37. Planet-Disk Interactions
Sijme-Jan Paardekooper et al. in Protostars and Planets VII
38. The Role of Disk Winds in the Evolution and Dispersal of Protoplanetary Disks
Ilaria Pascucci, et al. in Protostars and Planets VII
39. Magnetic ﬁelds in star formation: from clouds to cores
Kate Pattle, et al. in Protostars and Planets VII○ 40. Ionise hard: interstellar PO+ detection
Víctor M. Rivilla, et al. Accepted in Frontiers in Astronomy and Space Sciences○41. Precursors of the RNA-world in space: Detection of (Z)-1,2-ethenediol in the interstellar
medium, a key intermediate in sugar formation
Víctor M. Rivilla et al. Accepted for publication in The Astrophysical Journal Letters○ 42. Cluster Formation in GGD12-15: Infall Motion with Rotation of the Natal Clump
Tomomi Shimoikura, et al. ApJ, 928:76(16pp)

42. Cluster Formation in GGD12-15: Infall Motion with Rotation of the Natal Clump
Tomomi Shimoikura, et al. ApJ, 928:76(16pp)
GGD12-15
12COJ=2-1
blue
IRS 9McClass I/0

Compact HII VLA1（B0.5)
双極分⼦流６ʻ
駆動源 Class I/0のIRS 9Mc
Young cluster 98±10メンバ〜4Myr
VLA1<1Myr

VLA1
CHII

Class 0/1red2pc5ʼハーシェル
Clump
C18O(1-0)~2pc,2800M8
C18O(3-2)~1pc
Core
C18O(3-2)~0.3pc, 530M8Little+1989

HC_3N J = 10 ‒ 9 NRO
N_2H^+ J = 1 ‒ 0 NRO
CCS J _N=8_7 - 7_6 NRO
CS J = 2 ‒ 1 NRO
SO J _N=2_3 - 1_2
C^18O J = 1 ‒ 0^13CO J = 1 ‒ 0^12CO J = 1 ‒ 0 NRO
C^18O J = 3 - 2 JCMT
^13CO J = 3 ‒ 2 JCMT

位置速度図１−２★低速度成分は落下運動かè回転しながら落下

12CO （⾚⻘別）積分強度図

C18O

HC3N

Blue:-2~6km/s

断続的なアウトフロー
CSのアウトフロー

Red:-15~30km/s
C18O

⾼速度成分の勾配

12CO
Red:-15~30km/s

低速度成分の勾配

Blue:-2~6km/s
rは球座標の動径
Rは円柱座標の動径C18O(J=3-2)観測

視線アウトフローの軸C18O(J=3-2)モデル
短軸

⻑軸短軸

⻑軸⻘⾚⾚Red LobeBlue Lobe⻘

⾚⻘

41. Precursors of the RNA-world in space: Detection of (Z)-1,2-ethenediol in the interstellar medium, akey intermediate in sugar formation
Víctor M. Rivilla et al. Accepted for publication in The Astrophysical Journal Letters
RNAワールド仮設：RNA (→リボ核酸 ) を遺伝⼦とする原始⽣命世界のこと。地球上の⽣物が現実に住んでいる世界 (DNAワールド) が出現する以前に，この地球上に存在していたと想定され，⽣命の起源や⽣物進化と関連して関⼼が⾼まっている。（コトバンク）
RNA：リボヌクレオチド＝リン酸基 - D-リボース（５炭糖） - 核酸塩基
RNAの前駆体は、初期の地球環境に供給されたか？あったか？
アルデヒド基カルボニル基アルデヒド基カルボニル基C 2H 4O 2
異性体

グリセルアルデヒド
C3H6O3(3炭糖)
隕⽯でグリコールアルデヒド
HOCH2-CHO(2炭糖)
ISMでethenediol(CHOH)2
G+0.693-0.027分⼦雲 (SgrB2領域)
Yebes 40m + IRAM 30m

Tex=8.5±0.6K
Nmol=(1.8±9.1)x1013cm-2
abundance=1.3x10-10
C2H4O2 の異性体
CH3COOH 酢酸
HCOOCH3 ギ酸メチル
HOCH2CHO グリコールアルデヒド(CHOH)2 ethenediol
未未(5)Minimum energy principle （最も安定な分⼦が最も多く存在）は成り⽴たない。
個々の分⼦の⽣成パスを要検討

