SFN #279 No.6~10
黒瀬一平

Resolved observations of transition disks

ALMAの分解能によって明らかになった遷移円盤の構造に関する論文。
Radio continuumによる軸の非対称は空気力学的な捕獲によるダストの分離として解釈できる。最近の観測進捗や来期の改善に向けた所見がtions of transition disks3
まとめてある。
•Figure 2. Comparison between the observed H-band polarised intensity image of HD 142527 (a- from Avenhaus et al. 2014a) and 3D
radiative transfer predictions (b- from Marino et al. 2015a, this is an updated version of their Fig. 2). The kinematics of C18 O(2-1)
emission (Perez et al. 2015a) give the orientation of the outer disk; the white contours in a- correspond to systemic velocities, so that
the PA of the outer disk lies at ⇠ 160 deg East of North, as indicated on b-. The inner disk shadows cast on the outer disk are best
reproduced with a PA of 172 deg, the curvature of their outline (or silhouette) is reminiscent of the observations for the Eastern side.
The similarities with the observations are particularly good given the idealisations of the model, which assumes a circular cavity.

outer PA

Whitney et al.
inner disksilhouettes

innerPAmolecular-line observations with ALMA may provide
the necessary clues from the gas kinematics.
3 GAS IN CAVITIESModels predict that young giant protoplanets carve a
deep gap in the dust component of protoplanetary disks,
and a shallower gap in the gas and very small grains(VSGs) components (e.g. Paardekooper & Mellema
2006; Fouchet et al. 2010). The clearing of the protoplanetary gap is thought of as an important mechanism
underlying the class of TDs, and residual gas in cavities
has thus been intensely searched for.

mm sized grain

3.1 Ro-vibrational gas and very small grains

S. Casassus Long-slit spectroscopy has provided indirect evidence
HD142527,H-band(Obs,model)
Intra-cavity
reproduced with permission),with
a3D
radiative
transfer predic- kinematics
Intra-cavity kinematics
9◦◦◦ of HD◦ 142527◦ (a- from◦ Avenhaus et al. 2014a) and 3D
son between
the observed H-band polarised◦intensity
image

1. Figure adapted from
Whitney et al. (2013, c AAS,
4r (JHK) images of the Class II model in which the inner 1 AU of the disk isFigure
Casassus
misaligned at 30◦ withS.respect
to the rest of the disk.

of 60 and at six azimuthal angles: 0 , 60 , 120 , 180 , 240 , and 300 . The
intoconfiguration.
a radius of The2 AU.
tionimages
in JHK arefor azoomed
warped disk
fieldAt
is 4thisAU
redictions (b- from Marino et al. 2015a, this is an updated version of their Fig. 2). The
kinematicsof C18 O(2-1)
onaside.
cked from view at several azimuthal angles. This is seen in the light curves of the rotating disk in Figure 27.
al. 2015a) give the orientation of the outer disk; the white contours in a- correspond to systemic velocities, so thatdisk lies
160 degjournal.)
East of North, as indicated on b-. The inner disk shadows cast on the outer disk are best
ilablein atthe⇠onlinefor gas inside cavities, under the assumption of azimuthal symmetry and Keplerian rotation (Carr et al.
2001; Najita et al. 2003; Acke & van den Ancker 2006;
van der Plas et al. 2008; Salyk et al. 2009). SpectroPA of 172 deg, the curvature of their outline (or silhouette) is reminiscent of the observations for the Eastern side.
there
issofaronlyoneclear
caseofawarp,i.e.
inastrometry has also been used to infer a residual gas
h the observations are particularly good given the idealisations of the model, which assumes a circular cavity.
HD 142527. Next-generation adaptive-optics cameras,
mass from ro-vibrational CO emission (Pontoppidan
such as SPHERE and GPI, should soon provide subet al. 2008; van der Plas et al. 2009; Pontoppidan et al.
stantial
improvements,
particularlythroughpolarised2011). A comprehensive analysis is presented in van dermolecular-line observations with ALMA may provide
which appears ideally suited toPlas et al. (2015) and Banzatti & Pontoppidan (2015).
the necessary clues from the gasdi↵erential-imaging
kinematics.
trace illumination e↵ects, and so identify warps. FirstThe general picture is that dust cavities do indeed conresults from such new AO imaging are indeed revealtain some amount of residual gas, as expected in theing
intriguing
intensity
modulations,as inregions
MWC
758
context of dynamical clearing.
3 GAS IN Figure
CAVITIES
4. Comparison
Figure adaptedfromCasassusal. (2015a,part inof the centralFigure 8.
of observedand modeletCO(6-5)kinematics
of HD 142527. The origin of coordinates is set tothestellar
position.
Velocity-integrated
intensityin
CO(6-5)isshowningreyscale.
The
coloredcontours
forvlsr haveconstant
intervalare
and thought to be well coupled(Benisty withet al.permission)2015), HD
135344B
The
smallest
grainstheir Fig. 26, c AAS, reproduced, showing
the (Wahhaj et al. 2015)
1 (as in Fig. 1). a): Observed moment maps extracted on the MEM datacubes. b): moments extracted onarespreadover[0.21,7.87]
kmsModels predict
that
young
giant
protoplanets
carveaobserved CO(6-5) kinematics
in thecentralregions(Wagnerof HD 142527, al. 2015). Followup
and inHD
100453
gas,model
so thatthey can be used as proxies. Therthe radiative transfer prediction,aftersmoothingto the resolution etof the MEM datacubes. c): same as withb) butthein nativeresolutions,andcomparing
withmodel
predictions
fortheaccretion
throughdeep gap in the
dust
component
ofprotoplanetarydisks,
without smoothing. Regions without contours and near the origin correspond to higher velocities. d): same as b) but with a slow velocity
component
perpendiculartoFig.
the (2016)
plane (vwarpin
theresolutiontext).
PASA
thewarp
5disk(convolved
theofand a shallower
gap represented
in
the gasin
andverysmall atgrains
the centroid map). Thedoi:10.1017/pas.2016.xxx
origin of coordinates is set to the stellar
order of 105 yr if the outer disk has a mass of 0.1 M .
(VSGs) components(e.g. Paardekooper & Mellema
position.
A Kozai cycle would result in (damped) oscillations be2006; Fouchet et al. 2010). The clearing of the prototween the current inclined circular orbit, and a highly

