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Title:
Mass-losing Semiregular Variable Stars in Baade's Windows
Authors:
Alard, C.; Blommaert, J. A. D. L.; Cesarsky, C.; Epchtein, N.; Felli, M.; Fouque, P.; Ganesh, S.; Genzel, R.; Gilmore, G.; Glass, I. S.; Habing, H.; Omont, A.; Perault, M.; Price, S.; Robin, A.; Schultheis, M.; Simon, G.; van Loon, J. Th.; Alcock, C.; Allsman, R. A.; Alves, D. R.; Axelrod, T. S.; Becker, A. C.; Bennett, D. P.; Cook, K. H.; Drake, A. J.; Freeman, K. C.; Geha, M.; Griest, K.; Lehner, M. J.; Marshall, S. L.; Minniti, D.; Nelson, C.; Peterson, B. A.; Popowski, P.; Pratt, M. R.; Quinn, P. J.; Sutherland, W.; Tomaney, A. B.; Vandehei, T.; Welch, D. L.
Affiliation:
AA(; DASGAL, UMR CNRS 335, Observatoire de Paris, 21 Avenue de l'Observatoire, Paris F75014, France.; Institut d'Astrophysique de Paris, CNRS, 98bis Boulevard Arago, Paris F75014, France.), AB(; ISO Data Centre, Astrophysic Division, Space Science Department of ESA, Apartado 50727, Madrid E28080, Spain.), AC(; ESO, Karl-Schwarzschild-Strasse 2, D-85740, Garching, Germany.), AD(; Observatory de la Cote d'Azur, Departement Fresnel, BP 4229, F 06304 Nice Cedex 4, France.), AE(; Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi, 5, Firenzi I-50125, Italy.), AF(; ESO, Casilla 19001, Santiago, Chile.), AG(; Physical Research Laboratory, Astronomy and Astrophysics Division, Navarangpura, Ahmedabad 380 009, India.), AH(; Max-Planck-Institut für extraterrestrische Physik, Karl-Schwarzschild-Strasse 1, Postfach 1603, D-85740 Garching, Germany.), AI(; Institute of Astronomy, The Observatories, Madingley Road, Cambridge CB3 0HA, UK.), AJ(; South African Astronomical Observatory, P.O. Box 9, Observatory 7935, South Africa.), AK(; Sterrewacht Leiden, P.O. Box 9513, 2300 RA Leiden, The Netherlands.), AL(; Institut d'Astrophysique de Paris, CNRS, 98bis Boulevard Arago, Paris F75014, France.), AM(; Laboratoire de Radioastronomie Millimétrique, ENS and CNRS, 24 Rue Lhomond, F-75005 Paris, France.), AN(; AFRL, Hanscom AFB, MA, 01731.), AO(; Observatoire de Besançon, BP 1615, F-25010 Besançon Cedex, France.), AP(; Institut d'Astrophysique de Paris, CNRS, 98bis Boulevard Arago, Paris F75014, France.), AQ(; DASGAL, UMR CNRS 335, Observatoire de Paris, 21 Avenue de l'Observatoire, Paris F75014, France.), AR(; Institute of Astronomy, The Observatories, Madingley Road, Cambridge CB3 0HA, UK.), AS(; Lawrence Livermore National Laboratory, Livermore, CA 94550.; Center for Particle Astrophysics, University of California, Berkeley, Berkeley, CA 94720.), AT(; Supercomputing Facility, Australian National University, Canberra, ACT 0200, Australia.), AU(; Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218.), AV(; Mount Stromlo and Siding Spring Observatories, ANU, Weston Creek, ACT 2611, Australia.), AW(; Departments of Astronomy and Physics, University of Washington, Seattle, WA 98195.), AX(; Physics Department, University of Notre Dame, Notre Dame, IN 46556.; Center for Particle Astrophysics, University of California, Berkeley, Berkeley, CA 94720.), AY(; Lawrence Livermore National Laboratory, Livermore, CA 94550.; Center for Particle Astrophysics, University of California, Berkeley, Berkeley, CA 94720.), AZ(; Lawrence Livermore National Laboratory, Livermore, CA 94550.), BA(; Mount Stromlo and Siding Spring Observatories, ANU, Weston Creek, ACT 2611, Australia.), BB(; Department of Astronomy, University of California, Santa Cruz, Santa Cruz, CA 95064.), BC(; Center for Particle Astrophysics, University of California, Berkeley, Berkeley, CA 94720.; Department of Physics, University of California, San Diego, La Jolla, CA 92093.), BD(; Department of Physics, University of Sheffield, Sheffield S3 7RH, UK.), BE(; Lawrence Livermore National Laboratory, Livermore, CA 94550.), BF(; Departmento de Astronomia, P. Universidad Catolica, Casilla 104, Santiago 22, Chile.), BG(; Department of Physics, University of California, Berkeley, Berkeley, CA 94720.), BH(; Mount Stromlo and Siding Spring Observatories, ANU, Weston Creek, ACT 2611, Australia.), BI(; Lawrence Livermore National Laboratory, Livermore, CA 94550.), BJ(; Center for Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139.), BK(; ESO, Karl-Schwarzschild-Strasse 2, D-85740, Garching, Germany.), BL(; Center for Particle Astrophysics, University of California, Berkeley, Berkeley, CA 94720.; Department of Physics, University of Oxford, Oxford OX1 3RH, UK.), BM(; Departments of Astronomy and Physics, University of Washington, Seattle, WA 98195.), BN(; Department of Physics, University of California, San Diego, La Jolla, CA 92093.), BO(; Departments of Physics and Astronomy, McMaster University, Hamilton, ON L8S 4M1, Canada.)
Publication:
The Astrophysical Journal, Volume 552, Issue 1, pp. 289-308. (ApJ Homepage)
Publication Date:
05/2001
Origin:
UCP
ApJ Keywords:
Astronomical Data Bases: Miscellaneous, Galaxy: Bulge, Infrared: Stars, Stars: AGB and Post-AGB, Stars: Fundamental Parameters, Stars: Late-Type, Stars: Variables: Other
DOI:
10.1086/320440
Bibliographic Code:
2001ApJ...552..289A

Abstract

By cross-correlating the results of two recent large-scale surveys, the general properties of a well-defined sample of semiregular variable stars have been determined. ISOGAL mid-infrared photometry (7 and 15 μm) and MACHO V and R light curves are assembled for approximately 300 stars in the Baade's windows of low extinction toward the Galactic bulge. These stars are mainly giants of late M spectral type, evolving along the asymptotic giant branch (AGB). They are found to possess a wide and continuous distribution of pulsation periods and to obey an approximate logP-Mbol relation or set of such relations. Approximate mass-loss rates M in the range of ~1×10-8 to 5×10-7 Msolar yr-1 are derived from ISOGAL mid-infrared photometry and models of stellar spectra adjusted for the presence of optically thin circumstellar silicate dust. Mass-loss rates depend on luminosity and pulsation period. Some stars lose mass as rapidly as short-period Mira variables but do not show Mira-like amplitudes. A period of 70 days or longer is a necessary but not sufficient condition for mass loss to occur. For AGB stars in the mass-loss ranges that we observe, the functional dependence of mass-loss rate on temperature and luminosity can be expressed as M~TαLβ, where α=-8.80+0.96-0.24 and β=+1.74+0.16-0.24, in agreement with recent theoretical predictions. If we include our mass-loss rates with a sample of extreme mass-losing AGB stars in the Large Magellanic Cloud and ignore T as a variable, we get the general result for AGB stars that M~L2.7, valid for AGB stars with 10-8<M<10-4 Msolar yr-1.
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