The Star Formation Newsletter#308, 41-50
島和宏 (京都)

41

https://arxiv.org/abs/1807.01429

Mass [MJ]

M⊕
2.1453.3
2825S555.9
1km0.01
93.61M ⊕M⊕
2.272528
00.1
0.2
multiple planetarysystem の観測例：633S
1089.02M ⊕6M⊕
1.37
27.0
23 km
230
しかし、太陽系に似てる (内側に岩石惑星、外側にガス惑星) 観測はまだない
S710
10
km
0.01
120.91M
1⊕M⊕
2.66
62.4
23
20
100m− fmigI=0100m− fmigI=0.01
S863.610km
0.1S2 134.66M ⊕S0M ⊕ この研究の目的
2.75
2334
110∗
S932.8km zone24での岩石惑星0116.44M ⊕phaseにおける100habitableM⊕
1.49post-gas
22−110∗ habitable plantes;(potentiallyPHPs)と水の含有量の進化S
100km
0.0168.88M ⊕M⊕
1.41
29.1
1928
10−2156.55
F
195.30226.431271.84
S
164.40141.881010−3 (paper 1, ガスが無くなるまで計算)
gas-phase model−410 0 isothermal discs, without
radial 1Dmodel,
gravitational 0.2
interactions
0.1
0.5
0.6

F

10−5

原始惑星
(dry)

m − fmigI=00S
10 S5 16

ガス惑星

=0.01
100m−− ffmigI010km
migI=0.01

1S72

S1010−110−110−210−2−310−3−41010−4−51010−510110100110100km=0.01
10km −− ffmigI
migI=0Semimajor−axis[au]*SS106氷型惑星

Σp [g cm−2]

原始惑星
(icy)
Mass [MJ]− fmigI=01
10 1km10km−ffmigI=0100m=0− f−migI
=0.01
migI

微惑星の面密度10fmigI=0.01
10010km −Semimajor−axis-> N-body simulation [au]に切り替え

S7−111S

mass remotion
原始惑星のうち~ 50 % -> 中心星~ 35 % -> ejected~ 23 % -> 他の原始惑星

微惑星のうち~ 11% -> 中心星~ 89 % -> ejected~ 0.3 % -> 他の原始惑星

HZ class A

微惑星のサイズが小さいときにPHPができやすい(他のパラメータより、微惑星のサイズが一番結果に影響する)

微惑星のサイズ

微惑星のサイズが小さいときは
water-rich の PHP になる42

https://arxiv.org/abs/1807.09815

43

https://arxiv.org/abs/1807.06680

44

https://arxiv.org/abs/1807.09134

45

https://arxiv.org/abs/1806.07397

46

https://arxiv.org/abs/1807.07334

47

https://arxiv.org/abs/1807.03499

low-mass young stellar objects (Class I-II YSOs)-> steady mass accretion では 星の質量・光度を説明できない-> episodic mass accretion のはず
FU Orionis objects (FUors)-> the most active accretion outbursts (~1000 倍上昇)
研究の目的
outburst の機構は何か？

Takami et al.

FU Oriarcnear-IR
HiCIAOtailスバル望遠鏡
PDI modeare marked as *A*, *A’*, *B*, and *C*.

V1057 Cyg

10

Takami et al.

Near-Infrared Imaging Polarimetry of FUors
9Figure 3. Same as Figure 2 but for V1057 Cyg observed at H-band (1.65 µm). In the PI image Z
in theleft, we show the black
CMaV1735
Cyg
contours near the central source with arbitrary scales to clarify the small arc-like structure marked as *B*. We show PI⇥R2images in the middle and the right, and the white regions in the right image show the distribution of optical emission observed
by Herbig et al. (2003) using the Hubble Space Telescope.

change considerably. This is due the fact that the subtraction of polarized halo was not perfect in Paper I(Appendix B).
3.4. Z CMa (Figure 5)
The PI images obtained in the J-, H-, and K-bands(1.25, 1.65 and 2.2 µm, respectively) show (A) a brightemission component extending to the south to ⇠0.00 4
from the star; and (B) an elongated structure in thesouth at a ⇠200 scale. These have been shown throughprevious near-infrared imaging and imaging polarimetry(Millan-Gabet & Monnier 2002; Canovas et al. 2015, ;Paper I). As reported in previous publications, its position angle from the star is di↵erent from those of known
jets observed by Whelan et al. (2010) by 20 –30 . The
PI⇥R2 images at three wavelengths also show faint extended emission to the west (*C*), o↵set from the jet
direction by 20 –30 but in an opposite side from *B*.

