RT Line Simulation Study of YSO Outflow in Early Stage - towards - - PowerPoint PPT Presentation

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RT Line Simulation Study of YSO Outflow in Early Stage - towards - - PowerPoint PPT Presentation

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RT Line Simulation Study of YSO Outflow in Early Stage - towards ALMA era - Masako YAMDA(ASIAA) Masahiro MACHIDA, Shu-ichiro INUTSUKA(Kyoto University) Kohji TOMISAKA(NAOJ) 2008 12 22 Introduction : YSO Outflow

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SLIDE 1

RT Line Simulation Study of YSO Outflow in Early Stage

  • towards ALMA era -

Masako YAMDA(ASIAA)、Masahiro MACHIDA, Shu-ichiro INUTSUKA(Kyoto University)、 Kohji TOMISAKA(NAOJ)

2008年12月22日月曜日

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SLIDE 2

Introduction : YSO Outflow

✦

ubiquitous phenomena in star forming region

✦

  • bs. : wide variations in morphology, velocity...

✦

Studies of YSO outflow :

✦

in star formation processes : angular momentum transfer/ final mass determination/(possible) triggering mechanism in sequential star formation…

✦

physics in outflow : driving mechanism??

✦

Driving mechanism : several models, but still unclear

✦

B force-driven?

✦

collapse of rotating magnetized molecular core (Lorentz force／centrifugal force)

✦

disk wind, X-wind...

✦

entrainment by high-velocity optical jet?

✦

Difficulty in observational study of driving mechanism : spatial extent /evolution / τ

✦

launching region[<100AU, 102 yr]⇔ current obs.[~103-104AU, 103-104yr]

✦

complex velocity field of several components : infall of envelope/disk ~ rotation of disk ~ outflow

✦

launching mechanism ⇔ early stage of evolution ← deeply embedded in progenitor mol. core

3D non-LTE radiative transfer approach

Belloche et al.2002

2008年12月22日月曜日

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SLIDE 3

Calculations

✦ Hydrodynamic simulations:

✦

3D nest grid, resistive MHD

✦

initial condition : rotating Bonnor-Ebert sphere (M=0.6Mo, R=2000AU, Tkin=10K)

✦

EOS : taken from 1D radiation hydro. simulation (Masunaga & Inutsuka, 2000) + some modification

✦

long evolution, and large spatial extent

✦

stop calculations slightly after the first core formation

✦ Radiative Transfer: [ray tracing with long characteristics method]

✦

non-LTE level population up to J=10 for each grid

✦

assume uniform chemical abundance distribution

✦

  • abs. coeffs. profile :

purely thermal velocity, no micro-turbulence

Hogerheijde&van der Tak(2000)

12CO

CS SiO ncrit ~102[1/cc] ~105[1/cc] ~105[1/cc] E10 5.5K 2.35K 2.08K

2000AU

2008年12月22日月曜日

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SLIDE 4

Dead region B dissipation

(1012cm-3<n<1015cm-3)

B amplification B amplification

B B B

Isothermal Phase Adiabatic Phase Second Collapse & Protostellar Phases

Adiabatic core (First core) Formation H2 dissociation (endoergic reaction)

To MS

protostar (second core)

Gas Temperature

Log T (K) 10 102 103 104

1D Radiative Hydrodynamics

Log n (cm-3) 1010 1015 1020 105

Spatial Scale (AU)

104 100 1 0.1

Larson (1969) Tohline (1982) Masunaga & Inutsuka (2000)

Molecular Cloud Core Protostar

Calculations (cont.) : hydro. evolution

adopt slightly harder EOS in order to calculate longer period and larger extent

2008年12月22日月曜日

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SLIDE 5

✦ simulations:

✦

a spatially/temporary snap shot result is cut-out from Nested Grid simulation ⇒ emission/absorption in outer part do not enter

  • ur results [current limitation of our RT scheme]

✦

AMR/nested grid RT scheme (by Prof. Tomisaka , experimental) ⇒outer envelope is not completely thin, and introduces un-negligible changes!

My analysis/results are taken as qualitatively, not quantitatively!

L=7

Calculations (cont.)

