2001ApJ...546..484D

A quantitative study of the luminous blue variable NGC 2363-V1 in the Magellanic galaxy NGC 2366 (D=3.44 Mpc) is presented, based on ultraviolet and optical Hubble Space Telescope STIS spectroscopy. Contemporary WFPC2 and William Herschel Telescope imaging reveals a modest V-band brightness increase of ∼0.2 mag per year between 1996 January-1997 November, reaching V=17.4 mag, corresponding to M_V=-10.4 mag. Subsequently, V1 underwent a similar decrease in V-band brightness, together with a UV brightening of 0.35 mag from 1997 November to 1999 November. The optical spectrum of V1 is dominated by H emission lines, with Fe II, He I and Na I also detected. In the ultraviolet, a forest of Fe absorption features and numerous absorption lines typical of mid-B supergiants (such as Si II, Si III, Si IV, C III, C IV) are observed. From a spectral analysis with the non-LTE, line-blanketed code of Hillier & Miller, we derive stellar parameters of T_*=11 kK, R_*=420 R_☉, log (L/L_☉)=6.35 during 1997 November, and T_*=13 kK, R_*=315 R_☉, log (L/L_☉)=6.4 for 1999 July. The wind properties of V1 are also exceptional, with M{dot}≃4.4x10^–4M_☉.yr^–1 and v_∞≃300 km.s^–1, allowing for a clumped wind (filling factor=0.3) and assuming H/He∼4 by number. The presence of Fe lines in the UV and optical spectrum of V1 permits an estimate of the heavy elemental abundance of NGC 2363 from our spectral synthesis. Although some deficiencies remain, allowance for charge exchange reactions in our calculations supports a SMC-like metallicity, that has previously been determined for NGC 2363 from nebular oxygen diagnostics. Considering a variety of possible progenitor stars, V1 has definitely undergone a giant eruption, with a substantial increase in stellar luminosity, radius, and almost certainly mass-loss rate, such that its stellar radius increased at an average rate of ∼4 km.s^–1 during 1992 October-1995 February. The stellar properties of V1 are compared to other LBVs, including η Car and HD 5980 during its brief eruption in 1994 September, the latter newly analyzed here. The mass-loss rate of the HD 5980 eruptor compares closely with V1, but its bolometric luminosity was a factor ∼6 times larger.