星形成ゼミ (SFN #305 34-43) 2018/6/22 辰馬
34. The unexpectedly large proportion of high-mass star-forming cores in a Galactic ministarburst, Motte et al., http://arxiv.org/pdf/1804.02392
35. Layers in the Central Orion Nebula, OʼDell, http://arxiv.org/pdf/1804.06491
36. Formation of close-in super-Earths in evolving protoplanetary disks due to disk winds, Ogihara
et al., http://arxiv.org/pdf/1804.01070
37. Formation of the terrestrial planets in the solar system around 1 au via radial concentrationof planetesimals, Ogihara et al., http://arxiv.org/pdf/1804.02361
38. High-resolution near-IR Spectral mapping with H2 and [Fe II] lines of Multiple Outﬂows around
LkHα 234, Oh et al., https://arxiv.org/pdf/1804.01673
39. New places and phases of CO-poor/CI-rich molecular gas in the Universe, Papadopoulos etal., https://arxiv.org/pdf/1804.09654
40. Distribution of Serpens South protostars revealed with ALMA, Plunkett et al., http://arxiv.org/
pdf/1804.02405
41. Circumstellar Disk Lifetimes In Numerous Galactic Young Stellar Clusters, Richert et al.,https://arxiv.org/pdf/1804.05076
42. Multiple Stellar Fly-Bys Sculpting the Circumstellar Architecture in RW Aurigae, Rodriguez etal., http://arxiv.org/pdf/1804.09190
43. A Cavity of Large Grains in the Disk Around the Group II Herbig Ae/Be Star HD 142666,
Rubinstein et al., https://arxiv.org/pdf/1804.07343.pdf!1

Laboratoire Lagrange, Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Blvd de l’Observatoire, CSof close-in
34229,Formation
06304 Nice Cedex
4, Francesuper-Earths in evolving protoplanetary disks due to disk winds
Masahiro Ogihara1 , Eiichiro Kokubo1 , Takeru K. Suzuki2 , and Alessandro Morbidelli3
E-mail contact: masahiro.ogihara at nao.ac.jp
1
Division of Theoretical Astronomy, National Astronomical Observatory of Japan, 2-21-1, Osawa, Mitaka, 181-8588
Planets with masses 2larger than about 0.1 Earth-masses undergo rapid inward migration (type I migration) in a 3
Tokyo, Japan; School of Arts & Sciences, University of Tokyo, 3-8-1, Komaba, Meguro, 153-8902 Tokyo, Japan;
standard protoplanetary disk. Recent magnetohydrodynamical simulations revealed the presence of magnetically
Laboratoire Lagrange, Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Blvd de l’Observatoire, CS
driven disk winds, which would alter the disk profile and the type I migration in the close-in region. We investigate
34229, 06304 Nice Cedex 4, France
orbital evolution of planetary embryos in disks that viscously evolve under the eﬀects of disk winds. The aim is
E-mailcontact:masahiro.ogihara
at nao.ac.jp
to discusseﬀectsof altereddisk profiles
on type I migration. In addition, we aim to examine whether observed
distributions
close-insuper-Earths
be reproducedby simulations
includeof disk(typewinds.
We perform
Planetsofwith
masseslarger thancan
about
0.1 Earth-masses
undergothat
rapid
inwardeﬀects
migration
I migration)
in aprotoplanetary
disk. formation
Recent magnetohydrodynamical
the presence
magneticallyN-bodystandard
simulationsof super-Earthfrom planetary embryos,simulations
in which arevealed
recent modelfor diskofevolutionisdisk winds,
alter the disk
the type
I migration
the close-in
region.simulations
We investigate
used. driven
We explore
a widewhichrangewouldof parameters
andprofile
draw andgeneraltrends.
We alsoincarryout N-bodyofevolutionof planetary
embryos inin suchdisksdisksthat underviscously
evolveunder theWeeﬀectsof disk
The aim isclose-inorbital
super-Earthformationfrom embryos
variousconditions.
find thatthe winds.
type I migration
to discusssuppressed
eﬀects of alteredprofilesIn addition,
we occurs,
aim to examine
whetherobserved
is significantly
in manydisk
cases.
Evenonintype
casesI migration.
in which inward
migration
the migration
timescale
distributions
close-insuper-Earths
can type
be reproducedby simulations
that include
eﬀectsdisksurface
winds. density
We perform
is lengthened
to 1 ofMyr,
which
mitigates theI migration
problem. Thisis because
theofgasisN-bodysuper-Earthfrom planetary
embryos,which
recentmodel
disk
evolution isdecreased
and simulations
has a flatterofprofilein the formation
close-in region
due to disk
winds. inWe
find athat
when
the fortype
I migration
used. Wesuppressed,
explore a widerange
of parameters
andinstability
draw generaltrends.
Wedepletion,
also carryleadingout N-bodysimulations ofis significantly
planets
undergolate orbital
duringthe gasto a non-resonant
close-in super-Earthfrom embryos
in suchundervarious conditions.
We findthatmass
the type
I migration
configuration.
We also findformationthat observed
distributions
ofdisks
close-insuper-Earths(e.g., period
ratio,
ratio)
can beis significantly
suppressedin thatmanyincases.
in of
cases
in which systems
inward migration
occurs,the migration
timescalereproduced.
In addition,
we showsome Even
results
simulations,with a chainof resonant
planets,
like
islengthened
to
1
Myr,
which
mitigates
the
type
I
migration
problem.
Thisisbecausethegas
surfacedensityisthe TRAPPIST-1 system, form.
decreased and has a flatter profile in the close-in region due to disk winds. We find that when the type I migration
Accepted
by A&A suppressed, planets undergo late orbital instability during the gas depletion, leading to a non-resonant
is significantly
configuration. We also find that observed distributions of close-in super-Earths (e.g., period ratio, mass ratio) can be
0.1地球質量より大きい惑星はガス円盤との相互作用によりすぐに中心星へと落ちてしまう
http://arxiv.org/pdf/1804.01070
reproduced. In addition, we show that in some results of simulations, systems with a chain of resonant planets, like(type
I migration)the
TRAPPIST-1
system, form. planets in the solar system around 1 au via radial concenFormation of the terrestrial

36
36

•

trationof planetesimals
Accepted
by A&Asuper-Earths)が見つかっている• しかし、中心星に近いところでスーパーアース(close-in
1123
http://arxiv.org/pdf/1804.01070
Masahiro
Ogihara , Eiichiro Kokubo , Takeru K. Suzuki , and Alessandro Morbidelli
1

Division of Theoretical Astronomy, National Astronomical Observatory of Japan, 2-21-1, Osawa, Mitaka, 181-8588
磁気駆動円盤風でtypeI migrationを止めることができるかもしれないof theterrestrial
solar
systemaroundau via Tokyo,
radial Japan;
concen3
Tokyo,Formation
Japan; 2 Schoolof Arts& Sciences,planets
UniversityinoftheTokyo,
3-8-1,
Komaba,Meguro,1 153-8902
tration of planetesimals
Laboratoire Lagrange, Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Blvd de l’Observatoire, CS
1Masahiro
Eiichiro Kokubo1 , Takeru K. Suzuki2 ,super-Earthsが再現できるか調べた
and Alessandro Morbidelli3
シミュレーションを用いて円盤風の影響と、close-in
34229,
06304 NiceOgihara
Cedex 4,, France
1
Division masahiro.ogiharaof Theoretical Astronomy,
National Astronomical Observatory of Japan, 2-21-1, Osawa, Mitaka, 181-8588
E-mail contact:at nao.ac.jp
Tokyo, Japan; 2 School of Arts & Sciences, University!2 of Tokyo, 3-8-1, Komaba, Meguro, 153-8902 Tokyo, Japan; 3
No planets exist inside the orbit of Mercury and the terrestrial planets of the solar system exhibit a localized con-

•

37
•

• Type I migrationとは…
• 惑星と円盤ガスとの重力相互作用による惑星軌道移動の一種• 円盤にギャップを開けるほど質量の大きくない地球型惑星(

type II migration)• 例えば1 auの地球だとおよそ数十万年(< 円盤寿命数百万年)で軌道移動する• Close-in super-Earthsとは…
• < 100地球質量(もしくは< 10地球半径) かつ < 1 au(もしくは< 200日軌道周期)• 2017年8月の時点で、432個の系の中に1087個見つかっている• その場形成か、形成後の軌道移動の2通りのモデルが提唱されている• 磁気駆動円盤風とは…
• 磁気流体力学(MHD)シミュレーションで明らかになった円盤風• 磁気回転不安定(MRI)駆動円盤風と、磁気遠心力円盤風の2種類• 円盤ガスの面密度を変える → type I migrationを止めることができるかもしれない!3

