Relativistic hydrodynamical simulations of the effects of the stellar wind and the orbit on high-mass microquasar jets
| Autor: | Maxim V Barkov, V Bosch-Ramon |
|---|---|
| Přispěvatelé: | Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), Consejo Nacional de Investigaciones Científicas y Técnicas (Argentina), Generalitat de Catalunya |
| Jazyk: | angličtina |
| Rok vydání: | 2022 |
| Předmět: |
High Energy Astrophysical Phenomena (astro-ph.HE)
Radiation mechanisms: non-thermal Hidrodinàmica Astrophysics::High Energy Astrophysical Phenomena FOS: Physical sciences Astronomy and Astrophysics Outflows Stars: winds X-ray binaries X-rays: binaries Space and Planetary Science Hydrodynamics Astrophysics::Solar and Stellar Astrophysics Astrophysics::Earth and Planetary Astrophysics Astrophysics - High Energy Astrophysical Phenomena Estels binaris de raigs X |
| Zdroj: | Dipòsit Digital de la UB Universidad de Barcelona |
| Popis: | High-mass microquasar jets, produced in an accreting compact object in orbit around a massive star, must cross a region filled with stellar wind. The combined effects of the wind and orbital motion can strongly affect the jet properties on binary scales and beyond. The study of such effects can shed light on how high-mass microquasar jets propagate and terminate in the interstellar medium. We study for the first time, using relativistic hydrodynamical simulations, the combined impact of the stellar wind and orbital motion on the properties of high-mass microquasar jets on binary scales and beyond. We have performed 3-dimensional relativistic hydrodynamic simulations, using the PLUTO code, of a microquasar scenario in which a strong weakly relativistic wind from a star interacts with a relativistic jet under the effect of the binary orbital motion. The parameters of the orbit are chosen such that the results can provide insight on the jet-wind interaction in compact systems like for instance Cyg X-1 or Cyg X-3. The wind and jet momentum rates are set to values that may be realistic for these sources and lead to moderate jet bending, which together with the close orbit and jet instabilities could trigger significant jet precession and disruption. For high-mass microquasars with orbit size a ∼ 0.1 AU, and (relativistic) jet power Lj∼1037(M˙w/10−6M⊙yr−1) erg s−1, where M˙w is the stellar wind mass rate, the combined effects of the stellar wind and orbital motion can induce relativistic jet disruption on scales ∼1 AU. VB-R acknowledges the support by the Spanish Ministerio de Ciencia e Innovación (MICINN) under grant PID2019-105510GB-C31 and through the ‘Center of Excellence María de Maeztu 2020–2023’ award to the ICCUB (CEX2019-000918-M), and by the Catalan DEC grant 2017 SGR 643. VB-R is Correspondent Researcher of CONICET, Argentina, at the IAR. |
| Databáze: | OpenAIRE |
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