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A Modern Guide to Quantitative Spectroscopy of Massive OB Stars

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Abstract

Quantitative spectroscopy is a powerful technique from which we can extract information about the physical properties and surface chemical composition of stars. In this chapter, I guide the reader through the main ideas required to get initiated in the learning process to become an expert in the application of state-of-the-art quantitative spectroscopic techniques to the study of massive OB stars.

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Notes

  1. 1.

    By D. Jones, J. García-Rojas and Petr Kabáth (co-PI’s of the ERASMUS+ project “Per aspera ad astra simul”).

  2. 2.

    This diagram can be considered as an equivalent to the HRD, but only using stellar parameters derived spectroscopically (see also [18]).

  3. 3.

    Poelarends et al. [22] propose a fiducial value of 9 M⊙ for the minimum initial mass of massive stars at solar metallicity, where massive star is defined as a star that is massive enough to form a collapsing core at the end of its life and, thus, avoid the while dwarf fate [23].

  4. 4.

    Actually, it is not yet completely clear whether the group of stars marked as B supergiants (B Sgs) are post-MS stars, MS stars or, even, some of them are post red supergiant stars (see Section 6.1 in [23] and references therein).

  5. 5.

    Due to their high temperatures and luminosities, OB stars are sometimes also quoted as blue massive stars, and the O and B supergiants, as blue supergiants.

  6. 6.

    For example, N iii–iv–v and Si iv–iii–ii lines in the early-O and the early-B stars, respectively (see Sect. 3.4).

  7. 7.

    Also, different implementations of the associated model atoms—including a more or less detailed description of the energy levels and transitions of specific ions—are required.

  8. 8.

    For this type of stars, the Gaia RVs range is basically populated by a few Paschen lines.

  9. 9.

    Corresponding to the transitions N vλλ1239/43 Å, Si ivλλ1394/403 Å, and C ivλλ1548/51 Å.

  10. 10.

    Most of the ideas presented along this section can be easily extrapolated to any quantitative spectroscopic analysis of the UV and IR spectral windows, with the only difference that other diagnostic lines, model atoms, and physical assumptions in the modeling of the stellar wind must be considered. Also some parameters and abundances may be more difficult (or even impossible in some cases) to be constrained just using the UV and/or IR part of the spectrum.

  11. 11.

    Linear Stark broadening mainly affect the wings of the H and, to a less extent, the He ii lines; indeed, this effect is mainly used to constrain the surface gravity (see Sect. 3.6).

  12. 12.

    Quadratic Stark broadening, which is much less pronounced than the linear one, mainly affects the shape of the He i lines.

  13. 13.

    Into the line-of-sight.

  14. 14.

    The most common value used for A is 0.660, which corresponds to a limb-darkening coefficient of 𝜖 = 0.6 (see, however, Fig. 3 in [101]).

  15. 15.

    With the same equivalent width as the observed profile.

  16. 16.

    In many cases, a stellar atmosphere code includes the computation of the emergent spectrum.

  17. 17.

    Model atoms—including information about energy levels and the main collisional and radiative transitions between levels and/or the continuum—are a very important ingredient of stellar atmosphere code. They will be only occasionally mentioned along this chapter; however, basic knowledge of how models atoms are implemented and used in stellar atmosphere and diagnostic codes is the forth pillar a quantitative stellar spectroscopist should dominate, along with basic concepts of observational stellar spectroscopy, radiative transfer and stellar atmosphere modeling.

  18. 18.

    http://nova.astro.umd.edu.

  19. 19.

    http://kookaburra.phyast.pitt.edu/hillier/web/CMFGEN.htm.

  20. 20.

    http://www.astro.physik.uni-potsdam.de/~wrh/PoWR/powrgrid1.php.

  21. 21.

    log Q = log \({\dot {M}}\) – 1.5 log R – 1.5 log v ∞ [121]. This parameter is used as a proxy of the wind properties in the optical analyses because this spectral window does not include any diagnostic line reacting exclusively (or mainly) to the mass-loss rate (\({\dot {M}}\)) or the wind terminal velocity (v ∞).

  22. 22.

    iacob-gbat [69] is a grid-based automatic tool for the quantitative spectroscopic analysis of O-stars. The tool consists of an extensive grid of FASTWIND models, and a variety of programs implemented in IDL to handle the observations, perform the automatic analysis, and visualize the results. The tool provides a fast and objective way to determine the stellar parameters and the associated uncertainties of large samples of O-type stars within a reasonable computational time.

  23. 23.

    Microturbulence (ξ t) is a free parameter that was included in the stellar abundance analyses to solve the discrepancy found in the line abundances from weak and strong lines. Its physical meaning is supposed to be related to the small scale turbulent motions of the stellar plasma which could mainly affect the strong lines close to saturation.

  24. 24.

    This is the case for the spectral synthesis method, where the effect of microturbulence or the existence of wrongly modeled lines (see [82]) is not so easily identified.

  25. 25.

    Either directly or by using equivalent widths of a selected sample of diagnostic lines.

  26. 26.

    For example, effective temperature and surface gravity, abundance and microturbulence, mass loss rate and the β parameter.

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Acknowledgements

I want to warmly thank all those friends and colleagues from which I’ve been able to learn and discuss about quantitative spectroscopy since my first years as PhD student at the Instituto de Astrofísica de Canarias. Special thanks to A. Herrero, M. A. Urbaneja, C. Villamariz, F. Najarro, C. Trundle, D. J. Lennon, J. Puls, N. Castro, M. Garcia, F. Nieva, C. Sabín-Sanjulian, K. Rübke, G. Holgado, S. Berlanas, and A. de Burgos. Let this text serves to spread part of the knowledge I’ve acquired from all of you during these years.

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  1. Instituto de Astrofísica de Canarias, La Laguna, Tenerife, Spain

    Sergio Simón-Díaz

  2. Departamento de Astrofísica, Universidad de La Laguna, La Laguna, Tenerife, Spain

    Sergio Simón-Díaz

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  1. Astronomical Institute of the Czech Academy of Sciences, Ondrejov, Czech Republic

    Petr Kabáth

  2. Instituto de Astrofisica de Canarias, La Laguna, Spain

    David Jones

  3. Department of Theoretical Physics and Astrophysics, Masaryk University, Brno, Czech Republic

    Marek Skarka

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Simón-Díaz, S. (2020). A Modern Guide to Quantitative Spectroscopy of Massive OB Stars. In: Kabáth, P., Jones, D., Skarka, M. (eds) Reviews in Frontiers of Modern Astrophysics. Springer, Cham. https://doi.org/10.1007/978-3-030-38509-5_6

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