
concludewith
aWeseriesofofplanetesimals
andeventuallyplanetarysystems.
Dent,
I.
de
Gregorio-Monsalvo,G.
Duchêne,C.
C.
Espaillat,
P.
VillenaveF
present12
setof
criteria,
weclassify
objects
by
their
SEDs
as
protostars,
pre-mssequencestars
withdisks,
andgalaxies.
A
total
field
with
the
use
of
stellarpolarimetry
anddistance.
This
standalone
tomographic
inversion
methodpresents
anthehotter,more
massivecompanions
likediscs,
PZ
Tel
Bbirthand
Pic locations
b,
and
the
cooler51 Erib, Jupiter’s
which
is andsuﬃciently
cool
for
Early
water
deliverytoterrestrial
planetregions
duringthestagesofformation
of
the
U
BV
I
variability
survey
in
the
young
open
cluster
NGC
6611
based
on
observations
obtainedduring34
nights
Giovanni
P.
RosottiF
Proto-planetary
theenvironmentofplanets,areanexampleofastructurecomC(CC)
meteorites.
This
study’s
results
show
that
Jupiter’s
growthnecessitatessomemixingofNCCCmaterials.
from
K
to
M.
Based
on
the
propermotion/parallax
valuesandonthecolor-magnitude
diagrams,
about
20
component
shows
four
filaments
between
-63
and
-55
km/s
formingaspiralstructure
converging
in
a
hub,
the
secondlate-stage
giantnurseries:
impacts thatgenerateofwarm
dustyatdebris,themostanticipatedvisiblesignpostof terrestrial
planetALMA
multiwavelength
observations
theprotoplanetarydiskaroundthenearby(d⇠100
pc)
young
solar
analogMP
Planetaryvortices
formedsmoothviscositytransitionof172
protostars
are
found
in
Aquila,tightly
concentratedinthemolecular
filaments
that
threadtheclouds.
Ofthese,
methanetoform
withinits
photosphere.
andmigration
in total,
the
Grand
Tack
model
spanning
one
year.
In
we
found
95
variablestars.
Mostof thesestars
areclassified
asaperiodic
and
irregular
monly
found
in astrophysics,
accretion
discs.
Identifying
theproper
mechanism
responsible
fororbitaccretionis witha long-standing
emission-line
stars
are
flaggedasnon-members.
The
relativemotionoftheemission-line
stars
respect
tooffilamentarycomponent
at
-72
km/s
harborsamassiveyoung
stellarobjectandpossiblyinteracts
with
the
hub.
The
formation
inprogress.
While
there
is
now
evidence
that
Earth-sized
terrestrial
planets
significant
fraction
Zs.
Regaly,K.
Kadam,
D.
Tarczay-Nehez
F
ExcitationofRossbywave
instability
anddevelopmentofalarge-scale
Mus
(PDS
66).
These
observations
at
0.89
mm,
1.3
mm,
and
2.2
mm
have
angularresolutionsof⇠
1",
0.05",
and0.25",
71 (42%)sequence
are Class0discovery
protostars,
54
(31%)
are
Class
IJHK
protostars,
43 the(25%)
areflat-spectrum
protostars,
and4 could(2%)
Directimagingofasuper-Jovian
aroundyoung
Sun-like
star
AF
LeporisMasahiro
Ogihara,Hidenori
Genda,
Yasuhito
SekineF
The
formationandsubsequentmigrationofgas
giantspre-main(PMS)
stars.
The
analysis
of
the
2MASS
photometryandfour-colour
IRAC
photometry
problem,datingbackseveraldecades.
The
commonpictureisthat
accretionisaconsequenceofturbulence,
with
S
the
ionizing
sourcesuggestthepossibility
the‘rocketeﬀect’
scenario
inleadingtheremnant
cloud
(BRC
31).
clumpsharbouring
the
three
main
YSOs
inof
the
regionaremassive(187-535
Msun),
have
luminosities
consistentwithsolar-typestars,
theanticipateddusty
debrissignatureof
theirformationisrarelydetected.
Here
we
discuss
severalvortex
at
the
outer
dead
zone
edge
of
protoplanetary
discs
is
one
of
the
theoriesthat
explains
horseshoe-like
respectively,
and
probe
the
dust
and
gas
in
the
systemwith
unprecedented
detailandsensitivity.
The
disk
appears
14young
ALMA
Band
6proposed
high-resolution
observationsoftheBright
transitionaldiskaroundSY
Cha
are ClassIIsources.
Ten
ofL.
the
Class
0 in
protostars
are
PACS
Red
Sourcessimilar
toAnnethosebinary.
discoveredinRobert
J.
De
Rosa,
Eric
Nielsen,
Zahed
Wahhaj,Jean-Baptise
Ruﬃo,
Paul
G.
Kalas,
E.
Peck,
Lea
6the
3 whichsignificantly
aﬀect
the
material
mixing
Solar
System.
In
thisstudy,
weuse
N-bodysimulations
toinvestigate
revealed
165
Class
II
young
stellarsources,20
ofareirregular
variables
and
one
is
an
eclipsingTheseseveralinstabilities
for
its
origin.
While
traditionally
field
used
to
be
a
purelytheoreticalendeavour,
B-typestars,
havecentraldensities
ofdiscs.
10cm
andobservations,
drive
large
outflows.
Majority
ofemission
thevelocity-coherent
clumps
ways
in
which
our
current
ideas
about
terrestrial
planetformation
imply
transportmechanisms
capableoferasingtheAnalysis
of
the
first
infrared
spectrumofquasi-bound
H2
line
in
Herbig-Harobrightness
distributionintransition
Formationofsuchvorticesrequiresarelatively
sharp
viscositytransition.
smooth
down
to
the
4
au
resolution
of
the
1.3
mm
in
contrast
with
most
disks
observed
atcomparable
Ryuta
Orihara,Munetake
Momose,Takayuki
Muto,
Jun
Hashimoto,
Hauyu
BaobabLiu,
Takashi
TsukOrion.
We
comparethe
SEDsbytoa(abridged)
gridofradiative
transfermodelstoconstraintheluminosities,
envelope
densities,
A.
Hirsch,WilliamRobersonF
Expandingthesampleofdirectly
imagedcompanions
tonearby,
young
how
much
water
is
transported
into
the
regionoftheterrestrial
planetformation
duringthegrowthandmigration
classifications,complemented
JHK
UKIDSS
photometry
and
riH↵
VPHAS
photometry,
were
used
to
identify
thelandscapeisnowchanging
thanksmainlytonewobservational
facilities
such
as
the
ALMA
radio
interferometer.
+0.11 of protostars
inthe region
show
virialparameters
between2-7,
which
considering
thedetection
impliescollapseto <be 2
anticipateddebrissignature.
A
tenuous
gas
disk
may
be
regenerated
via"takeout"(i.e.,
theliberationofplanetary7
Detailed
modelling,
however,
indicatesthat
viscositytransitions
at
the
outer
edge
of
the
dead
zone
is
relatively
smooth.
spatialscales.
The
dust
disk
has
a
radius
of
60±5
au,
a
dust
mass
of
0.14
M
,
and
a
mm
spectral
index
Extension
ofimprovements
HOPS
Out
to
500
(eHOPS).
I.
and
of
Jup
agoshi,
Kudo,
Sanemichi
Takahashi,
Yi
Yang,
Yasuhiro
Hasegawa,
Ruobing
Dong,
MihokoKonishi,andenvelope
massesof theprotostars.
A andcomparison
oftheeHOPS-Aquila
to
the
HOPS
protostars
inModeling
Orion
that
0.06
stars
that
are
amenabletodetailed
astrometricandweak-lined
spectroscopic
studiesisIdentification
criticalforthecontinued
development
and4 finds
phasesofTomoyuki
in
the
Grand
model.
We
found
that
Jupiter’s
growthwasaccompaniedbysignificant
ThankstoJupiter
large
inTackspatialspectralresolution
andsensitivity
have
the
study
of mass
disc
24
candidates
forclassical
T
Tauri
stars
andParSecs
30
T
Tauri
stars.
In(which
addition
toenabled
thePMS
variables,
we37

Early water delivery to terrestrial planet regions during the stages of Jupiter’s formationand migration in the Grand Tack model

Masahiro Ogihara, Hidenori Genda, Yasuhito Sekine F The formation and subsequent migration of gas giants could

significantly aﬀect the material mixing in the Solar System. In this study, we use N-body simulations to investigate
how much water is transported into the region of the terrestrial planet formation during the growth and migration
phases of Jupiter in the Grand Tack model. We found that Jupiter’s growth was accompanied by significant masstransport, and that a substantial amount of water (about 10 times Earth’s ocean mass for the initial planetesimal
distribution based on the minimum-mass solar nebula) was transported into the terrestrial planet region. The total
amount delivered increased further during Jupiter’s migration phase (totaling about 10-40 times Earth’s ocean mass),
which was less dependent on simulation parameters. In addition, at these stages, terrestrial planets were not fullygrown. Therefore, water supplied during these early stages could interact with metallic iron during the core formationof protoplanets and/or growing Earth. Since hydrogen in water molecules can dissolve into their cores, this could
explain the density deficit observed in the current Earth core. Notably, Jupiter could play an important role as a”barrier” in explaining the dichotomy of the isotopic compositions between noncarbonaceous (NC) and carbonaceous(CC) meteorites. This study’s results show that Jupiter’s growth necessitates some mixing of NC and CC materials.

