We have developed a self-consistent physical model for superstellar cluster winds based on combining a 1D steady-state adiabatic wind solution and a non-equilibrium ionization calculation. Comparing with the case of collisional ionization equilibrium, we find that the non-equilibrium ionization effect is significant in the regime of a high ratio of energy to mass input rate and manifests in a stronger soft X-ray flux in the inner region of the star cluster. Implementing the model in X-ray data analysis softwares (e.g. xspec) directly facilitates comparisons with X-ray observations. Physical quantities such as the mass and energy input rates of stellar winds can be estimated by fitting observed X-ray spectra. The fitted parameters may then b...
We detail method and report results from an ensemble of three-dimensional hydrodynamical and N-body ...
In order to compare the x-wind with observations, one needs to be able to calculate its thermal and ...
We present simulations of the multiphase interstellar medium (ISM) at solar neighbourhood conditions...
We have developed a self-consistent physical model for super stellar cluster winds based on combinin...
The spectral code for non-equilibrium plasma has been developed based on the updated atomic database...
We present hydrodynamical simulations of galactic winds from star-forming galaxies including non-equ...
The densities in the outer regions of clusters of galaxies are very low, and the collisional timesca...
We study the impact of stellar winds and supernovae on the multiphase interstellar medium using thre...
The densities in the outer regions of clusters of galaxies are very low, and the collisional timesca...
The X-ray emission from a simulated massive stellar cluster is investigated. The emis-sion is calcul...
We present models for temperature and ionization structure of low, uniform-density (n ~ 0.3 cm^-3) ...
Mathematical and Physical Sciences: 1st Place (The Ohio State University Edward F. Hayes Graduate Re...
The X-ray emission from a simulated massive stellar cluster is investigated. The emission is calcula...
International audienceContext. X-ray imaging observatories have revealed hydrodynamic structures wit...
[[abstract]]In order to compare the X-wind with observations, one needs to be able to calculate its ...
We detail method and report results from an ensemble of three-dimensional hydrodynamical and N-body ...
In order to compare the x-wind with observations, one needs to be able to calculate its thermal and ...
We present simulations of the multiphase interstellar medium (ISM) at solar neighbourhood conditions...
We have developed a self-consistent physical model for super stellar cluster winds based on combinin...
The spectral code for non-equilibrium plasma has been developed based on the updated atomic database...
We present hydrodynamical simulations of galactic winds from star-forming galaxies including non-equ...
The densities in the outer regions of clusters of galaxies are very low, and the collisional timesca...
We study the impact of stellar winds and supernovae on the multiphase interstellar medium using thre...
The densities in the outer regions of clusters of galaxies are very low, and the collisional timesca...
The X-ray emission from a simulated massive stellar cluster is investigated. The emis-sion is calcul...
We present models for temperature and ionization structure of low, uniform-density (n ~ 0.3 cm^-3) ...
Mathematical and Physical Sciences: 1st Place (The Ohio State University Edward F. Hayes Graduate Re...
The X-ray emission from a simulated massive stellar cluster is investigated. The emission is calcula...
International audienceContext. X-ray imaging observatories have revealed hydrodynamic structures wit...
[[abstract]]In order to compare the X-wind with observations, one needs to be able to calculate its ...
We detail method and report results from an ensemble of three-dimensional hydrodynamical and N-body ...
In order to compare the x-wind with observations, one needs to be able to calculate its thermal and ...
We present simulations of the multiphase interstellar medium (ISM) at solar neighbourhood conditions...