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Verfasst von:Latour, Marilyn [VerfasserIn]   i
 Heber, U. [VerfasserIn]   i
 Irrgang, A. [VerfasserIn]   i
 Schaffenroth, V. [VerfasserIn]   i
 Geier, S. [VerfasserIn]   i
 Hillebrandt, W. [VerfasserIn]   i
 Röpke, Friedrich [VerfasserIn]   i
 Taubenberger, S. [VerfasserIn]   i
 Kromer, M. [VerfasserIn]   i
 Fink, M. [VerfasserIn]   i
Titel:Quantitative spectral analysis of the sdB star HD 188112
Titelzusatz:a helium-core white dwarf progenitor
Verf.angabe:M. Latour, U. Heber, A. Irrgang, V. Schaffenroth, S. Geier, W. Hillebrandt, F. K. Röpke, S. Taubenberger, M. Kromer, M. Fink
E-Jahr:2016
Jahr:05 January 2016
Umfang:17 S.
Teil:volume:585
 year:2016
 pages:1-17
 extent:17
Fussnoten:Gesehen am 16.06.2020
Titel Quelle:Enthalten in: Astronomy and astrophysics
Ort Quelle:Les Ulis : EDP Sciences, 1969
Jahr Quelle:2016
Band/Heft Quelle:585(2016) Artikel-Nummer A115, 17 Seiten
ISSN Quelle:1432-0746
Abstract:<i>Context. <i/>HD 188112 is a bright (<i>V<i/> = 10.2 mag) hot subdwarf B (sdB) star with a mass too low to ignite core helium burning and is therefore considered a pre-extremely low-mass (ELM) white dwarf (WD). ELM WDs (<i>M<i/> ≲ 0.3 <i>M<i/><sub>⊙<sub/>) are He-core objects produced by the evolution of compact binary systems.<i>Aims. <i/>We present in this paper a detailed abundance analysis of HD 188112 based on high-resolution <i>Hubble <i/>Space Telescope (HST) near- and far-ultraviolet spectroscopy. We also constrain the mass of the star’s companion. <i>Methods. <i/>We use hybrid non-LTE model atmospheres to fit the observed spectral lines, and to derive the abundances of more than a dozen elements and the rotational broadening of metallic lines. <i>Results. <i/>We confirm the previous binary system parameters by combining radial velocities measured in our UV spectra with the previously published values. The system has a period of 0.60658584 days and a WD companion with <i>M<i/> ≥ 0.70 <i>M<i/><sub>⊙<sub/>. By assuming a tidally locked rotation combined with the projected rotational velocity (<i>v<i/> sin <i>i<i/> = 7.9 ± 0.3 km s<sup>-1<sup/>), we constrain the companion mass to be between 0.9 and 1.3 <i>M<i/><sub>⊙<sub/>. We further discuss the future evolution of the system as a potential progenitor of an underluminous type Ia supernova. We measure abundances for Mg, Al, Si, P, S, Ca, Ti, Cr, Mn, Fe, Ni, and Zn, and for the trans-iron elements Ga, Sn, and Pb. In addition, we derive upper limits for the C, N, O elements and find HD 188112 to be strongly depleted in carbon. We find evidence of non-LTE effects on the line strength of some ionic species such as Si ii and Ni ii. The metallic abundances indicate that the star is metal-poor, with an abundance pattern most likely produced by diffusion effects.
DOI:doi:10.1051/0004-6361/201527445
URL:Bitte beachten Sie: Dies ist ein Bibliographieeintrag. Ein Volltextzugriff für Mitglieder der Universität besteht hier nur, falls für die entsprechende Zeitschrift/den entsprechenden Sammelband ein Abonnement besteht oder es sich um einen OpenAccess-Titel handelt.

Volltext ; Verlag: https://doi.org/10.1051/0004-6361/201527445
 Volltext: https://www.aanda.org/articles/aa/abs/2016/01/aa27445-15/aa27445-15.html
 DOI: https://doi.org/10.1051/0004-6361/201527445
Datenträger:Online-Ressource
Sprache:eng
K10plus-PPN:1700627279
Verknüpfungen:→ Zeitschrift

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