w power-law#$! viscosity"
φ,zw
spectively.
Fortheparameters,
weemploythesamevaluesas−5
Shakura&Sunyaev(1973)
αparameterization.
Paramdisk0- same-values-denpower-law
ctive
turbulentviscosity
based
on
a
2
e
disk
idoro
et
al.
2017).
AccordingtoSuzukietal.
(2016),
evolutionofgas
surface
spectively.
Fortheparameters,
weemploy
the
as
.
(2)
=
10
Σ
HΩ
∂Σ
1
∂
2
∂
planetaryembryosin awhich
zlaw
fsive
g
g αφ,z and C w are
disk
used
as
measuresoftheangularmoeters
2 disk2 momentum
2due
disk1
activeEq.
(2)strongstandardin
Suzukietal.
(2016),
are
based
on
MHD
simulations
wind
torque
and
mass
loss
due
to
disk
winds,
reoss
due
to
the
wind
torque
and
mass
loss
to
winds,
reα
and
C
are
used
as
measuresoftheangulareters
Hansen& MurrayΣg,ini= by(r
Σg αr,φ cequation:
√
φ,z
w
sity
is
calculated
solvingthediﬀusions ) + r αφ,zαviscosity
parameterization.
Param円盤ガス進化モデル(Suzuki
et
al.
2016)
r
(MMSN)
model
thatseveralobserved
prop•nSuzukietal.
(2016),
which
are
based
on
MHD
simulations
N)
model
inactiveEq.
strongstandard∂t torquer consider∂rrΩmass∂r disk2
2(2) πreα;(Suzuki
et
al.
2010;
Bai
2013).
We
two
cases
for
loss
due
to
the
wind
torque
and
mass
loss
due
to
disk
w
r,φ
of
in-situformation
loss
due
to
the
wind
and
loss
due
to
disk
winds,rtheparameters,
weemploythesamevaluesas
spectively.
Fortheparameters,
weemploythesamevalues
as
#$
!
"
can
be
reproduced.
-periods)
disk3−4
active(2) Σweakmeasuresoftheangularmomentum−5−3 2 Eq.foratplanets
yssomefoundthatplanets
Ω
Σ
HΩ
∂Σ
α
;
(Suzuki
et
al.
2010;
Bai
2013).
We
consider
two
cases
1
∂
2
∂
α
=
8×10
represents
MRI-inactive
disks,
and
α
=
8×10
tary
embryos
in
a
g
g
g
r,φ
spectively.
Fortheemploythevaluesasr,φr,φsimulations,a(2016),constant
αparameters,
is used(αwe=
10
Wesameset−4
2disk42 ).
2For
spectively.
theparameters,
weemploy
the
same
v
φ,zon
φ,z
;
however,agas
disk
shouldactive10strongel.
(2016),
which
are
based
MHD
simulations
−C
,
(1)
α
c
)
+
r
α
=
(r
Σ
n
Suzuki
et
al.
which
are
based
on
MHD
simulations
√
√
w
r,φ
φ,z
g
butions
of
s −5
−5
−3
and
mass
loss
due
to
disk
winds,
reralobserved
proprepresents
MRI-active
disks.
MRI-inactive
disks
correspondtoπ simulations−5
that
distributionsofinSuzukietal.
(2016),
which
are
based
on
MHD
∂t
r
∂r
rΩ
∂r
2
disk5
inactive
Eq.
(2)
weak
2π
α
=
8×10
represents
MRI-inactive
disks,
andα=
8×10embryos
becausethegrowthperlimits
on
C
as
C
=
1
×
10
and
2
×
10
for
inactive
o
r,φ
r,φ
w
w
in
Suzukietal.
(2016),
which
are
based
on
MHD
sim
α
;
2010;
Bai
2013).
We
consider
two
cases
for
heir
simα
;
(Suzuki
et
al.
2010;
Bai
2013).
We
consider
two
cases
for
−4
can
be
reproduced.
r,φ
cases
that
take
into
account
a
dead
zone
by
non-ideal
MHD
efr,φ
disk6
inactive
10 for αr,φstrong;(Suzuki
et
al.
2010;
Bai
2013).
We
consider
two
cases
ers,
we
employthesamevaluesashorter
than
the
disk
lifetime.
duced
by
their
simΣ
Ω
有効乱流粘性(Shakura&
Sunyaev
1973):-elyg•drepresents
activedisks,
respectively.
Insimulations,valuesofC
are
MRI-active
disks.
disks
towcorrespond
whereΩMRI-inactiveistheKeplerianfrequency.
Here
there
are
three param−3(Suzuki
et
al.
2010;
Bai
2013).
We
consider
two
com−5
−3
a
gas
disk
shouldfects.
Here
radially
constant
valuesareassumed.
For
thedescripdisk7
activeEq.
(2)strongt0 = 0 cases
yr
−C
,
(1)
−5
−3
√
w
represents
MRI-inactive
disks,
and
α
=
8×10
α
=
8×10
represents
MRI-inactive
disks,
and
α
=
8×10
ated
the
in-situaccretion
of
α
=
8×10
represents
MRI-inactive
disks,
and
α
=
8×10
r,φ
e
r,φ
r,φ
r,φ than
r,φ2π
ich
are
based
on
MHD
simulations
nerallysmallertheupperlimitsbecausetheparameter
nbecause
ation
relatively
cometers;
αr,φindicates
andisk8eﬀectiveturbulentviscosity
based ona 1 MyractiveEq.
(2) strongt0 =thegrowthofα,
weusually
use
−5
edge
due
cases
that
take
into
account
a
dead
zone
by
non-ideal
MHDefφ,zαcases= Figs.
8×10
represents
MRI-inactiveand
αyrr,φ =dysimulations
that
includeMRI-inactive円盤:(非理想MHD効果によるdeadzoneを考慮)w
represents
MRI-active
disks.
MRI-inactive
disks
correspond
totodisks,•r,φRI-active
disks.
MRI-inactive
disks
correspondtorepresents
MRI-active
disks.
MRI-inactive
disks
correspond
disk9
inactiveEq.
(2)strongt=
0
Shakura&Sunyaev(1973)
αviscosity
parameterization.
Param0isconstrainedbyenergetics
(see
2
and
6
in
Suzuki
et
al.
n
the
disk
lifetime.
α
;
13).
We
consider
two
for
tions
also
disk
inner
edge
due
r,φ
&−0.66%fects.
Herepower-law
radially
constant
valuesareassumed.
For
thedescripwhereΩrepresents
iseters
theaccountKeplerianfrequency.
Here
there
are
three
parama simple
disk
disk10inactiveEq.
(2)strongt0 = 1 Myr
cases
that
take
into
a
dead
zone
by
non-ideal
MHD
efMRI-active
disks.
MRI-inactive
disks
corre
α
and
C
are
used
as
measuresoftheangularmomentum
Σ
φ,z
w
into
account
a
dead
zone
by
non-idealMHD
efn-situ
accretion
of
cases
that
take
into
account
a
dead
zone
by
non-ideal
MHD
efg
16).
We
usuallyuse
the“strong
DW”
regime
(Eqs.
18
and
19
−3
ge
assum−5eters;
αindicates
aneﬀectiveturbulentviscosity
based
on a winds, rear
nebular(MMSN)
model
sis
calculations
also
RI-inactive
disks,
and
α
=
8×10
r,φ
MRI-active円盤:
.
(2)
αφ,z
=
10
ftions
•
ion
of
α
,
we
usuallyuser,φ
直線のモデル(disk0)は円盤風のない円盤
fects.
Here
radially
constant
valuesareassumed.
For
thedescriploss
due
to
the
wind
torque
and
mass
loss
due
to
disk
φ,z
that
include
cases
that
take
into
accountathe
deadzone by non-ideal M
Suzukietal.
2016),
while
severalsimulations
areperformed
Σthat
3),
while
ially
constant
valuesareassumed.
For
thedescripfects.
Hereradially
constant
valuesareassumed.
For
descripg,ini
Shakura&Sunyaev(1973)
αviscosity
parameterization.
Param981).
They
found
planets.
spectively.
the parameters, we employ the same values astionof αdisksuse Forto
kes.
inner
edge
assumMRI-inactive
correspond
φ,z , we usually
power-law
disk
not
show
the
“weak
DW”
regime
(Eqs.
20
and
21
in
Suzuki
et
al.
&
%
α
and
CwHereareusedasmeasuresof theangularmomentumeters
observed
that
distributionsofradially
constant
valuesareassumed.
For
theφ,zfects.
円盤風トルクによる角運動量損失:
edrngusually
use
−0.66
ion
of
α
,
we
usuallyuse•−4inSuzukietal.
(2016),
which
are
based
on
MHD
simulations
φ,z(MMSN)
model
In
some
simulations,a%dueconstant
αMHD
used
(αand
10 loss). We
setto disk winds, reetal.
2013),whileΣ
φ,z is torque
φ,z =
&
a
dead
zone
by
non-ideal
efg
loss
to
the
wind
mass
due
be
reproducedbytheir
sim−0.66
16).
−5,found(Suzuki
et
al.
2010;
Bai
We consider two(2)cases for αr,φ ;
tion
of
α
,
we
usuallyuse
Σ
−5φ,z−5 2013).
thatplanets
g
.
α
=
10
−5
upper
limits
on
C
as
C
=
1
×
10
and
2
×
10
for
inactiveφ,zw &comw&initial
spectively.
Fortheparameters,
weemploy the same values
as%obtaina αgasrelatively
arths
does
not
show
valuesareassumed.
For
thedescrip−5
−3
.
(2)
=
10
−0.66
mation
of
−0.66
grths
The
surfacedensity
profile
is
given
by
φ,z
Σ
α
=
8×10
represents
MRI-inactive
disks,
and
α
=
8×10
hat
distributions
of
r,φ
r,φ
g,ini
Σ
Σ
and
activedisks,
respectively.
In (2016),
simulations,of Cwonare
Σg,iniet al.
g
g inSuzukiwhichvalues
are
based
MHD simulations
tside
the
disk
inner
edge
due
−5
&
%
zuki
et
al.
−0.66
represents
MRI-active
disks.
MRI-inactive
disks(2)correspond toﬂatな傾き
uced
by
their
sim.
(2)
.
αon
=
10
'
(
(
'
generallysmaller
than
the
upper
limitsbecausetheparameter
φ,z
−3/2
α
(Suzuki
et
al.
2010;
Bai
2013).
We
consider
two
cases
for
synthesis
calculations
also
Σ
r,φ ;
g
r
−r
円盤風による質量損失(上限値):•
yg,ini−5 2into−4−4by non-ideal
cases
that
take
a(α.deadzone
MHD efΣ
4some−2accountnn-situapointedrelatively
comg,ini
−5=
−3
C
is
constrainedbyenergetics
(see
Figs.
and
6
in
Suzukietal.
In
simulations,aconstant
α
is
used
=
10
We
set
In
some
simulations,aconstant
α
is
used
(α
=
10
).
We
set
α
10
=
1.7
×
10
exp
g
cm
.
(3)
w
formation
of
ar
the
disk
inner
edge
assumφ,zφ,z and αr,φ = 8×10
αr,φ = 8×10
disks,
φ,z MRI-inactive
φ,zni
φ,z represents
kisk
ses(e.g.,
fects.
Here
radially
constant
values
are
inner
edge
due
1
au
30
au
−5
−5 assumed. For the descripΣ2016).
We
usuallyuse
the“strong
DW”
regime
(Eqs.
18
and
19
−5
−5
g,ini
nupper(e.g.,Idaetal.
2013),
while
represents
MRI-active
disks.
MRI-inactive
disks
correspond
upper
limitsonCCtionasC1αw×=, 10
1 ×usually
10and
and
2×
10
for
inactive tow
MRI-inactive円盤:
elofSuzukietal.
limits
on
C
as
=
2
×
10
for
inactive-roducing
•
−4
of
we
use
−4
is
calculations
also
w
w
φ,z
in Suzukietal.
2016),
while
severalsimulations
areperformed
ations,aconstant
α
is
used
(α
=
10
).
We
set
In
some
simulations,aconstant
α
is
used
(α
10 of). CWe
setnsuper-Earths
does
not
show
(2)
cases
that
take
into
account
a
dead
zone
by=
non-ideal
MHD
efφ,z
φ,z
φ,z
φ,z
and
activedisks,
respectively.
Insimulations,valuesarewegas
surfacedensity
at
r
=
1
au
is
ten
times
more
massive
d
inner
edge
assuminds.
They
pointedandactivedisks,
respectively.
In
valuesofCare&values% simulations,
−4
using
the
“weak
DW”
regime
(Eqs.
20
and
21
in
Suzuki
et
al.
w
−5
−0.66
−5
−5
fects.
Here
radially
constantareassumed.
For
thedescripgenerally
smaller
than
the
upper
limitsbecausetheparameterIn
somesimulations,aconstant
α
is
used
(α
=
10
MRI-active円盤:
Σns-etinvestiCas
Cwhile1C×w 10for inactive
upper
limitson
as orderCwand=to12consider
×
and
2disk
× 10
for inactive
φ,z
φ,z
the
MMSN
model
in
early
evolual.
2013),w•
w =−5 10 g2016).
. 2 and 6the(2) −5α,by=upper10nrthssomecases(e.g.,
tionofweenergetics
usuallyuse
ated
the in-situ
formationofαφ,zthe
generallysmallerthanlimitsbecauseparameter
φ,z
−5
C
is
constrained
(see
Figs.
in
Suzuki
et
al.
k
w
does
notinitial
show
Σis
n.
We
note
that
in
this
work
we
lateCofstage
ofplanetks,
respectively.
Insimulations,valuesCareandactivedisks,
respectively.
Insimulations,values
of
C
are
upper
limits
on
as
C
=
1
×
10
and
2
×
10
for
g,ini
−4 considerThegas
surfacedensity
profile
given
by
w
w
iven
disk
w
w
disk
model
of
Suzukietal.
tantis2016).
usedN-body(αby=
10%use ).theset&We
初期ガス面密度:C
constrainedenergetics
(see
Figs.
2
and
6
in
Suzukial.
help
inreproducing
We
usually“strong
DW”
regime(Eqs.
18 andet19
φ,zφ,zl w• isα−0.66
mationandstart
simulations
withplanetaryembryos.
Σyllersimulaendisk
winds.
They
pointed
than
the
upper
limitsbecausetheparameter
generallysmaller
than
the
upper
limitsbecausetheparameter'(( disks,'g whileandactiverespectively.
Insimulations,values
o
−4
−5
−3/2
−5
−5
In
some
simulations,aconstant
α
is
used
(α
=
10
).
We
set
f
in
Suzukietal.
2016),
severalsimulations
areperformed
r
−r
φ,z
φ,z
.DW”
(2)
αφ,z
=10
10thetimen-situformationofcases2016).
We
usuallyuse“strong
(Eqs.
18
and
19
ths.
=
1
×
10
and
2
×
for
inactive4the−2 regime
king
intoaccount
growthoftheembryos,
we
refer
to
ppressedinsome(e.g.,
observed= 1.7
×al.10the(see
exp
gin
cm
. 20
(3)
Σg,ini−5−5positiveな傾き
g,ini
ned
by
energetics
Figs.
2
and
6
Suzukietal.
C
constrainedbyenergetics
(see
Figs.
2
and
6
in
Suzukietal.forbecauses wofΣisgenerallysmaller
than
the
upper
limitsupper
limits
on
C
as
C
=
1
×
10
and
2
×
10
inactive the p
using
“weak
DW”
regime
(Eqs.
and
21
in
Suzukietal.
elSuzuki
et
w
w
1
au
30
au
ch
would
help
in
reproducingnSuzukietal.
2016),
while
severalsimulations
areperformedly.
Insimulations,values
of
C
are
tby
the
disk
evolutionas“initial
(t
=
0)”
in
N-bodysimdeinds.
simr-Earthsisinvesti0 inw
andactivedisks,
respectively.
Insimulations,valuesofC
Theypointed2016).
−4w are2016).
We
usuallyuse
the“strong
DW”
regime
(Eqs.
18
and
19
ally
use
the
“strong
DW”
regime
(Eqs.
18
and
19
C
is
constrainedbyenergetics
(see
Figs.
2
and
6 in Suzw
In
some
simulations,aconstant
α
is
used
(α
=
10
).
We
set
super-Earths.
φ,z
φ,z
ven
disk
The
gas
surfacedensity
at
r
=
1
au
is
ten
times
more
massivetions.
We
use
t
=
0.1
Myr
for
our
standard
model
in
this
using
the
“weak
DW”
regime
(Eqs.
20
and
21
in
Suzukietal.
初期時刻:
0because
limitstheparameter
generallysmaller than
the
upper
limits•etically
drivendisk
nfuppersome
cases(e.g.,
The
initialgassurfacedensity
profile
is
given
by
−5
−5because the parameternSuzukietal.
2016),
while
severalsimulations
areperformed.
2016),
while
severalsimulations
areperformed
se-in
super-Earthsisinvestilimits
on
Cto
as
Cusually=by1early× 10
and2 “strong
×2.4
10 2forinactive2016).
We
use
the
DW”
regime
(Eqs.
1
w
w
than
the MMSN upper
model
in
order
considerdiskevoluofglobalper.
Fortemperature
evolution,we
referreaderstoSectionCisconstrainedenergetics
(see
Figs.
and
6
in
Suzuki
et
al.
help
in
reproducingw2016).
!4
tics
(see
Figs.
2
and
6
in
Suzukietal.
ith
N-bodysimula'(( of'ofmagneticallydrivendisk
andactivedisks,
respectively.
Instagesimulations,values of et
Cwal.
are
−3/2
Weregime
note that DW”
in this work
we consider
late
using
the
“weak
regime(Eqs.
and21
in Suzuki
ak tion.
DW”(Eqs.
20 and21 in 20
Suzukiet planetal.

