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1999PASP..111..465S - Publ. Astron. Soc. Pac., 111, 465-481 (1999/April-0)
Emission-line properties of the Large Magellanic Cloud bubble N70.
SKELTON B.P., WALLER W.H., GELDERMAN R.F., BROWN L.W., WOODGATE B.E., CAULET A. and SCHOMMER R.A.
Abstract (from CDS):
We compare the emission-line photometry with that derived from similar imaging of the Orion Nebula and with data collected from the literature on other emission-line regions in the LMC. Compared with the Orion Nebula, N70 shows much higher [S II]/Hα intensity ratios that increase smoothly with radius–from less than 0.3 near the center to greater than 1.0 toward the outer filamentary shell. The measured intensity ratios in N70 more closely match the range of excitation spanned by giant and supergiant H II shells and by some of the supernova remnants observed in the LMC. The contending ionization and excitation processes in the interior and outer shell of N70 are evaluated in terms of the available data. EUV photons probably contribute most of the inner nebula's ionization, whereas a combination of photoionization plus collisional ionization and excitation of sulfur atoms by low-velocity shocks seems to best fit the emission-line luminosities and intensity ratios observed in the outer shell. Considerations of the radiative and mechanical energetics that are involved may indicate the need for one or two supernova explosions having occurred during the last ∼Myr.
Abstract Copyright: ∼
Journal keyword(s): Galaxies: Magellanic Clouds
Simbad objects: 20
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