THE STAR FORMATIONNEWSLETTER
No. 275 (#41-45)
塚越崇(茨城大)27 Nov. 2015

1. V899 Mon: An Outbursting Protostar With Peculiar Light Curve And
Its Transition Phases
2. Impact of supernova and cosmic-ray driving on the surface
brightness of the galactic halo in soft X-rays
3. How do giant planetary cores shape the dust disk? HL Tau system
4. Variability and dust filtration in the transition disk
J160421.7-213028 observed in optical scattered light
5. Episodic molecular outflow in the very young protostellar cluster
Serpens Southquiescent

V899 Mon: An Outbursting Protostar With Peculiar Light CurveAnd Its Transition Phases
Outburst of V899 Mon
J.P. Ninan et al.

• V899 Mon長期間モニター• FUor/EXor型変光星(d~905pc)• 最初のバースト(2009)~二回目の

1st

7

2nd

Figure 3. Light curve of V899 Mon showing its first outburst, short quiescentcircles are R-band magnitudes from our observations and blue circles are CRTS
POSS-2 epochs’ R magnitudes are also shown for comparison as black squares.

バースト(2012)• photometry & spectroscopy

Figure 3. Light curve of V899 Mon showing its first outburst, short quiescent phase and current ongoing second outburst phase. Red
circles are R-band magnitudes from our observations and blue circles are CRTS magnitudes converted to R magnitudes. POSS-1 andPOSS-2 epochs’ R magnitudes are also shown for comparison as black squares.

• 2m-HCT & 2m-IGO• UBVRI, JHK• SALT HRS• opt. high resolution spec.

1st• GMRTQ• 1280 MHz continuum imaging• non detection• Herschel• WISE

2nd

Figure 4. Positions of V899 Mon in the J-H/H-K CC diagram
during the quiescent phase (black circle), first outburst (red circle)
and the second outburst phase (green squares and blue triangles).
The solid curve shows the locus of field dwarfs, and the dash-dottedcurve shows the locus of giants (Bessell & Brett 1988). The dottedline represents the locus of classical T-Tauri (CTT) stars (Meyer
et al. 1997). The diagonal straight dashed lines show the reddening
vectors (Rieke & Lebofsky 1985), with crosses denoting an AVdi↵erence of 5 mag. Typical error bars of each data point are
shown in the bottom right corner.

Figure 5. NIR J/J-K color magnitude diagram showing the
movement of V899 Mon during its quiescent (black circle), first outburst phase (red circle) and second outburst phase (green squares
and blue triangles). The arrow shows the reddening vector (Rieke& Lebofsky 1985), which corresponds to an AV of 3 mag. Typicalerror bars of each data point are shown in the top right corner.

the temperature of the source during those epochs weredi↵erent than the ongoing second outburst. However,since CV RI is a weighted di↵erence between two colors
and could not tell unambiguously whether the intrinsic

Transition phaseが赤い=>バーストに関係する物質は、
初期はcoldで徐々にhotになる。
=>中心星ではなく円盤起源(かも)10Ninan et al.

Figure 6. V -band light curve of V899 Mon showing evolution of its V-R and V-I colors. Color of the outer ring shows V-R and the color
at the center shows V-I. We see both the colors were reddest during the transition from the quiescent phase to the outburst phase.

• 90umより短波長はfit可能•

Robitaille+2007• FIR超過の起源は不明~12K, ~12M⦿相当
Figure 7. V , R and I light curves of V899 Mon (circles, squares and triangles respectively), color-coded with the extinction invariant
color CV RI .

3.2. Stellar Properties

V899 Mon was observed in WISE 12 µm and 22 µm
bands on 2010 March 17, within one month after our NIR
observations in J, H and K bands from HCT on 2010or an early Class II YSO (Greene et al. 1994) during its
peak outburst phase.
U -B, B-V , V -R and R-I colors of Siess et al. (2000)
isochrones can be used to constrain photometrically theOutburst of V899

• quiescentで質量降着率↓

only
apert
whet
bidde
durin

1st

• Mass loss rate
• Lbolから導出=1x10-7 M⦿/yr• [OI]から導出=2.6x10-7 M⦿/yr• Outburst phaseでHa P-Cygni
14=>
outflow activity↑

Ninan et al.

2nd

Q-phase(a) Emission component

Q-phase1st

2nd
Figure 16. Relative change in accretion rates estimated fromvarious lines during the transition from the first outburst phase to

Flu
lines
perat
ratio
by co
V899
of de
II]
671
an es
The
dens
Ferla
Mon
to 20
2⇥10
On
other
stanc
(2006
( 63
temp
tio [C
a tem
But t
a tem
To b

• 短いQ-phaseについて• 円盤不安定性モデルで考えると円盤物質をreplenishするには短すぎる•

円盤物質が減る前に降着を止める機構を考える?

