Last edited by Kagajar
Tuesday, July 28, 2020 | History

3 edition of Blanketed model atmospheres for early-type stars found in the catalog.

Blanketed model atmospheres for early-type stars

Robert L. Kurucz

Blanketed model atmospheres for early-type stars

by Robert L. Kurucz

  • 322 Want to read
  • 24 Currently reading

Published by Smithsonian Institution : for sale by the Supt. of Docs., U.S. Govt. Print. Off. in Washington .
Written in English

    Subjects:
  • Early stars -- Atmospheres.

  • Edition Notes

    StatementRobert L. Kurucz, Eric Peytremann, and Eugene H. Avrett.
    ContributionsPeytremann, Eric, joint author., Avrett, Eugene H., 1933- joint author., Smithsonian Astrophysical Observatory.
    Classifications
    LC ClassificationsQB843.E2 K87
    The Physical Object
    Paginationv, 186 p. :
    Number of Pages186
    ID Numbers
    Open LibraryOL4854024M
    LC Control Number75603223

    The ESA catalogue gives absolute fluxes for 43 O-type stars, mostly reddened, with a spectral resolution of 35–40 A, depending on the channel, in the wavelength range – A. The Copernicus catalogue gives spectra between and A for 17 O-type stars, with low reddening, at A : Carlo Morossi, Roberto Stalio, Lucio Crivellari. which is another typical approximations of classical model atmospheres, breaks down for early-type stars, in particular for O stars. We thus drop the approximation of LTE and compute non-LTE (NLTE) models. ArehydrostaticO-star model atmosphere relevant? At the very outset, we have to clarify one crucial question. It is well known that the most.

    We use a spherical non-LTE fully line-blanketed model atmosphere to fit the full multiwavelength spectrum, including the extreme-ultraviolet (EUV) continuum observed by the Extreme Ultraviolet Explorer, of the B2 II star Canis Majoris (CMa). The available spectrophotometry of CMa from Å to 25 μm is best fitted with model parameters T eff = Cited by: cesses in stellar atmospheres, led to an increasing complexity in the models. As a result, codes emerged that can tackle a wide range of stellar and wind parameters. After a brief address of the fundamentals of stellar atmosphere modeling, the current stage of clumped and line-blanketed model atmospheres will be discussed. Finally, the path for the.

    Example of a computed evolutionary scenario of separation of mercury isotopes due to LID in mercury-rich (solar + 5 dex) main sequence stellar atmosphere (T eff = 10, K, log g = 4, V rot = 0, V turb = 0) is given in Fig. otions that Cited by: 4. @article{osti_, title = {O-star parameters from line profiles of wind-blanketed model atmospheres}, author = {Voels, S A}, abstractNote = {The basic stellar parameters (i.e. effective temperature, gravity, helium content, bolometric correction, etc) of several O-stars are determined by matching high signal-to-noise observed line.


Share this book
You might also like
In defense of women

In defense of women

Ecological anatomy of woody plants with special reference to leaf variations

Ecological anatomy of woody plants with special reference to leaf variations

US labour unions today

US labour unions today

Italian food

Italian food

economy of Tudor Worcester.

economy of Tudor Worcester.

The musicians business & legal guide /compiled and edited by Mark Halloran ; a presentation of the Beverley Hills Bar Association Committee for the Atrs.

The musicians business & legal guide /compiled and edited by Mark Halloran ; a presentation of the Beverley Hills Bar Association Committee for the Atrs.

Geology underfoot in southern Utah

Geology underfoot in southern Utah

Curse you, Jack Dalton!

Curse you, Jack Dalton!

Carpet testing.

Carpet testing.

The French Revolution.

The French Revolution.

Raindrop Algorithm Based Controller for Chopper Driven PMDC Motor

Raindrop Algorithm Based Controller for Chopper Driven PMDC Motor

Battery materials 1970

Battery materials 1970

works of James Gillray

works of James Gillray

Capsules of New Jersey history

Capsules of New Jersey history

Auto-oxidation potential of raw and retored oil shale

Auto-oxidation potential of raw and retored oil shale

Expedited site assessment tools for underground storage tank sites

Expedited site assessment tools for underground storage tank sites

Blanketed model atmospheres for early-type stars by Robert L. Kurucz Download PDF EPUB FB2

Not Available adshelp[at] The ADS is operated by the Smithsonian Astrophysical Observatory under NASA Cooperative Agreement NNX16AC86ACited by: COVID Resources.