ALMA Band 6 high-resolution observations of the transitional disk around SY Cha

Ryuta Orihara, Munetake Momose, Takayuki Muto, Jun Hashimoto, Hauyu Baobab Liu, Takashi Tsukagoshi, Tomoyuki Kudo, Sanemichi Takahashi, Yi Yang, Yasuhiro Hasegawa, Ruobing Dong, Mihoko Konishi,
Eiji Akiyama F In this study, we reported the results of high-resolution (0.14 arcsec) Atacama Large Millime-

ter/submillimeter Array (ALMA) observations of the 225 GHz dust continuum and CO molecular emission lines from13⌃g,vis = 1320

ort.
10 9 M yr 1
10 4
as calculated
accordingto the enve⇣ r ⌘ 3/8
Water
delivery
2
⇥
g
cm
, (1)
tz contraction using Eqs. (41)–(42)1 au !
地球の海の起源、地球コアの密度欠損の原因（コアへの水の供給）
2021) (see also Hori & Ikoma 2010),⇣ ↵ ⌘ 1Ṁg
海の起源は惑星形成後の質量降着だと思われてきたが、コアへ水を供給するには惑星形成中に水が必要。
the planet
using Eqs. (15)–(16) of⌃g,irr = 2500
9 M yr 1
4101020) (see also Tanigawa & Tanaka⇣ r ⌘ 15/14
Tackモデル(木星が3.5auで形成した後1.5
auまで落下したのち今の軌道
5.2 au に移動する)
3
ccretionGrandusing Eq.
(19) of Ogihara &
2
⇥
g
cm
, (2)
stops gasaccretionwhenitreachesで木星の成長期、移動期に水がどの程度地球型惑星に供給されるかを調べる。
1 au
For
the gas disk model, although disk models thatur fiducial
Jupitercore gained attention
account setup,for diskthewinds
have recently
9
where
we
assumeṀ=10exp[(tg
ss in N体計算
about
1
Myr.
When
Jupiter(Suzuki et al. 2016; Ogihara et al. 2018b), we used a sim1
1Myr)/(0.5
Myr)]
M
yr
for the fiducial case andple two-component
power-law (e.g.,
disk model (e.g., Bitsche limited
by
the
disk
accretion
３成分
4
↵
=
10
. Jupiter opens a density gap in its vicinity,
et
al.
2015;
Liu
et
al.
2019).
In
thismodel,
thediskis8) and becomes near linear growth.
dividedinto the inner region, wherea=3.5
the temperatureis also considered in this study by using a かけてMjまで成長
which
was
model
木星：初期質量10Me,
au,
先行研究の形成モデルを使って1Myrt of Jupiter’s growth rate, we also
determined by viscous heating (vis), and theinouterre- the depth and width of the gap is determined
whichwheregion,
Jupitergrows
quickly->a=
1.5 inauabout-> 5.2
au と移動(t=1.5Myr)
where
stellarirradiation(irr)
determines
the diskby
giant
planet
mass
and
disk
properties(e.g.,
viscosity)
Youdin2014)
bychangingthedisktemperature. Each region has a dominant heating mechplanetary
embryos：0.05Me
40個(Kanagawaet al. 2017; Shibata & Ikoma 2019).
anism and switches from the viscous regime to the irragas drag damps
the eccentricity
andregimeinatthe
a specificradius(see Eq. (14)As
ofaerodynamicalLiuplanetesimal:
1.3-6auに分布、0.005Me
1106個or
0.0025Me
2212個、MMSNの面密度分布
ation,diation
migration
Grand
Tack
et al. (2019) for location). The gas surface inclination
density in of planetesimals, we calculated the drag force
d basedon Walsh et al. (2011)
each region is expressed byby the following
formula (Adachi et al.
1976).
activeガスによる微惑星のe,iのdumping015).ガス(passive
Jupiter movedor
inwardon )a!1/2⇣ ↵ ⌘ 3/4
Ṁ
2
and moved
outwardafter
reachinggC⇡R⇢g vrelD⌃g,vis = 1320
9 M yr 1
4
Faero =
vrel ,(3)
10
10
he outward migration, as stated in
2M
⇣
⌘
3/8
r
and Carter et al. (2015), the migra2
⇥
g cm
, (1)
where
⇢g is the gas density, vrel is the relative velocity
1
aud down by considering exponential !
で力を計算
⇣
⌘
betweentheplanetesimal and gas, and R is the radius
1Ṁ↵g
ed at its current
orbit⌃g,irr =2500 (a =9 5.2 au)1
4 planetesimals and is varied between 5–500 km to de10 M yr
10 of
⇣ r ⌘ 15/14 termine the e↵ect of gas damping strength. The drag⇥g coefficient
cm 2 , (2) C is calculated according to the Mach numD
1 au

木星成長期
時間と共に水が内側に供給される

3.2. Migration phase

We consider how mass transport omoves according to the Grand Tack mcorresponds to the simulation by Wal
Notably, while Walsh et al. (2011)
tially uniform distribution of planetes
conditions, the planetesimal distributio
growth significantly di↵ered in our sused the final distribution of planetein Jupiter’s growth phase as the initia
Jupiter’s migration phase.
Figure 4(a) shows a typical result ophase for the fiducial case; a continuati
Figure 2.a<2
The auの領域に供給される水の微惑星サイズ(横軸)依存性
amount of water delivered into the region
fiducial case in the growth phase. Mo
of a < 2 au during the growth phase of Jupiter in each simtransported from Jupiter’s outer orbit tulation. The
initial water mass fraction of the planetesimal
小さいほどガスのdumping
で散乱が起こりにくく、is the value described in Section 2. Three runs were per(a < 3.5 au) during the Jupiter growth p
formed in内側に供給されない
each setting. Squares represent results for higher
into the more inner orbit during the Jup
resolution simulations.
gration (t = 1085 kyr). This results in
成長が10倍速いモデル（オレンジ）では供給量が増える
transport to the inner region. At thisFurthermore,
we show the simulation results with difscattering of planetesimals from Jupi
R＝5kmで~1Meo(地球海質量)
ferent parameters. Figure 3 (panels a and b) indicates
into the inner orbit was limited. The
R=500kmで~20-30Meo
the simulation
results for di↵erent sizes of 供給
planetesithe further transport of planetesimals
mals. Regarding the dependence on the planetesimalin Jupiter’s inner orbit. Jupiter then chsize, the transport efficiency of planetesimals was foundtion direction to outward and reaches

木星移動期s Figure 1 but for di↵erent parameters. (a) The planetesimal is 5 km in size and the eccentricity damping
a<3.5
auに供給された水は内側への移動で
planetesimal is 500 km in size and the eccentricity damping is weak. (c) Jupiter is in rapid growth withon a timescale
about
0.1 Myr. The planetesimal is 50 km in size.
<1.5 ofauに掃き集められる

Figure 5. Same as Figure 2, but the total amount of water
最終的に a<2 auに>10Meoの水が供給
delivered into the region of a < 2 au during the growth andmigration phase of Jupiter.

ots of the system during the migration phase. Jupiter moves inward and outward according to the Grandur fiducial setting with planetesimal of 50 km in size. (b) The planetesimal is 5 km in size.

where the plus/minus sig
in fitting. This equation
well for di↵erent sizes an
cept for R = 5 km. On
noted that this fitting fo
in Appendix B, where th
configuration of giant pla
By combining Eq. (4)materials, the transport f
can be calculated. By as
tribution of water,⌃d,w = 10⌘w

where ⌘w is the initial wa
etesimal described in Sec
livery can be calculated
yields 31 MEO and is con
ter delivery shown in Fi
in Figure 6 are obtainedwater distribution. The
be used to estimate the
distribution. Although w
mary focus of this papermaterials delivered into

the fiducial case, the final transport between the cases
地球の形成期に十分な水を供給できるので、コア密度欠損を説明できる。

y between the cases R = 50 km andot di↵er significantly.
e results when Jupiter was growing
growth phase was considered. The
same as when Jupiter grows moreof R = 50 km and 500 km did not di↵er. In addition,
the final water transport did not depend on Jupiter’s
growth timescale. Therefore, the amount of water delivered did not depend much on the simulation parametersagreement with previous results and an improved quantification of uncertainties in cloud properties.

42 The ALMA view of MP Mus (PDS 66): a protoplanetary disk with no visible gaps
down to 4 au scales

Á. Ribas, E. Macías, P. Weber, S. Pérez, N. Cuello, R. Dong, A. Aguayo, C. Cáceres, J. Carpenter, W. R. F.
Dent, I. de Gregorio-Monsalvo, G. Duchêne, C. C. Espaillat, P. Riviere-Marichalar, M. Villenave F We present

ALMA multiwavelength observations of the protoplanetary disk around the nearby (d⇠100 pc) young solar analog MP
Mus (PDS 66). These observations at 0.89 mm, 1.3 mm, and 2.2 mm have angular resolutions of ⇠ 1", 0.05", and 0.25",
respectively, and probe the dust and gas in the system with unprecedented detail and sensitivity. The disk appears
smooth down to the 4 au resolution of the 1.3 mm observations, in contrast with most disks observed at comparable
spatial scales. The dust disk has a radius of 60±5 au, a dust mass of 0.14+0.11
0.06 MJup , and a mm spectral index < 2in the inner 30 au, suggesting optically thick emission from grains with high albedo in this region. Several molecular
gas lines are also detected extending up to 130±15 au, similar to small grains traced by scattered light observations.
Comparing the fluxes of diﬀerent CO isotopologues with previous models yields a gas mass of 0.1 1MJup , implying
a gas to dust ratio of 1-10. We also measure a dynamical stellar mass of Mdyn =1.30±0.08 M and derive an age of
7-10 Myr for the system. The survival of large grains in an evolved disk without gaps/rings is surprising, and it ispossible that existing substructures remain undetected due to optically thick emission at 1.3 mm. Alternatively, small
structures may still remain unresolved with the current observations. Based on simple scaling relations for gap-opening
planets and gap widths, this lack of substructures places upper limits to the masses of planets in the disk as low as 2
M -0.06 MJup at r > 40 au. The lack of mm emission at radii r > 60 au also suggests that the gap in scattered lightbetween 30-80 au is likely not a gap in the disk density, but a shadow cast by a puﬀed-up inner disk.