•

1stと2ndで増光メカニズムが違う?

• Q-phaseでP-Cygniが消える=>magnetic accretion funnel絡み• V899はFUorかEXorか• バースト期間はEXor的 (Q-phaseは短め)• 放射/吸収を示すスペクトル =>FUor - EXorのtransition phase• Lbolや質量降着率もFUor - EXorのtransition phaseImpact of supernova and cosmic-ray driving on the surface brightness of the galactic halo in soft
X-raysThomas Peters et al.

• Milky Way halo - 起源は不明のhot diffuse plasma• X線強度~ 0.5-7 x 10-12 erg cm-2
• モデルは様々だが観測の輝度を再現出来ていない• 超新星爆発と宇宙線のfeedbackを入れた計算• SILCC projectのsimulation結果の一つ•

詳細な初期設定はWalch+2015やGirichidis+2015など

5How do giant planetary cores shape the dust disk? HL Tau system
Giovanni Picogna and Wilhelm Kley
Picogna, Wilhelm Kley: How do giant planetary cores shape the dust disk?
Tauのような多重リング構造を2つの微惑星で作る• HLGiovanni• FARGOによる計算• initial setup
1

0.1

1.5

2

2.5

3

1 Mth
5 Mth
10 Mth

1.6
1.4
/ 0

• planetParameter • 25/50Range
AUに置く
Planet mass [Mth ]1, 5, 10
• 0.07-0.7M
Dust size [cm]0.1, 1, 10,J 100• 降着なし、軌道変化なし

1

1.8

1.2

log

els

0.5

r [25 au]drift velocity profile at• theサイズ分布あり
equilibrium for the di↵erent
modelled.

• フラットな分布

1 Mth
5 Mth
10 Mthlog / 0• gas
• powar low Σ, T
• kepler rotation• viscosity α=0.004• dust• 250000 Lagrangian particles• spherical particle

100 orbits

1
0.8

wz=(∇xV)z

0.6
0.4

0.5

1

1.5

2
r [25 au]

2.5

3

ticles follow closely that of the gas.
惑星質量が大きい時
reasingly• larger
gaps. The dm parti- (0.7MJ)el) have cleared almost completely
ガス分布
e a stopping •timecloser to one nearheir evolution is faster.
• ギャップで渦度ピーク

e (5Mth )•spiral armに沿って渦度も分布

単一惑星の時より物質が集まりやすい• up
et should still open
a gap in thelonger timescale,since from eq. (3)• ダスト分布2.

•co-orbital regionに残るのはm-sizeのみ•

planet間のリングは細い(5:3軌道共鳴軌道)

igure 3 (first panel) we can see thatcm-sizeでvortexが見やすい• theble gap opened byinner planet,nt
planetary
cores
shape
the
dust disk?
->リングが細くなるtimescaleと関係
llower than the massive
cores
case,
econd panel). The outerplanet still
m-sizedof the inner one (Figure 10), but its
has has barely modified the unperution at its location.
e by the outer planet is less dramaticve case, the reduction of the surface
inders the development of vortices

planet carves a gap in the dust disk
icles sizes (Figure 11). Instead, thes able to clean its gap only for them and m), while it takes 300 orbits

mm-sized

0.7MJ

Fig. 4. Gas surface density (top panel) and vorticity distribution (bottom
panel) at the end of the simulation for the massive cores case.

planet with the vortices enhance the eccentricity of the dust particles trap into it, favouring their escape and thus depleting thesolid concentration inside the vortex.
The capacity of collect particles by a vortex is closely linked
to its orbital speed. If a vortex has a Keplerian orbital speed, thendust particles with the same orbital frequency will remain in thevortex for many orbits and slowly drift to its centre due to dragforces. On the other hand, a particle in a vortex orbiting witha non-Keplerian frequency will experience a Coriolis force inthe Keplerian reference frame and, if the drag force is unable tocounteract it, the particle will leave the vortex location (Youdin

0.35MJ

cm-sized

0.07MJ

cm-sized• 惑星質量が中くらいのとき(0.35MJ)• やや浅くなるがガスgapを生成• 内側では容易にgap生成、外側ではsmall
grainのgap生成に時間がかかる• 大きいダストではclumpingが見える• 惑星質量が小さいとき(0.07MJ)• clearなガスgapが見えない• 大きなダストでは短時間でgapが生成される。cm-sizeは時間がかかる

