THE STAR FORMATIONNEWSLETTER
No. 263
塚越崇(茨城大)28 Nov. 2014

POISSON project III. Investigating the evolution of the mass accretion rate
S.Antoniucci et al.

• POISSON (Protostellar Optical-Infrared Survey on NTT)•

この論文ではLupus, Serpens領域の結果を紹介• 大きなサーベイで星進化と降着現象の関係を調べる• BrγからLaccを導出=>Maccに変換•

他領域のデータも使用する• L*とLaccに良い相関• Macc Mß, Macc t-ηを与えると進化傾向が良く見える

Antoniucci et al.: AccretPlanet-vortex interaction: How a vortex can shepherd a planetary embryo
S.Ataiee et al.

• 円盤渦による惑星(種)への影響をhydroシミュレーションで調査•

円盤の面密度変化=>渦が形成される(dead zone or planet)• モデル計算•FARGO、ケプラー回転円盤、locally isothermal•

ガウシアン型のpressure bumpを埋め込み、渦の形成を与える•

渦の形成後(?)、惑星を渦周囲や渦内に埋め込む

S. Ataiee et al.: Planet-vortex interaction: How a

1.02
2 (t=390)

4 (t=470)

1.01

ap

1.00

0.99

0.98

1 (t=350)5(t=510)3 (t=440)

103t (orbit)

104Fi
grsit

1.02
2 (t=390)

4 (t=470)

1.01

ap

1.00

0.99

0.98

1 (t=350)5(t=510)3 (t=440)

103t (orbit)

104

The fate of scattered planets
B.C.Bromley et al.

• 巨大惑星によって弾き出された惑星とガス円盤の相互作用を計算•

遠い惑星が低離心率になる時の円盤状態を調べる• power-lawの低質量円盤モデル••

時間依存した散逸のどちらかを入れる•Σ*exp(-t/τ)の散逸•

時間とともにinner edgeが広がる(transition disk)

巨大ガス惑星は5AUに置く• 計算結果(次ページ)•

重い惑星ほど円軌道になりやすい•

expで散逸する円盤のほうが小さい半径で円軌道に•

inner holeが広がる場合、軌道の多様性が進む。スーパーアースでも100AUを超えて円軌道になる• HR8799の惑星(super-Jupiter at 70AU)を説明できるかもexp(-t/τ)散逸のケース

inner holeが広がるケース

面密度

カラーは惑星の初期位置: 100(赤), 200(緑), 300(青) AU
Fig. 4.— Simulation outcomes depicted as elliptical orbital paths for a suite of models. The x-y(細)1,3, plane;
10, 30(太)are
Mearthcoordinates線の太さは惑星の質量:
give planetary positions in theirorbitalmodels
oﬀset from one another sothat they are sorted in rows and columns according to model parameters. The first and second

Kinematics in Partially Ionized Molecular Clouds: Implications for the Transition toCoherence
N.D.Balley et al.

• 分子雲における電離度が、形成されたコアの速度構造や分子輝線プロファイルに与える影響を調査•Balley&Basu(2014)の発展 (Paper1)• 電離度を調べるには中性物質とイオンの振る舞いを調べる事が重要•

電離度分布を変えた際の中性分子とイオン分子の振る舞いを計算
4Bailey, Basu & Caselli

6• velocity ﬁeld(右上図)•SLのほうが速度分散大きい• 合成スペクトル(右下図)•

コアと低密度領域(LDG)の中性分子とイオン分子電離度分布の違いによってコア/クランプの速度構造に影響を与える

Bailey, Basu & Caselli

13

A near-IR spectroscopic survey of massive jets towards EGOs
A.Caratti o Garatti et al.

• 大質量星のprimary jet( molecular outﬂow)のサーベイ観測•

降着現象と密接に関わるので重要• SpitzerのGLIPSEサーベイから天体を選定•

4.5mum超過があるものがベース (extremely greened object; EGO)

• 最終的に18天体を選出•

中/大質量星に付随する、明らかなH2 ﬂow/jetでかつ明るいもの• 観測とデータ••

ESO New Technology Telescope(NTT)のカメラSoﬁ•

H2とKsのイメージング•

イメージングと低分散分光(R~600)の同時取得

アーカイブデータからSEDを作成

A. Caratti o Garatti et al.: NIR spectroscopy of massive jets from intermediate- and high-mass YSOs

• ノットと天体位置からジェットのposition angleを導出• 多くのサンプルで大きなprecession angleを示す• multiple jetの例もある
Fig. 1. H2 and continuum-subtracted H2 images (left and right panels) of the IRAS 13481-6124 jet. This jet is one of the few examples of jets withsmall precession angles and it has asymmetric lobes. Source and knots positions are indicated in the figures. Blue and red lobes are also reported
according to Kraus et al. (2010).
Fig. 1. H2 and continuum-subtracted H2 images (left and right panels) of the IRAS 13481-6124 jet. This jet is one of the few examples of jets withsmall precession angles and it has asymmetric lobes. Source and knots positions are indicated in the figures. Blue and red lobes are also reported
according to Kraus et al. (2010).

