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ASTRONOMY AND SODIUM IN THE SUN AND IN METAL-POOR STARS Astron. Astrophys. 338, 637–650 (1998) ASTRONOMY AND ASTROPHYSICS Sodium in the Sun and in metal-poor stars? D. Baumuller, K. Butler, and T. Gehren¨ Institut fur Astronomie und Astrophysik der Universit¨ ¨at M ¨unchen, Scheinerstrasse 1, D-81679 M ¨unchen,Germany
MICROSCOPIC NUCLEAR EQUATION OF STATE WITH THREE-BODY Astron. Astrophys. 328, 274{282 (1997) ASTRONOMY AND ASTROPHYSICS Microscopic nuclear equation of state with three-body forces and neutron star structure M. Baldo 1, I. Bombaci2, and G.F. Burgio 1 Dipartimento di Fisica, Universit a di Catania and I.N.F.N. Sezione di Catania, c.so Italia 57, I-95129 Catania, Italy 2 Dipartimento di Fisica, Universit a di Pisa and I.N.F.N. Sezione di Pisa ASTRONOMY AND BLUE STRAGGLERS IN OPEN CLUSTERS Astron. Astrophys. 356, 517–528 (2000) ASTRONOMY AND ASTROPHYSICS Blue stragglers in open clusters Part II? S.M. Andrievsky1;2,D.Schonberner¨ 1, and J.S. Drilling3 1 Astrophysikalisches Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany (DeSchoenberner@aip.de) 2 Odessa State University, Department of Astronomy, Shevchenko Park, 270014 Odessa, Ukraine ASTRONOMY AND A NUMERICAL TIME EPHEMERIS OF THE EARTH Astron. Astrophys. 348, 642–652 (1999) ASTRONOMY AND ASTROPHYSICS A numerical time ephemeris of the Earth A.W. Irwin 1 and T. Fukushima2 1 Department of Physics and Astronomy, University of Victoria, P.O. Box 3055, Victoria, British Columbia, Canada, V8W 3P6 (irwin@uvastro.phys.uvic.ca) 2 National Astronomical Observatory, 2-21-1, Ohsawa, Mitaka, Tokyo 181-8588, Japan INDICATORS OF STAR FORMATION: 4000A BREAK AND BALMER LINES Astron. Astrophys. 325, 1025{1030 (1997) ASTRONOMY AND ASTROPHYSICS Indicators of star formation: 4000A break and Balmer lines B.M. Poggianti1;2 and G. Barbaro3 1 Institute of Astronomy and Royal Greenwich Observatory, Madingley Road, Cambridge, UK, bianca@ast.cam.ac.uk 2 Kapteyn Instituut, PO Box 800, 9700 AV Groningen, The Netherlands 3 Dipartimento di Astronomia, vicolo VISIBLE NEUTRAL HELIUM LINES IN MAIN SEQUENCE B-TYPE STARS F. Leone & A.C. Lanzafame: Visible neutral helium lines in main sequence B-type stars 307 10 15 20 25 30 0.00 0.10 0.20 0.30 A0B9 B8B7 B6 B5 B3 B2 B1 B0 Spec. Type STAR FORMATION AND EVOLUTION IN ACCRETION DISKS S. Collin & J.-P. Zahn: Star formation and evolution in accretion disks 435 of these stars in Sect.3. Sect.4 is devoted to a discussionof the
ASTRONOMY AND SODIUM IN THE SUN AND IN METAL-POOR STARS Astron. Astrophys. 338, 637–650 (1998) ASTRONOMY AND ASTROPHYSICS Sodium in the Sun and in metal-poor stars? D. Baumuller, K. Butler, and T. Gehren¨ Institut fur Astronomie und Astrophysik der Universit¨ ¨at M ¨unchen, Scheinerstrasse 1, D-81679 M ¨unchen,Germany
MICROSCOPIC NUCLEAR EQUATION OF STATE WITH THREE-BODY Astron. Astrophys. 328, 274{282 (1997) ASTRONOMY AND ASTROPHYSICS Microscopic nuclear equation of state with three-body forces and neutron star structure M. Baldo 1, I. Bombaci2, and G.F. Burgio 1 Dipartimento di Fisica, Universit a di Catania and I.N.F.N. Sezione di Catania, c.so Italia 57, I-95129 Catania, Italy 2 Dipartimento di Fisica, Universit a di Pisa and I.N.F.N. Sezione di Pisa ASTRONOMY AND BLUE STRAGGLERS IN OPEN CLUSTERS Astron. Astrophys. 