2008年12月22日月曜日

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SLIDE 6

1000 500

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z 1000 500

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x 1000 500

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z 1000 500

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x 1000 500

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z 1000 500

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x 1000 500

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z 1000 500

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x

Non-LTE results : integrated intensity

✦

almost symmetric distribution of red/blue components

✦

in outflow & disk : red and blue contours show separate peaks

✦

not in perfect symmetry in red/blue contours due to optical thickness & velocity structure effects

✦

θ=30, 60deg. : almost circular envelope at the outer part ⇔infalling motion of envelope toward the center

✦

Δθ(10AU)=0.07” if D=140pc

θ=0, 30, 60, 90 deg. [SiO(J=7-6) E7=58K], barotropic

θ=0 θ=30 θ=60 θ=90 2,000AU

integrated intensity : full & blue/red

ALMA can resolve these structures (..and SMA as well?)

  • utflow

envelope

2008年12月22日月曜日

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SLIDE 7

Column density : dust continuum

✦

dust continuum : expect for higher angular resolution obs. compared with lines

κν = 0.1 × 0.25[mm] λ β

θ=0(pole-on) θ=30 θ=60 θ=90(edge-on)

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x[AU] 500 1000

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500 1000 y[AU]

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x[AU] 500 1000

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500 1000 y[AU]

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x[AU] 500 1000

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500 1000 y[AU]

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x[AU] 500 1000

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500 1000 y[AU]

0.00e+00 1.00e-02 2.00e-02 3.00e-02 4.00e-02 5.00e-02 6.00e-02 Tb[K]

(a) 150GHz (d) 650GHz (b) 220GHz (c) 350GHz (e) 850GHz

Td=10K~Tgas

Tb = Bν(1 − exp(−τν))

θ=60

✴high column density at

disk - difficult to look further inside

✴emission from outflow

component is quite weak

2008年12月22日月曜日

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SLIDE 8

Column density : dust continuum

✦

dust continuum : opt. thin in mm. bands - how about submm. band?

κν = 0.1 × 0.25[mm] λ β

θ=0(pole-on) θ=30 θ=60 θ=90(edge-on)

Td=10K~Tgas

Tb = Bν(1 − exp(−τν))

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x[AU] 500 1000

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500 1000 y[AU]

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x[AU] 500 1000

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500 1000 y[AU]

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x[AU] 500 1000

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500 1000 y[AU]

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x[AU] 500 1000

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500 1000 y[AU]

0.00e+00 5.00e-03 1.00e-02 1.50e-02 2.00e-02 2.50e-02 3.00e-02

τ0 (a) 150GHz (d) 650GHz (b) 220GHz (c) 350GHz (e) 850GHz max(τ)=11.9 max(τ)=0.80 max(τ)=6.94 max(τ)=0.40 max(τ)=2.01

2008年12月22日月曜日

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SLIDE 9

Excitation Temperature : CO

✦

adopt “standard” mol. abundance y=3x10-4

✦

ncrit(1-0)~102 cm-3 , ncrit∝J3

✦

huge optical thickness (τ0 up to 4,000) and high density (106 cm-3 < n < 1011 cm-3) in the simulation box, pop. energy distribution becomes LTE even at high J (J=10-9) (Tex = Tkin~10K)

Tex[K] n[cm-3]

J=1-0 J=2-1 J=3-2 J=4-3 J=7-6 J=5-4 J=8-7 J=6-5 J=9-8

12 10 8 6 4 2 12 10 8 6 4 2 12 10 8 6 4 2 106107 108 1091010 1011 106107 108 1091010 1011 106107 108 1091010 1011

1-0 4-3 7-6 2-1 5-4 8-7 3-2 6-5 9-8

Tex[K] n[cm-3]

J=1-0 J=2-1 J=3-2 J=4-3 J=7-6 J=5-4 J=8-7 J=6-5 J=9-8

2008年12月22日月曜日

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SLIDE 10

Excitation Temperature : SiO

✦

adopt “standard” mol. abundance y=2x10-8

✦

ncrit(1-0)~105 cm-3 ⇔ 106 cm-3 < n < 1011 cm-3

✦

low-J and in dense regime (n > 108 cm-3), pop. is LTE

✦

high-J and in tenuous regime (n < 108 cm-3), Tex decreases to ~ 5K ⇒non-LTE effects can be

