Evolved Cool Stars Winds

mass-loss rates from non dust driven winds

line substitute

Detailed studies of eclipsing binary (EB), spectroscopic (SB), wide binary (WB), and single (S) stars. These are not based on modeling of dust emission.

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      & Harper (unpublished)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Harper, unpublished - re-analysis of original data lead to small increae.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