356, 517–528 (2000) ASTRONOMY AND ASTROPHYSICS Blue stragglers in open clusters Part II? S.M. Andrievsky1;2,D.Schonberner¨ 1, and J.S. Drilling3 1 Astrophysikalisches Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany (DeSchoenberner@aip.de) 2 Odessa State University, Department of Astronomy, Shevchenko Park, 270014 Odessa, Ukraine ASTRONOMY AND A NUMERICAL TIME EPHEMERIS OF THE EARTH Astron. Astrophys. 348, 642–652 (1999) ASTRONOMY AND ASTROPHYSICS A numerical time ephemeris of the Earth A.W. Irwin 1 and T. Fukushima2 1 Department of Physics and Astronomy, University of Victoria, P.O. Box 3055, Victoria, British Columbia, Canada, V8W 3P6 (irwin@uvastro.phys.uvic.ca) 2 National Astronomical Observatory, 2-21-1, Ohsawa, Mitaka, Tokyo 181-8588, Japan ASTRONOMY AND ROSAT ALL-SKY SURVEY MAP OF THE CYGNUS LOOP B. Aschenbach & D.A. Leahy: ROSAT X-ray map of the Cygnus Loop 603 intensity of 861 c/s, the .52-.90keV map has 574 c/s, and the.91-2.01keV map has 224 c/s, for a total intensity of 1659 c/s ASTRON. ASTROPHYS. 333, 79-91 (1998) Astron. Astrophys. 333, 79-91 (1998) Astron. Astrophys. 333, 79-91 (1998) 4. Pattern velocity and Lindblad resonances. The non-axisymmetric structure in the disk has an angular pattern speed given by the angular velocity . Three radii in each galaxy are of specific interest because the pattern speed resonates with the eigenfrequencies of the ASTRONOMY AND COMPTONIZATION OF THE COSMIC MICROWAVE T.A. Enßlin & C.R. Kaiser: Comptonization of the cosmic microwave background by relativistic plasma 419 0 2 4 6 8 10 12 14-4-2 0 2 4 6 gg h-i j-i Fig.1.
ASTRON. ASTROPHYS. 342, 464–473 (1999) ASTRONOMY AND RAPID Astron. Astrophys. 342, 464–473 (1999) ASTRONOMY AND ASTROPHYSICS Rapid proton capture on accreting neutron stars – effects of uncertainty in the nuclear process A STATISTIC FOR DESCRIBING PULSAR AND CLOCK STABILITIES Astron. Astrophys. 326, 924{928 (1997) ASTRONOMY AND ASTROPHYSICS A statistic for describing pulsar and clock stabilities Demetrios N. Matsakis 1, J. H. Taylor2, and T. Marshall Eubanks 1 U.S. Naval Observatory, 3450 Massachusetts Avenue NW, Washington DC 20392-5420, USA 2 Joseph Henry Laboratories and Physics Department, Princeton University, Princeton NJ 08544, USA SOLAR-TYPE STARS WITH PLANETARY COMPANIONS: 51PEGASI AND K. Fuhrmann et al.: Solar-type stars with planetary companions: 51 Pegasi and 47 Ursae Majoris 1083 Fig.1aandb.H linepro lesof51 Peg(thickcurve,toppanel),47 UMa(thickcurve,bottompanel)andtheMoon(=reflectedsunlight,dotted ASTRON. ASTROPHYS. 333, 79-91 (1998) Astron. Astrophys. 333, 79-91 (1998) Astron. Astrophys. 333, 79-91 (1998) 4. Pattern velocity and Lindblad resonances. The non-axisymmetric structure in the disk has an angular pattern speed given by the angular velocity . Three radii in each galaxy are of specific interest because the pattern speed resonates with the eigenfrequencies of the ASTRONOMY AND NON-EXPLOSIVE HYDROGEN AND HELIUM BURNINGS M. Arnould et al.: Abundances from non-explosive H and He burnings 573 mentsfromCtoAlinvolvedinthenon-explosiveH(Sects.3–5) andHe(Sect.6)burnings,specialemphasisbeingputontheim- THE HYADES: DISTANCE, STRUCTURE, DYNAMICS, AND AGE 82 M.A.C. Perryman et al.: The Hyades: distance, structure, dynamics, and age the cluster. Distance estimates have been based on a varietyof
THE -STRUCTURE OF DISK GALAXIES TOWARDS THE GALAXY PLANES R. de Grijs et al.: The z-structure of disk galaxies 967 thin disk luminosity, which is thought to be locally isothermal (van der Kruit & Searle 1981a). The relations among the values for the density in theplane,