  • bserved (⇔12CO)

n[cm-3]

12 10 8 6 4 2 12 10 8 6 4 2 12 10 8 6 4 2 106107 108 1091010 1011 106107 108 1091010 1011 106107 108 1091010 1011

1-0 4-3 7-6 2-1 5-4 8-7 3-2 6-5 9-8

Tex[K] n[cm-3]

J=1-0 J=2-1 J=3-2 J=4-3 J=7-6 J=5-4 J=8-7 J=6-5 J=9-8

2008年12月22日月曜日

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SLIDE 11

Average Line Profile : CO

✦

huge optical thickness ⇒strongly saturated line profile

✦

very weak wing-like components around Vr=+/-2km/sec

✦

... but even in these wing components, τ0 ~100-400

✦

qualitative characteristics are quite independent on viewing angle θ

θ=30deg, solid line: intensity, dashed line:τ0 J=1-0 J=2-1 J=3-2

2008年12月22日月曜日

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SLIDE 12

Average Line Profile : SiO

✦

  • ptical thickness is still large, but smaller than 12CO : line profiles do not show

saturation

✦

<τ>SiO~0.01x<τ>CO : SiO will present inner structures that 12CO cannot

✦

non-LTE pop. & smaller τ ⇒double peak profile appears with respect to Vr=0 km sec-1

✦

qualitative characteristics are quite independent on viewing angle θ

✦

double-peak structure even in pole-on [θ=0] view

θ=30deg, solid line: intensity, dashed line:τ0 J=1-0 J=4-3 J=7-6

2008年12月22日月曜日

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SLIDE 13

Non-LTE results : PV diagram (CO)

✦

Huge τ and then almost feature-less PV diagram

✦

(a) : spiky structure up to +/- 5 km sec-1, wobble ones by several velocity components [outflow, rot. of outflow & disk, accretion of envelope, ...]

✦

(b) : small gradient from blue to red [mainly from disk]

✦

(c) : small gradient from red to blue in inner part [mainly from bipolar vel. of outflows]

CO(2-1), 30deg, vel. 1st-moment

  • 5.0

0.0 5.0 Vr[km sec-1] Angular Offset 100 200 300 400 500 K

(a)

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0.0 0.5 Vr[km sec-1] y[AU]

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500 1000 x[AU]

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500 1000

(a) (b) (c)

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0.0 2.0 4.0 Vr[km sec-1] Angular Offset 100 200 300 400 500 K

(b)

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0.0 2.0 4.0 Vr[km sec-1] Angular Offset 100 200 300 400 500 K

(c)

2008年12月22日月曜日

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SLIDE 14

Non-LTE results : PV diagram (CO)

✦

structures in (c) line

✦

spikes : appear all the PV diagrams of cuts through the very small near-center regions in FOV

✦

NOT appear in some of the cuts passing the very center

✦

velocity (+/- 5km sec-1) > bulk velocity of fluids (|v| up to 3 km sec-1)!

CO(2-1), 30deg, 1st-moment

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0.0 5.0 Vr[km sec-1] Angular Offset 100 200 300 400 500 K

(a)

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0.0 0.5 Vr[km sec-1] y[AU]

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500 1000 x[AU]

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500 1000

(a) (b) (c)

  • vel. gradient

(Δv~1km/sec)

2008年12月22日月曜日

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SLIDE 15

Non-LTE results : PV diagram (CO)

✦

  • utflow is driven by magneto-centrifugal force at rotating

first core : hourglass-shape B field ⇒ accretion on the axis(Vz<0), |Vz| large (~3km/sec)

✦

  • utflows are driven somewhat outer part (B bends)

✦

first core : Tkin rises by accretion shock (up to 180 K) ⇔Δvtherm~2km/sec

✦

vflow + vtherm ~ +/- 5km/sec

first coreの熱幅により流体の速度以上 の「速度」がPV図上に現れる density Tkin Vz

“velocity” greater than bulk motion appears due to thermal broadening!

