Induced Star Formation in the Orion and Monoceros Molecular Clouds Hsu-Tai Lee and Wen-Ping Chen...
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![Page 1: Induced Star Formation in the Orion and Monoceros Molecular Clouds Hsu-Tai Lee and Wen-Ping Chen National Central University, Institute of Astronomy.](https://reader035.fdocuments.us/reader035/viewer/2022062421/56649d595503460f94a39f4b/html5/thumbnails/1.jpg)
Induced Star Formation in tInduced Star Formation in the Orion and Monoceros he Orion and Monoceros
Molecular CloudsMolecular Clouds
Hsu-Tai Lee and Wen-Ping Chen
National Central University, Institute of Astronomy
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OutlineOutline
IntroductionSource of Data and ObservationsIndividual Molecular CloudDiscussion
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IntroductionIntroduction
The Orion & Monoceros molecular clouds are 2 nearby active star-forming regions
Orion OB1 association (450 pc)Mon R2 (830 pc)Orion-Eridanus bubble – a series of superno
va explosions in the Orion OB1
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Triggered Star FormationTriggered Star Formation
Elmegreen, B. G. 1998, ASP Conf. Ser., 148
Small Scale: Globule-SqueezingIntermediate Scale: Collect and CollapseLarge Scale: Shells and Rings
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Small scale triggeringSmall scale triggering
Direct squeezing of pre-existing clouds or globules by high pressure. This includes triggering in bright rims, proplyds, and small cometary globules.
OB stars
Molecular cloud
Young stars
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Intermediate scale triggeringIntermediate scale triggering
Compression of a nearby pre-existing cloud from one side, leading to a dense ridge of moving gas.
OB stars
Molecular cloud
Young stars
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Large scale triggeringLarge scale triggering
Accumulation of ambient gas into an expanding shell or ring partially surrounding the pressure source, with star formation in the shell or ring presumably triggered by gravitational collapse of swept-up gas.
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Pre-Main Sequence StarPre-Main Sequence Star
Classical T Tauri star (CTTS)Strong IR and UV excessStrong emission line
Weak-lined T Tauri star (WTTS)More evolved pre-main sequence starWeak emission lineStrong soft X-ray source
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CTTS WTTS
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Source of DataSource of Data
2MASS – J (1.25μm), H (1.65μm) and Ks (2.17μm) all sky survey
CO image – Dame, T. M. et al.(2001, ApJ)IRAS 100 μm – Schlegel, D. et al. ( 1998, A
pJ)Hα image – Finkbeiner, D. P. (2003, ApJS)
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ObservationsObservations
BAO 2.1m spectroscopic observations in early 2003
Low-resolution spectra have been observed for 32 PMS candidates
24 CTTSs, 4 M stars and 4 carbon starsMost of CTTSs are located at molecular clo
ud; M and carbon stars are not associated with molecular cloud
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Hα
Hβ
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Maddalena et al. 1986
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The Red dots are the CTTSs; blue dots are the O stars.
CO image Hα image
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Orion A & B Molecular CloudOrion A & B Molecular Cloud
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TheλOri is a O8III star, and it is surrounded by a ring molecular cloud (Duerr, Imhoff, & Lada, 1982, ApJ)
IRAS 100μm Hα image
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IC 2118, LDN 1616 IC 2118, LDN 1616 & LDN 1634 & LDN 1634
Hα image IRAS 100μm
LDN 1616
IC 2118LDN 1634
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LDN 1652 LDN 1652
Hα image CO image
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object scale Pressure source
λOri region S High mass star
IC 2118 region S High mass star
Orion A & B I Superbubble
LDN 1652 L or I Supperbubble
S – small scale triggering; I – intermediate scale triggering; L – large scale triggering
Triggered star formationTriggered star formation
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Discussion IDiscussion I
Our selection criterion is good to find CTTSs.For those bright-rimmed clouds associated w
ith both strong Hα and IR emission accompany star formation
High mass star interact with molecular cloud would trigger star formation
Superbubble can also induce star formation hundreds pc away (LDN 1652)
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Discussion IIDiscussion II
CTTSs outside the bright-rimmed cloud seem to be older than those inside the bright-rimmed cloud.
Compared with WTTSs, CTTSs are more closer to recent star formation. Our CTTS candidates can be used to trace the nearby star-forming region (< 2 kpc).
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