A Grid of Non-LTE Line-blanketed Model Atmospheres of O-Type Stars

By T. Lanz, I. Hubeny. 2002

540 citations recorded by the source corpus.

We have constructed a comprehensive grid of 680 metal line-blanketed, non-LTE, plane-parallel, hydrostatic model atmospheres for the basic parameters appropriate to O-type stars. The OSTAR2002 grid considers 12 values of effective temperatures, 27,500 K ≤ Teff ≤ 55,000 K with 2500 K steps, eight surface gravities, 3.0 ≤ log g ≤ 4.75 with 0.25 dex steps, and 10 chemical compositions, from metal-rich relative to the Sun to metal-free. The lower limit of log g for a given effective temperature is set by an approximate location of the Eddington limit. The selected chemical compositions have been chosen to cover a number of typical environments of massive stars: the Galactic center, the Magellanic Clouds, blue compact dwarf galaxies like I Zw 18, and galaxies at high redshifts. The paper contains a description of the OSTAR2002 grid and some illustrative examples and comparisons. The complete OSTAR2002 grid is available on-line.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics

View Paper: https://www.semanticscholar.org/paper/366b81b6df20b91761f2c9d57283bdf45d325be1

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In Astronomy and Astrophysics

1. P. Hopkins
2. C. Conroy
3. L. Hernquist
4. R. Dav'e
5. R. Somerville
6. A. Dekel
7. R. Maiolino
8. R. Genzel

In Atomic and Molecular Physics, and Optics

1. D. John Hillier
2. T. Lanz
3. J. Bouret
4. T. Ott
5. D. Massa
6. R. Genzel
7. E. Fitzpatrick
8. A. Sternberg

Citations in the corpus

• Modelling the nebular emission from primeval to present-day star-forming galaxies (2016, background): “…ionizing spectra come from the library of metal line-blanketed, non-local thermodynamic equilibrium (non-LTE), plane-parallel, hydrostatic models of Lanz & Hubeny (2003, 2007), which reach effective temperatures of up to 55,000 K and cover a wide range of metallicities (from zero to twice solar).”
• A new extensive library of PHOENIX stellar atmospheres and synthetic spectra (2013, methodology): “The NLTE stellar atmosphere code TLUSTY (Hubeny 1988) made possible a grid of NLTE atmospheres for O stars (Lanz & Hubeny 2003).”
• WHAT DRIVES THE EXPANSION OF GIANT H ii REGIONS?: A STUDY OF STELLAR FEEDBACK IN 30 DORADUS (2010, methodology): “To estimate these parameters as a function of radius in cloudy, we utilize the OSTAR2002 stellar atmosphere model for a metallicity Z/Z⊙ = 0.5 (Lanz & Hubeny 2003) and stellar temperature of T∗ = 35000 K.”
• An Analysis of the Shapes of Interstellar Extinction Curves. V. The IR-through-UV Curve Morphology (2007, methodology): “Because we include some O stars in the current sample, we have expanded our technique to incorporate the TLUSTY OSTAR2002 grid of line-blanketed, hydrostatic, NLTE, plane-parallel models by Lanz & Hubeny (2003).”
• SDSS-IV MaNGA : the impact of diffuse ionized gas on emission-line ratios, interpretation of diagnostic diagrams and gas metallicity measurements (2016, background): “The magenta line is a 42,300K, log g=4.22, solar metallicity O star generated by Tlusty (Lanz & Hubeny 2003).”
• Modeling the Panchromatic Spectral Energy Distributions of Galaxies (2013, background): “At the high temperature end, i.e., Wolf-Rayet and O-type main sequence stars, the state-of-the-art libraries are from Smith, Norris & Crowther (2002) and Lanz & Hubeny (2003), while for hotter compact objects (e.g., post-AGB stars) the most up-to-date models are from Rauch (2003).”
• Physical parameters and wind properties of galactic early B supergiants (2005, background): “Recent developments in model-atmosphere studies of hot stars routinely permit sophisticated metal-line blanketing in nonLTE to be considered, under either plane-parallel geometry (e.g., TLUSTY: Hubeny & Lanz 1995; Lanz & Hubeny 2003) or spherical geometry (e.g., CMFGEN: Hillier & Miller 1998).”
• SPITZER SAGE INFRARED PHOTOMETRY OF MASSIVE STARS IN THE LARGE MAGELLANIC CLOUD (2009, methodology): “We compare the observed colors with colors of plane-parallel non-LTE TLUSTY stellar atmosphere models (Lanz & Hubeny 2003, 2007) of appropriate metallicity and effective temperatures.”
• Lower mass loss rates in O-type stars: Spectral signatures of dense clumps in the wind of two Galactic O4 stars (2004, methodology): “For more details on these two codes, we refer to Hubeny & Lanz (1995), Lanz & Hubeny (2003), Hillier & Miller (1998), Hillier et al. (2003), and Bouret et al. (2003).”
• A CHARA ARRAY SURVEY OF CIRCUMSTELLAR DISKS AROUND NEARBY Be-TYPE STARS (2013, methodology): “We used the FUV flux ratio, temperatures, and gravities from Gies et al. (1998) and derived magnitude differences by scaling model spectral energy distributions from Lanz & Hubeny (2003).”
• Effects of gravitational darkening on the determination of fundamental parameters in fast-rotating B-type stars (2005, methodology): “For T 0eff < 15 000 K and T 0 eff > 27 000 K (T 0 eff concern rotationless model atmospheres) we used LTE calculations and the 2002 model atmospheres grid (Lanz & Hubeny 2003).”
• THE MASS OF THE BLACK HOLE IN CYGNUS X-1 (2011, methodology): “For the specific case of Cygnus X-1, the range of temperature–gravity pairs on the star contained points that are outside the OSTAR2002+BSTAR2006 model grids (Lanz & Hubeny 2003, 2007).”
• A LIBRARY OF THEORETICAL ULTRAVIOLET SPECTRA OF MASSIVE, HOT STARS FOR EVOLUTIONARY SYNTHESIS (2010, methodology): “Plane-parallel models, such as ATLAS (Kurucz 2005) or TLUSTY (Lanz & Hubeny 2003, 2007), cannot account for spectral lines forming in the wind and are obviously not suitable for our purpose.”
• First Results from the CHARA Array. I. An Interferometric and Spectroscopic Study of the Fast Rotator α Leonis (Regulus) (2005, methodology): “The spectra were computed using the code Synspec (Lanz & Hubeny 2003) and are based on solar abundance atmospheres models by R. L. Kurucz4 (for a chosen microturbulent velocity of 1 km s−1).”
• Ionizing Photon Emission Rates from O- and Early B-Type Stars and Clusters (2003, methodology): “…rates of Lyman continuum photons (Lyc; hν > 13.6 eV), and of helium continuum photons (He I; hν > 24.6 eV), are particularly important and fundamental parameters of O-type and early B-type stars (Mihalas 1967; Panagia 1973; Vacca, Garmany & Shull 1996; Schaerer & de Koter 1997; Lanz & Hubeny 2003).”
• The most massive stars in the Arches cluster (2007, methodology): “Here, we used the TLUSTY structures of Lanz & Hubeny (2003) for the hydrostatic part of the atmosphere.”
• The VLT-FLAMES survey of massive stars: surface chemical compositions of B-type stars in the Magellanic Clouds (2006, methodology): “In this table we list the species, wavelength, log gf value and also indicate if the line is considered as part of a blend of lines in the TLUSTY code, see Dufton et al., Allende Prieto et al. 2003 and Lanz & Hubeny 2003 for details.”