Syntheses of Triazolopyridine Derivatives with Nickel Peroxide

Ogura, Haruo; Mineo, Satoshi

doi:10.3987/r-1979-01-0190

Cited by 2 publications

(6 citation statements)

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“…The molecular ring is composed of well separated, dense and massive cores, most of which are collapsing. Such regular spacing rule of the cores could not be pre-existing clumps but are formed by external triggering, which is a strong evidence for the "collect and collapse" process (Deharveng, Zavagno, & Caplan 2005;Ogura 2010). This situation contradicts the RDI model, in which the dense clumps into which the radiatively induced shocks drive are pre-existing.…”

Section: Collect and Collapse Scenariomentioning

confidence: 85%

“…This situation contradicts the RDI model, in which the dense clumps into which the radiatively induced shocks drive are pre-existing. Additionally, the large scale sequential star formation discussed in Section 4.4.1 also favors the "collect and collapse" process rather than the "RDI" model (Elmegreen & Lada 1977;Ogura 2010).…”

Section: Collect and Collapse Scenariomentioning

confidence: 99%

“…Two models have been proposed to explain the effect of massive stars on star formation: collect and collapse (Elmegreen & Lada 1977) and radiation-driven implosion (RDI; Lefloch & Lazareff 1994;Ogura 2010). The former takes place in a larger spatial size (∼10 pc) with a longer timescale (a few Myr), whereas the latter takes place in a smaller spatial size (∼1 pc) with a shorter timescale (0.5 Myr; Ogura 2010).…”

Section: Introductionmentioning

confidence: 99%

“…In the "collect and collapse" scenario, the ionization front (IF) generated from the Hii region gathers molecular gases and collects a dense shell between the IF and the SF. The gas and dust in the collected layer collapse to form stars when they reach the critical density (Chen et al 2007;Ogura 2010). This process can selfpropagate and lead to sequential star formation (Elmegreen & Lada 1977).…”

Section: Introductionmentioning

confidence: 99%

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Triggered Star Formation Surrounding Wolf-Rayet Star Hd 211853

Liu

Zhang

et al. 2012

ApJ

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The environment surrounding Wolf-Rayet (W-R) star HD 211853 is studied in molecular, infrared, as well as radio, and Hi emission. The molecular ring consists of well-separated cores, which have a volume density of 10 3 cm −3 and kinematic temperature ∼20 K. Most of the cores are under gravitational collapse due to external pressure from the surrounding ionized gas. From the spectral energy distribution modeling toward the young stellar objects, the sequential star formation is revealed on a large scale in space spreading from the W-R star to the molecular ring. A small-scale sequential star formation is revealed toward core "A", which harbors a very young star cluster. Triggered star formations are thus suggested. The presence of the photodissociation region, the fragmentation of the molecular ring, the collapse of the cores, and the large-scale sequential star formation indicate that the collect and collapse process functions in this region. The star-forming activities in core "A" seem to be affected by the radiation-driven implosion process.

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Section: Collect and Collapse Scenariomentioning

confidence: 85%

Section: Collect and Collapse Scenariomentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Triggered Star Formation Surrounding Wolf-Rayet Star Hd 211853

Liu

Zhang

et al. 2012

ApJ

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“…Theoretically, the ionization front (IF) generated from an Hii region can generate a shock front (SF) in molecular clouds and gather molecular gas to form a dense shell between the IF and the SF (Elmegreen & Lada 1977;Whitworth et al 1994). The gas and dust in the collected layer collapse to form stars when they reach the critical density (Chen et al 2007;Ogura 2010;Whitworth et al 1994). This socalled "collect and collapse" process can self propagate and lead to sequential star formation (Elmegreen & Lada 1977;Whitworth et al 1994).…”

Section: Introductionmentioning

confidence: 99%

PLANCK COLD CLUMPS IN THE Λ ORIONIS COMPLEX. I. DISCOVERY OF AN EXTREMELY YOUNG CLASS 0 PROTOSTELLAR OBJECT AND a PROTO-BROWN DWARF CANDIDATE IN THE BRIGHT-RIMMED CLUMP PGCC G192.32–11.88

Zhang

Kim

et al. 2016

ApJS

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We are performing a series of observations with ground-based telescopes toward Planck Galactic cold clumps (PGCCs) in the λ Orionis complex in order to systematically investigate the effects of stellar feedback. In the particular case of PGCC G192.32-11.88, we discovered an extremely young Class 0 protostellar object (G192N) and a proto-brown dwarf candidate (G192S). G192N and G192S are located in a gravitationally bound bright-rimmed clump. The velocity and temperature gradients seen in line emission of CO isotopologues indicate that PGCC G192.32-11.88 is externally heated and compressed. G192N probably has the lowest bolometric luminosity (∼ 0.8 L ) and accretion rate (6.3×10 −7 M yr −1 ) when compared with other young Class 0 sources (e.g. PACS Bright Red sources (PBRs)) in the Orion complex. It has slightly larger internal luminosity (0.21 ± 0.01 L ) and outflow velocity (∼14 km s −1 ) than the predictions of first hydrostatic cores (FHSCs). G192N might be among the youngest Class 0 sources, which are slightly more evolved than a FHSC. Considering its low internal luminosity (0.08 ± 0.01 L ) and accretion rate (2.8×10 −8 M yr −1 ), G192S is an ideal proto-brown dwarf candidate. The star formation efficiency (∼0.3%-0.4%) and core formation efficiency (∼1%) in PGCC G192.32-11.88 are significantly smaller than in other giant molecular clouds or filaments, indicating that the star formation therein is greatly suppressed owing to stellar feedback.

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Syntheses of Triazolopyridine Derivatives with Nickel Peroxide

Cited by 2 publications

References 0 publications

Triggered Star Formation Surrounding Wolf-Rayet Star Hd 211853

Triggered Star Formation Surrounding Wolf-Rayet Star Hd 211853

PLANCK COLD CLUMPS IN THE Λ ORIONIS COMPLEX. I. DISCOVERY OF AN EXTREMELY YOUNG CLASS 0 PROTOSTELLAR OBJECT AND a PROTO-BROWN DWARF CANDIDATE IN THE BRIGHT-RIMMED CLUMP PGCC G192.32–11.88

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