THE BE/X-RAY BINARY LS I +61 235/RX J0146.9+6121: PHYSICAL Astron. Astrophys. 322, 183{192 (1997) ASTRONOMY AND ASTROPHYSICS The Be/X-ray binary LS I +61 235/RX J0146.9+6121: physical parameters and V/R variability P. Reig 1, J. Fabregat2, M.J. Coe , P. Roche3, D. Chakrabarty4;5, I. Negueruela1, and I. Steele6 1 Physics and Astronomy Department, Southampton University, Southampton. SO17 1BJ, UK 2 Departament d’Astronomia i Astrof sica, ASTRONOMY AND THE NUCLEAR BULGE Astron. Astrophys. 348, 768–782 (1999) ASTRONOMY AND ASTROPHYSICS The nuclear bulge I. K band observations of the central 30pc S. Philipp1;2, R. Zylka2, P.G. Mezger1, W.J. Duschl 2;1, T. Herbst3, and R.J. Tuffs4 1 Max-Planck-Institut f¨ur Radioastronomie, Auf dem H ugel 69, D-53121 Bonn, Germany¨ 2 Institut fur Theoretische Astrophysik, Tiergartenstrasse 15, D-69121 Heidelberg, Germany¨ CAUSTICS OF THE RESTRICTED THREE-BODY PROBLEM Astron. Astrophys. 331, 1108{1112 (1998) ASTRONOMY AND ASTROPHYSICS Caustics of the restricted three-body problem D.E. Santos Jr.1, R. Vieira Martins1, O.C. Winter2, and R.R. Cordeiro3 1 Observatorio Nacional, Rua Gal. Jos e Cristino 77, 20921-400 Rio de Janeiro, Brazil (e-amil: desj@on.br and rvm@on.br) 2 Grupo de Din^amica Orbital e Planetologia, Campus Guaratinguet a, UNESP, CP205 CEP 12500 SOLAR-TYPE STARS WITH PLANETARY COMPANIONS: 51PEGASI AND K. Fuhrmann et al.: Solar-type stars with planetary companions: 51 Pegasi and 47 Ursae Majoris 1083 Fig.1aandb.H linepro lesof51 Peg(thickcurve,toppanel),47 UMa(thickcurve,bottompanel)andtheMoon(=reflectedsunlight,dotted ASTRONOMY AND NON-EXPLOSIVE HYDROGEN AND HELIUM BURNINGS Astron. Astrophys. 347, 572–582 (1999) ASTRONOMY AND ASTROPHYSICS Non-explosive hydrogen and helium burnings: abundance predictions from the NACRE reaction rate compilation? A STATISTIC FOR DESCRIBING PULSAR AND CLOCK STABILITIES Astron. Astrophys. 326, 924{928 (1997) ASTRONOMY AND ASTROPHYSICS A statistic for describing pulsar and clock stabilities Demetrios N. Matsakis 1, J. H. Taylor2, and T. Marshall Eubanks 1 U.S. Naval Observatory, 3450 Massachusetts Avenue NW, Washington DC 20392-5420, USA 2 Joseph Henry Laboratories and Physics Department, Princeton University, Princeton NJ 08544, USA VISIBLE NEUTRAL HELIUM LINES IN MAIN SEQUENCE B-TYPE STARS F. Leone & A.C. Lanzafame: Visible neutral helium lines in main sequence B-type stars 307 10 15 20 25 30 0.00 0.10 0.20 0.30 A0B9 B8B7 B6 B5 B3 B2 B1 B0 Spec. Type ASTRON. ASTROPHYS. 342, 464–473 (1999) ASTRONOMY AND RAPID Astron. Astrophys. 342, 464–473 (1999) ASTRONOMY AND ASTROPHYSICS Rapid proton capture on accreting neutron stars – effects of uncertainty in the nuclear process ASTRONOMY AND SODIUM IN THE SUN AND IN METAL-POOR STARS Astron. Astrophys. 338, 637–650 (1998) ASTRONOMY AND ASTROPHYSICS Sodium in the Sun and in metal-poor stars? D. Baumuller, K. Butler, and T. Gehren¨ Institut fur Astronomie und Astrophysik der Universit¨ ¨at M ¨unchen, Scheinerstrasse 1, D-81679 M ¨unchen,Germany
ASTRONOMY AND A NEW NON-LINEAR LIMB-DARKENING LAW FOR LTE Astron. Astrophys. 363, 1081–1190 (2000) ASTRONOMY AND ASTROPHYSICS A new non-linear limb-darkening law for LTE stellar atmosphere models Calculations for −5:0 log +1;2000K Te 50000K at several surfacegravities?
