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Stellar molecular jets trace by maser emission
Hiroshi Imai (Kagoshima University)
Stellar molecular jets trace by maser emission
Hiroshi Imai (Kagoshima University)
IAU Symposium 242: 14 March 2007, Alice Springs, Australia
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Stellar molecular jets trace by maser emission
Hiroshi Imai (Kagoshima University)
Stellar molecular jets trace by maser emission
Hiroshi Imai (Kagoshima University)
Combination of collaborations withPhilip Diamond, Wouter Vlemmings (Jodrell Bank Obs., UK)Mark Morris (UCLA, USA)Raghvendra Sahai (JPL/NASA, USA)Shuji Deguchi (Nobeyama Radio Obs., Japan)Jun-ichi Nakashima (ASIAA, Taiwan)Sun Kwok (Univ. Hong Kong, China)Kumiko Obara, Toshihiro Omodaka (Kagoshima Univ., Japan)Tetsuo Sasao (NAOJ, Japan)
Combination of collaborations withPhilip Diamond, Wouter Vlemmings (Jodrell Bank Obs., UK)Mark Morris (UCLA, USA)Raghvendra Sahai (JPL/NASA, USA)Shuji Deguchi (Nobeyama Radio Obs., Japan)Jun-ichi Nakashima (ASIAA, Taiwan)Sun Kwok (Univ. Hong Kong, China)Kumiko Obara, Toshihiro Omodaka (Kagoshima Univ., Japan)Tetsuo Sasao (NAOJ, Japan)
IAU Symposium 242: 14 March 2007, Alice Springs, Australia
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Transition from spherically symmetric
to asymmetric mass loss flow
Transition from spherically symmetric
to asymmetric mass loss flow
When/how is a bipolar jet launched in the final stellar evolution?
When/how is a bipolar jet launched in the final stellar evolution?
Egg Nebula ⓒ NASA
Betelgeuse ⓒ NASA
Hen2-90 (Sahai et al. 1998)
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“Water fountains” in AGB/post-AGB phases“Water fountains” in
AGB/post-AGB phases
Molecular rather than optical emission jetsExpansion velocity Vexp(H2O) >> Vexp (OH1612MHz)
(~30 km/s)Evolved stars
difficulty in evolved star identificationc.f identification with SPITZER/AKARI
1612 MHz OH maser withperiodic flux variation
Detection of SiO masers
Molecular rather than optical emission jetsExpansion velocity Vexp(H2O) >> Vexp (OH1612MHz)
(~30 km/s)Evolved stars
difficulty in evolved star identificationc.f identification with SPITZER/AKARI
1612 MHz OH maser withperiodic flux variation
Detection of SiO masers
W43A
IRAS16342-3814
IRAS19134+2131
High velocity stellar H2O maser sources(Likkel et al. 1992)High velocity stellar H2O maser sources(Likkel et al. 1992)
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10 water fountains identified to date 10 water fountains identified to date
W43A(Diamond et al. 1985; Imai et al. 2002, 2005; Vlemmings et al. 2006)
IRAS 19134+2131 (Imai et al. 2004; 2007 in prep.)
IRAS 16342-3814 (Sahai et al. 1999; Morris et al. 2003; Claussen et al. 2004)
OH 12.8-0.9 (Boboltz & Marvel 2005)
IRAS18286-0959 (Deguchi et al. 2007; Imai et al. in prep.)
IRAS18460-0151 (Deguchi et al. 2007; Imai et al. in prep.)
IRAS18596+0315 (Deacon et al. 2007)IRAS15445-5449 (Deacon et al. 2007)IRAS15544-5332 (Deacon et al. 2007)IRAS18043-2116 (Deacon et al. 2007)
W43A(Diamond et al. 1985; Imai et al. 2002, 2005; Vlemmings et al. 2006)
IRAS 19134+2131 (Imai et al. 2004; 2007 in prep.)
IRAS 16342-3814 (Sahai et al. 1999; Morris et al. 2003; Claussen et al. 2004)
OH 12.8-0.9 (Boboltz & Marvel 2005)
IRAS18286-0959 (Deguchi et al. 2007; Imai et al. in prep.)
IRAS18460-0151 (Deguchi et al. 2007; Imai et al. in prep.)
IRAS18596+0315 (Deacon et al. 2007)IRAS15445-5449 (Deacon et al. 2007)IRAS15544-5332 (Deacon et al. 2007)IRAS18043-2116 (Deacon et al. 2007)
Chapman’stalkChapman’stalk
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Recent topics of water fountainsRecent topics of water fountains
MHD jets! (Vlemmings’ talk)Lifetime and timing
Equatorial flow?Ballistic corkscrew jets?
Location and motion in the GalaxyPrecursors of water fountain
(e.g. WX Psc, IRC-10414)
MHD jets! (Vlemmings’ talk)Lifetime and timing
Equatorial flow?Ballistic corkscrew jets?
