K2 III | alpha Boo | 2 x10(-10) | (S) Drake |
K5 III | alpha Tau | 1.4 x10(-11) | (S) Carpenter et al. 2001 |
M3 III | gamma Cru | 4.5 x10(-10) | (S) Carpenter et al. 2001 |
G4 IIa | 22 Vul | 1.1 x10(-8) | (EB) Schroder & Reimer 1989 |
G9 IIb | HR 6902 | 0.8-3.4 x10(-11) | (EB) Kirsch et al. 2001 |
K3 II | alpha TrA | ~10(-9) | (S) Harper et al. 2001 |
M2 II | delta Sge | 2 x10(-10) | (SB) Reimer & Schroder 1983 |
M5 II | alpha Her | 1.5 x10(-7) | (WB) Thiering & Reimers 1993 |
K4 Ib | zeta Aur | 5 x10(-9) | (EB) Baade et al. 1996, Harper et al. 2005 |
K4 Ib | 31 Cyg | 1.6 x10(-8) | (EB) Grafener 1995 |
K4 Ib | lambda Vel | 3 x10(-9) | (S) Carpenter et al. 1999 |
K5 Ib | 32 Cyg | 1.5 x10(-8) | (EB) Baade 1989 |
M1 Iab | KQ Pup | >2 x10(-6) | (WB) Muratorio et al. 1992 |
M1.5 Iab | alpha Sco | 1 x10(-6) | (WB) Hjellming & Newell 1983, Hagen et al. 1987 |
| | | & Harper (unpublished) |
M2 Iab | alpha Ori | 3 x10(-6) | (S) Harper et al. 2001 (& mean estimate) |
Note: the number of significant figures is NOT a reflection of the accuracy of the estimate
Note: there has been a slight decrease in the mass loss rates from recent eclipsing binary studies.
Note: lower limits to the mass loss rate can be found from cm-radio continuum observations, as long as
the tau=1 surface lies where the wind has reached its terminal velocity.
Baade et al., 1996, ApJ, 466, 979: HST/GHRS, confirmed by VLA observations, Harper et al. 2005 AJ
Baade, R., 1989, in Reviews in Modern Astronomy 2 (Springer Verlag: Berlin), ed. G. Klare, p. 324
Carpenter et al., 1999, ApJ, 521, 382: UV line profiles using SEI + S-MULTI
Carpenter, K.G., Robinson, R.D., & Harper, G. M., 2001, ASP Conf. Ser. 223, Ed. R.J. Garcia,
R. Rebolo, & M.R. Zapatero Osorio: SEI modeling of UV profiles
Drake, S., 1985, in Progress in stellar spectral line formation theory (Dordrecht: Reidel), p. 351-357.:
cm-radio fluxes consistent with Mg II line profile model
Grafener, G., 1995, Diplomarbeit, University of Hamburg
Hagen, H.-J., Hempe, K., & Reimers, D., 1987, A&A, 184, 256: IUE line profiles
Harper, unpublished - re-analysis of original data lead to small increae. New radio observations in are now in hand
and a revision may follow.
Harper et al., 1995, ApJ, 452, 407: Firm lower limit of 1.6 x10(-10) from Mg II line profile. HST observations of Si III suggest Mg II is
not dominant ion - mass loss rate is higher.
Harper et al., 2001, ApJ, 551, 1073: multi-wavelength VLA interferometry +HST/GHRS Fe II absorption
Kirsch, T., Baade, R., & Reimers, D., 2001, A&A, 379, 925: IUE Si IV/C IV absorption profiles T(wind) ~ 80,000 K
Muratorio, G., et al., 1992, A&A, 258, 423: Self Absorption Curve Model
Reimers, D. & Schroder, K.-P., 1983, A&A, 124, 241: IUE EW'sf Fe II mult. 9
Schroder, K.-P., & Reimers, D., 1989, A&A, 208, 223
Thiering, I. & Reimers, D., 1993, A&A, 274, 838