Two-dimensional modeling of density and thermal structure of dense circumstellar outflowing disks

Kurfürst, Petr; Feldmeier, Achim; Krtička, Jiřı́

doi:10.1051/0004-6361/201731300

Cited by 14 publications

(25 citation statements)

References 67 publications

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“…We assume an isothermal initial temperature structure of the CSM (of both the components) within the computational domain, given as T sw = T csd = 0.7T eff (cf. Carciofi & Bjorkman 2008;Kurfürst et al 2018). This also indicates the initial counterpressure of the CSM as P = ρa 2 , where the square sound speed a 2 is given by Eq.…”

Section: Methodsmentioning

confidence: 99%

“…Carciofi & Bjorkman 2008). For simplicity we omit the vertical (relatively shallow) variations of the temperature profile (e.g., Sigut & Jones 2007;Kurfürst et al 2018). However, the temperature profile serves in our study only as a basis for determining the initial gas pressure of CSM (where ρ may be either ρ sw or ρ csd ),…”

Section: Circumstellar Equatorial Disks Structurementioning

confidence: 99%

“…Integrating the density profiles, we estimate the total mass of the CSM components: for spherically symmetric component of CSM we obtain the total mass M sw = 4πR 2 ρ 0,sw r 1 R dr ≈ Krtička et al 2011;Kurfürst et al 2014Kurfürst et al , 2018.…”

Section: Model A: High Density Of the Surrounding Mediamentioning

confidence: 99%

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Modeling of interactions between supernovae ejecta and aspherical circumstellar environments

Kurfürst

Krtička

2019

A&A

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Received ABSTRACTContext. Massive stars are characterized by a significant loss of mass either via (nearly) spherically symmetric stellar winds or preexplosion pulses, or by aspherical forms of circumstellar matter (CSM) such as bipolar lobes or outflowing circumstellar equatorial disks. Since a significant fraction of most massive stars end their lives by a core collapse, supernovae (SNe) are always located inside large circumstellar envelopes created by their progenitors. Aims. We study the dynamics and thermal effects of collision between expanding ejecta of SNe and CSM that may be formed during, for example, a sgB[e] star phase, a luminous blue variable phase, around PopIII stars, or by various forms of accretion. Methods. For time-dependent hydrodynamic modeling we used our own grid-based Eulerian multidimensional hydrodynamic code built with a finite volumes method. The code is based on a directionally unsplit Roe's method that is highly efficient for calculations of shocks and physical flows with large discontinuities. Results. We simulate a SNe explosion as a spherically symmetric blast wave. The initial geometry of the disks corresponds to a density structure of a material that orbits in Keplerian trajectories. We examine the behavior of basic hydrodynamic characteristics, i.e., the density, pressure, velocity of expansion, and temperature structure in the interaction zone under various geometrical configurations and various initial densities of CSM. We calculate the evolution of the SN -CSM system and the rate of aspherical deceleration as well as the degree of anisotropy in density, pressure, and temperature distribution. Conclusions. Our simulations reveal significant asphericity of the expanding envelope above all in the case of dense equatorial disks. Our "low density" model however also shows significant asphericity in the case of the disk mass-loss rateṀ csd = 10 −6 M yr −1 . The models also show the zones of overdensity in the SN -disk contact region and indicate the development of Kelvin-Helmholtz instabilities within the zones of shear between the disk and the more freely expanding material outside the disk. P. Kurfürst et al.: Modeling of adiabatic interactions between supernovae ejecta and circumstellar disks that corresponding to viscous outflowing disks, which are typical for classical Be stars. However, we may assume to find this disk type in sgB[e] stars as well (for a review see, e.g., Zickgraf 1998; Hillier 2006), where a disk or rings of high density material have been detected (Kraus et al. 2013). Other types of dense equatorial disks or disk-like density enhancements may also be formed owing to, for example, magnetically compressed winds or binarity and accretion around certain classes of, for instance, B[e] stars (e.g., Hillier 2006), luminous blue variables (e.g., Schulte-Ladbeck et al. 1994;Davies et al. 2005), and post-AGB stars (e.g., Heger & Langer 1998).Although there have been a number of studies regarding interactions of SNe expansion with various forms of spherically symmet...