Empirical constraints on turbulence in proto-planetary discs

Giovanni P. Rosotti F Proto-planetary discs, the birth environment of planets, are an example of a structure com-monly found in astrophysics, accretion discs. Identifying the mechanism responsible for accretion is a long-standing
problem, dating back several decades. The common picture is that accretion is a consequence of turbulence, withseveral instabilities proposed for its origin. While traditionally this field used to be a purely theoretical endeavour,the landscape is now changing thanks mainly to new observational facilities such as the ALMA radio interferometer.
Thanks to large improvements in spatial and spectral resolution and sensitivity (which have enabled the study of discsubstructure, kinematics and surveys of large disc populations), multiple techniques have been devised to observationally measure the amount of turbulence in discs. This review summarises these techniques, ranging from attempts at

where uncertainty
Mdust is disk
dust
mass,
F
is
the
flux
at
the
observed⌫(10 % for Band 7 and 5 % for Bands 6 and 4).
frequency ⌫, Tabled is thedistance tothe source,
⌫for
is MP
the dust
3. Summaryof results
derivedMus. opacity
解析結果まとめatthefrequency
⌫,
and
B
(T
⌫ dust ) is the blackbody emission at the
MP Mus (PDS66)
olved in both the 1.3 mm and 2.2 mm observations. We used corresponding frequency andParameter
dust temperature
Value T dust . Since wepertureto estimate continuum fluxes from these im- have observations at three di↵erent
TWphotometry
Hya に次いで近傍にある(97.9pc)、
can computeM⇤,dyn frequencies,
1.30 ±we
0.08M
ges, obtaining 370±40 mJy at 0.89 mm, 148±7 mJy at 1.3 mm, three dust mass values. We adopted
standard
for the opac1.2values± 0.1Lgas rich 円盤(r~130au)を持つ classical T Tauri star (1.3Msun, 7-10Myr) L⇤
nd 49±2 mJy at 2.2 mm (see Table 4). These uncertainties are ity and dust temperatures of Age
† =2.3 cm2 /g and T
230 GHz
7 - 10 Myr dust = 20 K
散乱光が60-80auで暗くなる
argelydominated by absolute calibration and not the noise in the (e.g., Andrews & Williams V2005),
and a 3.98
distance
d=98 pc± 0.04ofkm/s
LSR
mages.
The emission at 1.3 mm and 2.2 mm extends up to 60 au (Gaia Collaboration et al. 2022).
+0.11 at 0.89 mm
Fortheobservations「若い太陽系」として有効な研究対象
M
0.14
dust
0.06 MJup00
0.6 ), as determined from the 3-5 contours. To ease the com- and 2.2 mm, we computed thevalue using a⌫ Jup
Mgascorresponding
0.1-1M
arisonwith other studies,
we also list6theradii enclosing
68 % power-law dependence of the††
opacity
with60frequency,
i.e. ⌫ =ALMAでBand
7 (0.89mm),(1.3mm),4 (2.2mm)で観測
Rdust± 5 aund 90 % of the total flux in Table 5. Based on the most com- 230 GHz ⇥ (⌫/230 GHz) , where††isbetween
0.0-0.6
for
most
12
R
130
±
15
au
gas ( CO)(~1”,0.05”~4au,
0.25”)
act antenna configuration in each band (Table 1), the maximum protoplanetary disks (e.g., Tazzari
et al. 2021,
also
in agreement
i
32
±
1
dust
SPHEREのデータ解析も行う
ecoverable
scales are ⇠10.800 , 2.900 , and 8.300 at 2.2 mm, 1.3 mm with the range of 0.1-0.4 derived
for MP 10
Mus
in Sec. 4.2). We
PA
±
1
dust
nd 0.89 mm, respectively2 , which are significantly larger than bootstrapped the dust massesDoLP
and their uncertainties
by adopting
0.46 ± 0.08%
he observed disk size. Therefore, the observations are likely uncertainties of 5 K for T dust and
20 % for 98
AoLP
8 , and a uniform
230 ±
GHz
ダスト連続波ecovering
all the emission fromdisk. no.
We
A&Atheproofs: manuscript
ms also produced
distribution of values between 0 and 0.6. The derived disk dust
+0.1(†) Based on the
+0.07
+0.07
mages with a lower robust value of -0.5 to try to reveal masses are 0.16
Notes.
derivedluminosity
and theMIST
isochr
M
,
0.13
M
,
and
0.13
M
at
Jup
Jup
Jup
0.04 and model
0.04The observed contin
0.05 1.3 mm observations
Fig. 2. ALMA
00(††) of MP Mus.
2016;
Choi
et(theal. 2016).
The uncertainties
corresponmall substructures, reaching angular resolutions of 0.89⇥0.66 , 0.89 mm, the
リング、ギャップ、非軸対象構造は
1.3(Dotter
mm,
and
2.2
mm
reportedvaluescorrespond
frank radial profile (middle) are shown. The residuals (right) are displayed i
00
00
00
00
beam
size
of16
the%,
observations.
.06 ⇥0.04 , and 0.25 ⇥0.19 at 0.89 mm, 1.3 mm, and 2.2 mm to the medianandthe
観測されず and 84 % percentiles). These valcorresponding to ⇠75, 4, and 20 au at 98 pc). Interestingly, the ues are allTable
compatible
withencompassing
each other,
adopt
final
5. Disk radius
68 and% andwe90 %of theatotal
flux.dust major+0.11
mass value of
M
=
0.14
M
as
the
average
of
the
three
dust
Jup
0.06
solved in both the 1.3 mm and 2.2 mm observations. ↵=1.3
We u
See ALMA Technical Handbook
measurements.
observ
aperture photometrytoestimate
continuum
fluxesfromtheseComponent
R68 % (au) R90 % (au)inclinages,Continuum
obtaining(1.3370±40mJy30±5at 0.89 mm,
148±7 mJy at 1.3 m
mm)
45±5
ment
rticle number, page 4 of 20
and 49±2mJy (2.2
at 2.2mm (seeTable 4).
These uncertainties
Continuum
mm)
30±20
45±20
directlargelyGas
dominatedby absolutecalibrationand not the noisein(12 CO (2-1))
80±15
110±15decreaimages. The emission at 1.3 mm and 2.2 mm extends upslope
to 6(0.600 ), as determined from the 3-5 contours. To ease bumpthe c

eam size of the observations.

eralstar-forming
regions (e.g. Ricci
al. 2010b,a;k
calculates
super-resolution
radialetprofilesof Ribas et al. 2017; Tazzari et al. 2021). Using the derived con017;
Tazzari etazimuthalal. 2021).symmetry,
Using the aderived
con- tinuum fluxes, we computed three spectral indices in di↵ersks assuming
condition
Spectral
index
,hewe
computed
three
spectralindices indi↵er- ent wavelength ranges: ↵0.89 1.3 mm = 2.4 ± 0.3, ↵1.3 2.2 mm =case of MP Mus. We
tried di↵erent
combih↵ranges:↵0.89 1.3
0.3,
↵1.3
= mm
平均wsmooth’sandhyperparameters
and
found
2.12
± 0.11,↵0.89 2.2 mm = 2.25 ± 0.13 (including the abmm = 2.4 ± Fig.
2.2 mm3.
Radialprofilesofno
the 1.3
continuum
and COand(2-1) emissionof MP Mus. The
continuum
profile derived from the synthesizednd ↵β~0.1-0.4
=
2.25
±
0.13
(including
theab0.89 2.2 mm → mm size ダスト
ALMA image is shown as a red line, and the orange line corresponds to12

the resulting profile from frank (Jennings et al. 2020). The profile forthe 12 CO (2-1) line is also shown as a blue line. The 1- uncertainties
Article number,pageof (2-1)
20 are also plotted as red and blue shaded
動径分布
内側ほど小さい：光学的に厚い、大きいダストのドリフト
for the continuumand512 CO
areas. In all cases, we adopted a disk inclination and PA of 32 and 10 .
For comparison, the FWHM of the continuum and 12 CO (2-1) beams
β<0 :光学的に厚く アルベド大
ダスト質量は過小評価
are also shown
as solid horizontal red and blue lines, respectively.

Lines

Article number, page 5 of 20

solute calibration uncertainties of ALMA). These values werefrom the integrated fluxes and they reflect the average
半径〜130 auの lled disk, computed
DCO+で〜20
au
でgapが見える
spectral index in the disk only, but the spectral index is expected
to vary spatially as a result of factors such as radial changes in the
ケプラー回転から中心星質量~1.3Msun
optical depth and grains sizes. To investigate such spatial variations, we combined the resolved 1.3 mm and 2.2 mm observa12COから aring の兆候や裏面が見えない→幾何的に薄い
tions to produce a resolved map of the spectral index. During thisprocess,the most extendedMsun
configuration of the available Band 6
COから見積もったgas mass
10^-4~10^-3
data was excluded to avoid problems with very di↵erent coverage of the uv-planedi↵erent bands. The 1.3 and 2.2 mm data Fig. 4. Derived millimeter spectral index for MP Mus between 1.3 andgas/dust ~1-10 gasのdissipation?
COatabundance?
were jointly imaged with the tclean algorithm, the mtmfs de- 2.2 mm. Top: Spectral index map. Only pixels with S/N>5 are considered. The solid and dashed contours correspond to ↵1.3 2.2 mm of 2 andconvolver, and nterms=2, and we then used the resulting alpha 2.5, respectively. The image beam is shown on the bottom left corner.
image as the spectral index map. After various tests we adopted Bottom: Corresponding de-projected ↵1.3 2.2 mm radial profile and una robust parameter of 0.0 in this case, which yielded a beam of certainties (solid red line and area). The beam FWHM is shown as a0.200 ⇥0.1700 . The derived spectral index map and its radial pro- horizontal red line. The dashed line marks the ↵ = 2 transition.
ダストにgap構造が見えないのに、large
dustが残っている。光学的厚みかresolutionの問題で見えないbump?
file are shown in Fig. 4. As expected, the value of ↵1.3 2.2 mm is
not constantthroughout
the disk and increases as a function of
惑星質量に上限(~0.5-4Mj forr>10
au)
radius, ranging from ⇠1.7 in the inner regions to ⇠3 in the outer moments are listed in Table 6. Note that each project used different antenna and correlator configurations, so the spectral and
parts
of
the
disk.
These
resultsarediscussedinfurther
detailin
散乱光のgapは内側でpu ed up したinner rimが作る影
spatial resolutions are di↵erent for each line (also listed in TaSec. 4.2.
ble 6). In the case of the Band 6 observations, we only used theobservations from project 2017.1.01419.S to generate the cubes
3.2. Gas lines(data from 2017.1.01167.S have a significantly higher angular
ff

