Galactic ring nebulae associated with Wolf-Rayet stars. VI - NGC 3199, anon /MR 26/, RCW 58, and RCW 104

Chu, You‐Hua

doi:10.1086/159768

Cited by 47 publications

(38 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…The dynamical age derived for the H bubble around WR 23 agrees with previous results by Chu (1982) and shows that the interstellar bubble has been blown during the present WR phase. Errors in dynamical ages are about 70%.…”

Section: Main Physical Parameters Of the Bubblessupporting

confidence: 89%

“…Based on interferometric Hα profiles, Chu (1982) and Georgelin et al (1986) found that the ionized gas has negative velocities, generally in the range −31 to −1 km s −1 , with a mean velocity of about −20 km s −1 , indicating that the nebula is related to the Carina complex. (All velocities in this paper are referred to the LSR).…”

Section: Wr 23 and Anon (Wr 23)mentioning

confidence: 99%

“…(All velocities in this paper are referred to the LSR). The expansion velocity and the dynamical age of the Hα nebula around WR 23 were estimated as 15−30 km s −1 and (2−4) × 10 5 yr, respectively (Georgelin et al 1986;Chu 1982). Marston (1996) analyzed  images at 60 and 100 µm (with angular resolutions of about 6 and 4 , respectively) and noted an infrared shell coincident in position with the optical filamentary nebula Anon (WR 23).…”

Section: Wr 23 and Anon (Wr 23)mentioning

confidence: 99%

See 2 more Smart Citations

H I bubbles surrounding southern optical ring nebulae: Anon (WR 23) and RCW 52

Cappa

Niemelä

Martín³

et al. 2005

A&A

View full text Add to dashboard Cite

Abstract.We analyze the interstellar medium in the environs of two hot and massive stars, HD 92809 (=WR 23, WC6) and LSS 1887 (O8V), which ionize the optical ring nebulae Anon (WR 23) and RCW 52, respectively. Our analysis is based on neutral hydrogen (H) 21 cm line data, which reveal interstellar bubbles surrounding the massive stars and their optical ring nebulae. The H bubble related to WR 23 is 13.3 pc in radius and is expanding at 10 km s −1 . The associated atomic neutral mass is 830 M . The H structure related to LSS 1887 is about 6.3 pc in radius, has an expansion velocity of 7 km s −1 and an associated atomic neutral mass of 100 M . These H features are the neutral counterparts of the optical ring nebulae and were mainly created by the action of the stellar winds of the massive stars on their environs. The dynamical age of the H bubble around WR 23 (7 × 10 5 yr) suggests that it was created during the WR phase of stellar evolution. However, the large tangential motions of WR 23 and LSS 1887 suggest that part of the observed optical and H structures may be due to a bow shock. The analysis of the distribution of emission in the far infrared and in the CO(1−0) molecular line in the environs of WR 23 and LSS 1887 reveals that there are also infrared and molecular counterparts of the detected H bubbles.

show abstract

Section: Main Physical Parameters Of the Bubblessupporting

confidence: 89%

Section: Wr 23 and Anon (Wr 23)mentioning

confidence: 99%

Section: Wr 23 and Anon (Wr 23)mentioning

confidence: 99%

See 1 more Smart Citation

H I bubbles surrounding southern optical ring nebulae: Anon (WR 23) and RCW 52

Cappa

Niemelä

Martín³

et al. 2005

A&A

View full text Add to dashboard Cite

show abstract

“…Hence, in this special circumstance, features can have a large range in distance without exhibiting a corresponding difference in velocity. RCW48 is a large ionised region appearing as a collection of thin filaments and exhibiting a centre-edge velocity gradient (Deharveng & Maucherat 1974;Chu 1982). The MHS also detected this velocity gradient, with the outer part having a mean velocity of about −8·6 km s −1 .…”

Section: Morphology and Nature Of Extended Emission Featuresmentioning

confidence: 99%

First Results from the Combination of the AAO/UKST and Marseille Hα Surveys

Russeil

Parker

2001

Publ. – Astron. Soc. Aust

View full text Add to dashboard Cite

show abstract

“…The Wolf-Rayet Nebula RCW 58 RCW 58 is a nebula surrounding the Wolf-Rayet star WR 40, and which has been formed by the current stellar wind sweeping up wind material from previous evolutionary stages, some of which is clumpy (Chu 1982;Smith et al 1988). The clumps are ionized by the central star and typically have the following properties: r c ≈ 0.1 pc, T c ≈ 10 4 K, n c ≈ 10 3 cm −3 (Arthur, Henney & Dyson 1996).…”

Section: The Helix Nebula (Ngc 7293)mentioning

confidence: 99%

Mass-Loaded Flows

Pittard

Diffuse Matter From Star Forming Regions to Active Galaxies

View full text Add to dashboard Cite

A key process within astronomy is the exchange of mass, momentum, and energy between diffuse plasmas in many types of astronomical sources (including planetary nebulae, wind-blown bubbles, supernova remnants, starburst superwinds, and the intracluster medium) and dense, embedded clouds or clumps. This transfer affects the large scale flows of the diffuse plasmas as well as the evolution of the clumps. I review our current understanding of mass-injection processes, and examine intermediate-scale structure and the global effect of mass-loading on a flow. I then discuss mass-loading in a variety of diffuse sources.Comment: Comments: To be published as a chapter in 'Diffuse Matter from Star Forming Regions to Active Galaxies' - A volume Honouring John Dyson. Eds. T. W. Harquist, J. M. Pittard and S. A. E. G. Falle. 25 pages, 7 figure

show abstract

Galactic ring nebulae associated with Wolf-Rayet stars. VI - NGC 3199, anon /MR 26/, RCW 58, and RCW 104

Cited by 47 publications

References 0 publications

H I bubbles surrounding southern optical ring nebulae: Anon (WR 23) and RCW 52

H I bubbles surrounding southern optical ring nebulae: Anon (WR 23) and RCW 52

First Results from the Combination of the AAO/UKST and Marseille Hα Surveys

Mass-Loaded Flows

Contact Info

Product

Resources

About