INDICATORS OF STAR FORMATION: 4000A BREAK AND BALMER LINES Astron. Astrophys. 325, 1025{1030 (1997) ASTRONOMY AND ASTROPHYSICS Indicators of star formation: 4000A break and Balmer lines B.M. Poggianti1;2 and G. Barbaro3 1 Institute of Astronomy and Royal Greenwich Observatory, Madingley Road, Cambridge, UK, bianca@ast.cam.ac.uk 2 Kapteyn Instituut, PO Box 800, 9700 AV Groningen, The Netherlands 3 Dipartimento di Astronomia, vicolo ASTRON. ASTROPHYS. 344, 973–980 (1999) ASTRONOMY AND Astron. Astrophys. 344, 973–980 (1999) ASTRONOMY AND ASTROPHYSICS Linear adiabatic dynamics of a polytropic convection zone with an isothermal atmosphere SIO PRODUCTION IN INTERSTELLAR SHOCKS Astron. Astrophys. 321, 293{304 (1997) ASTRONOMY AND ASTROPHYSICS SiO production in interstellar shocks? P. Schilke1, C.M. Walmsley2, G. Pineau des Forets^ 3, and D.R. Flower4 1 I. Physikalisches Institut der Universitat zu K ¨oln, Zulpicher Str. 77, D-50937 Koln, Germany 2 Osservatorio di Arcetri, Largo E. Fermi 5, I-50125 Firenze, Italy 3 DAEC, Observatoire de Paris, F-92195 Meudon SOLAR-TYPE STARS WITH PLANETARY COMPANIONS: 51PEGASI AND K. Fuhrmann et al.: Solar-type stars with planetary companions: 51 Pegasi and 47 Ursae Majoris 1083 Fig.1aandb.H linepro lesof51 Peg(thickcurve,toppanel),47 UMa(thickcurve,bottompanel)andtheMoon(=reflectedsunlight,dotted ASTRONOMY AND NON-EXPLOSIVE HYDROGEN AND HELIUM BURNINGS Astron. Astrophys. 347, 572–582 (1999) ASTRONOMY AND ASTROPHYSICS Non-explosive hydrogen and helium burnings: abundance predictions from the NACRE reaction rate compilation? A STATISTIC FOR DESCRIBING PULSAR AND CLOCK STABILITIES Astron. Astrophys. 326, 924{928 (1997) ASTRONOMY AND ASTROPHYSICS A statistic for describing pulsar and clock stabilities Demetrios N. Matsakis 1, J. H. Taylor2, and T. Marshall Eubanks 1 U.S. Naval Observatory, 3450 Massachusetts Avenue NW, Washington DC 20392-5420, USA 2 Joseph Henry Laboratories and Physics Department, Princeton University, Princeton NJ 08544, USA VISIBLE NEUTRAL HELIUM LINES IN MAIN SEQUENCE B-TYPE STARS F. Leone & A.C. Lanzafame: Visible neutral helium lines in main sequence B-type stars 307 10 15 20 25 30 0.00 0.10 0.20 0.30 A0B9 B8B7 B6 B5 B3 B2 B1 B0 Spec. Type ASTRON. ASTROPHYS. 342, 464–473 (1999) ASTRONOMY AND RAPID Astron. Astrophys. 342, 464–473 (1999) ASTRONOMY AND ASTROPHYSICS Rapid proton capture on accreting neutron stars – effects of uncertainty in the nuclear process ASTRONOMY AND SODIUM IN THE SUN AND IN METAL-POOR STARS Astron. Astrophys. 338, 637–650 (1998) ASTRONOMY AND ASTROPHYSICS Sodium in the Sun and in metal-poor stars? D. Baumuller, K. Butler, and T. Gehren¨ Institut fur Astronomie und Astrophysik der Universit¨ ¨at M ¨unchen, Scheinerstrasse 1, D-81679 M ¨unchen,Germany
ASTRONOMY AND A NEW NON-LINEAR LIMB-DARKENING LAW FOR LTE Astron. Astrophys. 363, 1081–1190 (2000) ASTRONOMY AND ASTROPHYSICS A new non-linear limb-darkening law for LTE stellar atmosphere models Calculations for −5:0 log +1;2000K Te 50000K at several surfacegravities?
