Chemical Abundances in the Secondary Star in the Black Hole Binary A0620−00

Hernández, J. I. González; Rebolo, R.; Israelian, G.; Casares, J.; Maeder, A.; Meynet, Georges

doi:10.1086/421102

Cited by 43 publications

(5 citation statements)

References 51 publications

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“…Using the derived stellar parameters, we determine the element abundances from the absorption-line equivalent width (EW) measurements of the elements given in Table 4, except for lithium and sulfur for which we use a χ 2 procedure to find the best fit to the observed features (e.g., González Hernández et al 2004, 2006. The atomic data for O, C, S, and Zn are taken from Ecuvillon et al (2004Ecuvillon et al ( , 2006, those of Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr, Mn, Co, and Ni are from Gilli et al (2006), and those for Sr, Y, and Ba are from Reddy et al (2003).…”

Section: Chemical Abundancesmentioning

confidence: 99%

“…Tycho G shares a high Li content with a known sample of binary companions of neutron stars and black holes (Martín et al 1994a;González Hernández et al 2004. However, we know that cataclysmic variables, whose compact objects are white dwarfs, do not show such high Li abundances (Martín et al 1995).…”

Section: Chemical Abundancesmentioning

confidence: 99%

“…Moreover, the orbital elements just before the explosion are also different; in particular, the separations are larger. Given the orbital history up to the explosion, it is reasonable to find fast rotators around black holes and neutron stars (González Hernández et al 2004Hernández et al , 2005Hernández et al , 2008b. The companion stars of these compact objects do not transfer mass to the star that becomes a core-collapse SN.…”

Section: Projected Rotational Velocity Of Tycho Gmentioning

confidence: 99%

See 2 more Smart Citations

The Chemical Abundances of Tycho G in Supernova Remnant 1572

Hernández

Ruiz‐Lapuente

Filippenko

et al. 2009

ApJ

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We present an analysis of the chemical abundances of the star Tycho G in the direction of the remnant of supernova (SN) 1572, based on Keck high-resolution optical spectra. The stellar parameters of this star are found to be those of a G-type subgiant with T eff = 5900 ± 100 K, log(g/cms 2) = 3.85 ± 0.30 dex, and [Fe/H] = −0.05 ± 0.09. This determination agrees with the stellar parameters derived for the star in a previous survey for the possible companion star of SN 1572 (Ruiz-Lapuente et al.). The chemical abundances follow the Galactic trends, except for Ni, which is overabundant relative to Fe, [Ni/Fe] = 0.16 ± 0.04. Co is slightly overabundant (at a low significance level). These enhancements in Fe-peak elements could have originated from pollution by the SN ejecta. We find a surprisingly high Li abundance for a star that has evolved away from the main sequence. We discuss these findings in the context of companion stars of SNe.

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Section: Chemical Abundancesmentioning

confidence: 99%

Section: Chemical Abundancesmentioning

confidence: 99%

Section: Projected Rotational Velocity Of Tycho Gmentioning

confidence: 99%

See 1 more Smart Citation

The Chemical Abundances of Tycho G in Supernova Remnant 1572

Hernández

Ruiz‐Lapuente

Filippenko

et al. 2009

ApJ

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“…It is unclear whether this scenario would be valid here but, in any case, the large orbital period decays measured clearly have very important implications on the evolution and lifetime of SP-BHXBs, which, according to the standard models, is typically ∼ 5 × 10 9 yr. In addition, the companion stars with spectral types earlier than K5V show high Li abundances (Martín et al 1996;González Hernández et al 2004, 2006, similar to those of low mass stars of the young (120 Myr) Pleiades cluster (Garcia Lopez et al 1994), which are not easily explained unless a Li preservation mechanism is invoked, on the basis of high rotation velocities of the companion stars kept during the evolution of tidally locked BHXBs (Maccarone et al 2005;Casares et al 2007). A shorter lifetime, of ∼ 10 7 − 10 8 yr, would alleviate this high-Li problem in BHXBs as well as the long-standing birthrate problem of millisecond pulsars and low-mass BHXBs (Naylor & Podsiadlowski 1993;Podsiadlowski et al 2002).…”

Section: Discussionmentioning

confidence: 99%

Extremely fast orbital decay of the black hole X-ray binary Nova Muscae 1991

Hernández

Suárez-Andrés

Rebolo

et al. 2016

Monthly Notices of the Royal Astronomical Society: Letters

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We present new medium-resolution spectroscopic observations of the black hole X-ray binary Nova Muscae 1991 taken with X-Shooter spectrograph installed at the 8.2m-VLT telescope. These observations allow us to measure the time of inferior conjunction of the secondary star with the black hole in this system that, together with previous measurements, yield an orbital period decay of ˙ P = −20.7 ± 12.7 ms yr −1 (−24.5 ± 15.1 µs per orbital cycle). This is significantly faster than those previously measured in the other black hole X-ray binaries A0620-00 and XTE J1118+480. No standard black hole X-ray binary evolutionary model is able to explain this extremely fast orbital decay. At this rate, the secondary star would reach the event horizon (as given by the Schwarzschild radius of about 32 km) in roughly 2.7 Myr. This result has dramatic implications on the evolution and lifetime of black hole X-ray binaries.

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“…Actually, previous studies of a few RLOF BHs with low spin do indicate short accretion time. For instance, A0620-00 (González Hernández et al 2004) and LMC X-3 (Sørensen et al 2017) are thought to have short accretion time (∼ 10 7 yr ). So similar to the NS LMXBs, the spin value of RLOF BHs (𝑎 * < 0.3) also depends on the mass transfer rate, then the positive relations between the spin parameters and the orbital parameters are expected.…”

Section: Bh Xrbsmentioning

confidence: 99%

An apparent positive relation between spin and orbital angular momentum in X-ray binaries

Yan

Zhang

2023

Monthly Notices of the Royal Astronomical Society

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The origin of current angular momentum (AM) of the black hole (BH) in X-ray binary (XRB) is still unclear, which is related with the birth and/or the growth of the BH. Here we collect the spin parameters a* measured in BH XRBs and find an apparent bimodal distribution centered at ∼ 0.17 and 0.83. We find a positive relation between the spin parameter and the orbital period/orbital separation through combining distinct XRB categories, including neutron star (NS) low-mass X-ray binaries (LMXBs), Roche-lobe overflow (RLOF) BH XRBs and wind-fed BH XRBs. It seems that the AM of the compact star and the binary orbit correlates by combining the different XRB systems. These positive relations imply that accretion process is a common mechanism for spinning up the compact star in these diverse XRB systems. We infer that the low and high spin BH XRBs may experience different evolution and accretion history, which corresponds to the bimodal distribution of the BH spin parameters. The low spin BHs (a* < 0.3) are similar to the NS LMXBs, the compact star of which is spun-up by the low-level accretion, and the high spin BHs (a* > 0.5) had experienced a short hypercritical accretion ($\gg \dot{M}_\mathrm{Edd}$) period, during which, the BH spin dramatically increased.

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Chemical Abundances in the Secondary Star in the Black Hole Binary A0620−00

Cited by 43 publications

References 51 publications

The Chemical Abundances of Tycho G in Supernova Remnant 1572

The Chemical Abundances of Tycho G in Supernova Remnant 1572

Extremely fast orbital decay of the black hole X-ray binary Nova Muscae 1991

An apparent positive relation between spin and orbital angular momentum in X-ray binaries

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