見た目が通常の Class I-II YSOs とは大きく違う
さらに、4つの中でも全て見た目が異なる-> gravitationally unstable disk にから形成されたのでは？
14Takami et al.

and showed optical extended emission with a signifi
cantly wider
opening angle (120 -150 ) and a large anVorobyov(2016)
gular scale (⇠4000 ). These structures can naturally be
attributed to scattered light at a cavity edge, and it iunlikely that there is another thin cavity edge inside likecircumstellar
disktheastructure*B* associatedwith の計算
Z CMa.
Throughout, it is more likely that the tail-like structuresassociated with FU Ori (*C*) and Z CMa (*B*) refragmentationsult from the processes associated with a gravitationally-> episodicが有力
unstabledisk than aaccretion
jet or an outflow
cavity. It is note
worthy that hydrodynamical simulations by Vorobyov
et al. (2017) show that a stellar encounter with a gravi
あるコアは弾き飛ばされる
tationallyunstable disk also result in creation of simila
tailFU Ori and Z CMa are actually associ->structures.
tail 構造の形成？
ated with a stellar component which is usually assumed
to be a close binary companion (e.g., Garcia et al. 1999
Wang et al. 2004; Reipurth & Aspin 2004; Whelan et al2010; Beck & Aspin 2012; Canovas et al. 2015, see alsoSection 3) rather than an external intruder. However
their binarity has not been confirmed based on kine
matics or spectroscopy, implying that these “companTakami et al.

Figure 8. The proposed sequence for the geometries of the disk and the envelope. See text for details.

(A) of the above processes gradually clears
he repetition
optically
envelope
outer envelope
towardthick
the ClassII phase. This tranon is observed
millimeter
dust emission (Section-> indiskはまだ見えないand millimeter CO emission at large scales (Kóspáll. 2017a), and also via the mid-IR silicate featureh absorption and emission for early and late phases,(C)ectively(Quanz et al. 2007).
n summary,our results
are consistent
with the scewind
が envelopeを吹き飛ばすo that many low-mass YSOs experience FUor out-> near-IR で観測できる
sts triggered by gravitational instability in disks inr Class I (and perhaps Class 0) evolutionary phases.
s supports the conclusion of Dunham & Vorobyov12), who provided an explanation for the observed
ometric luminosities and temperatures with their(E)We present near-IR imaging polarimetry of five csical FU Ori-type objects (FU Ori, V1057 Cyg, V1
wind が止まると gas がまた降ってくる
Cyg, V1735 Cyg, Z CMa) with Subaru-HiCIAO. S
teredlightassociatedt̲ﬀ
~ 5000yr with circumstellar dust wasserved around at least four of them (FU Ori, V1057 CV1735 Cyg, Z CMa), and possibly around the rem
Class I phase の寿命より短い
ing object (V1515 Cyg) as well. Their polarized insity distribution shows a variety of morphologies warms (FU Ori, V1735 Cyg), tails or streams (FUZ CMa), spikes (V1057 Cyg), and fragmented distrtions (V1735 Cyg). These significantly di↵er from s
tered light observed toward many other normal yostellar objects (Class I-II objects). The observed aand fragmented structures are attributed to gravitat

48

https://arxiv.org/abs/1806.02434

49https://arxiv.org/abs/1807.07723

50

https://arxiv.org/abs/1807.10766

etion Rate of PDS 70b

3PDS 70
ongoing accretion star
K7 pre-main sequence
T Tauri type star

PDS 70b
directly imaged exoplanet
こっちも accretion してるかもvery young (< 10 Myr) ならshocked hot gas ( ~ 10000K)が Hαで見えるはず

0b is the only clearly detected point source at >95% confidence. Right:
0 system. The image is assembled from the H↵ image tracing accretion
この天体でHαは初？
e planet’s thermal
emission and starlight scattered by the disk (Müller etis not shown
hereの中でdue to thedifficulty in capturing
the extreme contrast
gapaccretion
してる惑星としては2例目

classical angular diﬀerential imaging(cADI)
projection onto eigenimages(Karhunen-Loeve Image Processing)Fig. 1.— Left: MagAO H↵ SDI+ image of PDS 70. PDS 70b is the only clearly detected point source at >95% confidence. Right:
Schematic false color diagram of the components of the PDS 70 system. The image is assembled from the H↵ image tracing accretion
GAPlanetS
onto the planet (red) and the infrared image (blue) showing the planet’s thermal emission and starlightscattered by pipeline
the disk (Müller etal. 2018). Note that the primary star also has H↵ emission that is not shown here due to the difficulty in capturing the extreme contrast
ratio.