distributed in a ring-like region between
rmite scheme with a hierarchicentral star. We use rin = 0.1 au and rout =原始惑星同士が衝突したら完全に合体すると仮定• collide, perfect accretion
lanetsmodel. The solid distribution is based on−3nal
density
of
ρ
=
3
g
cm
in Fig. 2. Timetion:
evolution of semimajor axis for disk0 mod• 内部密度:! rconnected"sof a planet.
Σ0 = 15. The filled circles
withsolid lines repre−2= -3/2)
Σd,0 of the linesg indicates
cm , (sthewithplanetary embryos thatauの円環状に分布:
are of particles. Σ• 初期の原始惑星は0.1-2
d =color
The
mass (colo
1 au
between rin and rout from the• r初期は0.1-1地球質量(孤立質量)の原始惑星を20-50個分布させる
where the scaling factor for solid amoun
and
=
2
au
for
our
standardout
Ogiharaal.: Formationof close-insuper-Earths
t no. ogihara_etal_2018
A&A proofs: manuscript no.Masahiro
ogihara_etal_2018
A&A
proofs:etmanuscript
no. ogihara_etal_2018
Masahiro
Ogihara et al.: Formation of close-in sup
slope
(s)
are
parameters.
In Section
3, 0.1
sim
is
used.
The
massesofthesmallest
planetatbased on a power-law
distribu円盤風のない円盤
MRI-active
MRI-inactive
isolationmass(MMiso⊕ ,=rlargestat 2 auwith
are the
0.029
M⊕ and0.27(type
In addition
I migration)
to the due
a-dampingto the (type I migration)
due toplanet
the toplanets
few indicatesruns. The thenumberof initial
particlesislandinteraction
the gas between
disk, weplanets
con- and the gas The
disk, wecon-barcolor
planetarymass.
All plaer
icity
theandtidalinclination.
damping ofRegardeccentricity andRegardWhen
calculating
the isolation
mass,
the
(8)inclination.
bryos
undergorapid
inwardmigration
beforegas
disorces,
the prescription
we use Eqs.
of (38)-(40)damping forces, we use Eqs. (38)-(40)assumedto be
tenMyr.
times
the mutual
planets
after
≃ 0.3
When
planets Hill
get
Tanakais corrected& Wardby (2004)
Ogihara(aettypoal. is corrected byno
Ogiharaet al.remain
Kokubo& Ida
Onfromthe otherhand, iid amount(Σ)factorandthe solid
07))
cording
withtoaEqs.
correction(11)(12)according
to Eqs.star(11)(aand<(12)d,0and0.05au), they
are1998).
removedsimulations
Cresswellplanetswith& Nelsonhigh eccentrici(2008)
planets
with higheccentriciembryos with
M = 0.2 Mif
randomlypon3, simulations
startforwithpro⊕ arethetypeImigrationisproblematic,
Mars-sized
and inclinations.
thegasinitialpower-lawE(Miso = 2πa∆aΣd ) except for a form beforetothe
dispersal
phase.distribution
In cases ofoflarg
particles
is Nand= 100− 400.
articles is typically N = 20−50. isolation massislargerinwardmigration of suc.lid
N-bodydistribution
method and initial solid distribution
mass, the orbital separation is faster, leading to earlier loss of planets onto the sta
es method
are basicallyof N-bodythe same
simulations
as in are basically the same as in
utual
Hill
radius(∆a= 10 r ; that
Marsiswould
have evolution
grown to halfof
its final ma
al.
vious
2017).
studies
Orbital(e.g.,evolution
Ogihara is
et al. 2017).HOrbital
evolution
3.
Orbitalofplanetaryemer hand,
Section4, planetary
Myr(Dauphas & Pourmand 2011). So Mars would hmiteculatedschemeby ainwith
fourth-ordera hierarchiHermite
scheme witha hierarchinets
individual
collide,time
perfectstep.accretion
When planets
collide, perfectaccretion
randomly
distributed
accordingWe seeeven
orbitalof planetary emb
inwardmigration
forevolution
disk0 model.
−3−3
ssumed.
lFig.
densityWeofρassume= 3 g ancm
in Fig.
densityof原始惑星は生き残るρdisk0= 3modelg cm
in Fig. axis
従来のtype
Isemimajor
migration
外側へ軌道移動するものもある
2.
Time
evolution
ofinternal
axis
for
2. of
Time
evolutionof assuming
semimajor
2.
Time
for
disk0
evolution
modelof assuming
semimajor
axis
for disk0
mod
tion
of
Eq.
(8).
The
numberaltereddensity
profiledue
todisk
winds.
Figure3
shows
resultsofsimulations
for
our
stan
erminingaΣplanet.
radiusof aΣplanet.
Thephysicalfilled circles
connected
the size= 15.solid
The lines
filledrepresent
circles connected
Σ0 with= 15.solid
The lines
filledrepresent
circles connected
the size with solid lines repre
0 = 15. the0 withterestedin Thehow
type
Ilinesmigrationismassalteredith
Westart N-bodyembryos
simulations
that
with
embryosof planetary
particles.
The
color
of
thearelines
indicates
the Themass(colorbar).
of planetary
particles.
thearelines
indicatesof particles.
the
mass
color
(colorof bar).
theindicates the(colosofcolortheofthat
MRI-active
case(disk1).
The
evolutionofgas
ributedetween in
rin aandring-likerout fromregionthe between rin andsity
rout forfromdisk1
the is shown
simulations
with
isolation-massemb!5 body
in
Fig.
1(a).
The
surfacedens
tral
d r star.
= 2We
auuse
for rour=standard
0.1 au and r = 2 au for our standard
out

in

out

• 原始惑星の初期面密度を増やすと…
MRI-active

MRI-inactive
外側へ

内側へ
軌道移動

内側へ
軌道移動

!6

•
•
•

model4
disk1
20
hand, results for model1 show that there is nmodel5
disk2
40
ing. The mass-ratio distribution is almost com
円盤風によってtype I migrationが抑制されることがわかった
model6
disk2
20
Fig. 7. Cumulative
distributionsWeof final
orbitalserved distribution.
discuss
theconfiguration
reason forof(c),
first-ordermean-motion
resonances(Mpmodel7disk1
50
rout = 1 au indicate locations
In
panel
cumulative
distributions
ofthe
ガス散逸後の軌道不安定性も考慮し、close-insuper-Earthsのその場形成を調べる
Black solid lines in each panel represent observ
model8disk1
30
rout = 0.5 au distribution.
shown.
Weandfindhere inthat
the planetdisks,massrespec
is la
for
model1,model3,model4
MRI-activemodel9disk1
17rout = 0.3 auof close-insuper-Earths.
This areis simply
power-lawmass
diskmassは80地球質量
based
on the MMSN.
Panels (d)-(f)same a
初期は0.2地球質量の原始惑星を0.1-2auに分布、totalmodel10 disk1
80
solid slope= -1
massforof model2,initial particles
is large
for respectively
model1 (Mindicate resultsmodel5, andmodel6,model11 disk1
80
solid slope = -2
we present results of simulations with smalle

MRI-active

the massMRI-inactive
distribution shifts to smaller mass.

4.1.2. Inactive disk with positive disk slope (Figure 8 shows the result of a simulation in an(see Fig. 1 for disk evolution). As seen in Sec
more aﬀected by migration than in active disk
planets grow to M ≃2極化
5 M⊕ and can undergo
while planets formed at r ! 1 au have massmigrate outward. In the result of Fig. 8, manto the central star. At the end of the simulati
vided into two groups: interior to 0.1 au and e
do not observe such a bimodal distribution i
Earth systems. We see the chaotic nature of N
which causes diﬀerences in final orbital confi
diﬀerent runs using the same disk model. In→ 原始惑星の軌道が不安定になり、巨大衝突が起きる
Fig. 8. As planetsin Fig. 6that
but formodel2in anrMRI-inactive
disk.
Time evolution of semimajor
axis for simulation of close-in•Fig.16.Myr付近でガス散逸
remaininside≃ 1 au at theendsuper-Earth formation that uses model1.
do not undergo significant inward migration.
evolution is more or less similar to that shown• MRI-inactiveでは、中心星へと落下する原始惑星があり、分布は2極化する
Figure 7(d)-(f) shows cumulative distributi
4.1.1. Active disk with flat disk profile (model1)
a wide varietyof planetary
masses disks.
in the Red
observed
configurationsin inactivelines disindvarietyshouldnotbereproducedbyonly one
sep
Figure 6 shows the time evolution of semimajor axis for ourthis
stanoften
runs
of
simulations
formodel2.
The!7 tings. In fact, as is discussed in Section 5.3, planets ob
dard model (model1) in an MRI-active disk (see Fig. 1 fordisk bution and the mass distribution are diﬀerent• Total massを減らすと…
Masahiro Ogihara
et al.:
Formation
close-in super-Earths
Masahiro
Ogiharaet al.: ofFormationof close-in super-Earths
MRI-active
Masahiro Ogihara
et al.:
Formation
close-in super-Earths
Masahiro
Ogiharaet al.: ofFormation
ofMRI-inactive
close-in super-Earths

40地球質量20地球質量

落下しない

Fig. 9. As Fig.
in Fig.
(a) model3
and model4(b),model4
in!8which
9. 6Asbut
in for
Fig.model3
6 but for(a) and(b),thein which
the As Fig.
Fig. 10.
in Fig.
butinformodel5(a) model5
and model6(b) model6
in MRI
10.6AsFig.
6 but for(a) andinitial total mass is decreased.

