Astronomy and Astrophysics – Astronomy
Scientific paper
May 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aas...188.6106c&link_type=abstract
American Astronomical Society, 188th AAS Meeting, #61.06; Bulletin of the American Astronomical Society, Vol. 28, p.924
Astronomy and Astrophysics
Astronomy
Scientific paper
Bright diffuse X-ray emission has been detected in large H II complexes, such as the Carina Nebula in the Galaxy and the 30 Doradus nebula in the LMC. This indicates the existence of hot (10(6) K) gas; however, it is unclear whether stellar winds or supernova remnants dominate the heating. To resolve this issue, we have selected N66, the largest H II region in the Small Magellanic Cloud (SMC), for a detailed case study. N66 contains an OB association with unevolved O3 members. This strongly implies that supernovae have not yet occurred and that the X-ray-emitting gas is predominantly heated by stellar winds. The young evolutionary stage of N66 is further supported by the small velocity widths of the Hα line profile observed in the H II region. Therefore, the X-ray emission of N66 can unambiguously provide insight into the stellar wind heating of hot gas. We have analyzed the soft X-ray emission of N66, using both a proprietary ROSAT HRI observation (50 ks) and an archival ROSAT PSPC observation (26.6 ks). We find that the X-ray emission from the direction of N66 is dominated by a known foreground supernova remnant(SNR), 0057-7226, and that no obvious X-ray emission is detected outside the projected SNR boundary. The PSPC count rate of the SNR is (4.1+/- 0.1)x 10(-3) counts s(-1) arcmin(-2) , while the 3-sigma upper limit for the H II region is 1.0x 10(-4) counts s(-1) arcmin(-2) . This upper limit is similiar to those of the X-ray-dim superbubbles in the LMC. However, it is lower than the observed X-ray count rate ~ 8x 10(-3) counts s(-1) arcmin(-2) of Carina Nebula and (4-8)x 10(-3) counts s(-1) arcmin(-2) of 30 Doradus by 1 ~ 2 orders of magnitude. The aforementioned disparity in X-ray surface brightness is intrinsic, since N66 has the smallest extinction among the three. This suggests that the X-ray-bright H II complexes cannot be powered solely by stellar winds. SNR shocks must have provided additional heating.
Chang Tsung-Hui
Chu Y.-H. Y.-H.
Joner Michael D.
No associations
LandOfFree
The Heating of Hot Gas in H II Complexes: Stellar Winds VS SNR Shocks does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with The Heating of Hot Gas in H II Complexes: Stellar Winds VS SNR Shocks, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and The Heating of Hot Gas in H II Complexes: Stellar Winds VS SNR Shocks will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1354935