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Titolo:
Mass-losing semiregular variable stars in Baade's windows
Autore:
Alard, C; Blommaert, JADL; Cesarsky, C; Epchtein, N; Felli, M; Fouque, P; Ganesh, S; Genzel, R; Gilmore, G; Glass, IS; Habing, H; Omont, A; Perault, M; Price, S; Robin, A; Schultheis, M; Simon, G; van Loon, JT; Alcock, C; Allsman, RA; Alves, DR; Axelrod, TS; Becker, AC; Bennett, DP; Cook, KH; Drake, AJ; Freeman, KC; Geha, M; Griest, K; Lehner, MJ; Marshall, SL; Minniti, D; Nelson, C; Peterson, BA; Popowski, P; Pratt, MR; Quinn, PJ; Sutherland, W; Tomaney, AB; Vandehei, T; Welch, DL;
Indirizzi:
Observ Paris, DASGAL, CNRS, UMR 335, F-75014 Paris, France Observ Paris Paris France F-75014 , CNRS, UMR 335, F-75014 Paris, France CNRS, Inst Astrophys Paris, F-75014 Paris, France CNRS Paris France F-75014 S, Inst Astrophys Paris, F-75014 Paris, France ESA, Dept Space Sci, Div Astrophys, ISO Data Ctr, E-28080 Madrid, Spain ESA Madrid Spain E-28080 Astrophys, ISO Data Ctr, E-28080 Madrid, Spain ESO, D-85740 Garching, Germany ESO Garching Germany D-85740ESO, D-85740 Garching, Germany Observ Cote Azur, Dept Fresnel, F-06304 Nice 4, France Observ Cote Azur Nice France 4 zur, Dept Fresnel, F-06304 Nice 4, France Osservatorio Astrofis Arcetri, I-50125 Florence, Italy Osservatorio Astrofis Arcetri Florence Italy I-50125 125 Florence, Italy ESO, Santiago, Chile ESO Santiago ChileESO, Santiago, Chile Phys Res Lab, Astron & Astrophys Div, Ahmedabad 380009, Gujarat, India Phys Res Lab Ahmedabad Gujarat India 380009 edabad 380009, Gujarat, India Max Planck Inst Extraterr Phys, D-85740 Garching, Germany Max Planck Inst Extraterr Phys Garching Germany D-85740 arching, Germany The Observatories, Inst Astron, Cambridge CB3 0HA, England The Observatories Cambridge England CB3 0HA , Cambridge CB3 0HA, England S African Astron Observ, ZA-7935 Observatory, South Africa S African Astron Observ Observatory South Africa ZA-7935 y, South Africa Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands Sterrewacht Leiden Leiden Netherlands NL-2300 RA RA Leiden, Netherlands ENS, Lab Radioastron Millimetr, F-75005 Paris, France ENS Paris France F-75005 ab Radioastron Millimetr, F-75005 Paris, France CNRS, F-75005 Paris, France CNRS Paris France F-75005CNRS, F-75005 Paris, France AFRL, Hanscom AFB, MA 01731 USA AFRL Hanscom AFB MA USA 01731AFRL, Hanscom AFB, MA 01731 USA Observ Besancon, F-25010 Besancon, France Observ Besancon Besancon France F-25010 sancon, F-25010 Besancon, France Univ Calif Lawrence Livermore Natl Lab, Livermore, CA 94550 USA Univ CalifLawrence Livermore Natl Lab Livermore CA USA 94550 A 94550 USA Univ Calif Berkeley, Ctr Particle Astrophys, Berkeley, CA 94720 USA Univ Calif Berkeley Berkeley CA USA 94720 trophys, Berkeley, CA 94720 USA Australian Natl Univ, Supercomp Facil, Canberra, ACT 0200, Australia Australian Natl Univ Canberra ACT Australia 0200 rra, ACT 0200, Australia Space Telescope Sci Inst, Baltimore, MD 21218 USA Space Telescope Sci Inst Baltimore MD USA 21218 , Baltimore, MD 21218 USA Australian Natl Univ, Mt Stromlo & Siding Spring Observ, Weston Creek, ACT2611, Australia Australian Natl Univ Weston Creek ACT Australia 2611 , ACT2611, Australia Univ Washington, Dept Astron, Seattle, WA 98195 USA Univ Washington Seattle WA USA 98195 , Dept Astron, Seattle, WA 98195 USA Univ Washington, Dept Phys, Seattle, WA 98195 USA Univ Washington SeattleWA USA 98195 on, Dept Phys, Seattle, WA 98195 USA Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA Univ Notre Dame Notre Dame IN USA 46556 pt Phys, Notre Dame, IN 46556 USA Univ Calif Santa Cruz, Dept Astron, Santa Cruz, CA 95064 USA Univ Calif Santa Cruz Santa Cruz CA USA 95064 n, Santa Cruz, CA 95064 USA Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA Univ Calif San Diego La Jolla CA USA 92093 t Phys, La Jolla, CA 92093 USA Univ Sheffield, Dept Phys, Sheffield S3 7RH, S Yorkshire, England Univ Sheffield Sheffield S Yorkshire England S3 7RH S Yorkshire, England Pontificia Univ Catolica Chile, Dept Astron, Santiago 22, Chile PontificiaUniv Catolica Chile Santiago Chile 22 ron, Santiago 22, Chile Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA Univ Calif Berkeley Berkeley CA USA 94720 pt Phys, Berkeley, CA 94720 USA MIT, Ctr Space Res, Cambridge, MA 02139 USA MIT Cambridge MA USA 02139MIT, Ctr Space Res, Cambridge, MA 02139 USA Univ Oxford, Dept Phys, Oxford OX1 3RH, England Univ Oxford Oxford England OX1 3RH d, Dept Phys, Oxford OX1 3RH, England McMaster Univ, Dept Phys, Hamilton, ON L8S 4M1, Canada McMaster Univ Hamilton ON Canada L8S 4M1 ys, Hamilton, ON L8S 4M1, Canada McMaster Univ, Dept Astron, Hamilton, ON L8S 4M1, Canada McMaster Univ Hamilton ON Canada L8S 4M1 on, Hamilton, ON L8S 4M1, Canada
Titolo Testata:
ASTROPHYSICAL JOURNAL
fascicolo: 1, volume: 552, anno: 2001,
parte:, 1
pagine: 289 - 308
SICI:
0004-637X(200105)552:1<289:MSVSIB>2.0.ZU;2-7
Fonte:
ISI
Lingua:
ENG
Soggetto:
ASYMPTOTIC GIANT BRANCH; LONG-PERIOD VARIABLES; SHOCK-WAVE INTERPRETATION; LARGE-MAGELLANIC-CLOUD; SOUTH-GALACTIC-CAP; MIRA VARIABLES; RED GIANTS; CIRCUMSTELLAR CO; PULSATION MODE; EMISSION-LINES;
Keywords:
astronomical data bases : miscellaneous; Galaxy : bulge; infrared : stars; stars : AGB and post-AGB; stars : fundamental parameters; stars : late-type; stars : variables : other;
Tipo documento:
Article
Natura:
Periodico
Settore Disciplinare:
Physical, Chemical & Earth Sciences
Citazioni:
57
Recensione:
Indirizzi per estratti:
Indirizzo: Alard, C Observ Paris, DASGAL, CNRS, UMR 335, 21 Ave Observ, F-75014 Paris, France Observ Paris 21 Ave Observ Paris France F-75014 14 Paris, France
Citazione:
C. Alard et al., "Mass-losing semiregular variable stars in Baade's windows", ASTROPHYS J, 552(1), 2001, pp. 289-308

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 mum) 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 log P-M-bol relation or set ofsuch relations. Approximate mass-loss rates (M) over dot in the range of similar to 1x10(-8) to 5 x 10(-7) M-. yr(-1) are derived from ISOGAL mid-infrared photometry and models of stellar spectra adjusted for the presence ofoptically 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 AGE 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) over dot proportional to (TLbeta)-L-alpha, where a = -8.80(-0.24)(+0.96) and beta = + 1.74(-0.24)(+0.16), in agreement with recent theoretical predictions. If we include our mass-loss rates with a sample of extreme mass-losing AGE stars in the Large Magellanic Cloud and ignore T as a variable,we get the general result for AGE stars that (M) over dot proportional to L-2.7, valid for AGB stars with 10(-8) < (M) over dot ( 10(-4) M-. yr(-1).

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Documento generato il 01/12/20 alle ore 08:23:26