• 観測との比較 → 様々な円盤モデルを混ぜれば観測を再現できる
A&A proofs: manuscript no. ogihara_etal_2018
MRI-active

MRI-inactive
観測
80地球質量40地球質量20地球質量Fig.
anel7.(a)Cumulative
shows the period
distributions
ratio ofofadjacent
final orbital
pair configuration.
(Pout /Pin ), in which
Panel (a)vertical
shows
lines
the period ratio of adjacent pair (Pout /Pin ), in whichRs).
indicate
Panellocations(b) showsof thefirst-ordermass ratio
mean-motion
Mout /Min . resonances
Panel (c) shows(MMRs).
the planetary
Panel (b)mass
shows the mass ratio Mout /Min . Panel (c) shows the pl
distribution.
distributionsBlackof close-in
solid lines
super-Earths.
in each panel
Red, represent
green, andobserved
blue lines
distributions
indicate resultsof close-in super-Earths. Red, green, and blue lines inforely.model1,
Black dashedmodel3,lineandin panelmodel4(b)inshows
MRI-active
the result
disks,of Ogihara
respectively.
et al.Black(2015a)dashedfor aline in panel (b) shows the result of Ogihara et al.
power-law
anels (a)-(c)diskbutbasedfor MRI-inactiveon the MMSN.
disks.
PanelsRed,(d)-(f)green,areandsameblueaslines
panelsin panels(a)-(c)(d)-(f)but for MRI-inactive disks. Red, green, and blue lines inindicate results for model2, model5, and model6, respectively.

あまり違いがない

あまり違いがない

4.2. Dependence on total mass
4.2. Dependence on total mass
.7.Panel
Cumulative(a) shows
distributions
the period of
ratio
final
of orbital
adjacent
configuration.
pair (Pout /PinPanel), in which(a) showsverticalthe periodlines ratio of adjacent pair (Pout /Pin )Hereweshows
presentofN-bodysimulations,in which
the
Here
total
weshows
present
N-bodysimulations,
in wh
MRs).
cate locations
Panel
(b)
of
first-ordertheresultsmassmean-motion
ratio
Moutresonances/M(c)showsPaneltheplanetary(b)
masstheresults
massofratio
Mout /M
in . Panel(MMRs).
in . Panel (c) shmass ofembryos
reducedfromgreen,
ourstandard
model,
mass
and
ofof
initialembryos
is reducedRed,
fromgreen,
our standard
edibution.
distributions
Black
solid
ofinitial
close-inlines
insuper-Earths.
eachispanel
representRed,
observed
and blue
distributions
lines
indicateclose-inresultssuper-Earths.
and bldiscuss their dependence on final orbital configurations. discuss their dependence on final orbital configuratio
model1,
tively. Blackmodel3,dashedand linemodel4in panelin MRI-active(b) shows disks,
the result
respectively.
of OgiharaBlack
et al.dashed(2015a)line
forina panel (b) shows the result of Ogi
er-laws panelsdisk(a)-(c)basedbutonforthe
MRI-inactive
MMSN. Panels
disks.
(d)-(f)
Red,aregreen,
sameandas bluepanelslines(a)-(c)in panels
but for(d)-(f)MRI-inactive disks. Red, green, and bl
y.cate results
for model2,
model5,model6,4.2.1.
Active disk
with andsmaller
total respectively.
mass (model3, model4)
4.2.1. Active disk with smaller total mass (model3

We see in Fig. 7(c) that the planetary mass in the result of
Wesimsee in Fig. 7(c) that the planetary mass in the reulations
model1 is systematicallylarger than the massulationsof obmodel1 is systematicallylarger than the
4.2. for
Dependence
on total mass
4.2.for
Dependence
on total mass
served close-in super-Earths. We perform N-body simulations
served close-in super-Earths. We perform N-body
withHeresmallermass.
Figureof9(a)and (b)show resultsin
withofwhichtypsmaller
mass.results
Figureof9(a)and (b)simulatio
show rewetotalpresent
results
N-bodysimulations,Herethewetotaltotal
present
N-body!9ical masssimulations
for model3(Mistotreduced= 40 M⊕from) and model4(M
icaltotmass
simulations=model,for model3(Mis= 40 M⊕ )fromand mod
tot reducedof initialembryos
our standardof initial
andembryosourTokyo, Japan; 2 School of Arts & Sciences, University of Tokyo, 3-8-1, Komaba, Meguro, 153-8902 Tokyo, Japan; 3Formationof Universitéthe terrestrial
planetsin the desolarsystemaroundau devia
radial concenLaboratoire
Lagrange,Côte d’Azur,
Observatoire
la Côted’Azur,
CNRS, 1
Blvd
l’Observatoire,CSof Cedexplanetesimals
34229,tration
06304 Nice
4, France
Ogihara1 , Eiichiro
Kokubo1 , Takeru K. Suzuki2 , and Alessandro Morbidelli3
E-mailMasahirocontact: masahiro.ogihara
at nao.ac.jp

37
37

1

Division
Theoretical
Astronomy,
National
Astronomical
Observatoryof solar
Japan,
2-21-1,exhibit
Osawa,a Mitaka,
181-8588
No planets
exist ofinside
the orbitof Mercury
and theterrestrial planetsof thesystemlocalized
con2
Tokyo,According
Japan; Schoolof Arts& Sciences,
Universityof Tokyo, 3-8-1,disks,
Komaba,Meguro,153-8902 Tokyo,
Japan; 3figuration.
to thermal
structure
calculationof protoplanetary
a silicate
condensationline (∼1300
Laboratoire
Lagrange,
Université
Côted’Azur,de lad’Azur, CNRS,
Blvd de l’Observatoire,K) is locatedaround0.1 au fromthe Sunexceptfor Observatoire
the early phaseof Côtedisk evolution,and planetesimals
could haveCS
Nice Cedex
4, France
formed34229,
inside06304
the orbitof Mercury.
A recent study of disk evolution that includes magnetically driven disk winds
contact:masahiro.ogihara
at nao.ac.jp
showedE-mailthat thegas diskobtains a positive
surface density slope inside ∼1 au from the central star. In a region withpositivepressure
undergooutward planets
radial drift.
the radial
drift ofNomidplane
planets exist
insidegradient,
the orbitplanetesimalsof Mercury andthe terrestrialof the We
solarinvestigate
system exhibit
a localized
conplanetesimals
andAccording
type I migrationof planetary
in a ofdisk
that viscouslydisks,evolveswith magneticallydiskfiguration.
to thermal
structureembryos
calculation
protoplanetary
a silicate
condensationdriven
line (∼1300
winds.K)
Weis show
a casein which
planets
remainin theclose-inRadialdrifts of planetesimals
are simulated
locatedaround0.1 auno
fromthe Sunexceptfor theearlyregion.
phase ofdisk evolution,and planetesimals
could haveusing aformed
recentinsidedisk theevolution
model
that A
includesof disk
disk evolution
winds. The
stagemagneticallyof planet formationis alsoorbit ofMercury.
recent eﬀects
study ofthatlate
includesdriven disk
winds
examinedby performing
simulationsof planetary
embryos.
demonstratethat
the middle
stage
of disk
showedthat the gasN-bodydisk obtains
a positive
surface density
slopeWe
inside∼1 au fromthein
centralstar. Ina regionwithevolution,planetesimals
can undergo
convergent
radial drift
in aoutward
magnetorotational(MRI)-inactive
disk, ofpositive
midplane pressure
gradient,
planetesimals
undergoradial drift. instability
We investigate
the radial drift
in whichthe pressureis created,
and accumulate
narrow
inner edge driven
at ∼0.7
planetesimals
andmaximum
type I migrationof planetary
embryos in aa disk
thatring-likeviscouslyregion
evolveswith
withanmagneticallydisk
au from
the Sun.
We aalso
thatnoplanetaryembryos
thatclose-in
may growfromthe narrow
do notwinds.
We showcaseshowin which
planets remainin theregion.
Radialdrifts ofplanetesimalplanetesimalsring
are simulated
exhibitusing
significant
type
I migrationin the lateof diskevolution.
The origin
thestage
localized
configurationa recent
disk
evolution modelthat stage
includeseﬀectsof disk winds.
Theoflateof planet
formationofisthealsoexamined
byofperforming
N-body simulations
planetaryembryos.
demonstratein the bymiddlestage of disk
terrestrial
planets
the solar system,in particularofthe
deficit ofclose-inWe
planets,
can be that
explained
the convergent
planetesimals
undergoradial drift
in a inmagnetorotational
instability (MRI)-inactive disk,
radial evolution,
drift of planetesimals
incan
disks
with aconvergent
positive pressure
gradient
the close-in region.
in which the pressure maximum is created, and accumulate in a narrow ring-like region with an inner edge at ∼0.7
au from the Sun. We also show auから1.5
that planetaryauに集まっており、水星より内側に惑星がいない
embryos that may grow from the narrow planetesimal ring do not
太陽系の地球型惑星は0.38
exhibit significant type I migration in the late stage of disk evolution. The origin of the localized configuration of the
25 deficit of close-in planets, can be explained by the convergent
terrestrial planets of the solar system, in particular the
シリケイトが蒸発するのは1300
radial drift of planetesimals in disks withKでおよそ0.1
a positive pressureauであり、水星の内側にも微惑星があっgradient in the close-in region.

•
•

たはず
25
• 磁気駆動円盤風を考えれば微惑星が外側へと軌道移動する• シミュレーションを用いて水星より内側に惑星ができないことを再現できるか調べた!10• 円盤ガスモデルは先ほどの論文(本資料4ページ目)と同じ• まずはガス抵抗による微惑星のradial driftへの円盤風の影響を調べる
M. Ogihara et al.: Formation of solar• ガス面密度が上がるとMRIのactivityが下がるので、MRI-inactiveを仮定
104• 微惑星同士の重力相互作用、衝突は無視する• 円盤ガスが進化すると、圧力極大が外側へと移動→ 微惑星が細い円環状に集まる• ストリーミング不安定により形成される微惑星は
1 kmより大きい

Solid surface density (g/cm2)• 0.3-3 auに1016 g (3 g cm-3で1 km)の微惑星を置く

3

10

0

1045 yr
10 yr
5

3×10 yr

102
101
100
10-1

→ 微惑星サイズが大きくなるとガス抵抗が効かなくなる 0.2

1
Radial distance (au)5

→ 初期が10 kmより大きい微惑星だと、細い円環状に集まらない•

Fig. 2. Time evolution of solid surface density. Planetesimals
1 km are placed between r = 0.3 and 3 au. The disk is consid
MRI-activeだと円盤ガスの分布はﬂatなので、微惑星は円環状には集まらないが、
MRI-inactive.

radial driftはゆっくりになり、影響は少なくなる

time. Second, mutual interactions between planetesimal!11 back reaction of planetesimals on the gas disk are n

10

•

1

0.2
1
5
10-1 → その後の進化を調べる
円盤風があると微惑星が細い円環状に分布する
Radial distance (au)

100 Myr

103

cm-2)

10

-1

102

10-2

0.7-1 auに0.005地球質量の原始惑星を400個、面密度が一定になるようランダムに置く•g. 2. Time evolution of solid surface density. Planetesimals with R ≃
10

10-3
0.1

km
are placed= 0.3 and
3 au. The
disk is considered to be
1
rrestrial
planetsbetween
withoutrforming
close-inplanets2
初期の軌道離心率・傾斜角は小さく(10 )、巨大ガス惑星(木星など)は置かない
RI-inactive.
Radial distance (au)•1(a) inactive

1

104

104
100 yr

3

10

-1

-1

ガス面密度

102

2

10-2

-2

10

103

10
ガス面密度
. Orbital
evolution of planetary embryos via type I
10

2

-2

migration
10-3

10
1

10

10-3

Eccentricity

Eccentricity

1 Myr

-1

Gas surface density (g cm-2)

-3

1
1 Myr

10

-1

ガス面密度
10-2
10-3

103

103
102
10
1

Gas surface density (g cm-2)

100 yr and theme. Second, mutual interactions between planetesimals
10
10
ack reaction of planetesimals on the gas disk are neglected.
ガス面密度
When solid particles accumulate in a narrow ring, where 10the10
ust-to-gas ratio is close to unity, the back reaction on the 10gas
sk should
be important. The evolution in Fig. 2 is therefore1 an
10ealized result. We will investigate these eﬀects in future works.

