The ionizing and heating power of ultraluminous X-ray sources under the geometrical beaming model

Kovlakas, Konstantinos; Fragos, Tassos; Mesinger, Andrei

doi:10.1051/0004-6361/202244252

Cited by 7 publications

(8 citation statements)

References 55 publications

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“…As such, we must transform the observed XLF quantities (number counts, or relative contribution to the total population, and L obs ) into the intrinsic physical properties from Table 1. To do so, we follow a methodology similar to the approach outlined in Kovlakas et al (2022).…”

Section: Parameterization Of Sed Shapementioning

confidence: 99%

“…Further combining Equation (8) with Equations ( 5) and (6) enables solving for  m in terms of L obs and L Edd . In particular, this can be accomplished via an analytic approximation as outlined in Kovlakas et al (2022):…”

Section: Parameterization Of Sed Shapementioning

confidence: 99%

“…Accreting stellar-mass compact objects (i.e., XRBs) are one such product of binary evolution, and they have long been considered as a potential source of high-energy ionizing photons (e.g., Garnett et al 1991;Schaerer et al 2019;Kovlakas et al 2022). Recent photoionization modeling that combines XRBs with stellar populations hints that XRBs may be sufficient to reproduce observed high-ionization emission line strengths in some cases (e.g., Senchyna et al 2020;Simmonds et al 2021).…”

Section: Introductionmentioning

confidence: 99%

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Modeling the High-energy Ionizing Output from Simple Stellar and X-Ray Binary Populations

Garofali,

Basu-Zych,

Johnson

et al. 2023

ApJ

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We present a methodology for modeling the joint ionizing impact due to a “simple X-ray population” (SXP) and its corresponding simple stellar population (SSP), where “simple” refers to a single age and metallicity population. We construct composite spectral energy distributions (SEDs) including contributions from ultraluminous X-ray sources and stars, with physically meaningful and consistent consideration of the relative contributions of each component as a function of instantaneous burst age and stellar metallicity. These composite SEDs are used as input for photoionization modeling with Cloudy, from which we produce a grid for the time- and metallicity-dependent nebular emission from these composite populations. We make the results from the photoionization simulations publicly available. We find that the addition of the SXP prolongs the high-energy ionizing output from the population—and correspondingly increases the intensity of nebular lines such as He ii λ1640,4686, [Ne v] λ3426,14.3 μm, and [O iv] 25.9 μm by factors of at least two relative to models without an SXP spectral component. This effect is most pronounced for instantaneous bursts of star formation on timescales >10 Myr and at low metallicities (∼0.1 Z ⊙), due to the imposed time- and metallicity-dependent behavior of the SXP relative to the SSP. We propose nebular emission line diagnostics accessible with JWST suitable for inferring the presence of a composite SXP + SSP, and we discuss how the ionization signatures compare to models for sources such as intermediate-mass black holes.

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Section: Parameterization Of Sed Shapementioning

confidence: 99%

Section: Parameterization Of Sed Shapementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Modeling the High-energy Ionizing Output from Simple Stellar and X-Ray Binary Populations

Garofali,

Basu-Zych,

Johnson

et al. 2023

ApJ

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“…where in the second line we have estimated the number of ionizing photons emitted per second from the binary as Φ ; L bin /(2 Ry), where Ry =13.6 eV, motivated by the high effective temperatures of both the stripped core (T eff ≈ 10 5 K; e.g., Götberg et al 2019) and the BH/NS accretion disk (e.g., Kovlakas et al 2022). The characteristic maximum mass-loss rate at radii r ∼ R g (assuming…”

Section: Photoionization Mass Lossmentioning

confidence: 99%

Long-term Evolution of Massive-star Post-common-envelope Circumbinary Disks and the Environments of Fast Luminous Transients