In the HL
Tausystem,althoughseveralrings
haveplausible
been obnear
infra-red(NIR)emission.
One ofthe most
explato solve thisitissue
the apresenceof multiple
giantrateplanets
served in itsnation
dust emission,
has isstill
very highaccretion
6
can2.13
createa commonand thus enhance
the accretion
onto the starthat
Ṁ =
⇤ 10
M /yrgap(Robitailleet al. 2007).
This rate
acrossthemexchanging
torque
with
the
disk,
while
depletingis a prove that, at least in this system, the rings observed in the thedust component, through a filtration mechanism that, together
dust emission
are not related to rings in the gas distribution.
with dust growth, can explain the absence of a strong NIR emisSince wesion
foundthattransitionala wide ringobserved
in disks
our simuin (pre-)disksiscomparedto full(Zhu et al.
lations only 2012).
for the
small
mass
case
and
a
clear
gap
visibleFor a full review of the topic see Espaillat is
et al.
(2014)
for the outer planet
in system,
the intermediate
and rings
massive
In the only
HL Taualthough several
have core
been observed
in
its
dust
emission,
it
has
still
a
very
high
accretioncases, we choose to run a di↵erent model with an inner small rate
onto
star Ṁ= 2.13 ⇤ 10 6mass
M /yrcore(Robitailleet al.to2007).
mass core andantheouterintermediatein ordercom-This
is
a
prove
that,
at
least
in
this
system,therings
observedin thethe outcome of our simulations with the gap’が見える
HL Tau system.
‘wide’pareringが見える軽い惑星と‘clear
dust emission are not related to rings in the gas distribution.
We rescaled theSince
systemand runwe foundthataadi↵erent
wide ringsimulation
is observed inin orderour simuto compare itlations
to theonly
realforone,
thecaseinner
32.3
the placing
small mass
andplaneta clearatgap
is au
visible重い惑星の場合のcombination
corresponding
D2planet
gap (see18 - top panel)and thecore
for tothetheouter
onlyFigurein the intermediate
and massive
we keeping
choose tothe
run2:1a di↵erent
model iswith
an innerouter one at cases,
64.6 au,ratio, which
close
to thesmall
mass
core
and
an
outer
intermediate
mass
core
in
order
B5 location. Comparing the 2D surface density distributiontoatcom32.3AUと64.6
AUpare
the outcomeof theour deprojected
simulations with
the in
HLthe
Tauconsystem.
the end of thesimulation
with
image
We rescaled the system and run a di↵erent simulation in ordertinuum emission and their slices (Figures 18-19) we can outline Fig. 18. Top panel: deprojected image from the mm continuum of HL
to compare it to the real one, placing the inner planet at 32.3 auseveral sharedfeatures anddi↵erences.
gap18createdby thecorresponding
to theD2 gap (seeThe
Figure- top panel)and theTau. Bottom panel: cross-cuts at PA=138 through the peak of the mm
inner planet outerhas aoneveryat similar
configuration
as
the
one
observed.
64.6 au, keeping the 2:1 ratio, which is close to thecontinuum of HL Tau ALMA Partnership et al. (2015).
On the otherB5
hand
there Comparing
are no clearthevisible
featuresinsideits or- at
location.
2D surface
density
distribution
the
end
of
the
simulation
withthedeprojected
imagein thebit in the observed imaged while a variety of inner structures
areconand their slices(Figures18-19)arewemainly
can outline Fig. 18. Top panel: deprojected image from the mm continuum of HLvisible in thetinuum
outputemissionof the simulation.
These
featuresseveralsharedfeaturesanddi↵erences.
The
gap
createdby the Tau. Bottom panel: cross-cuts at PA=138 through the peak of the mmdue to the inner wave generated by the planet. The strong gap
inner planet has a very similar configuration as the one observed. continuum of HL Tau ALMA Partnership et al. (2015).
that is visible
close to the star is instead not physical and it is
On the other hand there are no clear visible features inside its orrelated to thebitinnercondition.
the outerpartof the are
外側惑星位置近辺で少々違いあり
in the boundaryobserved imaged
while aInvariety
of inner
structures
disk, severalvisibledi↵erences
can ofbethe
oulined.
TheThesemajor
one isin the output
simulation.
featuresarethemainlyhigh surfacedue
density
thewavehorseshoeregion,is related
to the ininnergeneratedby the whichplanet. The
strong gap
horseshoeregionで柱密度大
isto the star
not distribution.
physical and it is
to our choicethatofanvisible
initialclose
flat profile
for istheinstead
particle
related
to
the
inner
boundary
condition.
Inthepart of the
Although this approximation was chosen to extend theoutersimulateddisk,
severaldi↵erencescanbeoulined.
The
major
one itis thetime preventing a fast depletion of material from the outer disk,
highsurfacedensityinthehorseshoeregion,which
isrelateddust
filtrationによるstrong
depletion
also favoured
the dust trapping by the outerplanet. Moreover, theto our choice of an initial flat profile for the particle distribution.
particle ringAlthough
is more thisdepleted
than
in
the
observed
image.
approximation was chosen to extend
theThus,simulated
we expect thattheplanetary
mass
responsiblefortheobserved
time preventing a fast depletion of material from the outer disk, it
円盤の質量(柱密度)を減らした計算でもconsistentouter gap should
be slightly
smaller
than
one adopted
in this thealso favoured
the dust
trappingby thethe outerplanet. Moreover,particle
is moredepletedthan
in the observed
image.
simulation. A
final ring
remarkis thestrongdepletionof dustparti-Thus,
weexpectthattheplanetary
mass
responsiblefortheobserved
cles just inside the outer planet location due to its dust filtration
outer
gap
shouldbeslightly
smaller
than
the
one
adoptedin thismechanism, which is clear from the bottom panel of Figure 18.
simulation. A final remark is the strong depletion of dust partiDue to this e↵ect,ininsidea multiplanetarysystem,a planet
is notcles justthe outer planet
location
due to its
dust necfiltration
essary located
where
the
gap
is
deeper
but
it
could
be
at
the
rim 18.
mechanism, which is clear from the bottom panel of Figureof the gap preventing
theparticlesofacertain
size
to
cross
itsnecDue to this e↵ect, in a multiplanetary system, a planet is not• 内側に軽い惑星,外側に重い惑星で再計算••• gap構造などはよく似ている
•