Fig. 2.— 2018 May 3/4 MagAO H↵ SDI+ data reductions utilizing cADI for the angular step (left), utilizing KLIP-ADI (center), andutilizing the GAPlanetS pre-processing and pyKLIP+SDI pipeline (right). All three methods yield a consistent detection of PDS 70b. The
smaller dashed white circle (diameter = FWHM) indicates the most recent position of PDS 70b in Müller et al. (2018), which is consistentwith the H↵ detection’s position in each pipeline (see the discussion on astrometric uncertainties in §3.1). The color scale is normalized
and identical to that in the left panel of Fig. 1.

the proceeding analysis. While all thee pipelines provide

Both of these positions are consistent within 1- of eachRigliaco et al. (2012) (4)式より光度Lacc RṀacc ⇠ 1.25
GMJupiterくらいThe Mass Accretion Rate of PDS 70b<latexit sha1_base64="1I3K576ApuYrtQjx/YiossxYcnU=">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</latexit>

5-9 MJup くらい<latexit sha1_base64="x9bhd/aelxgMtWjMviHiZjDX5Nw=">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</latexit>

upper limit

the square root of thesponding false positive
combined image, or ar
lent agreement with th4.2. A Giant PThe H↵ emission fro
ject is still accumulati
environment. Thus, ition, and its current m
be used to estimate thbrightnessのtain. Considering tha
the order of ⇠10 MJup不定星
grow even an additiona
dispersal lifetime, evencretion rate of 10 7 M
extremely high, it is u
higher than the value cFig. 5.— The scaling relation of PDS 70b’s mass accretion rate
惑星の質量の不定性
absence of a dramaticwith planet mass and extinction.
The mass ranges of Keppler et al.

惑星の mass accretion rateṀP DS70b = 10 8±1 MJup /yr<latexit sha1_base64="6/dtYEU9mO5pT6pRny+2T4d/kVg=">AAACmXichVFNSxtBGH7cWk1jq7G9FLwsBksPVd+VQIJQUNuDCEI0jQquht11NEv2i91JIC77B/wDhfbUQhHxTwi9VO8e/AnSo4VeeuibzUJppfoOM/PMM+/zzjMzZuDYkSS6GlAeDD4cGs49yo88fjI6Vhh/uhH57dASdct3/HDLNCLh2J6oS1s6YisIheGajtg0W296+5sdEUa2772T3UDsuMaBZ+/bliGZahRK+p4v49WkEVff1spkJuprVaPdeLqiB66qJfor3TVkM3TTnJV2kMx2w0ahSDOUhnobaBkoIouqXziGjj34sNCGCwEPkrEDAxG3bWggBMztIGYuZGSn+wIJ8qxtc5bgDIPZFo8HvNrOWI/XvZpRqrb4FId7yEoVU3RJJ3RD3+iUrunXf2vFaY2ely7PZl8rgsbY0fPaz3tVLs8SzT+qOz1L7KOSerXZe5AyvVtYfX3n8P1NbX59Kn5Bn+k7+/9EV/SVb+B1flhf1sT6R+T5A7R/n/s22Jib0RivlYoLS9lX5DCBSbzk9y5jAcuoos7nfsAZznGhTCiLyrKy0k9VBjLNM/wVSu03dsSdFA==</latexit>

現在の年齢⇠ 5 Myr<latexit sha1_base64="aPUQAdhHJlg3N9Tx4T4s/Rr6eWc=">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</latexit>→ 現在の質量 ( 数木星質量 ) には足りないありえそうなシナリオ
run-away gas accretion で木星型惑星ができる(ここでほぼ惑星の質量が決まる)

gap をつくる

今の accretion rate だと惑星の質量はせいぜいあと10%も増えない(それでもHαは出すくらいの accretion はある)