fi

fl

議論

nurseries: vortices formed at smooth viscosity transition
44 Planetary
Zs. Regaly, K. Kadam, D. Tarczay-Nehez F Excitation of Rossby wave instability and development of a large-scalevortex at the outer dead zone edge of protoplanetary discs is one of the leading theories that explains horseshoe-likebrightness distribution in transition discs. Formation of such vortices requires a relatively sharp viscosity transition.
Detailed modelling, however, indicates that viscosity transitions at the outer edge of the dead zone is relatively smooth.
In this study, we present 2D global, non-isothermal, gas-dust coupled hydrodynamic simulations to investigate thepossibility of vortex excitation at smooth viscosity transitions. Our models are based on a recently postulated scenario,
wherein the recombination of charged particles on the surface of dust grains results in reduced ionisation fraction andin turn the turbulence due to magnetorotational instability. Thus, the alpha-parameter for the disc viscosity depends
on the local dust-to-gas mass ratio. We found that the smooth viscosity transitions at the outer edge of the dead zone
can become Rossby unstable and form vortices. A single large-scale vortex develops if the dust content of the disc iswell coupled to the gas, however, multiple small-scale vortices ensue for the case of less coupled dust. As both typeof vortices are trapped at the dead zone outer edge, they provide suﬃcient time for dust growth. The solid content
collected by the vortices can exceed several hundred Earth masses, while the dust-to-gas density ratio within often
exceeds unity. Thus, such vortices function as planetary nurseries within the disc, providing ideal sites for formationof planetesimals and eventually planetary systems.

Direct imaging discovery of a super-Jovian around the young Sun-like star AF Leporis

Robert J. De Rosa, Eric L. Nielsen, Zahed Wahhaj, Jean-Baptise Ruﬃo, Paul G. Kalas, Anne E. Peck, Lea
A. Hirsch, William Roberson F (abridged) Expanding the sample of directly imaged companions to nearby, youngstars that are amenable to detailed astrometric and spectroscopic studies is critical for the continued development andvalidation of theories of their evolution and atmospheric processes. The recent release of the Gaia astrometric catalogue
allows us to eﬃciently search for these elusive companions by targeting those stars that exhibit the astrometric reflex
motion induced by an orbiting companion. The nearby (27 pc), young (24 Myr) star AF Leporis (AF Lep) was
targeted because of its astrometric acceleration, consistent with a wide-orbit planetary companion detectable withhigh-contrast imaging. We used the SPHERE instrument on the VLT to search for faint substellar companions in theimmediate vicinity of AF Lep. We used observations of a nearby star interleaved with those of AF Lep to eﬃciently
subtract the residual point spread function. This provided sensitivity to faint planetary-mass companions within 1
arcsec (⇠30 au) of the star. We detected the companion AF Lep b at a separation of 339 mas (9 au), within the inneredge of its unresolved debris disk. The measured K-band contrast and the age of the star yield a model-dependent

dze

in the U-prescription (Lyra et al. 2009b; Regály et al. 2012), which
es of Rossby wave instability(RWI)
is sharper than it is expected to form at the outer dead zone edge
ed in 観測されている渦構造の起源として有力視(Dzyurkevich et al. 2013). In our standard models, we assume that
ortex
'
=
0.2,
which
corresponds
to
'
=
(2
+
2/3)
.
To
dze
dze
dze
17b; dead zone outer boundary でのαの変化で引き起こせるか？
extend our investigation, we run models with 'dze = 4 dze forαの変化のスケールが<2Hで急に変われば不安定化できるが、certain cases. Note that the total width of the viscosity transition
to to dead zone outer boundary ではより緩やかにしか変化しない。
given by Equation (14) is about 2 'dze , which corresponds to 0.4
oling
and
0.6
in
the
standard
andextendedscenarios,
respectively.
elled 本研究
Additionally, the global viscosity is modified such that a change
Planetary nurseries 3
Les αのガス、ダスト面密度依存を考慮したモデルでRWIを起こせるか？
in the dust or gas concentration alters the viscosity. According to
2Dのガス・ダスト２成分のシミュレーションで調べる。
12 Zs. Regály,
K. Kadam & D. Tarczay-Nehéz
Dullemonda parametricU-prescription
can beravitational
potentialof the star &in aPenzlin
Table(2018)
1. Investigatedparametric–U models.
e A. Since the equations
are solved in
given
as
αのモデル
tem
model
qd
qg
(10)centred on the star, Equation (7)model C5model C3

(11)

´ d

´ g

case Acase Bcase Ccase Dcase E

0
-1
-1
-2
-1

-1
0
1
1
-1

10 -2

10 -4

Σ

ct potential, ind (A, q) arising due to qd
qg
entre of the system caused by any
disc
⌃g ™
⌃
©
©
™
d
ortancein, e.g., Mittal
ChiangU=&
Ubg,≠ 2015;
≠
Æ̈
Æ̈
s
(0)
(0)
ly & Vorobyov 2017a). The ⌃indirect⌃model C3*

10

Σg
Σd
α

-5

(15)

Σg
Σd
α

Σg
Σd
α

smooth viscosity transition

parametric α

dze

10 -3

steep viscosity transition

steep viscosity transition

10 -6

(0)
(0)
where ⌃g andaretheinitial
gas
and
dust
densities.
Valuesr,(8) ⌃dα̲bg ：ΔR=(2+2/3)Hordead4Hでなだらかに変化
at
disc
zone
the backgroundviscosity,
viscosity, UbgU
is defined
as of2the, azimuthally averaged surface mass density of the gas (⌃ ) and dust (⌃ ) and the value of U parameter in three models C3, C5,
mical
Figure7. RadialprofilesofU
arelimitedbetweenthebackground=10
bg
dinate system can be given as
andC3*. The profiles are calculated from snapshots taken by 800, 1400, and 1400 orbits at ' = 1, respectively. Dot-dashed curves show the initial profiles. U✓◆ profile
has a steep region in models where the local dust-to-gas density ratio grows beyond the initial value of 0.01. RWI is eventually RWI excited in models
4y we ’
1
'
'
dze
結論：φ<
and
MRI inactiveof
C3, and C3*.
m
9 0 ,: 0 the 0の時、Σgの揺らぎが>0の時（ダストの濃集を通して）(1 U) 1= 10
Ubgviscosity,=1
Udeadtanh . The assumption(14)
modcos(q )⌧
cos(q 0 )
0

10 -4

0.5

1.0

R

2.5

5.0 0.5

1.0

2
'dze
:
ating: 0 0 minimum
02
A9
effective viscosity is consistent withthe vertical
shear
αが減少、さらにΣgが大きくなるpositive
feadback
9 ,:for viscosity, RWI excitation occurs even when a smooth transition
The
outer
edge
of
the
disc
dead
zone
is
set
to
'
=
1.5.
Excitationdze
isassumed.
We
explain the formation of vortices in our simulampor- ’ minstability
9 0 ,: 0generatedviscosity(Stoll&
Kley2014).
With
regards
to
tion
with
the
help
of
Fig.
7. The figure shows azimuthally averaged
of RWI requires a sharp viscosity transition ( 'dze  2 dze , where→急なαの変化が実現してRWIが成長
n(q : )⌧ 02 sin(q : 0 ),(9)
profiles of gas and dust surface densities as well as the effective
etsch 9 0 ,: 0 Athevalues for qd and dze
qg =weinvestigatedfourcases,Table
1 C3, C5, and C3*. An enhancement in gas'dze⌘ is the disc scaleheightat thesee
viscosity
reduction),
9
U-parameterinmodelsformswhich
in all models due to the mismatch of the acin the U-prescription (Lyra et al. 2009b; Regálysurface
et al.density2012),
s not
cretion rate near the viscosity transition. Since such a profile createsR

2.5

5.0 0.5

g

d

1.0

R

2.5

5.0

ents of dust surface density, these conditions are satisfied only at a
relatively large Stokes number. On the other hand, small-sized dust
is well coupled to the gas motion and drifts slowly within the disc.
Such dust particles cannot maintain gradients required to sustain
small-scale vortices and thus, only a single large-scale vortex may
form. This trend for Stokes number is indeed observed in our simulations in Table 2. Thus, only a bimodal outcome is possible for

nre
te
s

4)

=
=
mer
es
nhe
ch

a
th
of
ns
he
is
d.
ns.
in
es
ry
ge

o,
le
th
eon
or
le

jmin values in parenthesis represents the minimum value reached by the endof simulation. The last column lists the maximum value of total midplanedensity in terms of Roche density at that radius. Models with asterisk use
extra wide 'dze = 4 dze viscosity transition.

シミュレーション結果
Large
vort.

CRWI
( #orb )jmin(dust/gas)αのモデルとStを変えた計算

Mod.

St

Small
vort.