(b) active

1
10

ow we examine the late stage of planet formation
100 Myr
100from
Myr plan101010
ary embryos.
As we showed in the previous subsection, plan10
1010
esimals can accumulate in a narrow-ring region. We therefore
10
10 the subsequent evolution for the initial embryo distribuonsider
0.46 au
10
100.56a auon. Hansen (2009) adopted
localized configuration for the ini11010
al embryodistribution and performed N-body simulations. 1We
0.1
1
10
0.1
1
10
se the same initial conditions as Hansen (2009). As an initial
Radial distance (au)Radial distance (au)
ondition (b)ofactive
N-body simulations, 400 planetary embryos with
10 1
ass M 1黒丸、青丸(>= 0.005 M⊕ are randomly
placed between 0.7 andFig. 3. Snapshots of the system for MRI-inactive disk (a) and MRI0.1地球質量)の大きさは原始惑星サイズを反映
yr eccenu according to a uniform surface density. Their 100
initialactive disk (b). The filled circles represent the size of particles. When
10
icities10and inclinations are set to be small (≃ 10−2 ). Although particles grow to more massive than 0.1 M⊕ , they are indicated by filled
赤丸は初期を孤立質量にしたときの計算の最初と最後の状態
ansen (2009)
considered the presence of Jupiter, we do not10in- blue circles. The red lines indicate the gas surface density (right axis).
10 giant planets in our simulations.
The red circles represent the initial and final orbital configurations ofude any
10from isolation-mass protoplanets.
For the disk evolution, as we stated in the previous section, it !1simulations
2
3

3

-1

-1

2

2

-2

-2

-3

-3

•

4

3

•

-1

2

-2

1

Gas su10-3

Yuseoung,
Daejeon34055, Republicof Korea; 7 NAOJ 10Chile Observatory, National Astron. Obs. of Japan, 2-21-1
E-mailcontact:frederique.motteat univ-grenoble-alpes.fr
Écolenormalesupérieure,
F-75005,
Inst.fürdeRadioastronomie,RadioAstronomieAuf
Millimétrique(IRAM),
300Bonn,rue de l
8Paris, France
Osawa,
Mitaka,Tokyo
181-8588,
Japan;
Max-Planck-Inst.
dem
Hügel
69,
53121
The
unexpectedly
large
proportionofhigh-mass
star-forming
cores
in
a
GalacticminiUnderstanding
the processes
thatdeterminethestellar11Initial
Mass Inst.,
Function(IMF) isaCologne,
critical unsolved
problem,with
Piscine,F-38406
Saint
Martind’Hères,
France;I.
Physik.
Universityof50937
Köln,
Germany9Germany;
LERMA, for
Obs.
de Paris,
PSL
Research University,
CNRS,
Sorbonne
Universités,
UPMC
Univ.
Paris 06,
starburst
profoundimplications
manyareas ofastrophysics.
Inmolecular
clouds,stars
areformedincores,
gas
condensations
10
E-mailcontact:frederique.motteat 3univ-grenoble-alpes.fr
École normale
supérieure,
F-75005,
Paris,
FranceInst.
Millimétrique300
rueclutch
de2 ,laQ.
1,2
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4 de RadioAstronomie
5
4 (IRAM),whicharesuﬃciently
dense
that
gravitational
collapseconvertsalarge
fraction
of
their
mass
into
a
star
or
small
F. Motte , T. Nony , F. Louvet , K.A.
Marsh
,
S.
Bontemps,
A.P.
Whitworth,A.
Men’shchikov
11
Piscine,F-38406
Saint
Martind’Hères,
France;I.massPhysik.
Inst., (CMF)
Universityof Cologne,
Germany
6,7
8
2
9 Function
5,10
2
Understanding
the ,processes
that determine
thestellarInitialMass(IMF)
is, 50937
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criticalunsolved
problem,
NguyenLuong
T. Csengeri, A.J.
Maury, A.
Gusdorf, E.isChapillon
Könyves, P.suggesting
Schilke11wit,
of stars.
In nearbystar-formation
regions,
the corefunctionstrikingly
similarto Köln,
the
IMF,

34
34

2
2 In molecular clouds, stars are formed in cores, gas condensation
profoundimplications
for Didelon
many
areas
ofM.
astrophysics.
A.
Duarte-Cabral
P.
GaudelE-mailcontact:frederique.motteat univ-grenoble-alpes.fr
that
the
shape
of
the IMF4 , may
simplybe&inherited
fromthe CMF. Here we present 1.3 mm observations, obtained
suﬃciently
densethat gravitational
converts
a large fractionof their massinto
aGrenoble,
star
small
clutc
1which are
with
ALMA,
largestinterferometer,of collapse
theInitialactivestar-formation
regionwhichmayorbemore
Univ. theGrenoble
Alpes,
CNRS,
Inst. thede stellar
Planétologie
etd’Astrophysiquede Grenoble,
France;Understanding
theworld’s
processes
thatdetermine
Mass
Function (IMF)
is W43-MM1,
a criticalF-38000
unsolved
problem,withInthenearbystar-formation
regions,core
massfunction(CMF)
is strikingly
similarto theGif-sur-Yvette
IMF, suggestin
2of stars. ofrepresentative
Galactic-disk
regions
where the
most
form.
The
unprecedented
resolutionof these
observations
Paris-Saclay/Dépt.
d’Astrophysique,
CEA,
CNRS,
Univ.
Paris
Diderot,
CEA-Saclay,
F-91191
profoundAIM
implications
for many areasof astrophysics.
Instars
molecular
clouds,stars
are formedin cores,gas condensations
3of the4 is markedly
that
the
shape
IMF
may simply
beCMF
inherited
from
the CMF.
wethatpresent
1.3ofmmobservations,obtainereveals,
forsuﬃciently
first time,a thatstatisticallyrobustatconverts
highmasses,aHere
slope
shallower
thantheFrance;Dept.
of Astronomy,
Univ.
deChile,
Las
Condes,Santiago,
Chile;
SchoolAstronomy,
which Cedex,
are
dense
gravitational
collapsea largewith
fractionof
their massinto Physics
a starorand
small
clutchwith seriously
ALMA,
the
world’slargestinterferometer,of origintheactivestar-formation
region d’Astrophysique
W43-MM1, which may
be mor
IMF.
This
challenges
ourunderstanding
theof3AA,the
IMF.
Cardiﬀ
Univ.,star-formation
QueensBuildings,
The
Parade,
CF24
UK;is5 strikingly
OASU/Lab.
Bordeaux,of stars.
In nearby
regions,
thecoreofCardiﬀ
massfunction(CMF)
similar to the IMF,desuggesting
6
representativeof theGalactic-disk
regionsFrance;
where moststarsAstronomy
form. Theand
unprecedented
resolutionof Daedeok
these observation
Univ.
CNRS,
Korea
Space Science
Inst.,
776
daero,
that theshapeof theAstronomy
IMF
mayF-33615
simply Pessac,
be inherited
from
the
CMF.
Here
we
present
1.3
mm
observations,obtained
Acceptedby Bordeaux,Nature7
reveals, forDaejeon
the first34055,
time, aRepublic
statisticallyrobust CMF
atChilehigh masses,with aNationalslope thatis markedly
than thYuseoung,of Korea;
NAOJ
Observatory,
Astron.
Obs.
ofshallower
Japan,
2-21-1
with
ALMA,
the
world’slargestinterferometer,oftheactivestar-formation
region
W43-MM1,
which
may
be
more
8
http://arxiv.org/pdf/1804.02392
IMF. This
seriouslychallenges
ourunderstandingof the origin
ofRadioastronomie,
the IMF.
Osawa,
Mitaka,Tokyo
181-8588,
Japan;
Max-Planck-Inst.
für
Auf dem ofHügel69,observations
53121 Bonn,representative of9the Galactic-disk regions where most stars form. The unprecedented resolution
these
Obs.
de Paris,
PSL CMF
Research
University,
Universités,
UPMC
Univ.thanParis
06,
Accepted
byLERMA,
Naturereveals,Germany;for the firsttime, aAstronomy
statisticallyrobustat10high
masses,CNRS,
with aSorbonne
slope thatis markedly
shallowertheÉcole normale supérieure, F-75005, Paris, France
Inst. de RadioAstronomie Millimétrique (IRAM), 300 rue de la
IMF. This
seriouslychallenges
ourunderstandingoftheoriginof the IMF.
LayersintheCentralOrion
Nebulahttp://arxiv.org/pdf/1804.02392
Piscine, F-38406 Saint Martin d’Hères, France; 11 I. Physik. Inst., University of Cologne, 50937 Köln, Germany
1
Acceptedby Nature
AstronomyC.
R. E-mailO’Dellcontact: frederique.motte at univ-grenoble-alpes.fr
1
http://arxiv.org/pdf/1804.02392
Layersofin
theCentralOrion
NebulaDepartment
Physics
and Astronomy,
Vanderbilt
University,
37235,
USA problem, with
Understanding
the processes
thatdetermine
the stellar
Initial Box
Mass1807-B,
FunctionNashville,(IMF) is aTN
criticalunsolved

35
implications
for many areas of astrophysics. In molecular clouds, stars are formed in cores, gas condensations
C.
R. O’Dell
E-mailprofoundcontact:
cr.odell at vanderbilt.edu
35which are suﬃciently dense that gravitational collapse converts a large fraction of their mass into a star or small clutch
1

