Ultra-Compact HII Regions and Massive Star Formation

By E. Churchwell. 2002

309 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics

View Paper: https://www.semanticscholar.org/paper/0998c3d13839e2bf5fc6134ba70221c72ffd51d7

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Atomic and Molecular Physics, and Optics

Citations in the corpus

GLIMPSE. I. An SIRTF Legacy Project to Map the Inner Galaxy (2003, methodology): “GLIMPSE data will provide information on the stellar content of all of the principal stages of massive star formation, summarized recently in Churchwell (2002).”
The Destruction of Cosmological Minihalos by Primordial Supernovae (2008, background): “The photons may downscatter to radio wavelengths, as observed in hypercompact H ii regions deepwithinmolecular cloud cores (Churchwell 2002; Rodrı́guez 2005).”
Toward Understanding Massive Star Formation (2007, background): “…Region (Genzel & Stutzki 1989) • Physical Conditions in Regions of Star Formation (Evans 1999) • Ultra-Compact HII Regions and Massive Star Formation (Churchwell 2002) • Massive Stars in the Local Group: Implications for Stellar Evolution and Star Formation (Massey 2003) • The First…”
OUTFLOW FEEDBACK REGULATED MASSIVE STAR FORMATION IN PARSEC-SCALE CLUSTER-FORMING CLUMPS (2009, background): “Wood & Churchwell (1989) estimated an age of ∼105 yr for UC H ii regions, which probably represent a relatively late stage of massive star formation, when the bulk of mass accretion has completed and the mass accretion rate becomes too low to trap the H ii region (Churchwell 2002).”
Interpreting Spectral Energy Distributions from Young Stellar Objects. I. A Grid of 200,000 YSO Model SEDs (2006, methodology): “The average values were chosen to match estimates of low-mass (Adams et al. 1987; Kenyon et al. 1993a,b; Whitney et al. 1997) and high-mass YSOs (Wolfire & Cassinelli 1987; Osorio et al. 1999; Omukai & Palla 2001; Churchwell 2002; Yorke & Sonnhalter 2002; McKee & Tan 2003; Bonnell et al. 2004).”
ISO Spectroscopy of Gas and Dust: From Molecular Clouds to Protoplanetary Disks (2004, background): “For higher mass objects where the temporal ordering is much less clear (Churchwell 2002), infrared spectroscopy is a powerful tool to characterize the earliest stages.”
Infrared Dark Clouds: Precursors to Star Clusters (2004, background): “" Hot cores are internally heated (50–250 K), small (<0.1 pc), massive (∼100–300 M ⊙ ), and dense (10 5 – 10 8 cm −3 ; see Table 1; Garay & Lizano 1999; Kurtz et al. 2000; Churchwell 2002).”
The RMS survey - 6 cm continuum VLA observations towards candidate massive YSOs in the northern hemisphere (2009, background): “These are generally classified as: unresolved, Gaussian, spherical, core-halo, cometary, irregular and bipolar (see Churchwell 2002, for a review).”
EMU: Evolutionary Map of the Universe (2011, background): “Ultracompact HII (UCHII) regions represent a young (,105 years old) phase in the development of an HII region (Churchwell 2002).”
A Catalog of CH3OH 70-61 A+ Maser Sources in Massive Star-forming Regions (2004, background): “Several relevant reviews are Garay & Lizano (1999), Evans (1999), and Churchwell (2002).”
High-resolution panchromatic spectral models of galaxies including photoionization and dust (2009, background): “At early times, each individual star is expected to be surrounded by a very compact H ii region where dust can absorb a significant fraction of the ionizing photons (Churchwell 2002; Dopita et al. 2003).”
The evolution of the spectral energy distribution in massive young stellar objects (2008, background): “If, as we have been assuming throughout our analysis and interpretation, the IR-P sources are representative of the UCHII phase with an expected timescale of ∼105 years (Churchwell 2002), then the duration of the phase traced by the MM-P sources we detect should be of the order of ∼5× 104 years.”
Modeling the Pan-Spectral Energy Distribution of Starburst Galaxies. IV. The Controlling Parameters of the Starburst SED (2007, background): “During this phase, the cluster acts as an ensemble of Ultra-Compact H II regions (UCHII), each trapped at sub-parsec scales around their individual massive parent stars (see Churchwell 2002, for a detailed review of UCHII regions).”