Reliable information about the coronavirus (COVID) is available from the World Health Organization (current situation, international travel).Numerous and frequently-updated resource results are available from this ’s WebJunction has pulled together information and resources to assist library staff as they consider how to handle.

late essentially “exact”, fully blanketed NLTE hydrostatic model stellar atmospheres. Earlier model atmospheres of B-type stars neglected either departures from Local Thermodynamic Equilibrium (LTE; Kurucz ) or the effect of line opacity from heavier species such as the initial H-He NLTE model atmospheres (Mihalas & Auer ).

of NLTE line-blanketed model atmospheres to late B-type and early A-type stars. Advancesinnumerical schemesappliedtostellaratmosphere modeling and large increases in computational resources during the last decade have provided the ability to calculate essentially ‘‘exact,’’ fully blanketed NLTE hydrostatic model stellar atmo-spheres.

SAO/NASA Astrophysics Data System (ADS) Title: Blanketed model atmospheres for early-type stars Authors: Kurucz, R. L., Peytremann, E., & Avrett, E.

Journal. Blanketed model atmospheres for early-type stars By Robert L Kurucz, Eric Peytremann and H Avrett Topics: Astrophysics and AstronomyAuthor: Robert L Kurucz, Eric Peytremann and H Avrett. We present recent progress in model atmospheres for hot stars.

A new generation of NLTE wind blanketed models, together with ground-based and ISO-SWS spectra of hot stars will allow reliable metal abundance determinations (Fe, Si, Mg, Na, etc) of these objects.

After checking the consistency of these results with those obtained from optical studies, we may confidently use Author: F. Najarro, D. Hillie, R. Kudritzki, P. Morris. We have constructed a comprehensive grid of metal line-blanketed, NLTE, plane-parallel, hydrostatic model atmospheres for the basic parameters appropriate to early B-type by: A Grid of NLTE Line-blanketed Model Atmospheres of Early B-Type Stars: Authors: Lanz, Thierry; Hubeny, Ivan: Affiliation: AA(Department of Astronomy, University of Maryland, College Park, MD ), AB(Steward Observatory, University of Arizona, Tucson, AZ ) Publication: The Astrophysical Journal Supplement Series, VolumeIssue 1.

Line-blanketed classical model atmospheres incorporating a band-model opacity are applied to determine the photospheric spectral energy distribution of the M2 supergiant Betelgeuse.

We find that our metal line-blanketed spherical models show significantly warmer temperature structures, kK at the formation depth of the Lyman continua, and predict stronger EUV fluxes, up to a factor of 5 in the H I Lyman continuum, compared with plane-parallel atmospheres that have identical model parameters.

We have made a detailed comparison of results of spectroscopic analysis using three differents types of model atmospheres: classical non-LTE H-He models; approximate non-LTE line-blanketed models (with only a subset of Fe and Ni lines: those originating from transitions between levels with measured energies); and non-LTE fully blanketed models.

The Cited by: ISBN: OCLC Number: Notes: "Proceedings of a workshop organized jointly by the UK SERC's Collaborative Computational Project No.

7 and the Instutut fur Theoretische Physik und Sternwarte, University of Kiel held at the University of Kiel, Germany September ".

We have constructed a comprehensive grid of metal line-blanketed, non-LTE, plane-parallel, hydrostatic model atmospheres for the basic parameters appropriate to O-type stars. The OSTAR grid considers 12 values of effective temperatures, 27,KCited by: Then, since the lines absorb energy, the temperature of the blanketed model must be greater than that of the line-free model in the region near continuum optical depth unity in order to produce more energy between the lines and to emit the same total amount of energy as the line-free model.

We have constructed a comprehensive grid of metal line-blanketed, non-LTE, plane-parallel, hydrostatic model atmospheres for the basic parameters appropriate to O-type stars. We describe the treatment of iron group line-blanketing in non-LTE model atmospheres for WR stars.

As an example, a blanketed model for the early. White Dwarf Model Atmosphere Iron Line Atmospheric Structure Early Type Star These keywords were added by machine and not by the authors.

This process is experimental and the keywords may be updated as the learning algorithm : Ivan Hubeny, Thierry Lanz. Thesis/Dissertation: Spherical, non-LTE, blanketed model stellar atmosphere for Phi Cas (FOIa).

blanketed tlusty model atmospheres, covering e ective-temperature and surface- gravity ranges of 15{55 kK and dex (cgs) down to the e ective Eddington limit, at 2, 1, (LMC), (SMC), and solar.

Get this from a library! The Atmospheres of early-type stars. [U Heber; C S Jeffery;] -- These workshop proceedings aim to provide a broad overview of recent developments in the study of hot stars, both from the observational and the theoretical point of view.

Included are first results.Spherically symmetric NLTE model atmospheres of hot hydrogen-helium first stars Article in The Astrophysical Journal Supplement Series (2) Author: Jiří Kubát.Local Thermodynamic Equilibrium (LTE) is known to be a useful simplifying assumption when computing line-blanketed model stellar atmospheres and synthetic spectra.

Element abundance adjustment can optimise agreement between a synthetic and an observed spectrum, providing a useful technique for abundance determination when spectrum lines are Author: A.

E. Lynas-Gray.