1.3x10-10(3)

(2)

未(1)
(4)

未ホルムアルデヒド
7x10-9中性ーラジカル反応（気相でも可）ビニルアルコール9.2x10-10
ダスト表⾯
２量化

未(7)
グリコールアルデヒド
複雑な糖へ
6x10-10(6)(6)

グリセルアルデヒド上限<0.93x10-10(7)

40. Ionise hard: interstellar PO+ detection
Víctor M. Rivilla, et al. Accepted in Frontiers in Astronomy and Space Sciences
PO+（１酸化リン）
G+0.693-0.027 Sgr B2領域
Yebes 40m, IRAM30m,APEX+PO J=1-0

対数軸0.0024
J=2-10.0024

First Detection
PO+/P>NO+/N, SO+/S0.0044

0.00440.12

0.12

P++OHàPO++H

電離P+OHàPO+H
P+H2OàPO+H2

Cosmic ray ionization of PO
C-shock Vs=20km/s

電離37. Planet-Disk Interactions
Sijme-Jan Paardekooper et al. in Protostars and Planets VII
Planet-disk interactions, where an embedded massive body interacts gravitationally with the protoplanetary disk it wasformed in, can play an important role in reshaping both the disk and the orbit of the planet. Spiral density waves arelaunched into the disk by the planet, which, if they are strong enough, can lead to the formation of a gap. Both eﬀects
are observable with current instruments. The back-reaction of perturbations induced in the disk, both wave-like andnon-wavelike, is a change in orbital elements of the planet. The eﬃciency of orbital migration is a long-standing problem
in planet formation theory. We discuss recent progress in planet-disk interactions for diﬀerent planet masses and disk
parameters, in particular the level of turbulence, and progress in modeling observational signatures of embeddedplanets.

38. The Role of Disk Winds in the Evolution and Dispersal of Protoplanetary DisksIlaria Pascucci, et al. in Protostars and Planets VIIThe assembly and architecture of planetary systems strongly depend on the physical processes governing the evolution
and dispersal of protoplanetary disks. Since Protostars and Planets VI, new observations and theoretical insights favordisk winds as being one of those key processes. This chapter provides a comprehensive review of recent observations
probing outﬂowing gas launched over a range of disk radii for a wide range of evolutionary stages, enabling an empirical
understanding of how winds evolve. In parallel, we review theoretical advancements in both magnetohydrodynamic andphotoevaporative disk wind models and identify predictions that can be confronted with observations. By linking theory
and observations we critically assess the role of disk winds in the evolution and dispersal of protoplanetary disks. Finally,
we explore the impact of disk winds on planet formation and evolution and highlight theoretical work, observations, andcritical tests for future progress.

39. Magnetic fields in star formation: from clouds to cores
Kate Pattle, et al. in Protostars and Planets VIIIn this chapter we review recent advances in understanding the roles that magnetic fields play throughout the starformation process, gained through observations and simulations of molecular clouds, the dense, star-forming phase of
the magnetised, turbulent interstellar medium (ISM). Recent results broadly support a picture in which the magnetic
fields of molecular clouds transition from being gravitationally sub-critical and near equipartition with turbulence in lowdensity cloud envelopes, to being energetically sub-dominant in dense, gravitationally unstable star-forming cores.
Magnetic fields appear to play an important role in the formation of cloud substructure by setting preferred directions forlarge-scale gas flows in molecular clouds, and can direct the accretion of material onto star-forming filaments and hubs.
Low-mass star formation may proceed in environments close to magnetic criticality; high-mass star formation remains
less well-understood, but may proceed in more supercritical environments. The interaction between magnetic fields and(proto)stellar feedback may be particularly important in setting star formation efficiency. We also review a range ofwidely-used techniques for quantifying the dynamic importance of magnetic fields, concluding that better-calibrated
diagnostics are required in order to use the spectacular range of forthcoming observations and simulations to quantify our
emerging understanding of how magnetic fields influence the outcome of the star formation process.