Exploring wind-driving dust species in cool luminous giants III : Wind models for M-type AGB stars

Exploring wind-driving dust species in cool luminous giants III : Wind models for M-type AGB stars

[1]  K. Menten,et al.  The wind of W Hydrae as seen by Herschel - II. The molecular envelope of W Hydrae , 2014, 1409.0396.

[2]  Walter Nowotny,et al.  Synthetic photometry for carbon-rich giants IV. An extensive grid of dynamic atmosphere and wind models , , 2014, 1404.7515.

[3]  U. Jørgensen.  Molecules in the Stellar Environment , 2013 .

[4]  B. Aringer,et al.  Exploring wind-driving dust species in cool luminous giants II. Constraints from photometry of M-type AGB stars , 2013, 1302.6572.

[5]  Peter G. Tuthill,et al.  A close halo of large transparent grains around extreme red giant stars , 2012, Nature.

[6]  S. Hofner,et al.  Dust-driven mass loss from carbon stars as a function of stellar parameters - II. Effects of grain size on wind properties , 2011, 1107.1771.

[7]  K. Ohnaka,et al.  Mid-infrared interferometric monitoring of evolved stars - The dust shell around the Mira variable RR Aquilae at 13 epochs , 2011, 1107.0909.

[8]  M. Lederer,et al.  Synthetic photometry for carbon-rich giants II. The effects of pulsation and circumstellar dust , 2011, 1103.5005.

[9]  S. Zeidler,et al.  Near-infrared absorption properties of oxygen-rich stardust analogs. The influence of coloring metal ions , 2011, 1101.0695.

[10]  T. Verhoelst,et al.  Observing and modeling the dynamic atmosphere of the low mass-loss C-star R Sculptoris at high angular resolution , 2010, 1010.1350.

[11]  J. Bernard-Salas,et al.  RUSTY OLD STARS: A SOURCE OF THE MISSING INTERSTELLAR IRON? , 2010, 1005.3489.

[12]  W. Nowotny,et al.  Line formation in AGB atmospheres including velocity effects Molecular line profile variations of long period variables , 2010, 1002.1849.

[13]  S. Hoefner,et al.  Dust driven mass loss from carbon stars as a function of stellar parameters - I. A grid of solar-metallicity wind models , 2009, 1209.4590.

[14]  S. Höfner.  Winds of AGB stars: does size matter? , 2008 .

[15]  S. Höfner,et al.  Winds of M-type AGB stars driven by micron-sized grains , 2008 .

[16]  M. Wittkowski,et al.  The Mira variable S Orionis: relationships between the photosphere, molecular layer, dust shell, and SiO maser shell at 4 epochs , 2007, 0705.4614.

[17]  P. Woitke.  Too little radiation pressure on dust in the winds of oxygen-rich AGB stars , 2006, astro-ph/0609392.

[18]  C. Helling,et al.  Dust in brown dwarfs. V. Growth and evaporation of dirty dust grains , 2006 .

[19]  H. Gail,et al.  Composition and quantities of dust produced by AGB-stars and returned to the interstellar medium , 2006 .

[20]  F. Herwig.  Evolution of Asymptotic Giant Branch Stars , 2005 .

[21]  J. Blommaert,et al.  Mira variables in the OGLE bulge fields , 2005, astro-ph/0506338.

[22]  U. Jørgensen,et al.  Dynamic model atmospheres of AGB stars : IV. A comparison of synthetic carbon star spectra with observations , 2004 .

[23]  Th. Henning,et al.  Steps toward interstellar silicate mineralogy - VII. Spectral properties and crystallization behaviour of magnesium silicates produced by the sol-gel method , 2003 .

[24]  S. Price,et al.  A Uniform Database of 2.4-45.4 Micron Spectra from the Infrared Space Observatory Short Wavelength Spectrometer , 2003 .

[25]  E. Sedlmayr,et al.  Self-consistent modeling of the outflow from the O-rich Mira IRC –20197 , 2003 .

[26]  M. Groenewegen,et al.  "Thermal" SiO radio line emission towards M-type AGB stars: A probe of circumstellar dust formation and dynamics , 2003, astro-ph/0302179.

[27]  U. Jørgensen,et al.  Dynamic model atmospheres of AGB stars - III. Effects of frequency-dependent radiative transfer , 2003 .

[28]  A. Andersen,et al.  Dust formation in winds of long-period variables V. The influence of micro-physical dust properties in carbon stars , 2002, astro-ph/0210282.

[29]  F. Kerschbaum,et al.  Mass loss rates of a sample of irregular and semiregular M-type AGB-variables , 2002, astro-ph/0206172.

[30]  H. Walker,et al.  Classification of 2.4-45.2 Micron Spectra from the Infrared Space Observatory Short Wavelength Spectrometer , 2002, astro-ph/0201507.

[31]  H. Gail,et al.  Mineral formation in stellar winds. II. Effects of Mg/Si abundance variations on dust composition in AGB stars , 2001 .

[32]  J. Bergeat,et al.  The effective temperatures of carbon-rich stars , 2001 .

[33]  M. Feast,et al.  Infrared colours for Mira-like long-period variables found in the Catalogue , 2000 .

[34]  J. Cassinelli,et al.  Introduction to Stellar Winds by Henny J. G. L. M. Lamers , 1999 .

[35]  J. Cassinelli,et al.  Introduction to Stellar Winds , 1999 .

[36]  Th. Henning,et al.  Aluminum Oxide and the Opacity of Oxygen-rich Circumstellar Dust in the 12-17 Micron Range , 1997 .

[37]  H. Shibai,et al.  Extinction spectra of corundum in the wavelengths from UV to FIR. , 1995 .

[38]  Peter G. Martin,et al.  Shape and clustering effects on the optical properties of amorphous carbon , 1991 .

[39]  M. Feast,et al.  A period–luminosity–colour relation for Mira variables , 1989 .

[40]  G. H. Bowen,et al.  Dynamical modeling of long-period variable star atmospheres , 1988 .

[41]  R. J. Bell,et al.  Optical properties of Al, Fe, Ti, Ta, W, and Mo at submillimeter wavelengths. , 1988, Applied optics.

[42]  P. Barber,et al.  Absorption and scattering of light by small particles , 1984 .

[43]  J. Lattimer,et al.  Chemical condensation sequences in supernova ejecta , 1978 .

[44]  A. Schuster.  On the absorption and scattering of light , 1920 .

[45]  J. Dorschner.  From Dust Astrophysics Towards Dust Mineralogy - A Historical Review , 2010 .

[46]  F. Molster,et al.  The Mineralogy of Interstellar and Circumstellar Dust in Galaxies , 2010 .

[47]  O. Heavens.  Handbook of Optical Constants of Solids II , 1992 .

[48]  D. Lynch,et al.  Handbook of Optical Constants of Solids , 1985 .

[49]  P. Wood,et al.  Pulsation and mass loss in Mira variables , 1979 .

[50]  O. Eggen.  Observations of large-amplitude red variables , 1975 .