2016201610 27()

R136()(ICRAR/)

Outline/!

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Cloud'Cloud!Collision︎!

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!R136!

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LMC'SMC!
︎D'!&!L'components !

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︎ D'!&!L'components!
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Formation of the O-type Stars! Stars having more than 20 M
! Staller wind, strong UV, SNe, etc..
However, it is not known
how the O-type stars are formed?
! Observational issues- few, distant from us etc..
! Theoretical issues- large mass accretion rate etc.
~ 10−4–10−3 M /yr[~10−6 M /yr for low-mass stars]

We!need!some!triggering!mechanisms/
Wolﬁre!&!Cassinelli!(1986)!

Numerical Simulations of the Cloud-Cloud Collisions
Step!1!
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Step!2!
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Step!3!

Habe & Ohta 92

Anathpindika+12

Numerical Simulations of the Cloud-Cloud Collisions

Inoue & Fukui 13, ApJL

courtesy!by!Inoue'san星間雲の超音速衝突(CCC)と大質量星星団形成
Observational Evidence (e.g., SSC Westerlund 2)/(ekh k(ekRoaiWcmvei 0 D BAvs(VLSR![km/s]
Furukawa+09!
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20 km/s		星間雲の超音速衝突(CCC)と大質量星星団形成
Observational Evidence (e.g., SSC Westerlund 2)/(ekh k(ekRoavei 0 D BAiWcmvs

SSC: 4:6(VLSR![km/s]
Furukawa+09!
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20 km/s		Large Magellanic Cloud (LMC)
Distance: ~50 kpc

R136- Age: ~1.5 Myr- Mass: ~105 Mo- The mass of R136 is ten times higher than that of the Milky Way SSC- 385 O stars, ~30 WR stars (Doran et al.2013)- The largest HII region in the Local group (Crowther et al.2010)

R136- Age: ~1.5 Myr- Mass: ~105 Mo- The mass of R136 is ten times higher than that of the Milky Way SSC- 385 O stars, ~30 WR stars (Doran et al.2013)- The largest HII region in the Local group (Crowther et al.2010)

K. Bekki and M. Chiba
Previous Study: Tidal interaction between
the LMC & SMC

SMC

-0.82

-0.27

Z-axis~ 0.2 Gyr

LMC
-0.14

0Z-axisSMCe.g.,Murai & Fujimoto 80
Fujimoto & Murai 84
Fujimoto & Noguchi 90
X-axisX-axisBekki & Chiba 07

rb
T = MC ( et to for ea nter o standtaTidals ede
Previous Study:
Ce S ar isinteractiont the c in the between the LMC & SMChaMtL ith e b tim k, skesshf t del w of th is e ic di he dio) mo t!HI,!
er µ B llipt :!COtt
Banµhds ( dard e ce c an s a e lso tse
tn stan s. Th 3 kp how te ahg
bri d the ation of 0. odel s k. Noeac t) an serv size s m disfrsu (lef e ob cell -les f theCoethelod with th th e SM hotoiphred ells w ugh t st isoooc00 t alth uterm
ha e oteurt f thdC C’sroeMtnM neLh he L ithi
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iMC t 8% nitial rm e mith
Sthe abou ere i ll fo ley-S s them n,e veaww
ldhaorotctiyt
fhuc 0Gig C (S ts s % o themno2
T = gas e LM pone ly ∼ d int med
ed d th com . On ferre s for inrre un ddr sed )sa2nts
9aro lly o s 19 be tra new s iscu r com ).
ica ohlf can and be d tella 005 t!
am & R MC tars can d s hu 2 disdssbfs
uk the S . Old SMC lly o Pra d ga ck o i
C the atica m & late e laof M136
Hs!
tulaw
n eL mib ho eyoshnem an sim kal(Bekki & Chiba 07)

thePrevious Study: L- & D-components
D'component!

L'component!

Luks!&!Rohlfs!(1992),!Mizuno!et!al.!(2001)

Green:!WRDstars! Disk/HIPrevious Study: L- & D-components
D'component!

L'component!

Luks!&!Rohlfs!(1992),!Mizuno!et!al.!(2001)

Green:!WRDstars! Disk!

/HIWR" CCScientific Purpose!
Datasetwo/HI

L- & D-components
b R136i 78i( GQtsa

CD OI

L OI

A

/ 1/78 ( GQ

A

78 ( GQ&CTGD
COQ]((&D], /: O

S, ///(&k2D !
&Wc T v Wc

9MQ IW(&&)

WisIL LDIH A I DLPv

Separation of L- & D-components!
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~ −50 km s−1/ /!

1.!
!(<!10!km/s)!
!!!!(e.g.,!ANTENNAE!GALAXIES!(NGC!4038/4039);!Whitmore!et!al.!2005)!
"!

!"  

 R136  Future Work (1): Numerical simulations/

Inoue et al.

Future Work (2): Other galaxy/

Summary/
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Cloud'Cloud!Collision︎!

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!R136!

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LMC'SMC!
︎D'!&!L'components !

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︎ D'!&!L'components!
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R136!

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