Location and motion in the GalaxyPrecursors of water fountain
(e.g. WX Psc, IRC-10414)
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Lifetime and timingLifetime and timing
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Dynamical age estimationDynamical age estimationH2O maser proper motions in W43A(Imai et al. 2002; Imai et al. 2005; Imai & Diamond in Prep.)H2O maser proper motions in W43A(Imai et al. 2002; Imai et al. 2005; Imai & Diamond in Prep.)
Jet velocity =145 km/s, dynamical age ~50 yrJet velocity =145 km/s, dynamical age ~50 yr
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Dynamical ages (now)Dynamical ages (now)
IRAS16342-3814: ~100 yr (Morris et al. 2004) OH12.8-0.9: ~70 yr (Boboltz & Marvel 2005)IRAS18286-0959: ~15 yr (Imai et al. in prep.)W43A: ~50 yr (Imai & Diamond in prep.)IRAS18460-0151: ~5 yr (Imai et al. in prep.)IRAS19134+2131: ~50 yr (Imai et al. in prep.)
IRAS16342-3814: ~100 yr (Morris et al. 2004) OH12.8-0.9: ~70 yr (Boboltz & Marvel 2005)IRAS18286-0959: ~15 yr (Imai et al. in prep.)W43A: ~50 yr (Imai & Diamond in prep.)IRAS18460-0151: ~5 yr (Imai et al. in prep.)IRAS19134+2131: ~50 yr (Imai et al. in prep.)
-23 - -10 km s-1 -121- -117 km s-1
IRAS 19134+2131
(Imai et al. in prep.)
IRAS 19134+2131
(Imai et al. in prep.)
~Human lifetime
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1612 MHz OH masers 1612 MHz OH masers
Imai et al. (2002)
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1612 MHz OH masers1612 MHz OH masers
OH maser shell (R~500 AU, Vexp=9km/s)Periodic OH maser variation (P~360d, Herman & Habing 1985)OH maser shell (R~500 AU, Vexp=9km/s)Periodic OH maser variation (P~360d, Herman & Habing 1985)
1612 MHz OH masers (Imai & Diamond in prep.)
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How visible is W43A?How visible is W43A?
SiO masers (Nakashima & Deguchi 2002; Imai et al. 2005)Dust envelope in 2.7 mm emission: R< 3000 AUEnvelope dynamical age T~ 260 years (OH), 1600 years (dust)
SiO masers (Nakashima & Deguchi 2002; Imai et al. 2005)Dust envelope in 2.7 mm emission: R< 3000 AUEnvelope dynamical age T~ 260 years (OH), 1600 years (dust)
SPITZER/GLIMPSEImage
(Deguchi et al. 2007)
SPITZER/GLIMPSEImage
(Deguchi et al. 2007)
20000 AU at 2.6 kpc
+H2O & OH masers
2.7 mm continuumImage (Imai et al.)
2.7 mm continuumImage (Imai et al.)
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Transition to pre-planetary nebula (PPN) phase
Transition to pre-planetary nebula (PPN) phase
IRAS 19134+2131(by R. Sahai)
Visible in visual lightVisible in visual lightVisible in mid-IRVisible in mid-IR
c.f. IRAS 16342-3814 (Sahai et al. 2001)
W43A(Deguchi et al. 2007)
c.f. OH12.8-0.9,IRAS18286-0959, IRAS18460-0151
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Quenching water fountainwithin < 1000 years
Quenching water fountainwithin < 1000 years
Gomez’s talkGomez’s talk
Photodissociationdestroying H2O molecules
Tip of jet achieves to the outer low-density region of a circumstellar envelope
Photodissociationdestroying H2O molecules
Tip of jet achieves to the outer low-density region of a circumstellar envelope
5000 AU
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Equatorial flowsEquatorial flows
W43AIRAS 18286-0959IRAS 18460-0151
W43AIRAS 18286-0959IRAS 18460-0151
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Wide opening angle biconicalSiO maser flow
(~15 km/s)|
within 10 AU|
H2O maser jet
(Imai et al. 2005)(Imai et al. in prep.)
Wide opening angle biconicalSiO maser flow
(~15 km/s)|
within 10 AU|
H2O maser jet
(Imai et al. 2005)(Imai et al. in prep.)
Where is a disk?Where is a disk?
SiO/H2O maser locationsSiO/H2O maser locations
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Proper motion in the equatorial flowProper motion in the equatorial flow
W43A(Imai & Diamond in prep)
W43A(Imai & Diamond in prep)
Flow velocity ~30 km/sFlow velocity ~30 km/s
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IRAS 18460-0151(Deguchi et al. 2007)IRAS 18460-0151(Deguchi et al. 2007)
Fastest (~350 km s-1) and youngest (t~5 yr) water fountain!
Equatorial flow (Vexp~30 km s-1)?
Fastest (~350 km s-1) and youngest (t~5 yr) water fountain!