2008年12月22日月曜日

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SLIDE 16
  • 4.0
  • 2.0

0.0 2.0 4.0 Vr[km sec-1] Angular Offset 100 200 300 400 K

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0.0 5.0 Vr[km sec-1] Angular Offset 100 200 300 400

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0.0 2.0 4.0 Vr[km sec-1] Angular Offset 100 200 300 400 K

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0.0 2.0 4.0 Vr[km sec-1] Angular Offset 100 200 300 400

Non-LTE results : PV diagram (SiO)

✦

various features in PV diagram [due to smaller τ than 12CO]

✦

“hole” or “gap” in some of the cuts, which do not appear in 12CO PVs

✦

cuts of slightly different positions show quite different structures (e.g. (e) & (d) ) ⇒ complex vel. structure

SiO(7-6), 60deg 1st-moment gap/hole

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0.0 0.5 1.0 Vr[km sec-1] y[AU]

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500 1000 x[AU]

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(a) (b) (c) (d)(e)

(b) (c) (e) (d) disk rot. in front..? weak signature from outflow..? disk rot. in front ..?

2008年12月22日月曜日

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SLIDE 17

Non-LTE results : vel. structure (CO)

✦

CO(2-1) vel. 1st moment

✦

Δv~1km/sec, irrespective of transition [J] ←large τ, velocity at the surface appears

✦

  • vel. gradient across

the outflow axis

✦

disk rotation : slower in outside region ⇒small vel. grad. at overlap region

  • f disk & outflow

0.00 0.05 0.10 0.15 0.20 Vr[km sec-1] z[AU]

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500 1000 x[AU]

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0.0 0.5 Vr[km sec-1] z[AU]

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500 1000 x[AU]

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500 1000 x[AU]

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500 1000

v =

  • Tbvrdvr

Tbdvr −1

θ=0[pole-on] θ=30 θ=60 θ=90[edge-on]

2008年12月22日月曜日

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SLIDE 18
  • 0.2
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0.0 0.1 0.2 Vr[km sec-1] z[AU]

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500 1000 x[AU]

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0.0 0.5 Vr[km sec-1] z[AU]

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Non-LTE results : vel. structure (SiO)

✦

SiO(7-6) vel. 1st moment

✦

Δv depends on viewing angle : nonLTE effects

✦

  • vel. gradient across

the outflow axis is smaller than CO

✦

centrifugal-force driven outflow ⇒sign(vz) change in pole-on view v =

  • Tbvrdvr

Tbdvr −1

θ=0[pole-on] θ=30 θ=60 θ=90[edge-on] inflowing disk

  • utflow

inflow along the rot. axis

2008年12月22日月曜日

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SLIDE 19
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0.0 0.1 0.2 Vr[km sec-1] z[AU]

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500 1000 x[AU]

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Non-LTE results : vel. structure (SiO)

✦

SiO(4-3) vel. 1st moment

✦

  • vel. gradient across

the outflow axis is clearer than SiO(7-6)

✦

non-LTE effects v =

  • Tbvrdvr

Tbdvr −1

θ=0[pole-on] θ=30 θ=60 θ=90[edge-on]

2008年12月22日月曜日

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SLIDE 20
  • 0.5

0.0 0.5 Vr[km sec-1] z[AU]

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500 1000 x[AU]

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Non-LTE results : vel. structure (SiO)

✦

SiO(2-1) vel. 1st moment

✦

  • vel. gradient across

the outflow axis is clearer than SiO(7-6) v =

  • Tbvrdvr

Tbdvr −1

θ=0[pole-on] θ=30 θ=60 θ=90[edge-on]

2008年12月22日月曜日

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SLIDE 21

Non-LTE results : PV diagram (SiO)

✦

  • rigin of “gap”-like structure in PV diagram [simple view]

✦

  • rot. of disk, and resultant rot. of outflow [outflow : magneto-centrifugal force driven]

⇒ small amount of matter without rotation (Vr = 0)

✦

2D probability distribution function roughly agree with this interpretation

  • vel. 1-st moment

SiO(4-3), 30deg v =

  • Tbvrdvr

Tbdvr −1

  • 1

.

  • .

