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Home All issues Volume 507 / No 3 (December I 2009) A&A, 507 3 (2009) 1555-1565 Full HTML
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Table 3:

Summary of the stellar properties of AFGL 2998 and other LBVs observed to undergo giant eruptions.
Star Epoch $R_{\ast}$ $T_{\rm eff}$ log( $L_{\ast}/L_{\odot}$) H/He $v_{\infty}$ log $\dot{M}$ /$\sqrt f$ Reference
    ($R_{\odot}$) (kK)     (km s-1) $M_{\odot}$ yr-1  
AFGL 2298 1996-9 - - >6.4 - - - a
  2001 Jun. 262 11.7 6.2 5.0 200 -4.3 a
  2002 Aug. 158 10.9 6.1 5.0 200 -3.9 a
  2006 Jun. 385 10.3 6.3 5.0 125 -4.3 a
  2007 May 312 10.9 6.2 5.0 125 -4.4 a
NGC 2363-V1 <1993 - - $\leq$ 5.9 - - - b
  1997 Nov. 356 13.5 6.58 4.0 325 -3.3 b, c
  1999 Jul. 201 18.5 6.63 4.0 290 -3.2 b, c
  2000 Oct. 225 17.5 6.63 4.0 - -3.3 c, d
  2001 Dec. 223 18.5 6.72 4.0 - -3.5 c, d
  2003 May 194 20.5 6.78 4.0 - -3.8 c, d
  2004 May - 26.0 6.80 - - <-3.4 c, d
HD 5980 1978-80 - 60.5 6.4 - - - e
  1993 Nov. - 52.0 6.5 - - - e
  1994 Sep. 280 23 7.05 0.7 500 -3.1 b
  1994 Dec. 130 35 6.50 2.5 600 -3.0 e
$\eta$ Car 1840's - - 7.5 - 650-3000 $\ga$-0.3 f, g
  1890's - - - - 200 -1.8 h, i
  1998.2 60-881 35.3-9.2 6.74 5.0 500 -3.0 j
P Cygni 1600's - - - - 137 -1.7 k
  1989-92 76 18.7 5.8 3.5 185 -4.5 l

Note 2. Those parameters that are not directly determined from non-LTE model atmosphere analysis - for example wind parameters derived from present day nebular properties - are given in italics. Due to the extreme mass loss rate for $\eta$ Car a degeneracy is present for the stellar radius and temperature (Hillier et al. 2001). References used in the construction of this table are a Clark et al. (2003a) and this study; b Drissen et al. (2001); c Petit et al. (2005); d Petit et al. (2006); e Koenigsberger et al. (1998) f Humphreys et al. (1999); g Smith et al. (2003); h Smith (2005); i Smith (2008); j Hillier et al. (2001); k Smith & Hartigan (2006); l Najarro (2001). Volume filling factors, f, range from 0.1 (HD 5980 and $\eta$ Car), through 0.3 (NGC 2363-V1) to 0.5 (P Cygni). Time averaged mass loss rates for $\eta$ Car and P Cygni derived from nebular masses are absolute (i.e. f = 1). Finally, note that the values of  $V_{\infty}$ presented for NGC 2363-V1 in 1997 & 1999 are from Drissen et al. (2001), while R*, $T_{\rm eff}$, $\log(L_{*})$ and $\dot{M}$ are from the updated models presented by Petit et al. (2005).


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