Fig. 2. Same as in Fig. 1 but for the IRAS14212-6131 flow. This object represents a good example of precessing flow with only one detected lobe.
The thin dashed lines show the measured precession angle. The positions of sources, knots, masers, EGOs, and H ii regions are indicated in the• 分子輝線(H2)と原子輝線が見える
ケースと、分子輝線しか見えないケースがある• ro-vibrational iagramから温度と密度を算出

A&A proofs: manuscript no. Massive_Jets_paper_astroph

gion within a 3 contour level above the sky background. Identified knots along with their coordinates, 2.12 µm fluxes, uncertainties, and projected areas in the sky, are reported in theAppendix (Columns 1–6 of Table A.1). Third, the AV (H2 ) andT (H ) values derived from our spectroscopy (Sect. 4.3.1 and TaFig. 5. 0.95–2.5 µm2 SofI spectrum of knots 4 and 5 in the G35.2N outflows. An asterisk near the line identification marks the de
2 and 3 sigma.
are indicatedby the symbol“ ”.
bleTelluricA.1)linesare
then used
to deredden
the 2.12 µm line flux andto derive the intensities of all H2 lines
by applying a radiative
Fig. 5. 0.95–2.5 µm SofI spectrum of knots 4 and 5 in the G35.2N
outflows. An asterisk near the line identification marks the de
2 and 3 sigma.
Telluriclinesgas
are indicatedby thesymbol“ ”. in Caratti o Garatti et al. 2006,
codewithin LTE(seedetails2008).

For those knots associated with a particular flow but not encompassed by any slit, we adopt an average value of the physicalparameters derived from the flow knots. Then, for each considered knot, our LTE code provides: a) the line intensities involving levels with 0  v  14 and 0  J  29 (Ev,J  50 000 K);b) the total H2 intensity; and c) the H2 luminosity by assuming
the distance to the source provided in Table 1. This process is repeated for all the knots associated with each flow, to estimate LH2of the flow. LH2 values are reported in Column 7 of Table 3. The
inferred values range from 0.5 to 45 L . This roughly reflects thelarge Lbol range in our sample. It is worth noting, however, that
theµminferred
LHof2Knotvalues
be lowervalues,
Fig. 6. 1.5–2.5
SofI spectrum
C in themight
IRAS16122-5047
flow. limits
Labels areof
as intheFig. real5.
because our estimate does not take into account part of the emission
fromthecold
Hin2 thecomponent,purerotationalagrams(Boltzmannplots)
to derive
density, visual traced
exumnbydensitythe5. molecules(Nv,J ) in the upp
Fig.
6. 1.5–2.5µm SofI
spectrumof
Knotcolumn
C
IRAS16122-5047
flow. Labels
aretheas inofFig.

• 高温(2500-3000K)、高密度(1018-20 cm-2)領域がH2の起源•

70%はno ionic emission -> 天体近くのoutﬂow cavityにおけるC-type shock•

30%はatomic emissionあり -> magnetically collimated jetのJ-type shock• ジェットのmorphology•

多くのprecessionやmultiple jet -> クラスターによる相互作用• 広がったH2放射+ノット -> 定常降着+バースト成分

A. Caratti o Garatti et al.: NIR spectroscopy of massive jets from intermediate- and high-mass YSOs

ever, in two out of seven cases (flows from IRAS 142126131 and GLIMPSE G035.0393-00.4735; see right panels ofFig. 2 and B.14) a marginal detection (between 2 and 3 )of H2 emission from the second lobe is observed. This suggests that the higher visual extinction towards one of the lobes
can hamper our observations in the NIR regime. Neverthe低質量星でも見られる関係に乗る
less, the presence of monopolar outflows from high-mass (Zapata et al. 2006; Fernández-López et al. 2013) as well as lowCOで得られてるものと同じベキ数
mass YSOs (Codella et al. 2014) has been observed in a few
sources through submm outflow tracers, such as SiO and CO.
The authors propose that such a monopolar geometry is due toanisotropic ambient cloud conditions or to an intrinsic asymmetry in the flow. In addition, the presence of close companion(s)might divert or even inhibit the ejection (see also Reipurth 2000;
Murphy et al. 2008, and discussion therein). Unfortunately, we
do not have any (sub)mm observations of theses flows to verify any of these scenarios. However, the Spitzer/GLIMPSE images show emission in excess at 4.5 µm located at the positionof the undetected lobe in four out of seven flows (namely IRAS
13484-6100, IRAS 14212-6131, IRAS 15450-5431, GLIMPSE
G035.0393-00.4735). Although the nature of such excess is controversial (e.g. De Buizer & Vacca 2010; Takami et al. 2012), it
has been often associated with outflows (Cyganowski et al. 2008;Tappe et al. 2012).

• 中心星光度とH2強度に相関あり••• 中心星質量とH2質量にも弱い相関=>重い星ほど質量を多く放出(ただし分散大きい)