5 . . 5 V r [ k m s e c

  • 1

] y [ A U ]

  • 1
  • 5

5 1 x [ A U ]

  • 1
  • 5

5 1

envelope

* there are other vel. component, and projection of these vel. also affects PV diagrams [infall in disk...]

2008年12月22日月曜日

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SLIDE 22

Bernes Problem (blue/red asymmetry)

✦ Infalling gas cloud of finite optical thickness produces double-horn line

profile skewed to blue-ward

✦

combination of LOS projection of infalling & non-LTE effects

✦

infalling motion skews iso-LOS-velocity contour [red/blue color]

✦

emission from regressing side experiences absorption, but approaching side does not ⇒ blue side becomes brighter

basically our results are combination of this kind of effect and bipolar outflow

Tex Tex Tex Tex

< <

2008年12月22日月曜日

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SLIDE 23

↑hydro(Machida, M. N.) ←column density(color)

  • range lines : PV cut

Non-LTE results : PV diagrams (CO. v.s. SiO)

2008年12月22日月曜日

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SLIDE 24

PV diagram : CO

CO, 30deg, y=2x10-4 J=1-0 J=2-1 J=3-2 J=4-3

2008年12月22日月曜日

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SLIDE 25

PV diagram : SiO

SiO, 30deg, y=2x10-8 J=2-1 J=4-3 J=7-6 J=8-7 disk(+outflo w?) rotation envelope τ gaps thermal broadening

2008年12月22日月曜日

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SLIDE 26

PV diagram : SiO

SiO, 60deg, y=2x10-8 J=2-1 J=4-3 J=7-6 J=8-7

2008年12月22日月曜日

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SLIDE 27

PV diagram : SiO

SiO, 90deg, y=2x10-8 J=2-1 J=4-3 J=7-6 J=8-7

2008年12月22日月曜日

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SLIDE 28

PV diagram : SiO [Vφ = 0 run]

SiO, 90deg, y=2x10-8 J=2-1 J=4-3 J=7-6 J=8-7

2008年12月22日月曜日

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SLIDE 29

PV diagram : SiO [Vφ = 0 run]

SiO, 0deg, y=2x10-8 J=2-1 J=4-3 J=7-6 J=8-7

2008年12月22日月曜日

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SLIDE 30

PV diagram : SiO [Vφ = 0 run]

SiO, 30deg, y=2x10-8 J=2-1 J=4-3 J=7-6 J=8-7

2008年12月22日月曜日

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SLIDE 31

PV diagram : SiO [Vφ = 0 run]

SiO, 60deg, y=2x10-8 J=2-1 J=4-3 J=7-6 J=8-7

2008年12月22日月曜日

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SLIDE 32

PV diagram : SiO [isothermal]

SiO, 0deg, y=2x10-8 J=2-1 J=4-3 J=7-6 J=8-7

2008年12月22日月曜日

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SLIDE 33

PV diagram : SiO [isothermal]

SiO, 30deg, y=2x10-8 J=2-1 J=4-3 J=7-6 J=8-7

2008年12月22日月曜日

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SLIDE 34

PV diagram : SiO [isothermal]

SiO, 60deg, y=2x10-8 J=2-1 J=4-3 J=7-6 J=8-7

2008年12月22日月曜日

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SLIDE 35

PV diagram : SiO [isothermal]

SiO, 90deg, y=2x10-8 J=2-1 J=4-3 J=7-6 J=8-7

2008年12月22日月曜日

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SLIDE 36

PV diagram : SiO [isothermal v.s. barotropic]

SiO, 90deg, y=2x10-8 J=2-1 barotropic isothermal

✦barotropic : 10K<Tkin<178K

⇔isothermal : Tkin = 10K

✦spiky structures disappear

⇒ thermal broadening origin confirmed!!

