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

41

https://arxiv.org/abs/1807.01429

S51 km0.01
93.61M ⊕multiple planetary
S6 system の観測例：633
10 km
089.02M ⊕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
S7
10 km
0.01
120.91M ⊕10 km
0.1134.66M ⊕この研究の目的S8S9∗ phase における100km zone での岩石惑星
0116.44M ⊕post-gas
habitable∗ habitable plantes;(potentiallyS10
100 kmPHPs)と水の含有量の進化
0.01
68.88M ⊕Mass [MJ]

00.10.2

156.55
195.30226.43271.84164.40141.88F

101100m− fmigI=0100m− fmigI=0.01

1

100S1S2S

10−1
10−210−310−410−5

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 Oriarc

near-IR
HiCIAO

tailスバル望遠鏡
PDI mode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？
14

Takami et al.

and showed optical extended emission with a signifi
cantly wider
opening angle (120 -150 ) and a large an
Vorobyov(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*) refragmentation
sult from the processes associated with a gravitationally-> episodicが有力
unstabledisk than aaccretion
jet or an outflowcavity. 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 al
2010; Beck & Aspin 2012; Canovas et al. 2015, see also
Section 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
opticallyenvelope
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~ 5000
yr 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 yo
stellar 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 70b3

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 consistent
with 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 th

4.2. A Giant P

The 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=">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</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)