1 in the Central Orion Nebula
LayersDepartmentof Physics
Astronomy,
Vanderbilt
Box 1807-B,
The
existenceof multiple
layersandin theinner Orion
NebulaUniversity,
has been revealed
usingNashville,data fromTN
an37235,
Atlas USAof spectra atof stars. In
nearbystar-formation
regions,
the
core
mass
function(CMF)
isstrikingly
similartothe
IMF,
suggesting
−1
1
2”
and
12
km
s
resolution.
These
data
were
sometimes
groupedover
Samples
of
10”
×10”
to
producehigh
SignalC. R. that
O’DellE-mailat mayvanderbilt.edu
thecontact:
shape ofcr.odell
the IMF
simply be inherited from the CMF. Here we present 1.3 mm observations, obtained
toNoise spectra and sometimes grouped into sequences of pseudo-slit Spectra of 12.8” – 39” width for high spatial
1
with
ALMA,
the
world’slargestinterferometer,of theactiveBox
star-formation
regionwhichmayofbemore aThe studies.
existenceof multiple
layerssystems
in theinner
Orion
Nebulahas
beenrevealed
usingW43-MM1,
datafrom(MIF),
an AtlasspectraDepartmentof Physics
andvelocity
Astronomy,
Vanderbilt
University,
1807-B,
Nashville,TN37235,
USA
resolution
Multiplewerefound:
V
tracesthe
Main
Ionization
Front
V
arisesMIF form. The unprecedented resolution of these observations
scat−1
representativeof
theresolution.
Galactic-disk
regions
where
most stars
2”
and
12
km
s
These
data
were
sometimes
groupedover
Samples
of
10”
×10”
to
producehigh Signa
E-mailcontact:
cr.odellatvanderbilt.edu
fromback-scatteringofV
emissionbyparticlesinthebackgroundPhotonDissociation
Region(PDR),
V
is an
MIF
low
reveals,
the first
time,
a statisticallyrobustat highwith Spectraa slope thatis markedly
shallower
thantheto Noiseforspectraandsometimes
groupedintoCMF
sequencesof masses,
pseudo-slitof 12.8”– 39” widthfor high
spatiaionized
layer
in
front
of
the
MIF
and
if
it
is
the
sourceofthestellarabsorption
lines
seen
in
the
Trapezium
stars,it
IMF.
This
challenges
ourinnerunderstandingof found:thehasoriginof revealed
the IMF. using data from an Atlas of spectra at
The existenceof seriously
multiple Multiple
layers invelocity
theOrion were
Nebulabeen
resolution
studies.
systemsV
MIF traces the Main Ionization Front (MIF), Vscat arise
must
lie12
between−1the foreground Veil and those stars, Vnew,[O III] may represent ionized gas evaporating from the Veil2” andkmsresolution.
These
data were sometimes grouped over Samples of 10” ×10” to produce high Signal
fromback-scatteringof V
Acceptedby
NatureAstronomy
MIF emission by particles in the background Photon Dissociation Region (PDR), Vlow is a
away
from
the observer.
There arefeaturessuch
as the BrightBar where
variationsof velocities
are dueto changing
to Noise
spectraandsometimes
groupedintosequencesof pseudo-slit
Spectraof 12.8”
– 39”
width
for
high
spatialionized
layer
in
front
of
the
MIF
and
if
it
is
the
sourceofthestellarabsorption
lines
seen
in
the
Trapezium
stars, i
http://arxiv.org/pdf/1804.02392
tilts
of
the
MIF,
but
velocitychanges
above
about
25”
arise
from
variations
invelocityofthebackground
PDR.
In
resolution
Multiplevelocity systems
werefound:
tracesthe
Main
Ionization
Front(MIF),
V
arisesscatmuststudies.
lie between
the foreground
Veil andthosestars,VVMIF
may
represent
ionizedgas
evaporating
from
the
Ve
new,[O III]afrom
region
25”
ENE
of
the
Orion-S
Cloud
one
finds
dramaticchanges
in
the
[O
III]
components,
includingthesignals
back-scattering
VMIF emission
byfeatures
particlessuchin thebackgroundPhoton(PDR),
Vlow
anaway from the ofobserver.
There areas theBright Bar
whereDissociation
variations ofRegion
velocities
are due
to ischangin
fromthelayer
V in front
and
VMIF,[Obecoming
equal,
indicating
shadowingof gas lines
fromseenstellarof greaterthanionizedof butthe
MIF III]and
if it isNebulathesourcethe arisestellarabsorption
in photons
theTrapezium
stars,
it I
tilts low,[Oof theMIF,
velocitychangesabove
aboutof25”
fromvariations
in velocityof thebackground
PDR.
LayersinIII]
theCentralOrion
24.6
This featureis also seenVeil
in areas
to thestars,
west Vand south oftherepresent
Orion-S Cloud.
musteV.
lie
betweentheENEandCloudthoseevaporatingfrom thearegion25”
oftheOrion-S
one
finds
dramaticchangesin theionized[O III] gas
components,
includingtheVeilsignalnew,[OIII] may
1 foreground
C. R. O’Dellaway fromtheobserver.
featuressuch as theBrightBar where
variations
offromvelocities
due toofchanging
Accepted
by
MNRAS
from
the
Vlow,[O III]Thereand Vareequal,
shadowingof gasstellararephotons
greater tha!13indicating
MIF,[OIII] becoming
1
Department of Physics and Astronomy, Vanderbilt University, Box 1807-B, Nashville, TN 37235, USA

35

38
38

39

39
39
39

39

8
Observatoryof Japan,National
InstitutesofNaturalSciencesNorth
A’ohoku
Hilo,
HI| 96720,
Yuseong-gu,
Daejeon34113,
Korea;
GeminiObservatory,
Casilla603,
La 650
Serena,Chileobservations
twoarcseconds
southwestof VLA
2. We foundthat(NINS),the previously
detected
FeIIPlace,jet with
|VLSR
> 100
5
−1
USA;
Schoolof MathematicalandPhysical
SOKENDAI
Graduate
University
forMultiple
Advanced
Studies),
High-resolution
Spectralmappingwith
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II]
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of
Outflows
km s contact:driven hyoh
byVLA
3B is also
detectedin Science,Hand confirm
that
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has
a position
angle about240◦ .
2 emission,
2 andE-mailatnear-IR
kasi.re.kr
6 ′′Hayama,240-0193,
Department
Observatory,
The
Universityof Arizona,
Spectra ofKanagawa
the redshiftedknots Japan;
at 14′′ −65
northeast ofof Astronomy/Steward
LkHα 234 are presented
for the first
time.
These spectra
alsoaround
LkHα
234
7
−1
We
presentahigh-resolution,near-IR
spectroscopic
studyof
multipleoutflows
in
the
LkHα
234
star
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region933
North
CherryTucson,
AZ
USA;
Korea
of 2Science
andGajeong-ro,provideclues
to1,2,3
theAvenue,
existenceof multiple
outflows.
We detected
high-velocity(50−120
kmTechnology,s ) H23,6
gas217in themultiple
4,5 85721,
1 University
Heeyoung
Oh,
Tae-Soo
Pyo,
Bon-Chul
Koo,
In-Soo
Yuk
,
Kyle
F.
Kaplan,Yong-Hyun
Lee1 ,
8 Spectrometer (IGRINS). Spectral mapping over the blueshifted emission
−1
using
the
Immersion
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Yuseong-gu,
DaejeonGemini
CasillaChileoutflows aroundLkHα34113,
Since thesegasesObservatory,move
at speeds
welloverLatheSerena,dissociation
velocity (> 40 km s 2,7), the3 234. Korea;
32 603,
2
KimberlyR.
Sokal,
Gregory
N.
Mace
,
Chan
Park
,
Jae-Joon
Lee,
Byeong-Gon
Park,WeNarae
HH
167 allowed
us to distinguishatjetleast
three
separate,
spatially
overlapped,
outflows Also,in H2position-velocity
and [Fe II] emission.
emissionmust
originate
fromtheitselfrather
than
H
gas
in
the
ambient
medium.
diagrams2
2contact: hyoh at kasi.re.kr
83
E-mailHwang,the
HwihyunKim
andthatDanielT. Jaﬀeshow
H2 diagram
emission
represents
notemission
a singlejet, butcomplexmultipleoutflows
by threephenomena,
known embedded
andthatexcitation
indicatefromknot
C in HH
167 come
fromdriven
two diﬀerent
shocks−1
present
a high-resolution,near-IR
spectroscopic
study ofthe LkHα234<starformation
1 We
sources:
MM1,
VLA2, andVLA
3. Thereis a redshiftedH
outflowoutflows
ata lowinvelocity,
VLSR+50
km 08826,s , region
with
2multiple
andphotodissociation.
DepartmentofPhysics
andAstronomy,
Seoul
National
University,
1 Gwanak-ro,
Gwanak-gu,
Seoul
Korea; 2−1
using Astronomy
theImmersion
INfraredSpectrometer
Spectralmapping
the34055,
blueshifted
emissionofrespect
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Korea
andGRating
Space Science
Yuseong-gu,
Department
AcceptedbyApJ
HH 167 allowed
us to distinguishat least
three2.
separate,
spatially
overlapped,in FeII
H2 andII]|Vemission.
Weobservations
twoUniversity
arcseconds
southwest
ofAustin,
VLA
We foundthatthepreviously
detectedjet [Fewith| > 100
4 outflows
LSRAstronomicalof Astronomy,
of
Texas
at
Austin,TX
78712,
USA;
SubaruTelescope,
National
https://arxiv.org/pdf/1804.01673
show
theby
H2VLA
emission
not ainsingle
jet, but complex
multipledrivenby threeangle
known
embeddedkm
s−1 thatdriven3B isrepresents
also detected
H2 emission,and confirm
that outflows
this jet has
a positionabout240◦ .
Observatory of Japan, National Institutesof Natural Sciences (NINS), 650 North A’ohoku Place, Hilo,
HI 96720,′′ Theresources:
VLA 2, knots
and VLAis a redshifted
at a lowforvelocity,+50 kms−1 , also
withSpectrathe redshifted
at 143.
−65′′ northeastof LkHαH234
are presented
the firstVtime.
spectra2 outflow
LSR <These
5 of MM1,
USA;
SchoolofMathematicalandPhysicalScience,
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Graduate
University
forAdvanced
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respectclues
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= −11.5We
kmdetected
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provideto theexistenceof multiple
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Hayama,Kanagawa
240-0193,
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ofAstronomy/Steward
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New placesandphasesoftheseCO-poor/Ci-richmoleculargas
inObservatory,
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observations
twoarcseconds
southwestofDepartment
VLA
2. We
found
that
the
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detected
FeII
jet
with
|V
|
>
100
outflows
aroundLkHα234. Since
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move
at speeds
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km
s
),
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7
933
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CherryAvenue,Tucson,AZ
85721,USA;
Korea
Universityof
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217
Gajeong-ro,
1,2,3
6,7 jet has a position angle about 240◦ .
km
s−1 must
drivenby VLAfrom
3B isthealso
detectedinandconfirmthat
thisPadelisP. Papadopoulos, Thomas
G.HthanBisbasZhiyu
Zhang
emissionoriginatejetitselfrather
H24,5gasandin theambient
medium.
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at
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presented
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C in HH
167
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Astrophysics,
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Universityof Thessaloniki,−1
provideclues tothe existenceof multiple
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detected high-velocity(50−120s ) HEfesiou
multiple2
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at kasi.re.kr
Thessaloniki,
GR-54124,
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for Astronomy,
Academy ofAthens,km
Soranou
GR-11527,−1
outflows
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andspectroscopic
Astronomy, Cardiﬀ
University,
Queen’s
Buildings,
The Parade,
Cardiﬀ,
CF24
Acceptedby
ApJ
We
presentahigh-resolution,near-IR
studyof
multipleoutflows
in
the
LkHα
234
star
formation
emissionmust
originate fromthe jet itself
rather thanH2 gas inCharlottesville,
the ambient medium.
Also,
position-velocity
diagramsregion
4
5
3AA,
UK;
DepartmentofAstronomy,
Universityof
Virginia,
VA
22904,
USA;
Max-Planck-Institut
using
the Immersion
GRatingINfraredSpectrometer
Spectralthe phenomena,
blueshifted shocks
emission of
https://arxiv.org/pdf/1804.01673
andexcitation
diagramindicatethat emissionfromknot(IGRINS).
CGarching,in HH 167
come mappingfrom
two overdiﬀerent
6
für
Extraterrestrische
Physik,Giessenbachstrasse
1,
D-85748
Germany;
Institutefor
Astronomy,
University
HH
167
allowed us to distinguish at least three separate, spatiallyoverlapped, outflows in H2 and [Fe II] emission. We
andphotodissociation.
7ofEdinburgh,Royal
Observatory,
Edinburgh,
EH9
3HJ,
UK;
EuropeanSouthern
Observatory,
show that the H2 emission represents not a single jet, but complex multiple
outflows
driven byHeadquarters,
three known Karlembedded
Acceptedby
ApJ
Schwarzschild-Strasse
2,D-85748,
Garchingbei
München,GermanyNewplacesof CO-poor/Ci-richmolecular
gasat inthevelocity,
Universe
sources:
MM1,and
VLAphases
2, and VLA
3. There is a redshifted
H2 outflow
a low
VLSR < +50 km s−1 , with
1,2,3
4,5 s−1 , that coincides6,7
https://arxiv.org/pdf/1804.01673
E-mail tocontact:
padelis atauth.gr
respect
thesystemic
velocityof VLSR G.
= −11.5
PadelisP.
Papadopoulos, Thomas
Bisbaskm
and Zhiyu Zhang with the H2 O masers seen in earlier radio
twoarcseconds
southwestof VLAdiscovered
2.Astronomy
We foundthat
the Rayspreviously
detected
FeIIthejetwith |V
1observations
LSR | 2> 100Inthis work we
theSection
workon
recentlyrole ofCosmic(CRs)
inregulating
CO/H
Departmentof extend
Physics,
ofthe
Astrophysics,
andMechanics,
Aristotle
University
ofaverage
Thessaloniki,
−1
◦
2
km
s
driven
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that
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jet
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angle
about
240
.
abundanceratio
inmolecular
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thus
their
CO
line
visibility)instarburst
galaxies,
and
find
that
it
can
lead
2
Thessaloniki,
GR-54124,
Greece;ResearchCenterfor
Astronomy,
AcademyofAthens,Soranou
Efesiou4,
GR-11527,
New places and phases of CO-poor/Ci-richmolecular
gas
in
the
Universe′′3
to a CO-poor/Ci-rich
phase
even
in ′′environments
Galacticor presented
in only
modestlyenhancedCRbackgrounds
Spectraof the redshifted
knots
at 14
−65
northeast4,5
ofwithLkHα
234 arefor the
first
time.
These
spectraAthens,Greece;SchoolH2ofgas
Physics
University,
Queen’s
Buildings,
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Parade,Cardiﬀ,
CF24 also
1,2,3 and Astronomy, Cardiﬀ
6,7
PadelisP.
Papadopoulos
ThomasG.
Bisbasand
Zhiyu
Zhang astro-chemistry4
expected
inDepartment
ordinarystar-forming
galaxies.
Furthermore,
theCharlottesville,same
CR-driven
raisesprovideto the existenceof, multiple
outflows.
We detected
high-velocity
km 5s−1) H2 thegas possibility
in the multiple
3AA,
UK;cluesof Astronomy,
Universityof Virginia,
VA (50−120
22904, USA;
Max-Planck-Institut
1of a widespread phase transition of molecular gas towards a CO-poor/Ci-rich 6phase in: a) molecular gas outflows
Department
Physics,
SectionAstrophysics,
Astronomy
andAristotleof(>Thessaloniki,
outflows
aroundofLkHα
234.
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wellMechanics,
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40
km s−1 ), thefürExtraterrestrische
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D-85748
Garching,
Germany;
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forvelocity
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University
2 active galactic nuclei (AGNs),
7 in andfound
inmuststar-forming
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Athens,Soranou
Efesiou
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emissionoriginate
from
the
jet
itself rather
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medium.
Also, position-velocity
diagramsofEdinburgh,Royal
Observatory,
EH9 than
3HJ,
UK;
Southern
Observatory,
Headquarters,
Karl2 gasEuropean
3of powerful radio galaxies. For main sequence galaxies we find that CRs can render some of theirradio-loudcores
Athens,Greece;Schoolof Physics
andemission
Astronomy,
Cardiﬀ
University,
Queen’s
Parade,phenomena,
Cardiﬀ, CF24
andexcitation
diagramindicate
that
from
knot
C in HH 167
comeBuildings,
from twoThediﬀerent
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bei München,
Germany4
526
molecularmass CO-invisible,
compounding
theof Charlottesville,
low metallicities.VAImaging
the twoMax-Planck-Institut
fine structure lines
3AA,
UK; gasDepartmentof Astronomy,
Universityof eﬀects
Virginia,
22904, USA;andphotodissociation.
E-mailcontact:
padelisatauth.gr6
of atomic
carbon withPhysik,
resolution
high enough to 1,
searchbeyondthe Ci/CO-brightregionswithcentralfürExtraterrestrische
Giessenbachstrasse
D-85748
Garching,
Germany; line
InstituteforassociatedAstronomy,
University
Accepted
by
ApJ
7
Inof
this
work wetheon therecently discoveredroleof European
Cosmic
Rays
(CRs)
in
regulating
theaverageCO/H
starbursts
canextend
revealObservatory,
suchworka CO-poor/Ci-richmolecular
providedthat
relativebrightness
sensitivity
levelsEdinburgh,Royal
Edinburgh,
EH9 3HJ, gas
UK;phase,
Southern
Observatory,
Headquarters,
Karl2
of Tb (Ci 1ratio− 0)/TJ=
1 clouds− 0)∼0.15
reached.
Thelinecapability
to search
for such
gas in theis nowat handabundanceinb(CO
molecular(andare
thus
their
CO
visibility)
in starburst
galaxies,
andGalaxyfind thatit canlead
Schwarzschild-Strasse
2,D-85748,
Garchingbei
München,Germany
https://arxiv.org/pdf/1804.01673
withthecontact:
new high-frequency
surveytelescope
HEAT deployedin Antarctica
andmodestly
future ones
to be deployedin DometoE-maila CO-poor/Ci-rich
H2 gasphase
evenin environmentswith Galactic
or in only
enhanced
CR backgrounds
padelisat auth.gr
A. ALMA
can searchfor such gas
in star-forming
spiral thedisks,
galactic
molecular
gas outflowsraises
and the CR-intense
expectedin ordinary
star-forming
galaxies.
Furthermore,same
CR-drivenastro-chemistry
possibilityIn
work
extendthe workonrecentlygas
discoveredrole
ofobjects.
Cosmic Rays
(CRs)
regulating
the average
CO/H2
New
placesand transition
phasesofCO-poor/Ci-richgas
in inthegalactic
and wecircumgalactic
gas-richenvironmentsofradio-loudofa thiswidespreadphaseof themolecular
towardsa molecularCO-poor/Ci-rich
phase
in:
a)Universe
molecular
gas outflows
abundance ratio in molecular1,2,3
clouds (and thus their CO 4,5
line
galaxies, and find that it can lead
!14 visibility) in starburst
6,7
Acceptedby
MNRAS
PadelisP.
Papadopoulos,
ThomasG.
Bisbas
and
Zhiyu
Zhang
to a CO-poor/Ci-rich H gas phase even in environments with Galactic or in only modestly enhanced CR backgrounds