A1
A2
A3
A4
A5
A5*

10 1
10 2
10 3
10 4
10 5
10 5

5
5
5
5
5
5

5
4
4
4
4
4

350
400
400
400
1500

16/10
16/14
15/15
15/15
34/34

B1
B2
B2*
B3
B4
B5
B5*

10 1
10 2
10 2
10 3
10 4
10 5
10 5

7.5 ⇥ 10 2
9.6 ⇥ 10 3
8.6 ⇥ 10 3
8.6 ⇥ 10 3
7.0 ⇥ 10 3

4
4
4
5
5
5
5

5
5
5
4
4
4
4

50
100
100
250
350
350
950

3/7
6/6
5/5
10/10
14/14
15/15
32/32

C1
C2
C3
C3*
C4
C5

10 1
10 2
10 3
10 3
10 4
10 5

4.9
3.6 ⇥ 10 2
3.4 ⇥ 10 2
1.2 ⇥ 10 2
9.0 ⇥ 10 3
8.7 ⇥ 10 3
7.2 ⇥ 10 3

4
4
5
5
5
5

5
5
4
4
5
5

50
150
650
1350
-

3/7
5/6
9/9
8/8
-

3.3
3.2 ⇥ 10 2
7.0 ⇥ 10 3
5.1 ⇥ 10 3
-

D1
D2
D3
D4
D5
D5*

10 1
10 2
10 3
10 4
10 5
10 5

4
4
5
5
5
5

5
5
4
4
4
4

50
100
200
300
350
1400

3/10
9/9
8/7
13/13
15/15
32/32

E1
E2
E3
E4
E5
E5*

10 1
10 2
10 3
10 4
10 5
10 5

4.4
1.2 ⇥ 10 1
1.3 ⇥ 10 2
9.3 ⇥ 10 3
8.7 ⇥ 10 3
6.8 ⇥ 10 3

4
4
5
5
5
5

5
5
4
4
4
4

50
100
120
150
150
200

5/9
6/7
8/6
10/10
10/10
10/10

4.4
8.8 ⇥ 10 2
1.1 ⇥ 10 2
1.0 ⇥ 10 2
1.0 ⇥ 10 3
9.8 ⇥ 10 3

dtot /dRoche

結果は３種類・RWI成長しない：St<10^-4でダストが集まりにくい
αのガス面密度依存が正べき（negative feadback）
・大きい一つの渦が形成：Stが小さい場合(<10^-3) 渦が合体
6 Zs. Regály, K. Kadam & D. Tarczay-Nehéz
・小さな複数の渦が形成：ダストの濃集が進んで小さな渦が維持

Figure 1. An example of the gas and dust surface density distribution, along with respective vortensity fields for the two cases–a single large-scale vortex

sedimentation for the dust, in which case,Table
2. Summary on the vortexA2excitation in models listed
in Table 1. MarkA1
A3
ing "5" corresponds to the absent of the given vortex type being multiplersmall-scale or single large-scale. jmin values show the minimum (i.e., theU.
(23)strongest phase) of vortex aspect ratio for gas/dust components, respectively.
d = g
St + U
ガス質量~2Mj
jmin values in parenthesis represents the minimum value reached by the endof simulation. The last column lists the maximum value of total midplane
ダスト質量
St=10^-1,
10^-2で100,
10Me
density in terms of Roche density at that radius. Models with asterisk use
The fragmentation size, 0 frag , is the maximum size of solid conextra wide 'dze = 4 dze viscosity transition.
stituent that can be reached due todust growth process,beforeSt=10^-2でdust/gas> the
1→streaming
instability

大きい渦

the grown particles are destroyed via mutual collision. We calculate
St=10^-1でRoch
を超える→重力崩壊可能(？)
the dust grain fragmentationdensity
according toBirnstiel et al. (2012) as

破壊で決まるダストサイズは ~6-12cm
2⌃g E 2frag
0 frag =,2
3cds U2 s

(24)

Mod.

St

A1
A2A5
A3
A4
A5
A5*

1
10 10
10 2
10 3
10 4
10 5
10 5

with the typical assumptions of fragmentation velocity, E frag =10 m s 1 , and the internal density of the dust aggregate, ds =B1
10 1
1.6 g cm 3 . The value of U is self-consistently calculated from sim2
ダスト質量
1~10
Me
B2
10
ulations according to Eq. (15) and ⌃g is calculated using the higher
2
B2*
10
bound
for MMSN.> In
the plots, maximuminstability
values of the quantities
dust/gas
1→streaming
B3
10 3
were global maximum throughout the computational grid. The cen4
B4
10
tralガス面密度は大きい渦より小さい
values were averaged across the centre of all the vortices. The
B5
10 5
averagevalue was calculated over the area of all vortices, which
B5*
10 5→ダストサイズは半分程度
gives a lower bound.
B5
1
C1
10
The simulations conducted in this study correspond to a2
C2
10
representative disc, which extends from 0.5 au to 5 au, with
3
C3
10
・どちらの場合でも渦の落下はdead
zone
outer
the outer boundary of the dead zone set at a radial
distanceof edge でC3*
10 3'dze = '0 = 1 au. In a typical protoplanetary disc, the dimensions
止まる
C4
10 4
are about an order of magnitude larger, with the outer edge of theC5
10 5
dead zone lying at about 15 au. However, since the self-gravity is→微惑星・惑星形成環境として有望
D1
10 1
not considered in our simulations, the disc can be spatially rescaled.
D2
10 2
In this process, we keep the gas surface density values at 1 au un-

小さい渦

Small
vort.

Large
vort.

CRWI
( #orb )jmin(dust/gas)

A4

dtot /dRoche

5 Regály,5K. Kadam- & D. Tarczay-Nehéz
Zs.
5
5
5
5
5

4
A5*
B1 4
4
4
4

350
400
400
400
1500

16/10B3
16/14 C1
15/15
15/15
34/34

7.5 ⇥ 10 2
9.6 ⇥ 10 3
8.6 ⇥ 10 3
8.6 ⇥ 10 3
7.0 ⇥ 10 3

4
4
4
5
5
5
5

5
5
5
4
4
4
4

50
100
100
250
350
350
950

3/7
6/6
5/5
10/10
14/14
15/15
32/32

4.9
3.6 ⇥ 10 2
3.4 ⇥ 10 2
1.2 ⇥ 10 2
9.0 ⇥ 10 3
8.7 ⇥ 10 3
7.2 ⇥ 10 3

4
4
5
5
5
5
4
4

B5*

C3

5
5
4
4
5
5

50
150
650
1350
-

3/7
5/6
9/9
8/8
-

5
5

50
100

3/10
9/9

3.3
3.2 ⇥ 10 2
7.0 ⇥ 10 3
5.1 ⇥ 10 3
4.4
1.2 ⇥ 10 1

B4

C3*

D1

Structure and Kinematics of Sh2-138 – A distant hub-filament system in the outer
31 Galactic plane
Kshitiz Mallick, Lokesh Dewangan, Devendra Ojha, Tapas Baug, Igor Zinchenko F We present a molecularline study of the Sh2-138 (IRAS 22308+5812) hub-filament system with an aim to investigate its structure andkinematics. Archival CO molecular line data from the Canadian Galactic Plane Survey (CO(J=1-0)) for the wider
region (50arcminx50arcmin) and the James Clerk Maxwell Telescope (CO(3-2), 13CO(3-2), and C18O(3-2)) for thecentral portion (5arcminx5arcmin) have been utilised. Analysis of the CO(1-0) spectra for the extended region in
conjunction with the hub and filament identification using column density map and the getsf tool, respectively, reveals
a complex structure with the spectral extraction for the central position displaying multiple velocity components.
Based on the Herschel 70 micron warm dust emission, one of the filaments in the extended region was inferred to be
associated with active star formation, and is host to a Bolocam 1.1 mm clump of 1606 Msun. Integrated intensity mapof 13CO(3-2) emission, constructed from clumps detected at above 5sigma in position-position-velocity space, reveals
three filamentary structures (labelled W-f, SW-f, and SE-f) in the central portion. Velocity gradients observed in
13CO(3-2) position-velocity slices point to longitudinal gas flow along the filaments into the central region. Filaments
W-f, SW-f, and SE-f were calculated to have observed line masses of 32, 33.5, and 50 Msun/pc , respectively. The
cloud was found to be dominated by supersonic and non-thermal motions, with high Mach numbers (>3) and low
thermal to non-thermal pressure ratio (0.01-0.1).

11

Disk
fragmentation
aroundamassive
protostar:a
comparisonoftwothree-dimensional
32 codesRaphaël Mignon-Risse, André Oliva, Matthias González, Rolf Kuiper, Benoît Commerçon F (Abridged) Most

massive stars are located in multiple systems. The modeling of disk fragmentation, a possible mechanism leading tostellar multiplicity, relies on parallel 3D simulation codes whose agreement remains to be evaluated. Using the Cartesian
AMR code RAMSES, we compare disk fragmentation in a centrally-condensed protostellar system to the study of Oliva& Kuiper (2020) performed on a grid in spherical coordinates using PLUTO. Two RAMSES runs are considered andgive qualitatively distinct pictures. When allowing for unlimited sink particle creation, gas fragmentation leads to a
multiple stellar system whose multiplicity is aﬀected by the grid when triggering fragmentation and by numericallyassisted mergers. On the other hand, using a unique, central, fixed sink particle, a centrally-condensed system forms,
similar to that reported in PLUTO. The RAMSES-PLUTO comparison is performed with the latter: agreement
between the two codes is found regarding the first rotationally-supported disk formation, the presence of an accretion
shock onto it, the first fragmentation phase. Gaseous fragments form and their properties are in agreement between
the two codes. As a minor diﬀerence, fragments dynamics causes the disk structure to be sub-Keplerian in RAMSES
whereas it is found to be Keplerian and reaches quiescence in PLUTO. We attribute this discrepancy to the central star
being twice less massive in RAMSES because of the diﬀerent stellar accretion subgrid models. In a centrally-condensed
system, the agreement between RAMSES and PLUTO regarding many of the collapse properties and fragmentation
process is good. Fragmentation occurring in the innermost region and numerical choices (use of sink particles, grid)
have a crucial impact when similar but smooth initial conditions are employed - more crucial than the code’s choice on the system’s outcome, multiple or centrally-condensed.

