The soft and hard X-rays thermal emission from star cluster winds with a supernova explosion

Castellanos-Ramírez, A.; Rodríguez-González, A.; Esquivel, A.; Toledo-Roy, J. C.; Olivares, J.; Velázquez, P. F.

doi:10.1093/mnras/stv795

Cited by 11 publications

(8 citation statements)

References 33 publications

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“…The evolutionary X-ray emission for the models was computed using emission coefficients in the low-density regime taken from chianti data base as function of the metallicity (see Figure 2 in Castellanos-Ramírez et al 2015) in the band of 0.6 to 10 keV (soft and hard X-ray band). Figure 8 shows the temperature, column densities and intrinsic X-ray emission maps, upper middle and lower panels, respectively, for the models M1, M2 and M3, left, center and right panels, respectively, at t=400 kyr.…”

Section: Numerical Resultsmentioning

confidence: 99%

“…Column 6 shows the luminosity. We used a super-solar metallicity for the wind and a sub-solar metallicity in the interstellar medium, 3 and 0.3 Z , respectively (see Castellanos-Ramírez et al 2015). We have carried out time integrations from t = 0 up to t = 0.4 Myr for all the models.…”

Section: Chandra X-ray Observations and Gas Dynamic Simulation Of Rcw...mentioning

confidence: 99%

“…Regarding the X-ray emission of superbubbles, is important take into account that the original work of Weaver et al (1977) overestimated the observed X-ray luminosity in some bubbles. And for example, others studies like Harper-Clark & Murray (2009) and Rogers & Pittard (2014) underestimate the X-ray emission (see (Castellanos-Ramírez et al 2015) for more information). Therefore, from a theoretical point of view, the X-ray luminosity in a bubble is expected.…”

Section: Introductionmentioning

confidence: 99%

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Kinematics of the Galactic Bubble RCW 120

Sánchez-Cruces,

Castellanos-Ramírez,

Rosado

et al. 2018

Preprint

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RESUMENPresentamos el estudio cinemático en las líneas de [SII]λλ6717, 6731 Å de la burbuja Galáctica RCW 120. Determinamos que la velocidad radial de esta burbuja se encuentra entre ∼-74 to ∼-6 km s −1 . Encontramos evidencia de expansión unicamente en la parte noreste de la nebulosa (de 20 a 30 km s −1 ). Encontramos alta densidad en la parte suroeste de la nebulosa (4000 cm −3 ) así como dos gradientes de densidad en la parte sur. Con la finalidad de explorar la dinámica, morfología y emisión óptica de RCW 120 presentamos simulaciones numéricas en 3D de esta burbuja usando el código Walicxe-3D. Los resultados numéricos predicen que en promedio la densidad del medio (en la parte sur del objeto) es de entre 3000 to 5000 cm −3 , lo que concuerda con los valores observados. Los modelos no predicen emisión en rayos X provenientes del cascarón debido a la velocidad de expansión baja.

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Section: Numerical Resultsmentioning

confidence: 99%

Section: Chandra X-ray Observations and Gas Dynamic Simulation Of Rcw...mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Kinematics of the Galactic Bubble RCW 120

Sánchez-Cruces,

Castellanos-Ramírez,

Rosado

et al. 2018

Preprint

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“…3D radiation-HD simulations were performed by Wünsch et al (2017), where they studied the impact of rapidly cooling winds on secondary stellar generations. In their 3D HD model Castellanos-Ramírez et al (2015) considered a supernova explosion in the context of massive stellar association, together with the effects of wind metallicity and thermal conduction. Detailed 3D HD modeling of massive star cluster feedback on the leftover from its parent molecular cloud was performed by Rogers & Pittard (2013, 2014.…”

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confidence: 99%

Inside the core of a young massive star cluster: 3D MHD simulations

Badmaev

Bykov

Kalyashova

2022

Monthly Notices of the Royal Astronomical Society

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Young massive star clusters inhabit regions of star formation and play an essential role in the galactic evolution. They are sources of both thermal and non-thermal radiation, and they are effective cosmic ray accelerators. We present the 3D magnetohydrodynamic (MHD) modeling of the plasma flows in a young compact cluster at the evolutionary stage comprising multiple interacting supersonic winds of massive OB and WR stars. The modeling allows studying the partitioning of the mechanical energy injected by the winds between the bulk motions, thermal heating and magnetic fields. Cluster-scale magnetic fields reaching the magnitudes of ∼ 300 μG show the filamentary structures spreading throughout the cluster core. The filaments with the high magnetic fields are produced by the Axford-Cranfill type effect in the downstream of the wind termination shocks, which is amplified by a compression of the fields with the hot plasma thermal pressure in the central part of the cluster core. The hot (∼ a few keV) plasma is heated at the termination shocks of the stellar winds and compressed in the colliding postshock flows. We also discuss a possible role of the thermal conduction effects on the plasma flow, analyse temperature maps in the cluster core and the diffuse thermal X-ray emission spectra. The presence of high cluster-scale magnetic fields supports the possibility of high-energy cosmic ray acceleration in clusters at the given evolutionary stage.

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“…v.lora@irya.unam.mx Full, 3D gasdynamical simulations of the production of a cluster wind through the interaction of many stellar winds were presented by Raga et al (2001); Rodríguez-González et al (2007; Hueyotl-Zahuantitla et al (2010); Palous et al (2013). The related problem of the detonation of a single supernova within a cluster wind was studied by Rodríguez-Ramírez et al (2014) and Castellanos-Ramírez et al (2015).…”

Section: Introductionmentioning

confidence: 99%

Huffing, and puffing, and blowing your house in: Strong stellar winds interaction with a super massive black hole

Lora,

Raga,

Canto

et al. 2021

Preprint

Self Cite

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We present analytic and numerical models of a cluster wind flow resulting from the interaction of stellar winds of massive stars, with a super massive black hole (SMBH). We consider the motion of the stars as well as the gravitational force of the SMBH. In the numerical simulations we consider two cases: the first one with the stars is in circular orbits, and the second one with the stars in eccentric orbits around the SMBH. We found that after the system reaches an equilibrium, the circular and elliptical cases are very similar. We found a very good agreement between the analytical and numerical results, not only from our numerical simulations but also from other high resolution numerical calculations. The analytical models are very interesting, since the properties of such complex systems involving strong winds and a massive compact object, can be rapidly inferred without the need of a numerical calculation.

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The soft and hard X-rays thermal emission from star cluster winds with a supernova explosion

Cited by 11 publications

References 33 publications

Kinematics of the Galactic Bubble RCW 120

Kinematics of the Galactic Bubble RCW 120

Inside the core of a young massive star cluster: 3D MHD simulations

Huffing, and puffing, and blowing your house in: Strong stellar winds interaction with a super massive black hole

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