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Section: Methodsmentioning

confidence: 99%

Section: Circumstellar Equatorial Disks Structurementioning

confidence: 99%

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Modeling of interactions between supernovae ejecta and aspherical circumstellar environments

Kurfürst

Krtička

2019

A&A

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“…The ER is reminiscent of similar ring-like circumstellar features observed in SN 1987A (e.g., Frank et al 2016 and references therein) and the B-type supergiant SBW1 (Smith et al 2013). Such structures may originate from mass loss facilitated by the rapid rotation of the progenitor, binary interactions, confinement of the shed mass by magnetic fields, and possible combinations of these factors (e.g., Kurfurst et al 2018 and references therein).…”

Section: Properties Of the Csmmentioning

confidence: 99%

Detailed X-Ray Mapping of the Shocked Ejecta and Circumstellar Medium in the Galactic Core-collapse Supernova Remnant G292.0+1.8

Bhalerao

Park

Schenck

et al. 2019

ApJ

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G292.0+1.8 (G292) is a young (∼3000 yr), Galactic textbook-type core-collapse supernova remnant (CCSNR). It is characterized by X-ray, optical and infrared emission from ejecta and circumstellar medium (CSM) features, and contains a pulsar (PSR J1124-5916) and pulsar wind nebula that have been observed in X-rays and radio. Previous studies have revealed a complex, dynamically evolving, oxygen-rich remnant, a striking relic from the explosion of a massive star. Here, using our deep (530 ks) Chandra ACIS data, we present high spatial-resolution maps (based on a regional grid size of a few arcsec) of the shocked CSM and metal-rich ejecta in G292. We make the first Chandra-detection of Fe-rich ejecta in G292. We identify the X-ray counterpart of the northern equatorial belt, a component of a ring-like CSM structure identified earlier in the infrared band. We show the detailed spatial distributions of ejecta enriched in O, Ne, Mg, Si, S and Fe. We find that the bulk of the Si, S and Fe-rich X-ray-emitting ejecta are located in the northwestern hemisphere of the remnant, opposite to the pulsar's projected angular displacement to the southeast from the SNR's center. This suggests that the pulsar's kick may have originated from gravitational and hydrodynamic forces during an asymmetric explosion, rather than from anisotropic neutrino emission. Based on abundance ratios and our estimated CSM and ejecta masses, we constrain the progenitor mass to 13 M M 30 M

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“…We calculated the thermal and radiative flux near the disk midplane as a diffusion approximation. We used our own Eulerian hydrodynamic code and special cylindrical-conical coordinate system (Kurfürst et al 2018).…”

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confidence: 99%

Modeling of hydrodynamic processes within high-mass X-ray binaries

Kurfürst

Krtička²

2018

Proc. IAU

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High-mass X-ray binaries belong to the brightest objects in the X-ray sky. They usually consist of a massive O or B star or a blue supergiant while the compact X-ray emitting component is a neutron star (NS) or a black hole. Intensive matter accretion onto the compact object can take place through different mechanisms: wind accretion, Roche-lobe overflow, or circumstellar disk. In our multi-dimensional models we perform numerical simulations of the accretion of matter onto a compact companion in case of Be/X-ray binaries. Using Bondi-Hoyle-Littleton approximation, we estimate the NS accretion rate. We determine the Be/X-ray binary disk hydrodynamic structure and compare its deviation from isolated Be stars’ disk. From the rate and morphology of the accretion flow and the X-ray luminosity we improve the estimate of the disk mass-loss rate. We also study the behavior of a binary system undergoing a supernova explosion, assuming a blue supergiant progenitor with an aspherical circumstellar environment.

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Two-dimensional modeling of density and thermal structure of dense circumstellar outflowing disks

Cited by 14 publications

References 67 publications

Modeling of interactions between supernovae ejecta and aspherical circumstellar environments

Modeling of interactions between supernovae ejecta and aspherical circumstellar environments

Detailed X-Ray Mapping of the Shocked Ejecta and Circumstellar Medium in the Galactic Core-collapse Supernova Remnant G292.0+1.8

Modeling of hydrodynamic processes within high-mass X-ray binaries

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