A CCD Search for Variable Stars in the Open Cluster NGC 6611

G. Michalska, Z. Kołaczkowski, R. Leiton, O. Szewczyk, K. Kinemuchi, V., M. Kalari F We present the resultsof the U BV IC variability survey in the young open cluster NGC 6611 based on observations obtained during 34 nights
spanning one year. In total, we found 95 variable stars. Most of these stars are classified as periodic and irregularpre-main sequence (PMS) stars. The analysis of the JHKS 2MASS photometry and four-colour IRAC photometry
revealed 165 Class II young stellar sources, 20 of which are irregular variables and one is an eclipsing binary. These
classifications, complemented by JHK UKIDSS photometry and riH↵ VPHAS photometry, were used to identify
24 candidates for classical T Tauri stars and 30 weak-lined T Tauri stars. In addition to the PMS variables, weon the system’s outcome, multiple or centrally-condensed.

33

A CCD Search for Variable Stars in the Open Cluster NGC 6611

G. Michalska, Z. Kołaczkowski, R. Leiton, O. Szewczyk, K. Kinemuchi, V., M. Kalari F We present the resultsof the U BV IC variability survey in the young open cluster NGC 6611 based on observations obtained during 34 nights
spanning one year. In total, we found 95 variable stars. Most of these stars are classified as periodic and irregularpre-main sequence (PMS) stars. The analysis of the JHKS 2MASS photometry and four-colour IRAC photometry
revealed 165 Class II young stellar sources, 20 of which are irregular variables and one is an eclipsing binary. These
classifications, complemented by JHK UKIDSS photometry and riH↵ VPHAS photometry, were used to identify
24 candidates for classical T Tauri stars and 30 weak-lined T Tauri stars. In addition to the PMS variables, we
discovered eight Scuti candidates. None of these were previously known. Furthermore, we detected 17 eclipsingbinaries where two were previously known. Based on the proper motions provided by the Gaia EDR3 catalogue, we
calculated the cluster membership probabilities for 91 variable stars. For 61 variables, a probability higher than 80%
was determined, which makes them cluster members. Only 25 variables with a probability less than 20% were regarded
to be non-members.

Spiral Structure and Massive Star formation in the Hub-Filament-System G326.27-0.49

Bhaswati Mookerjea, V. S. Veena, Rolf Guesten, F. Wyrowski, Akhil Lasrado F Hub-filament systems (HFSs) arepotential sites of formation of star clusters and high mass stars. To understand the HFSs and to provide observational
constraints on current theories that attempt to explainstar formation globally, we report a study of the region associatedwith G326.27-0.49 using infrared data of dust continuum and newly obtained observations on molecular tracers using
the APEX telescope. We use the spectroscopic observations to identify velocity-coherent structures (filaments andclumps) and study their properties at a resolution of 0.4 pc. The region contains two main velocity components: firstcomponent shows four filaments between -63 and -55 km/s forming a spiral structure converging in a hub, the second
filamentary component at -72 km/s harbors a massive young stellar object and possibly interacts with the hub. The
clumps harbouring the three main YSOs in the region are massive (187-535 Msun), have luminosities consistent with
B-type stars, have central densities of 106 cm 3 and drive large outflows. Majority of the velocity-coherent clumps
in the region show virial parameters between 2-7, which considering the detection of protostars implies collapse to be
gradual. We conclude that the region consists of a network of filaments through which mass accretes ( 10 4 Msun/yr)
onto the hub. The hub and some of the ends of filaments appear to be undergoing collapse to form new stars. This
study identifies a target region for future high resolution observations that could probe the link between the core andSpiral Structure and Massive Star formation in the Hub-Filament-System G326.27-0.49

34 Bhaswati Mookerjea, V. S. Veena, Rolf Guesten, F. Wyrowski, Akhil Lasrado F Hub-filament systems (HFSs) arepotential sites of formation of star clusters and high mass stars. To understand the HFSs and to provide observational
constraints on current theories that attempt to explainstar formation globally, we report a study of the region associatedwith G326.27-0.49 using infrared data of dust continuum and newly obtained observations on molecular tracers using
the APEX telescope. We use the spectroscopic observations to identify velocity-coherent structures (filaments andclumps) and study their properties at a resolution of 0.4 pc. The region contains two main velocity components: firstcomponent shows four filaments between -63 and -55 km/s forming a spiral structure converging in a hub, the second
filamentary component at -72 km/s harbors a massive young stellar object and possibly interacts with the hub. The
clumps harbouring the three main YSOs in the region are massive (187-535 Msun), have luminosities consistent with
B-type stars, have central densities of 106 cm 3 and drive large outflows. Majority of the velocity-coherent clumps
in the region show virial parameters between 2-7, which considering the detection of protostars implies collapse to be
gradual. We conclude that the region consists of a network of filaments through which mass accretes ( 10 4 Msun/yr)
onto the hub. The hub and some of the ends of filaments appear to be undergoing collapse to form new stars. This
study identifies a target region for future high resolution observations that could probe the link between the core andfilament evolution.

12

Investigating the morphology and CO gas kinematics of Sh2-112 region

35 Kshitiz Mallick, Saurabh Sharma, Lokesh Dewangan, Devendra Ojha, Neelam Panwar, Tapas Baug F We

present a study of the molecular cloud in Sh2-112 massive star forming region using the 3-2 transition of CO isotopologues - CO, 13CO, and C18O; supplemented in part by CGPS HI line emission and MSX data. Sh2-112 is an
optically visible region powered by an O8V type massive star BD +45 3216, and hosts two Red MSX Survey sources G083.7962+03.3058 and G083.7071+03.2817 - classified as HII region and young stellar object, respectively. Reduced
spectral data products from the James Clerk Maxwell Telescope archive, centered on the two RMS objects with 7’x7’
field of view each, were utilised for the purpose. The 13CO(3-2) channel map of the region shows the molecular
cloud to have filamentary extensions directed away from the massive star, which also seems to be at the edge of acavity like structure. Multiple molecular cloud protrusions into this cavity structure host local peaks of emission.
The integrated emission map of the region constructed from only those emission clumps detected above 5 level inthe position-position-velocity space aﬃrms the same. MSX sources were found distributed along the cavity boundary
where the gas has the been compressed. Spectral extraction at these positions yielded high Mach numbers and low
ratios of thermal to non-thermal pressure, suggesting a dominance of supersonic and non-thermal motion in the cloud.

Takeout and Delivery: Erasing the Dusty Signature of Late-stage Terrestrial Planet
Formation
Joan R. Najita, Scott J. Kenyon F The formation of planets like Earth is expected to conclude with a series oflate-stage giant impacts that generate warm dusty debris, the most anticipated visible signpost of terrestrial planet
formation in progress. While there is now evidence that Earth-sized terrestrial planets orbit a significant fraction ofsolar-type stars, the anticipated dusty debris signature of their formation is rarely detected. Here we discuss several
ways in which our current ideas about terrestrial planet formation imply transport mechanisms capable of erasing the
anticipated debris signature. A tenuous gas disk may be regenerated via "takeout" (i.e., the liberation of planetaryatmospheres in giant impacts) or "delivery" (i.e., by asteroids and comets flung into the terrestrial planet region) at
a level suﬃcient to remove the warm debris. The powerful stellar wind from a young star can also act, its delivered
wind momentum producing a drag that removes warm debris. If such processes are eﬃcient, terrestrial planets may
assemble inconspicuously, with little publicity and hoopla accompanying their birth. Alternatively, the rarity of warm
excesses may imply that terrestrial planets typically form very early, emerging fully formed from the nebular phasewithout undergoing late-stage giant impacts. In either case, the observable signposts of terrestrial planet formation

ratios of thermal to non-thermal pressure, suggesting a dominance of supersonic and non-thermal motion in the cloud.

and Delivery: Erasing the Dusty Signature of Late-stage Terrestrial Planet
36 Takeout
Formation
Joan R. Najita, Scott J. Kenyon F The formation of planets like Earth is expected to conclude with a series oflate-stage giant impacts that generate warm dusty debris, the most anticipated visible signpost of terrestrial planet
formation in progress. While there is now evidence that Earth-sized terrestrial planets orbit a significant fraction ofsolar-type stars, the anticipated dusty debris signature of their formation is rarely detected. Here we discuss several
ways in which our current ideas about terrestrial planet formation imply transport mechanisms capable of erasing the
anticipated debris signature. A tenuous gas disk may be regenerated via "takeout" (i.e., the liberation of planetaryatmospheres in giant impacts) or "delivery" (i.e., by asteroids and comets flung into the terrestrial planet region) at
a level suﬃcient to remove the warm debris. The powerful stellar wind from a young star can also act, its delivered
wind momentum producing a drag that removes warm debris. If such processes are eﬃcient, terrestrial planets may
assemble inconspicuously, with little publicity and hoopla accompanying their birth. Alternatively, the rarity of warm
excesses may imply that terrestrial planets typically form very early, emerging fully formed from the nebular phasewithout undergoing late-stage giant impacts. In either case, the observable signposts of terrestrial planet formation
appear more challenging to detect than previously assumed. We discuss observational tests of these ideas.

Early water delivery to terrestrial planet regions during the stages of Jupiter’s formationand migration in the Grand Tack model

Masahiro Ogihara, Hidenori Genda, Yasuhito Sekine F The formation and subsequent migration of gas giants could

significantly aﬀect the material mixing in the Solar System. In this study, we use N-body simulations to investigate
how much water is transported into the region of the terrestrial planet formation during the growth and migration
phases of Jupiter in the Grand Tack model. We found that Jupiter’s growth was accompanied by significant masstransport, and that a substantial amount of water (about 10 times Earth’s ocean mass for the initial planetesimal
distribution based on the minimum-mass solar nebula) was transported into the terrestrial planet region. The total
amount delivered increased further during Jupiter’s migration phase (totaling about 10-40 times Earth’s ocean mass),
which was less dependent on simulation parameters. In addition, at these stages, terrestrial planets were not fullygrown. Therefore, water supplied during these early stages could interact with metallic iron during the core formationof protoplanets and/or growing Earth. Since hydrogen in water molecules can dissolve into their cores, this could
explain the density deficit observed in the current Earth core. Notably, Jupiter could play an important role as a

(CC) meteorites. This study’s results show that Jupiter’s growth necessitates some mixing of NC and CC materials.