40
40

41
41

filamentary structure. Previous observations used
to study these distributions have been limited by two important
Universidad de Chile, Casilla 36-D, Santiago, Chile; 6 Department of Physics, State University of New York at Fredonia,
observational(1)
sensitivity
limits protostars
that leavethesources
undetected,
orCambridge,(2) resolution
7
Distributionof Serpens
Southrevealed
ALMA
Fredonia,factors:
NY 14063,
USA;
Harvard-Smithsonian
Centerforlowest-mass
Astrophysics, with
60 Garden
Street, MS 78,
MA limits thatcannot02138,
distinguishbinaries
and/or cluster members in close proximity.
USA
1
Adele L. Plunkett, Manuel Fernndez-López2 , Héctor G. Arce3 , Gemma Busquet4 , Diego Mardones5 ,Methods.
Recentmillimeter-wavelengthinterferometry observations can now uncover faint and/or compact sources incontact:
at 6,7
eso.org
and E-mailMichaelM. aplunket
Dunhamorder to study a more complete population of protostars, especially in nearby (D < 500 pc) clusters. Here we present
Aims. We investigated the masses and spatial distributions ′of pre-stellar
and protostellar candidates in
1
2 the young,′EuropeanSouthern
Observatory,
Av.
AlonsodeCórdova
3107,
Vitacura,
Santiago,
Chile;
Instituto
Argentino
ALMA
observations
of
1
mm
(Band
6)
continuum
in
a
3
×
2
regionatthecenterofSerpens
South. Our
angularde
low-mass star forming region Serpens South, where active star formation is known to occur
alongapredominant
3
Radioastronoma,
Plata(CONICET),1894,
Elisa,
Argentina;
Departmentof Astronomy,
Yaleresolutionof ∼1′′structure.
isCCT-La
equivalent
to observations∼400 au, corresponding
to Villascalesof envelopes
and/ordisks
of protostellar
sources.
filamentary
Previous
usedC.C.5,
to study
these
distributions
have been
limitedby twoimportant
University,Box
New 1Haven
CTleave
06520,
USA;
Institutde Ciències
Campusobservational
factors:(1) sensitivity
limitsthe lowest-masssources masses
undetected,
or de(2) l’Espai
resolution
limits that
Results.
We P.O.
detect52 208101,
sourceswithmm thatcontinuum,
andwe4 measureof 0.002–0.9
M⊙(IEEC-CSIC),
corresponding
to gas5
cannotbinaries envelope
and/ormembersin close proximity.
UAB,
Carrerde disk
Can and/or
Magrans,
S/Ncluster
E-08193,
Cerdanyola
delVallès,For
Catalunya,
Spain;
Departamento
Astronomı́a,and
dust
in distinguish
theof theprotostellar
system.
the deeply
embedded(youngest)desources
with
6observations can now uncover faint and/or compact sources in
Recentmillimeter-wavelength
Universidad
deChile,
36-D, Santiago,
Departmentof Physics,
State Universityof New Yorkat Fredonia,no
IR Methods.
counterparts,
weCasilla
find evidence
ofinterferometry
massChile;
segregationand clustering
according
to: the Minimum
Spanning
Treeorder to study a more complete
population of protostars, especially in nearby (D < 500 pc) clusters. Here we present
7
Fredonia,
NY 14063,ofUSA;
Harvard-Smithsonian
Centerfor Astrophysics,
60 Garden Street,
MS 78, Cambridge,MA
method,distribution
projected
separations between
uniquesources, and concentrationof higher-masssources near
ALMA observations of 1 mm (Band 6) continuum in a 3′ × 2′ region at the center of Serpens South. Our angular02138,
USA gastotheresolution
densecluster center.
of at∼1′′theis equivalentto ∼400 au, corresponding to scales of envelopes and/or disks of protostellar sources.
Conclusions.
The
mass
thecontinuum,
mm sources
is measure
likely primordial
rather M
thandynamical togiven
Results.
We
detect52 segregation
sourceswith 1ofmm
and wemasses of 0.002–0.9
gas the young⊙ corresponding
E-mailcontact:
aplunketat eso.org
in thecompareddisk and/orwith
envelopeof the protostellar
system.
Forfirst
the case
deeplytoembedded(youngest)with
age ofandthisdust
cluster,segregation
time. Thisis theshow thisfor mmsources
sources
in a low-mass
Aims.no We
investigatedspatialdistributionsof pre-stellar
protostellar
candidates
IR counterparts,
wethe
findmasses
evidenceandof mass
segregationand clustering
accordingand
to: the
Minimum Spanning
Treein the young,protostellar
clusterenvironment.
method,distribution
projected
separations
betweenuniquesources,
concentrationof higher-mass
low-massstar
forming ofregionSerpens
South,
where
activestar andformationis known
to occursourcesalongneara predominant
Accepted
A&A
to thebydense
gas at thecluster center.
filamentary
structure.
Previous
observations used to study these distributions have been limited by two important
Conclusions.
The
mass
segregation
the mmlikelyprimordial sources
rather than
dynamical or
given
young limits thatobservational factors: (1) sensitivity oflimitsthatsources
leave isthe
lowest-massundetected,(2) theresolution
http://arxiv.org/pdf/1804.02405
age of this cluster, compared with segregation time. This is the first case to show this for mm sources in a low-mass
cannotdistinguish binaries and/or cluster members in close proximity.
protostellar cluster environment.
Methods. Recent millimeter-wavelength interferometry observations can now uncover faint and/or compact sources in
6
Accepted by
A&A
StockerRoad,
Exeter,EX4 4QL, UK;
Huntingdon
Institutefor
X-raypc)
Astronomy,
Circumstellar
Disk
Lifetimes
In DevonNumerous
Galactic
Stellar
Clusters
orderUniversity
to studyofaExeter,
more
completepopulationof protostars,
especiallyinYoung
nearby(D< 500clusters.LLC,
Here we present
10677
FranksRoad,
Huntingdon,
PA
16652,
USA
1 continuum in a 3′1 × 2′ region at the
1
4
ALMA
observations
mmGetman(Band 6)
Serpens
South.
Our angularA.
J. http://arxiv.org/pdf/1804.02405
W.
Richert1 , of
K.1 V.
, E. D. Feigelson , M. A. Kuhn2,3 , center
P. S. ofBroos
, M.
S. Povich, M.
′′ gkosta at astro.psu.edu
E-mailcontact:
5 of
6 ∼400 au, corresponding to scales of envelopes and/or disks of protostellar sources.
resolution∼1G.
isP.equivalent
R.
Bate
and
Garmireto
Photometricdetectionsof dustcircumstellar
disks around pre-main
sequence(PMS)
stars,
coupled withof
Circumstellar
Lifetimes
In Numerous
Galactic
Young
StellarWe detect
52Disksourceswith
1 mmcontinuum,
and we measure
massesof Clusters
0.002–0.9
Mestimatesto gas⊙ corresponding
1Results.
2
Pennsylvania
State
University,
University
ParkPA
16802,
USA;
Universidad
deValparaiso,
Gran
Bretana1111,
stellarin
ages,
provideon the 1time
available
for planet
formation.
Most
previous embedded
studies
on disk
longevity,
1constraints
1 system.
1
4and dust
thedisk and/oroftheprotostellar
For2,3the(youngest)
with
A.
J. W.
Richert, K.
V.envelope
Getman, E.
D.
Feigelson,Astrophysics,
M. A. Kuhn
, P.deeply
S. Broos, M. S. Povich, M. sources
3
Playastarting
Ancha,
Valparaiso,
Chile;
Millenium
Instituteof
Av.
VicunaMackenna4860,
782-0436
Macul,
with
Haisch,Lada&
Lada(2001),
usestar
samplesfrom
PMS
clusters
but
donotconsiderdatasetswith
6
R.counterparts,
Bate5 andG.we
P. find
GarmirenoIRevidenceof mass segregation
andclustering
according
to:Pomona,the
Minimum
Spanning
Tree
45
homogeneous
photometricsensitivities
and/or ages placedon a uniform
timescale.
Here weconduct
the largest
studySantiago,
Chile;
California
State
Polytechnic
University,
3801
West
TempleAve,
CA
91768,
USA;
1
2sources, and concentration of higher-mass sources nearmethod,distributionof University,
projected
separations
betweenuniqueState
University
Park
PA 16802,
USA;
Universidad
Valparaiso,fromGran
to Pennsylvania
dateof the longevityof inner dust
disks using
X-ray
and 1–8
micrometre
infraredde
photometry
theBretana
MYStIX1111,
and
3
Playa
Ancha,
Valparaiso,
Chile;
Millenium
Instituteof Astrophysics,
4860, 782-0436
Macul,
to thedense
gas atthe69cluster
center.
SFiNCsprojects
foryoungclusters
in 32 nearby
star-forming
regions Av.
withVicuna
ages t ≤Mackenna
5 Myr. Cluster
ages are derived
4
5
Santiago,
Chile;
California
Statemethod
Polytechnic
University,
3801
West
TemplePomona,91768,magnetic
USA;bycombiningthemass
empirical
AgeJX
PMS
evolutionarymodels,whichAve,
treat
dynamo-generated
Conclusions.
The
segregationof thewithmmsourcesislikelyprimordial
ratherthanCAdynamical
given the young
27is thefieldsdiﬀerent comparedways. Leveraging
data to time.
identifyThis
disk-freeobjects,
imposesimilarstellarage ofthisincluster,with X-ray
segregation
first wecase
to show
thisfor mass
mm sensitivity
sources in a low-masslimits forcluster
disk-bearing
and disk-free YSOs while extending the analysis to stellar masses as low as M ∼ 0.1 M⊙ . We
protostellar
environment.