INDICATORS OF STAR FORMATION: 4000A BREAK AND BALMER LINES Astron. Astrophys. 325, 1025{1030 (1997) ASTRONOMY AND ASTROPHYSICS Indicators of star formation: 4000A break and Balmer lines B.M. Poggianti1;2 and G. Barbaro3 1 Institute of Astronomy and Royal Greenwich Observatory, Madingley Road, Cambridge, UK, bianca@ast.cam.ac.uk 2 Kapteyn Instituut, PO Box 800, 9700 AV Groningen, The Netherlands 3 Dipartimento di Astronomia, vicolo SPRINGERLINK: ASTRONOMY AND ASTROPHYSICS All past volumes of Astronomy & Astrophysics are now accessible on the internet such allowing the readers to search for all articles ever published in this journal.SZ CAMELOPARDALIS
R. Lorenz et al.: SZ Camelopardalis – an early-type eclipsing binary embedded in a multiple system 911 Fig. 1. Typical spectra of SZ Cam obtained with the Coude spectrograph at the 2.2m telescope of CalarAlto Observatory.
MICROSCOPIC NUCLEAR EQUATION OF STATE WITH THREE-BODY Astron. Astrophys. 328, 274{282 (1997) ASTRONOMY AND ASTROPHYSICS Microscopic nuclear equation of state with three-body forces and neutron star structure M. Baldo 1, I. Bombaci2, and G.F. Burgio 1 Dipartimento di Fisica, Universit a di Catania and I.N.F.N. Sezione di Catania, c.so Italia 57, I-95129 Catania, Italy 2 Dipartimento di Fisica, Universit a di Pisa and I.N.F.N. Sezione di Pisa SIO PRODUCTION IN INTERSTELLAR SHOCKS Astron. Astrophys. 321, 293{304 (1997) ASTRONOMY AND ASTROPHYSICS SiO production in interstellar shocks? P. Schilke1, C.M. Walmsley2, G. Pineau des Forets^ 3, and D.R. Flower4 1 I. Physikalisches Institut der Universitat zu K ¨oln, Zulpicher Str. 77, D-50937 Koln, Germany 2 Osservatorio di Arcetri, Largo E. Fermi 5, I-50125 Firenze, Italy 3 DAEC, Observatoire de Paris, F-92195 Meudon ASTRONOMY AND BLUE STRAGGLERS IN OPEN CLUSTERS Astron. Astrophys. 356, 517–528 (2000) ASTRONOMY AND ASTROPHYSICS Blue stragglers in open clusters Part II? S.M. Andrievsky1;2,D.Schonberner¨ 1, and J.S. Drilling3 1 Astrophysikalisches Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany (DeSchoenberner@aip.de) 2 Odessa State University, Department of Astronomy, Shevchenko Park, 270014 Odessa, Ukraine ASTRONOMY AND THE SUPERNOVA REMNANT RX J0852.0–4622: … Astron. Astrophys. 364, 732–740 (2000) ASTRONOMY AND ASTROPHYSICS The supernova remnant RX J0852.0–4622: radio characteristics and implications for SNR statistics STAR FORMATION AND EVOLUTION IN ACCRETION DISKS S. Collin & J.-P. Zahn: Star formation and evolution in accretion disks 435 of these stars in Sect.3. Sect.4 is devoted to a discussionof the
ASTRONOMY AND A NUMERICAL TIME EPHEMERIS OF THE EARTH Astron. Astrophys. 348, 642–652 (1999) ASTRONOMY AND ASTROPHYSICS A numerical time ephemeris of the Earth A.W. Irwin 1 and T. Fukushima2 1 Department of Physics and Astronomy, University of Victoria, P.O. Box 3055, Victoria, British Columbia, Canada, V8W 3P6 (irwin@uvastro.phys.uvic.ca) 2 National Astronomical Observatory, 2-21-1, Ohsawa, Mitaka, Tokyo 181-8588, Japan ASTRON. ASTROPHYS. 333, 79-91 (1998) Astron. Astrophys. 333, 79-91 (1998) Astron. Astrophys. 333, 79-91 (1998) 4. Pattern velocity and Lindblad resonances. The non-axisymmetric structure in the disk has an angular pattern speed given by the angular velocity . Three radii in each galaxy are of specific interest because the pattern speed resonates with the eigenfrequencies of the ASTRONOMY AND COMPTONIZATION OF THE COSMIC MICROWAVE T.A. Enßlin & C.R. Kaiser: Comptonization of the cosmic microwave background by relativistic plasma 419 0 2 4 6 8 10 12 14-4-2 0 2 4 6 gg h-i j-i Fig.1.
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