2020
DOI: 10.1093/mnras/staa3508
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Polarization simulations of stellar wind bow shock nebulae – II. The case of dust scattering

Abstract: We study the polarization produced by scattering from dust in a bow shock-shaped region of enhanced density surrounding a stellar source, using the Monte Carlo radiative transfer code SLIP. Bow shocks are structures formed by the interaction of the winds of fast-moving stars with the interstellar medium. Our previous study focused on the polarization produced in these structures by electron scattering; we showed that polarization is highly dependent on inclination angle and that multiple scattering changes the… Show more

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Cited by 13 publications
(15 citation statements)
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“…For this investigation, we used an enhanced version of the MCRT code slip (Hoffman 2007;Huk 2017;Shrestha et al 2018;Shrestha et al 2021) that includes binary star capabilities . Appendix A gives more information about the design of slip.…”
Section: Datamentioning
confidence: 99%
“…For this investigation, we used an enhanced version of the MCRT code slip (Hoffman 2007;Huk 2017;Shrestha et al 2018;Shrestha et al 2021) that includes binary star capabilities . Appendix A gives more information about the design of slip.…”
Section: Datamentioning
confidence: 99%
“…Monte Carlo radiative transfer (MCRT) codes have been used extensively to study disks in Be stars (Wood et al 1996a(Wood et al ,b, 1997Hoffman et al 2003;Carciofi & Bjorkman 2006. In addition, recent MCRT simulations have investigated the optical and IR polarization produced by the wind structures around massive, masslosing stars (Shrestha et al 2018(Shrestha et al , 2021. MCRT methods are necessary for these scenarios because the high optical depths that often exist in Be disks give rise to multiple-scattering effects that modify the polarization beyond typical analytical results (Wood et al 1996b;Shrestha et al 2018).…”
Section: Model the Wind/disk Properties Of The Sample Starsmentioning
confidence: 99%
“…8 at wavelengths short-ward of the Balmer jump in the UV spectral range, that the model predictions (thick line) are over-estimated compared to the observations (thin line) due to the presence of many UV metal lines which will provide diagnostics for the disk and stellar surface. The high-quality UV polarized spectra Polstar will obtain will enable more detailed constraints on the geometry of disks and other CSM configurations (e.g., bipolar outflows; Schulte-Ladbeck et al 1992), particularly when combined with sophisticated MCRT models taking into account non-LTE effects (Carciofi & Bjorkman 2006, line blanketing, and geometries more complex than simple 2D disks (Shrestha et al 2018(Shrestha et al , 2021.…”
Section: Model the Wind/disk Properties Of The Sample Starsmentioning
confidence: 99%
“…Polarimetric observations are thus a vital tool for revealing details of the mass-loss and mass-transfer structures in these binaries. Both continuum emission (arising from the stars) and line emission (arising from winds, CIRs, or other shock regions) may be polarized in a CWB system via scattering from wind clumps (Harries et al 1998;Davies et al 2005), accretion disks (Hoffman et al 1998), jets (Fox & Hines 1998), bow shocks (Shrestha et al 2018(Shrestha et al , 2021, and other asymmetric distributions of material or velocities within the system (Schulte-Ladbeck et al 1992;Villar-Sbaffi et al 2005;Fullard et al 2020). Because scattering near the orbital plane tends to produce repeatable effects over many binary cycles, spectropolarimetric monitoring allows us to reconstruct the 3-D shapes of the regions scattering both continuum and line emission (e.g., Lomax et al 2015;Fullard et al 2020).…”
Section: Colliding Winds In Massive Binariesmentioning
confidence: 99%