Equatorial flow (Vexp~30 km s-1)?
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IRAS 18286-0959(Deguchi et al. 2007)
IRAS 18286-0959(Deguchi et al. 2007)
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Ballistic corkscrew jetsBallistic corkscrew jets
IRAS 16342-3814W43A
IRAS 19134+2131
IRAS 16342-3814W43A
IRAS 19134+2131
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W43A in detail: Jet precessionW43A in detail: Jet precession
Precession period ~55 yearsPrecession angle amplitude ~5°Precession period ~55 yearsPrecession angle amplitude ~5°
-500
-250
0
250
500
-1000-50005001000
Maser spot (Oct. 1994)Precessing jet model (1994.8)
Y (A
U)
X (AU)
Maser spot (Apr. 2002)Precessing jet model (2002.3)
Imai et al. 2005Imai et al. 2005
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Corkscrew jet?Bow shock front?Corkscrew jet?
Bow shock front?
W43A (Imai & Diamond in prep)W43A (Imai & Diamond in prep)
Proper motions with a systemic velocity vector subtracted
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Corkscrew jet?Bow shock front?Corkscrew jet?
Bow shock front?(VLA)
500 AU at 8 kpc
(VLBA)
(VLBA)
Imai et al. (2004)Imai et al. (2004) Imai et al. (2007)Imai et al. (2007)
IRAS19134+2131IRAS19134+2131
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Corkscrew jet!Corkscrew jet!IRAS16342-3814(Sahai et al. 2005)
Lp image with Keck
What happens in the H2O maserproper motions?
Lp (red), Kp (green), HST (blue) image
IRAS16342-3814(Sahai et al. 2005)
Lp image with Keck
What happens in the H2O maserproper motions?
Lp (red), Kp (green), HST (blue) image
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Location and motion in the Milky Way Galaxy
Location and motion in the Milky Way Galaxy
IRAS19134+2131IRAS19134+2131
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Maser motion with respect toa position-reference QSO
- Exploring the roots of water fountain -
Maser motion with respect toa position-reference QSO
- Exploring the roots of water fountain -
Galacticrotation
H2O masers in IRAS 19134+2131 (Imai et al. 2007)H2O masers in IRAS 19134+2131 (Imai et al. 2007)
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Annual parallax and Galactic rotation
Annual parallax and Galactic rotation
Location and motion
in the Galaxy
Location and motion
in the Galaxy
Annual parallax distance = 8.0+0.9-0.7 kpc
Location: (R, θ, z)=(7.4+0.4-0.3 kpc, 62±5 deg, 650+70
-60 pc)3D velocity (VR, Vθ, Vz) =(3+53
-46, 125+20-28, 8+48
-39 )[km/s]
Annual parallax distance = 8.0+0.9-0.7 kpc
Location: (R, θ, z)=(7.4+0.4-0.3 kpc, 62±5 deg, 650+70
-60 pc)3D velocity (VR, Vθ, Vz) =(3+53
-46, 125+20-28, 8+48
-39 )[km/s]
ⒸKagaya
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Location and velocity in the GalaxyLocation and velocity in the Galaxy
Progenitors of bipolar PNe may be higher mass starslocated near the Galactic plane (Manchado 2004).
Single intermediate-mass evolved star can create both a collimated jet and an equatorial flow
(not accretion disk).(Blackman et al. 2001; S. Miyaji in private communication)
Progenitors of bipolar PNe may be higher mass starslocated near the Galactic plane (Manchado 2004).
Single intermediate-mass evolved star can create both a collimated jet and an equatorial flow
(not accretion disk).(Blackman et al. 2001; S. Miyaji in private communication)
Travel time from the Galactic plane
1.1-7.7 x 107 yearsM*< 5-5.8 M◉
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SummarySummaryMagneto-hydrodynamicalCorkscrew/precessing jetV> 100 km s-1, T~100 years
Magneto-hydrodynamicalCorkscrew/precessing jetV> 100 km s-1, T~100 years
Equatorial flowV~ 30 km s-1
Evolving from AGB envelope?
Equatorial flowV~ 30 km s-1
Evolving from AGB envelope?
M*< 5 Msun single AGB/post-AGB star(or binary <10 AU?)
M*< 5 Msun single AGB/post-AGB star(or binary <10 AU?)
Only 10 water fountainsin the whole Galaxy?Only 10 water fountainsin the whole Galaxy?
ⒸNSF
![IPD/Bim Thesis Proposal - engr.psu.edu · [IPD/BIM THESIS PROPOSAL] Jason Brognano, Michael Gilroy, Stephen Kijak, David Maser December 6, 2010 KGB Maser KGB Maser| BIM/IPD Thesis](https://img.pdfslide.us/doc/110x75/605d339025f9181d960e06e8/ipdbim-thesis-proposal-engrpsuedu-ipdbim-thesis-proposal-jason-brognano.jpg)