Tuna,

Metzger

2023

ApJ

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If the envelope of a massive star is not entirely removed during common envelope (CE) interaction with an orbiting compact (e.g., black hole (BH) or neutron star (NS)) companion, the residual bound material eventually cools, forming a centrifugally supported disk around the binary containing the stripped He core. We present a time-dependent height-integrated model for the long-term evolution of post-CE circumbinary disks (CBDs), accounting for mass and angular momentum exchange with the binary, irradiation heating by the He core, and photoevaporation wind mass loss. A large fraction of the CBD’s mass is accreted prior to its outwards viscous spreading and wind dispersal on a timescale of ∼104–105 yr, driving significant orbital migration, even for disks containing ∼10% of the original envelope mass. Insofar that the CBD lifetime is comparable to the thermal (and, potentially, nuclear) timescale of the He core, over which a second mass-transfer episode onto the companion can occur, the presence of the CBD could impact the stability of this key phase. Disruption of the core by the BH/NS would result in a jetted energetic explosion into the dense gaseous CBD (≲1015 cm) and its wind (≳1016 cm), consistent with the environments of luminous fast blue optical transients like AT2018cow. Evolved He cores that undergo core collapse still embedded in their CBD could generate Type Ibn/Icn supernovae. Thousands of dusty wind-shrouded massive-star CBDs may be detectable as extragalactic luminous infrared sources with the Roman Space Telescope; synchrotron radio nebulae powered by the CBD-fed BH/NS may accompany these systems.

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“…Similarly, Linden et al (2010) used the StarTrack code (Belczynski et al 2008) and found an increase of a factor of 3.5 when going to Z/Z = 0.2 for young bright HMXBs. The increased number of XRBs in low-metallicity environments, coupled with the metallicity evolution of the Universe (e.g., Fragos et al 2013a,b), points to the possibility of XRBs having a significant effect on the ionization of the interstellar medium in the local Universe as well as the intergalactic medium in the early Universe (e.g., Madau & Fragos 2017;Schaerer et al 2019;Kaur et al 2022;Kovlakas et al 2022).…”

Section: Introductionmentioning

confidence: 99%

X-ray luminosity function of high-mass X-ray binaries: Studying the signatures of different physical processes using detailed binary evolution calculations

Misra

Kovlakas

Fragos

et al. 2023

A&A

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Context. Many physical processes taking place during the evolution of binary stellar systems remain poorly understood. The ever-expanding observational sample of X-ray binaries (XRBs) makes them excellent laboratories for constraining binary evolution theory. Such constraints and useful insights can be obtained by studying the effects of various physical assumptions on synthetic X-ray luminosity functions (XLFs) and comparing them with observed XLFs. Aims. In this work we focus on high-mass X-ray binaries (HMXBs) and study the effects on the XLF of various, poorly constrained assumptions regarding physical processes, such as the common-envelope phase, core collapse, and wind-fed accretion. Methods. We used the new binary population synthesis code POSYDON, which employs extensive precomputed grids of detailed stellar structure and binary evolution models, to simulate the entire evolution of binaries. We generated 96 synthetic XRB populations corresponding to different combinations of model assumptions, including different prescriptions for supernova kicks, supernova remnant masses, common-envelope evolution, circularization at the onset of Roche-lobe overflow, and observable wind-fed accretion. Results. The generated HMXB XLFs are feature-rich, deviating from the commonly assumed single power law. We find a break in our synthetic XLF at luminosity ∼1038 erg s−1, similar to observed XLFs. However, we also find a general overabundance of XRBs (up to a factor of ∼10 for certain model parameter combinations) driven primarily by XRBs with black hole accretors. Assumptions about the transient behavior of Be XRBs, asymmetric supernova kicks, and common-envelope physics can significantly affect the shape and normalization of our synthetic XLFs. We find that less well-studied assumptions regarding the circularization of the orbit at the onset of Roche-lobe overflow and criteria for the formation of an X-ray-emitting accretion disk around wind-accreting black holes can also impact our synthetic XLFs and reduce the discrepancy with observations. Conclusions. Our synthetic XLFs do not always agree well with observations, especially at intermediate X-ray luminosities, which is likely due to uncertainties in the adopted physical assumptions. While some model parameters leave distinct imprints on the shape of the synthetic XLFs and can reduce this deviation, others do not have a significant effect overall. Our study reveals the importance of large-scale parameter studies, highlighting the power of XRBs in constraining binary evolution theory.

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The ionizing and heating power of ultraluminous X-ray sources under the geometrical beaming model

Cited by 7 publications

References 55 publications

Modeling the High-energy Ionizing Output from Simple Stellar and X-Ray Binary Populations

Modeling the High-energy Ionizing Output from Simple Stellar and X-Ray Binary Populations

Long-term Evolution of Massive-star Post-common-envelope Circumbinary Disks and the Environments of Fast Luminous Transients

X-ray luminosity function of high-mass X-ray binaries: Studying the signatures of different physical processes using detailed binary evolution calculations

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