HD142527,H-band(continuum(r),CO(3-2)(b),HCO+(g)HD142527のイラスト

HD142527,CO(6-5)

大きなダストが落下するのを防ぐ手段としての「ダスト捕獲」

大きなダスト落下するのを防ぐための「ダスト捕獲」

重力不安定性や惑星によって発生スパイラルは発生後円盤進化に影響On the origins of polarization holes in Bokglobules•

Bok globulesにおいて、中心領域の偏光度が減少しているのが確認されており、それを数値計算で再現しその条件(optical depth, dust size…)を調べた論文
モデルの熱輻射による偏光図

optically thin->polarized
optically thick->2色の減光

gas massの増加で偏光度合いは全体的に減少

mm/sub mmまで成長の必要

grain組成による変化

fによる変化Origin of the Lyman excess in earlytype stars•

early-type星周囲の電離領域における、free-free emissionとIR-emissionが各分解能の制限によって遠赤領域で観測的に制限されていた。

•→Hershelの到来でより正確に二つの計測をした結果、現在のHII領域の３分の１がより多くのLyman continuumを出している(Lyman eccess.)ことが分かった。もっともな理由としてはLyman continuumに加え accretion shockから出るUVphotonなど。

SiO

δV
Lyman photon rate vs Lbol

THE FIRST BROWN DWARF/PLANETARYMASS OBJECT IN THE 32 ORIONIS GROUP•

32 Orionis group内に初めて亜恒星天体WISEJ052857.69+090104.2を発見。以前はM型の巨星と報告されていたが、データの再解析からこの天体が表面重力が小さく、若いL1型の褐色矮星であることが分かった。THE FIRST BROWN DWARF/PLANETARYMASS OBJECT IN THE 32 ORIONIS GROUP•

変光する原始星SVS 13AのSMAによるCO(2-1)の観測。

•分子のʼ弾丸ʼによる高速なジェットが確認でき、議論からシステム速度付近の速度勾配はjetの回転によるもの。２つの弾丸が持つ角運動量はdense coresとほぼ同じ、原始星エンベロープの10倍、周星円盤の20倍あり、速度勾配が天体の回転によるものならば相当の量の角運動量が輸送されていることになり角運動量輸送問題の解決にジェットやoutﬂowの回転が鍵となるかもしれない

blue側にジェットのうねり各bulletのPV
2つのbulletにはdense coreと同等の角運動量が含まれている→角運動量を捨てる効率が良い
間欠的に起こる20~30回のoutburstによって角運動量が捨てられるシナリオと整合