41

find that the disk longevity estimates are strongly aﬀected27
by the choice of PMS evolutionary model. Assuming a disk
fraction
100% at zero age, the inferred disk half-life changes significantly, from t1/2 ∼ 1.3 − 2 Myr to t1/2 ∼ 3.5 Myr
Accepted
byofA&A
when switching from non-magnetic to magnetic PMS models. In addition, we find no statistically significant evidence
http://arxiv.org/pdf/1804.02405
that disk fraction varies with stellar mass within the first few Myr of life for stars with masses < 2 M⊙ , but oursamples may not be complete for more massive stars. The eﬀects of initial disk fraction and star-forming environment
are also explored.
!15

Circumstellar Disk Lifetimes In Numerous Galactic Young Stellar Clusters3

UK; Department of Physics and Astronomy, Swarthmore College, Swarthmore, PA 19081, USA; Department of
Physics
and Astronomy,
Vanderbilt
University,
Nashville,
TN 37235, USA; 9Architecture
Department of Physics,
University,
Multiple
StellarFly-Bys
Sculpting
the Circumstellar
in RWFisk
AurigaeNashville, TN 37208, USA; 101 Joint ALMA Observatory,
AlonsoVitacura, Santiago,
Chile;
1
2,3 de Crdova 3107, 763-0355
45
JosephE.
Rodriguez,
Ryan
Loomis,SylvieCabrit,ThomasJ.
Haworth,StefanoFacchini,
Cather11
I.R.A.M.,
300 rue de la Piscine, Domaine Universitaire, F-38406 Saint Martin dHres, France
ine Dougados3 , Richard A. Booth6 , Eric L.N. Jensen7 , Cathie J. Clarke6 , Keivan G. Stassun8,9 , William

42
42

10
E-mailF.R.
contact:
cfa.harvard.edu
Dentjoseph.rodriguez, Jérôme Petyat11,2
1
Harvard-Smithsonian
CenterBand
for Astrophysics,
60 Garden
MA 02138,
USA; 2 Sorbonne
We present
high-resolution ALMA
6 and 7 observationsof St,
theCambridge,
tidally disrupted
protoplanetarydisks ofUniversité,the RW
Observatoire
deobservations
Paris, Université
CNRS, LERMA,
F75014
France;Univ. Grenoble
Alpes,
Aurigaebinary. Our
revealPSL,
the presenceof additional
tidalParis,
streams
to the3 previously
observed
tidalCNRS,
arm
4
IPAG,
38000A.Grenoble,
France;Astrophysics
Group,
Imperial
College London,
Blackett
Prince Consort
aroundRW Aur
The observed
configurationof tidalstreamssurrounding
RW AurA andLaboratory,
B is incompatible
with
5
Road,
LondonSW72AZ, UK;
Max-Planck-Institutfür Extraterrestrische
Physik, Giessenbachstrasse
1, D-85748
a singlestar-disk
tidal
encounter,suggestingthat the RW Aurigae
system has undergone
multiple fly-by interactions.
6
Garching,
Germany;
Institute
Astronomy,
University
Madingley
Cambridge,
CB3with0HA,
We alsoresolve thecircumstellar
disksofaround
RW AurA and ofB, Cambridge,
with CO radiiof 68 auRoad,and 38au consistent8
UK; 7 Department
Physics
and Astronomy,
Swarthmore
Swarthmore,
PA 19081,
tidal truncation,and 2.5oftimes
smallerdust emission
radii. TheCollege,disks appear
misalignedby 12◦USA;
or 57◦ Department. Using newof
9
Physicsobservations
and Astronomy,
University,
Nashville,
TN 37235,
Department
Physics,
Fisk
University,
photometric
fromVanderbilt
the American
Associationof Variable
Star USA;
Observers(AAVSO)ofand
All Sky
Automated
Nashville,
TN37208,
USA; 10 Joint
ALMA
Observatory,
AlonsodeGroup
Crdova3107,
763-0355
Vitacura,
Santiago,
Chile;
SurveyforSuperNovae(ASAS-SN)archives,
we
have
also
identified
anadditional
dimming
event
of
the
primary
that
A
Cavityof
Large
Grainsinthe
Disk
AroundtheII
Herbig
Ae/Be
Star
HD
11
la Piscine,
DomaineUniversitaire,
F-38406
Saint Martinobservations,dHres, Francewe are beginning to
began
inI.R.A.M.,
late 2017300
andrueis decurrently
ongoing.
Withover a century
of photometric142666contact:
explorethe same
spatialscales as2 ,ALMA.
1 joseph.rodriguez
A.
E. E-mailRubinstein, E. Macias
C.atC.cfa.harvard.edu
Espaillat2 , K. Zhang1 , N. Calvet1 and C. Robinsin2

We present
by ApJhigh-resolution ALMA Band 6 and 7 observations of the tidally disrupted protoplanetary disks
1Accepted
2 of the RW

Departmentof Astronomy,
University
ofinMichigan,
1085Around
S. University
Ave.,
Ann Arbor,
MI 48109,
USA;Star
DepartA
Cavityof OurLarge
Grainsreveal
the
Disk
the
Group
Ae/Be
HD
Aurigaebinary.
observations
the presenceof additional
tidal
streamsII
to Herbig
the previously
observedtidalarm
http://arxiv.org/pdf/1804.09190
mentofAstronomy, Boston University, 725 Commonwealth Ave., Boston, MA 02215, USA
142666around RW Aur A. The observed configuration of tidal streams surrounding RW Aur A and B is incompatible with12
1
2
E-mailA.
arubinstein96
at gmail.com
E. Rubinstein, E.
Macias,suggesting
C. C. Espaillat
K. Aurigae
Zhang1 ,system
N. Calvet
and C. Robinsin
acontact:
singlestar-disk
tidal
encounter,that the2 ,RW
has undergone
multiple fly-by
interactions.
also resolve
circumstellar
aroundRWGroup
Aur
andB, with
CO
radii
of
68
auMI
and
38 auUSA;consistent
with
2
Departmentof theAstronomy,ofMichigan,
1085AIS.or
University
Ann
Arbor,
48109,
DepartHerbig1We
Ae/Be(HAeBe)stars
haveUniversity
beendisksclassified
into
Group
II,Ave.,which
wereinitially
thoughttobeflaredtidal
truncation,
andBoston
2.5
times
smallerI725
dust
emissionradii.Ave.,
TheBoston,disks
appearmisalignedby 12◦ orongoing57◦ . Usingnewmentof Astronomy,
University,
CommonwealthMA02215,
USAand flatdisks,
respectively.
SeveralGroupsourceshave beenshown
to havelarge
gaps,
suggesting
planetphotometricobservations
American
Association
Star
Observers
Automated
formation,
while
no
large
gaps fromhaveatthebeenfound inthe disks ofofVariable
Group II
sources.
We (AAVSO)
analyzed andthe AlldiskSkyaroundtheE-mailcontact:
arubinstein96
gmail.com
SurveyforSuperNovae(ASAS-SN)archives,
we
have
also
identified
anadditional
dimming
event
of
the
primary
thatGroup II source, HD 142666, using irradiated accretion disk
modelingofthebroad-band
spectralenergydistribution
28
HerbigAe/Be(HAeBe)have beenclassified
intooverGroup
I or GroupII, which were
initially thought
be flaredto
began inlate 2017
and stars
is currently
ongoing.
Witha centuryof photometricobservations,
we are tobeginningalong with the 1.3 millimeter spatial brightness distribution traced by Atacama Large Millimeter and Submillimeterandflat thedisks,
respectively.
SeveralGroup I sources have been shown to have large gaps, suggesting ongoing planet
exploresame
spatial scales
as ALMA.
Array (ALMA) observations. Our model reproduces the available data, predicting a high degree of dust settling information,
while
gaps have been found in the disks of Group II sources. We analyzed the disk around the
Accepted
by
ApJno large
the disk,which
isconsistent
with
Group
II classificationof HD
142666.
In addition,
thespectral
observed
visibilities
andGroup II source, HD 142666, theusingirradiatedaccretion disk
modelingof thebroad-band
energydistribution
synthesized
image
only be reproduced
when including
a traceddepletionof large grains
out to ∼16
auSubmillimeterin our disk
http://arxiv.org/pdf/1804.09190
along
with
thecould
1.3 millimeterspatial brightness
distribution
by Atacama
Large Millimeterandmodel,Array
althoughthe ALMA
observations
did not
have enoughangular resolution
to fullya resolve
the innerparts
of thein(ALMA)
observations.
Our model
reproduces
the available
data, predicting
high degreeof dustsettling
disk. These
resultssuggest thatdisks IIaroundGroup of
II HD
HAeBe
starsInhave
cavities
large grains
as well.
the disk,
whichmay
is consistent
with somethe Groupclassification
142666.
addition,the ofobserved
visibilities
andFurther
ALMA observations
Group
II sources areneededto discern
how commonly
cavitiesofsynthesizedimage couldofonly
be reproduced
when
includinga depletionof large grains
out occurto ∼16inauthis
in class
our disk
objects,
as wellas to reveal
their observations
possible origins.
model,
althoughthe ALMA
did not have enough angular resolution to fully resolve the inner parts of the
disk.byThese
Accepted
ApJ results may suggest that some disks around Group II HAeBe stars have cavities of large grains as well.
!16 28 to discern how commonly cavities occur in this class ofFurther ALMA observations of Group II sources are needed
https://arxiv.org/pdf/1804.07343.pdf

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