38

ALMA Band 6 high-resolution observations of the transitional disk around SY Cha

Ryuta Orihara, Munetake Momose, Takayuki Muto, Jun Hashimoto, Hauyu Baobab Liu, Takashi Tsukagoshi, Tomoyuki Kudo, Sanemichi Takahashi, Yi Yang, Yasuhiro Hasegawa, Ruobing Dong, Mihoko Konishi,
Eiji Akiyama F In this study, we reported the results of high-resolution (0.14 arcsec) Atacama Large Millime-

ter/submillimeter Array (ALMA) observations of the 225 GHz dust continuum and CO molecular emission lines fromthe transitional disk around SY Cha. Our high-resolution observations clearly revealed the inner cavity and the central
point source for the first time. The radial profile of the ring can be approximated by a bright narrow ring superimposedon a fainter wide ring. Furthermore, we found that there is13a weak azimuthal asymmetry in dust continuum emission.
For gas emissions, we detected 12 CO(2 1), 13 CO(2 1) and C18 O(2 1), from which we estimated the total gas massof the disk to be 2.2 ⇥ 10 4 M , assuming a CO/H2 ratio of 10 4 . The observations showed that the gas is present
inside the dust cavity. The analysis of the velocity structure of the 12 CO(2 1) emission line revealed that the velocity
is distorted at the location of the dust inner disk, which may be owing to warping of the disk or radial gas flow within
the cavity of the dust disk. High-resolution observations of SY Cha showed that this system is composed of a ring anda distorted inner disk, which may be common, as indicated by the survey of transitional disk systems at a resolutionof ⇠0.1 arcsec.

Survey of H↵ emission-line stars in the star-forming region IC 5070

Neelam Panwar, Jessy Jose, Rishi C F Actively accreting young stellar objects show H↵ emission line in theirspectra. We present the results of survey for H↵ emission-line stars in the star-forming region IC 5070 taken with
2-m Himalyan Chandra Telescope. Based on the H↵ slitless spectroscopy data, we identified 131 emission-line stars in⇠ 0.29 square degrees area of the IC 5070 region. Using Gaia Early Data Release 3, we estimated the mean propermotion and parallax of the emission-line stars. We also estimated the mean distance and reddening toward the region
using the emission-line stars, that are ⇠ 833 pc and ⇠2 mag, respectively. By examining the locations of these stars
in the color-magnitude diagrams constructed using Gaia and PanSTARRS1 data, we found that a majority of the H↵
emitters are young low-mass (< 1.5 M ) stars. We also compared our catalog of emission-line stars with the available
young stellar catalogs and found that most of them are Class II/ flat spectrum sources with the spectral type ranging
from K to M. Based on the proper motion/ parallax values and locations on the color-magnitude diagrams, about 20
emission-line stars are flagged as non-members. The relative proper motion of the emission-line stars with respect tothe ionizing source suggest the possibility of the ‘rocket eﬀect’ scenario in the remnant cloud (BRC 31).

of ⇠0.1 arcsec.

of H↵ emission-line stars in the star-forming region IC 5070
39 Survey
Neelam Panwar, Jessy Jose, Rishi C F Actively accreting young stellar objects show H↵ emission line in theirspectra. We present the results of survey for H↵ emission-line stars in the star-forming region IC 5070 taken with
2-m Himalyan Chandra Telescope. Based on the H↵ slitless spectroscopy data, we identified 131 emission-line stars in⇠ 0.29 square degrees area of the IC 5070 region. Using Gaia Early Data Release 3, we estimated the mean propermotion and parallax of the emission-line stars. We also estimated the mean distance and reddening toward the region
using the emission-line stars, that are ⇠ 833 pc and ⇠2 mag, respectively. By examining the locations of these stars
in the color-magnitude diagrams constructed using Gaia and PanSTARRS1 data, we found that a majority of the H↵
emitters are young low-mass (< 1.5 M ) stars. We also compared our catalog of emission-line stars with the available
young stellar catalogs and found that most of them are Class II/ flat spectrum sources with the spectral type ranging
from K to M. Based on the proper motion/ parallax values and locations on the color-magnitude diagrams, about 20
emission-line stars are flagged as non-members. The relative proper motion of the emission-line stars with respect tothe ionizing source suggest the possibility of the ‘rocket eﬀect’ scenario in the remnant cloud (BRC 31).

Extension of HOPS Out to 500 ParSecs (eHOPS). I. Identification and Modeling ofProtostars in the Aquila Molecular Clouds

Riwaj Pokhrel, S. Thomas Megeath, Robert A. Gutermuth, Elise Furlan, William J. Fischer, Samuel Federman,
John J. Tobin, Amelia M. Stutz, Lee Hartmann, Mayra Osorio, Dan M. Watson, Thomas Stanke, P. Manoj,
Mayank Narang, Prabhani Atnagulov, Nolan Habel, Wafa Zakri F We present a Spitzer/Herschel focused surveyof the Aquila molecular clouds (d ⇠ 436 pc) as part of the eHOPS (extension of HOPS Out to 500 ParSecs) census
of nearby protostars. For every source detected in the Herschel/PACS bands, the eHOPS-Aquila catalog contains 1850 µm SEDs assembled from 2MASS, Spitzer, Herschel, WISE, and JCMT/SCUBA-2 data. Using a newly developed
set of criteria, we classify objects by their SEDs as protostars, pre-ms sequence stars with disks, and galaxies. A totalof 172 protostars are found in Aquila, tightly concentrated in the molecular filaments that thread the clouds. Of these,
71 (42%) are Class 0 protostars, 54 (31%) are Class I protostars, 43 (25%) are flat-spectrum protostars, and 4 (2%)
are Class II sources. Ten of the Class 0 protostars are young PACS Bright Red Sources similar to those discovered inOrion. We compare the SEDs to a grid of radiative transfer models to constrain the luminosities, envelope densities,
and envelope masses of the protostars. A comparison of the eHOPS-Aquila to the HOPS protostars in Orion finds thatthe protostellar luminosity functions in the two star-forming regions are statistically indistinguishable, the bolometrictemperatures/envelope masses of eHOPS-Aquila protostars are shifted to cooler temperatures/higher masses, and the

the ionizing source suggest the possibility of the ‘rocket eﬀect’ scenario in the remnant cloud (BRC 31).

40

Extension of HOPS Out to 500 ParSecs (eHOPS). I. Identification and Modeling ofProtostars in the Aquila Molecular Clouds

Riwaj Pokhrel, S. Thomas Megeath, Robert A. Gutermuth, Elise Furlan, William J. Fischer, Samuel Federman,
John J. Tobin, Amelia M. Stutz, Lee Hartmann, Mayra Osorio, Dan M. Watson, Thomas Stanke, P. Manoj,
Mayank Narang, Prabhani Atnagulov, Nolan Habel, Wafa Zakri F We present a Spitzer/Herschel focused surveyof the Aquila molecular clouds (d ⇠ 436 pc) as part of the eHOPS (extension of HOPS Out to 500 ParSecs) census
of nearby protostars. For every source detected in the Herschel/PACS bands, the eHOPS-Aquila catalog contains 1850 µm SEDs assembled from 2MASS, Spitzer, Herschel, WISE, and JCMT/SCUBA-2 data. Using a newly developed
set of criteria, we classify objects by their SEDs as protostars, pre-ms sequence stars with disks, and galaxies. A totalof 172 protostars are found in Aquila, tightly concentrated in the molecular filaments that thread the clouds. Of these,
71 (42%) are Class 0 protostars, 54 (31%) are Class I protostars, 43 (25%) are flat-spectrum protostars, and 4 (2%)
are Class II sources. Ten of the Class 0 protostars are young PACS Bright Red Sources similar to those discovered inOrion. We compare the SEDs to a grid of radiative transfer models to constrain the luminosities, envelope densities,
and envelope masses of the protostars. A comparison of the eHOPS-Aquila to the HOPS protostars in Orion finds thatthe protostellar luminosity functions in the two star-forming regions are statistically indistinguishable, the bolometrictemperatures/envelope masses of eHOPS-Aquila protostars are shifted to cooler temperatures/higher masses, and theeHOPS-Aquila protostars do not show the decline in luminosity with evolution found in Orion. We briefly discuss
whether these diﬀerences are due to biases between the samples, diverging star formation histories, or the influence ofenvironment on protostellar evolution.

