Interaction of the supernova remnant HB3 with the ambient interstellar gas

The well-known shell supernova remnant (SNR) HB3 is part of a feature-rich star-forming region together with the nebulae W3, W4, and W5. We Study the HI structure around this SNR using live RATAN-600 drift curves obtained at a wavelength of 21 cm with all angular resolution of 2' in one coordinate over the radial-velocity range -183 to +60 km s(-1) in a wider region of the sky and with a higher sensitivity than in previous works by other authors. The spatial-kinematic distribution of HI features around the SNR clearly shows two concentric expanding shells of gas that surround the SNR and coincide with it in all three coordinates (a, 5, and V). The outer shell has a radius of 133 pc, a thickness of 24 pc, and an expansion velocity of 48 km s(-1). The mass of the gas in it is 2.3 x 105 M-circle dot. For the inner shell, these parameters are 78 pc, 36 pc, 24 km s-1, and 0.9 x 10(5) M-circle dot, respectively. The inner shell is immediately adjacent to the SNR. Assuming that the outer shell was produced by the stellar wind and the inner shell arose from the shock wave of the SNR proper, we estimated the age of the outer shell,; approximate to 1.7 x 10(6) yr, and the mechanical luminosity of the stellar wind, 1.5 x 10(38) erg s(-1). The inner shell has all age of approximate to 10(6) yr and corresponds to a total supernova explosion energy of approximate to 10(52) erg. (c) 2005 Pleiades Publishing, Inc.