Abstract
Fast stellar winds can sweep up ambient media and form bubbles. The evolution of a bubble is largely controlled by the content and physical conditions of the shocked fast wind in its interior. This hot gas was not clearly observed until the recent advent of Chandra and XMM-Newton X-ray observatories. To date, di use X-ray emission has been unambiguously detected from two circumstellar bubbles blown by WR stars, four planetary nebulae, and two superbubbles blown by young clusters. Model fits to the X-ray spectra show that the circumstellar bubbles are dominated by hot gas with low temperatures (≤ 3 × 106 K), while the interstellar bubbles contain significant fractions of hotter gas (≥ 5 × 106 K). In all cases, large discrepancies in the X-ray luminosity are found between observations and conventional models of bubbles. Future theoretical models of bubbles need to re-examine the validity of heat conduction and take into account realistic microscopic processes such as mass loading from dense clumps/knots and turbulent mixing. Chandra ACIS-S observation of NGC6888 will shed light on these astrophysical processes.
| Original language | English (US) |
|---|---|
| Pages (from-to) | 62-67 |
| Number of pages | 6 |
| Journal | Revista Mexicana de Astronomia y Astrofisica: Serie de Conferencias |
| Volume | 15 |
| State | Published - Dec 1 2003 |
| Event | Winds, Bubbles and Explosions: A Conference to Honor John Dyson - Patzcuaro, Michoacan, Mexico Duration: Sep 9 2002 → Sep 13 2002 |
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Keywords
- H II regions
- ISM: bubbles
- Planetary nebulae
- Stars: Wolf-Rayet
- Stars: mass loss
- X-rays: ISM
ASJC Scopus subject areas
- Space and Planetary Science
- Astronomy and Astrophysics
Cite this
An inside-out view of bubbles. / Chu, You Hua; Gruendl, Robert A.; Guerrero, Martín A.
In: Revista Mexicana de Astronomia y Astrofisica: Serie de Conferencias, Vol. 15, 01.12.2003, p. 62-67.Research output: Contribution to journal › Conference article
}
TY - JOUR
T1 - An inside-out view of bubbles
AU - Chu, You Hua
AU - Gruendl, Robert A.
AU - Guerrero, Martín A.
PY - 2003/12/1
Y1 - 2003/12/1
N2 - Fast stellar winds can sweep up ambient media and form bubbles. The evolution of a bubble is largely controlled by the content and physical conditions of the shocked fast wind in its interior. This hot gas was not clearly observed until the recent advent of Chandra and XMM-Newton X-ray observatories. To date, di use X-ray emission has been unambiguously detected from two circumstellar bubbles blown by WR stars, four planetary nebulae, and two superbubbles blown by young clusters. Model fits to the X-ray spectra show that the circumstellar bubbles are dominated by hot gas with low temperatures (≤ 3 × 106 K), while the interstellar bubbles contain significant fractions of hotter gas (≥ 5 × 106 K). In all cases, large discrepancies in the X-ray luminosity are found between observations and conventional models of bubbles. Future theoretical models of bubbles need to re-examine the validity of heat conduction and take into account realistic microscopic processes such as mass loading from dense clumps/knots and turbulent mixing. Chandra ACIS-S observation of NGC6888 will shed light on these astrophysical processes.
AB - Fast stellar winds can sweep up ambient media and form bubbles. The evolution of a bubble is largely controlled by the content and physical conditions of the shocked fast wind in its interior. This hot gas was not clearly observed until the recent advent of Chandra and XMM-Newton X-ray observatories. To date, di use X-ray emission has been unambiguously detected from two circumstellar bubbles blown by WR stars, four planetary nebulae, and two superbubbles blown by young clusters. Model fits to the X-ray spectra show that the circumstellar bubbles are dominated by hot gas with low temperatures (≤ 3 × 106 K), while the interstellar bubbles contain significant fractions of hotter gas (≥ 5 × 106 K). In all cases, large discrepancies in the X-ray luminosity are found between observations and conventional models of bubbles. Future theoretical models of bubbles need to re-examine the validity of heat conduction and take into account realistic microscopic processes such as mass loading from dense clumps/knots and turbulent mixing. Chandra ACIS-S observation of NGC6888 will shed light on these astrophysical processes.
KW - H II regions
KW - ISM: bubbles
KW - Planetary nebulae
KW - Stars: Wolf-Rayet
KW - Stars: mass loss
KW - X-rays: ISM
UR - http://www.scopus.com/inward/record.url?scp=70649083189&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=70649083189&partnerID=8YFLogxK
M3 - Conference article
AN - SCOPUS:70649083189
VL - 15
SP - 62
EP - 67
JO - Revista Mexicana de Astronomia y Astrofisica: Serie de Conferencias
JF - Revista Mexicana de Astronomia y Astrofisica: Serie de Conferencias
SN - 1405-2059
ER -