•
•

•

Variability and dust filtration in the transition disk J160421.7-213028 observed in opticalscattered light
P. Pinilla et al.

• 遷移段階円盤J1604 (145pc)• VLT/SPHERE/ZIMPOLのR’バンド観測• HiCIAO(H-band)と同じ構造を検出• サブミリ波よりピークが内側• rZIMPOL/rALMA~0.65• 5-10MJの惑星• dipの位置が移動している• 12.3 deg/yr• 60AUのケプラー回転では合わない=>内側の構造変化(影など)• MIRでの変動と関連しているかもFig. 1. R0 band (0.626 µm) VLT/SPHERE/ZIMP

intensity (P I), polar-coordinate Stokes parametershows that we had an optimal correction for the inlinear and in arbitrary units. The dashed lines in t
azimuthal profile is calculated in Fig. 3 to distingueast) of 85 . A tentative second dip was suggeof 255 .
This letter is organised as follows. In Sect. 2
the observations and data reduction. The mainEpisodic molecular outflow in the very young protostellar cluster Serpens South
Adele L. Plunkett et al.

• CARMA-7•

Serpens South (415pc)• ALMA cycle 1, Band6•

CO, 13CO, C18O J=2-1• CO: molecular outflow•

ノット構造
南北で同数(PV参照)•

速度↑でopening angle↓•

ほぼplane of the skye

• C18Oおよび連続波=> outflow+envelope

Episodic outflow in Serpens South

Offset from center (parsec)
0

18

R10
R9
R8

12

R7
R6

-6

-12

-18

15
10

3
2
1

R3

0

0
0.0 0.5 1.0 1.5 2.0 2.5∆τdyn (sin i/ cos i) (×103 yr)

0
6
12
18
24
Offset from center (arcsec)

R1

2.5

B4
B5
B6
B7
B8
B9
B10
B11

vc
-10

4

20

5

R2

protostar
B1
B2
B3

(d)

0.9′′
370 AU

0
10
20−1
VLSR (km s )

30

(c)
8
6
4
2
0

∆τdyn (sin i/ cos i) (×103 yr)

0

(b)

R5
R4

τdyn (sin i/ cos i) (×103 yr)

Offset (arcsec)

6|Vf low |(km s−1 )R115

N (ejecta)

(a)

25

0.012 0.024 0.036 0.048

0
6
12
18
24
Offset from center (arcsec)

(e)
2.0
1.5
1.0
0.5
0.0

0 1 2 3 4 5 6
τdyn (sin i/ cos i) (×103 yr)

9• ∆TdynとTdynの間に相関(Tdyn<3000yrのところ)• 平均∆Tdyn~310yrs => short period modeのジェット生成メカニズム• 複数knot構造の要因• (若い)高速ジェットとremnantとのinteractionによるshock• drag-induced momentum loss =>星周環境にturbulent motionを励起• C18Oエンベロープは回転+infallだがズレが残る
さらなる高分解能観測でjet launching point+disk formation解明へ