An inside-out view of bubbles

You Hua Chu, Robert A. Gruendl, Martín A. Guerrero

Research output: Contribution to journalConference article

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 languageEnglish (US)
Pages (from-to)62-67
Number of pages6
JournalRevista Mexicana de Astronomia y Astrofisica: Serie de Conferencias
Volume15
StatePublished - Dec 1 2003
EventWinds, Bubbles and Explosions: A Conference to Honor John Dyson - Patzcuaro, Michoacan, Mexico
Duration: Sep 9 2002Sep 13 2002

Fingerprint

bubble
bubbles
high temperature gases
x rays
gas
turbulent mixing
stellar winds
planetary nebulae
clumps
XMM-Newton telescope
conductive heat transfer
newton
observatories
astrophysics
observatory
luminosity
stars

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 journalConference article

@article{04c7b87f57014e8e9f073814a1f63168,
title = "An inside-out view of bubbles",
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.",
keywords = "H II regions, ISM: bubbles, Planetary nebulae, Stars: Wolf-Rayet, Stars: mass loss, X-rays: ISM",
author = "Chu, {You Hua} and Gruendl, {Robert A.} and Guerrero, {Mart{\'i}n A.}",
year = "2003",
month = "12",
day = "1",
language = "English (US)",
volume = "15",
pages = "62--67",
journal = "Revista Mexicana de Astronomia y Astrofisica: Serie de Conferencias",
issn = "1405-2059",

}

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 -