✦broad abs. profile at the center in

barotropic case, leading to smaller

  • ptical thickness at the outer part

✦otherwise quite similar (almost all the

region is of Tkin=10 K in barotropic runs)

2008年12月22日月曜日

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SLIDE 37

PV diagram : SiO [Vφ≠0 v.s. Vφ=0]

SiO, 90deg, y=2x10-8 J=4-3 Vφ≠0 Vφ=0

✦Vφ of disk & outflow introduces

blue/red change close to the center ⇔Vφ=0 run seems more “straight” in this plot

✦spiky structure still appear

⇒ origin is not in rotation and/or bulk motion, but thermal origin

✦rotation of outflow appear clearer in

  • vel. moment maps
  • 0.6
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0.0 0.2 0.4 0.6 Vr[km sec-1] z[AU]

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500 1000 x[AU]

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500 1000 x[AU]

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Vφ≠0 Vφ=0 SiO, 30deg, y=2x10-8 ∇v

2008年12月22日月曜日

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SLIDE 38

Rotation of Outflow : “disk-wind”-like model

*fist detection of

  • utflow rotation

*incl.=85deg.

✦disk-wind like model

: rotation is the key

✦symmetric around the center (not to

the equator) will be observed unless EXACTLY edge-on view SiO(4-3), y=2x10-8 Launhardt et al. 2008 model

  • bs.(IRAM/PdBI)
  • 1.0
  • 0.5

0.0 0.5 Vr[km sec-1] y[AU]

  • 1000
  • 500

500 1000 x[AU]

  • 1000
  • 500

500 1000

∇v

  • 0.6
  • 0.4
  • 0.2

0.0 0.2 0.5 0.6 Vr[km sec-1] z[AU]

  • 1000
  • 500

500 1000 x[AU]

  • 1000
  • 500

500 1000

color : v first moment black contour : 12CO(2-1) white contour : 270GHz

  • cont. w/ SMA

2008年12月22日月曜日

slide-39
SLIDE 39

Very rough analysis finishes.. what’s next?

2008年12月22日月曜日

slide-40
SLIDE 40

Line Profile Distribution : CO

θ=30deg,J=2-1

*(almost) featureless Tb[K] Vr [km/sec] very broad line width (~+/- 5 km sec-1)

2008年12月22日月曜日

slide-41
SLIDE 41

*asymmetric double- horn profile distribution in the FOV

Line Profile Distribution : SiO

θ=30deg,J=4-3

Vr [km/sec] Tb[K] very broad line width (~+/- 5 km sec-1)

2008年12月22日月曜日

slide-42
SLIDE 42

Line Profile Distribution : zoom-up θ=30deg,J=4-3

Vr [km/sec] Tb[K]

2008年12月22日月曜日

slide-43
SLIDE 43

Contribution Function [in progress]

✦ What component [envelope, disk, outflow.... /infall, outflow, rotation....]

dominates the intensity?

✦

contribution function analysis underway Cf(ν, τν) ≡ Sνe−∆τν

  • 1 − exp
  • −
  • dτνdl
  • *fractional

contributions from

  • utflow/envelope/disk

components (2) (3) (4) (5)

2008年12月22日月曜日

slide-44
SLIDE 44

Contribution Function [in progress](cont.)

✦ What component [envelope, disk, outflow.... /infall, outflow, rotation....]

dominates the intensity?

✦

contribution function analysis underway Cf(ν, τν) ≡ Sνe−∆τν

  • 1 − exp
  • −
  • dτνdl
  • *fractional

contributions from

  • utflow/envelope/disk

components (6) (7) (10) (11)

2008年12月22日月曜日

slide-45
SLIDE 45

Discussion & Summary

✦

non-LTE line transfer study of YSO outflow in young stage ⇔ launching mechanism?

✦

12CO, SiO rot. transitions → large difference in τ, and vel. structures in line emission

[PV diagram, line profile...]

✦

PV diagrams of SiO show “gap” structures

✦

rotation of disk & outflow, ..⇒ might be a possible evidence for ”disk-wind”-like models

✦

thermal width can bring larger “velocity” in line emission than true hydro. velocity

✦

Future :

✦

chemistry → no depletion, shock chemistry

✦

experiments with artificial abundance distribution underway

✦

boundary condition→envelope would not be negligible

✦

nested grid RT scheme is necessary

✦

realistic comparison of simulation and observation...

✦

SMA/ALMA simulation? [Brinch et al.2008]

✦

RT simulation data : standard FITS

any radio observers can do it! detailed analysis necessary

2008年12月22日月曜日