Starlight-polarization-based tomography of the magnetized interstellar medium: PASIPHAE’sline-of-sight inversion method
V. Pelgrims, G. V. Panopoulou, K. Tassis, V. Pavlidou, A. Basyrov, D. Blinov, E. Gjerløw, S. Kiehlmann, N.
Mandarakas, A. Papadaki, R. Skalidis, A. Tsouros, R. M. Anche, H. K. Eriksen, T. Ghosh, J. A. Kypriotakis, S.
Maharana, E. Ntormousi, T. J. Pearson, S. B. Potter, A. N. Ramaprakash, A. C. S. Readhead, I. K. Wehus F

We present the first Bayesian method for tomographic decomposition of the plane-of-sky orientation of the magnetic
field with the use of stellar polarimetry and distance. This standalone tomographic inversion method presents anenvironment on protostellar evolution.

tomography of the magnetized interstellar medium: PASIPHAE’s
41 Starlight-polarization-basedline-of-sight inversion method
V. Pelgrims, G. V. Panopoulou, K. Tassis, V. Pavlidou, A. Basyrov, D. Blinov, E. Gjerløw, S. Kiehlmann, N.
Mandarakas, A. Papadaki, R. Skalidis, A. Tsouros, R. M. Anche, H. K. Eriksen, T. Ghosh, J. A. Kypriotakis, S.
Maharana, E. Ntormousi, T. J. Pearson, S. B. Potter, A. N. Ramaprakash, A. C. S. Readhead, I. K. Wehus F

We present the first Bayesian method for tomographic decomposition of the plane-of-sky orientation of the magnetic
field with the use of stellar polarimetry and distance. This standalone tomographic inversion method presents animportant step forward in reconstructing the magnetized interstellar medium (ISM) in 3D within dusty regions. We
develop a model in which the polarization signal from the magnetized and dusty ISM is described by thin layers at
various distances. Our modeling makes it possible to infer14the mean polarization (amplitude and orientation) induced
by individual dusty clouds and to account for the turbulence-induced scatter in a generic way. We present a likelihood
function that explicitly accounts for uncertainties in polarization and parallax. We develop a framework for reconstructing the magnetized ISM through the maximization of the log-likelihood using a nested sampling method. We
test our Bayesian inversion method on mock data taking into account realistic uncertainties from Gaia and as expected
for the optical polarization survey PASIPHAE according to the currently planned observing strategy. We demonstratethat our method is eﬀective at recovering the cloud properties as soon as the polarization induced by a cloud to its
background stars is higher than ⇠ 0.1% for the adopted survey exposure time and level of systematic uncertainty. Our
method makes it possible to recover not only the mean polarization properties but also to characterize the intrinsic
scatter, thus creating new ways to characterize ISM turbulence and the magnetic field strength. Finally, we apply
our method to an existing data set of starlight polarization with known line-of-sight decomposition, demonstrating
agreement with previous results and an improved quantification of uncertainties in cloud properties.

The ALMA view of MP Mus (PDS 66): a protoplanetary disk with no visible gaps
down to 4 au scales

Á. Ribas, E. Macías, P. Weber, S. Pérez, N. Cuello, R. Dong, A. Aguayo, C. Cáceres, J. Carpenter, W. R. F.
Dent, I. de Gregorio-Monsalvo, G. Duchêne, C. C. Espaillat, P. Riviere-Marichalar, M. Villenave F We present

ALMA multiwavelength observations of the protoplanetary disk around the nearby (d⇠100 pc) young solar analog MP
Mus (PDS 66). These observations at 0.89 mm, 1.3 mm, and 2.2 mm have angular resolutions of ⇠ 1", 0.05", and 0.25",
respectively, and probe the dust and gas in the system with unprecedented detail and sensitivity. The disk appears
smooth down to the 4 au resolution of the 1.3 mm observations, in contrast with most disks observed at comparable
spatial scales. The dust disk has a radius of 60±5 au, a dust mass of 0.14+0.11
0.06 MJup , and a mm spectral index < 2in the inner 30 au, suggesting optically thick emission from grains with high albedo in this region. Several molecularbetween 30-80 au is likely not a gap in the disk density, but a shadow cast by a puﬀed-up inner disk.

constraints on turbulence in proto-planetary discs
43 Empirical
Giovanni P. Rosotti F Proto-planetary discs, the birth environment of planets, are an example of a structure com-monly found in astrophysics, accretion discs. Identifying the mechanism responsible for accretion is a long-standing
problem, dating back several decades. The common picture is that accretion is a consequence of turbulence, withseveral instabilities proposed for its origin. While traditionally this field used to be a purely theoretical endeavour,the landscape is now changing thanks mainly to new observational facilities such as the ALMA radio interferometer.
Thanks to large improvements in spatial and spectral resolution and sensitivity (which have enabled the study of discsubstructure, kinematics and surveys of large disc populations), multiple techniques have been devised to observationally measure the amount of turbulence in discs. This review summarises these techniques, ranging from attempts at
direct detection of turbulence from line broadening, to more indirect approaches that rely on properties of the dust or
consider the evolution of global disc properties (such as masses, radii and accretion rates) for large samples, and what
their findings are. Multiple lines of evidence suggest that discs are in fact not as turbulent as thought one decade ago.
On the other hand, direct detection of turbulence in some discs and the finite radial extent of dust substructures and insome cases the finite vertical extent strongly indicate that turbulence must be present at some level in proto-planetary
discs. It is still an open question whether this amount of turbulence is enough to power accretion or if this is instead
driven by other mechanisms, such as MHD winds.

15

of planetesimals and eventually planetary systems.

45

Direct imaging discovery of a super-Jovian around the young Sun-like star AF Leporis

Robert J. De Rosa, Eric L. Nielsen, Zahed Wahhaj, Jean-Baptise Ruﬃo, Paul G. Kalas, Anne E. Peck, Lea
A. Hirsch, William Roberson F (abridged) Expanding the sample of directly imaged companions to nearby, youngstars that are amenable to detailed astrometric and spectroscopic studies is critical for the continued development andvalidation of theories of their evolution and atmospheric processes. The recent release of the Gaia astrometric catalogue
allows us to eﬃciently search for these elusive companions by targeting those stars that exhibit the astrometric reflex
motion induced by an orbiting companion. The nearby (27 pc), young (24 Myr) star AF Leporis (AF Lep) was
targeted because of its astrometric acceleration, consistent with a wide-orbit planetary companion detectable withhigh-contrast imaging. We used the SPHERE instrument on the VLT to search for faint substellar companions in theimmediate vicinity of AF Lep. We used observations of a nearby star interleaved with those of AF Lep to eﬃciently
subtract the residual point spread function. This provided sensitivity to faint planetary-mass companions within 1
arcsec (⇠30 au) of the star. We detected the companion AF Lep b at a separation of 339 mas (9 au), within the inneredge of its unresolved debris disk. The measured K-band contrast and the age of the star yield a model-dependent
mass of 4 and 6 MJup , consistent with the mass derived from an orbital fit of 4.3+2.9
1.2 MJup . The near-infrared SEDof the planet is consistent with an object at the L–T spectral type transition, but under-luminous with respect tofield-gravity objects. AF Lep b joins a growing number of substellar companions imaged around stars in the young
Pic moving group. With a mass of between 3 and 7 MJup , it occupies a gap in this isochronal sequence between
the hotter, more massive companions like PZ Tel B and Pic b, and the cooler 51 Eri b, which is suﬃciently cool formethane to form within its photosphere.

Analysis of the first infrared spectrum of quasi-bound H2 line emission in Herbig-Haro7

Evelyne Roueﬀ, Michael G. Burton, Thomas R. Geballe, Hervé Abgrall F Context. Highly excited molecularhydrogen H2 has been observed in many regions of shocked molecular gas. A recently published K-band spectrum of
Herbig-Haro 7 (HH7) contains several vibration-rotation lines of H2 from highly excited energy levels that have notbeen detected elsewhere, including a line at 2.179 µm identified as arising from the v=2 J=29 level, which lies above
the dissociation limit of H2. One emission line at 2.104 µm in this spectrum was unidentified. Aims. We aim tocomplete the analysis of the spectrum of HH7 by including previously missing molecular data that have been recently
computed. Methods. We re-analysed the K-band spectrum, emphasising the physics of quasi-bound upper levels thatmethane to form within its photosphere.

46 Analysis of the first infrared spectrum of quasi-bound H2 line emission in Herbig-Haro7

Evelyne Roueﬀ, Michael G. Burton, Thomas R. Geballe, Hervé Abgrall F Context. Highly excited molecularhydrogen H2 has been observed in many regions of shocked molecular gas. A recently published K-band spectrum of
Herbig-Haro 7 (HH7) contains several vibration-rotation lines of H2 from highly excited energy levels that have notbeen detected elsewhere, including a line at 2.179 µm identified as arising from the v=2 J=29 level, which lies above
the dissociation limit of H2. One emission line at 2.104 µm in this spectrum was unidentified. Aims. We aim tocomplete the analysis of the spectrum of HH7 by including previously missing molecular data that have been recently
computed. Methods. We re-analysed the K-band spectrum, emphasising the physics of quasi-bound upper levels thatcan produce infrared emission lines in the K band. Results. We confirm the identification of the 2 1 S(27) line
at 2.1785 µm and identify the line at 2.1042 µm as due to the 1-0 S(29) transition of H2, whose upper level energy
is also higher than the dissociation limit. This latter identification, its column density, and the energy of its upper
level further substantiate the existence of a hot thermal component at 5000 K in the HH7 environment. Conclusion.
The presence of the newly identified 1 0 S(29) line, whose quasi-bound upper level (v=1, J=31) has a significant
spontaneous dissociation probability, shows that dissociation of H2 is occurring. The mechanism by which virtually
all of the H2 levels with energies from 20,000 K to 53,000 K is maintained in local thermodynamic equilibrium at asingle temperature of ⇠5,000 K remains to be understood.
16

Searching for Molecular Jets from High-Mass Protostars

Tatiana M. Rodriguez, Peter Hofner, Isaac Edelman, Esteban D. Araya, Viviana Rosero F We report Very Large

Array (VLA) observations in the Q-band toward 10 ionized jet candidates to search for SiO emission, a well-known
shocked gas tracer. We detected 7 mm continuum counterparts toward 90% of the jet candidates. In most cases, the jet
candidate is located toward the center of the 7 mm core, and the high masses (⇡ 100 M ) and densities (⇡ 107 cm 3 )of the cores suggest that the central objects are very young high-mass protostars. We detected SiO J = 1 0 emission
associated with 6 target sources. In all cases, the morphology and spectrum of the emission is consistent with whatis expected for molecular jets along an outflow axis, thus confirming the jet nature of 60% of our sample. Our datasuggest a positive correlation between the SiO luminosity LSiO , and both the bolometric luminosity LBol and theradio luminosity S⌫ d2 of the driving sources.