Previous simulations studying winds only focus on the line force due to photons from central active galactic nuclei.What properties of the winds will be when including the re-radiation force due to the scattered and r...Previous simulations studying winds only focus on the line force due to photons from central active galactic nuclei.What properties of the winds will be when including the re-radiation force due to the scattered and reprocessed photons(i.e.,the re-radiation effect)?We perform simulations to study the large-scale dynamics of accretion disk winds driven by radiation line force and re-radiation force.For the fiducial run,we find that the re-radiation force drives stronger outflows during the early stages.When the flows get into the steadiness,the UV radiation due to spectral lines dominates total radiation and the re-radiation effect could be negligible.The opening angle of winds narrows as the initial gas density increases.The larger the gas density is,the stronger the re-radiation effect will be.For MBH=10^(6)M_(⊙),ε=0.3,the outflows do become much stronger with the re-radiation effect and the winds still cannot escape from gravitational potential.We find that the detection probability of ultra-fast outflows and the properties of the winds are both consistent with the observations.展开更多
Black widows(BWs)are millisecond pulsars ablating their companion stars.The out-flowing material from the companion can block the radio emission of the pulsar,resulting in eclipses.In this paper,we construct a model f...Black widows(BWs)are millisecond pulsars ablating their companion stars.The out-flowing material from the companion can block the radio emission of the pulsar,resulting in eclipses.In this paper,we construct a model for the radio eclipse by calculating the geometry of the bow shock between the winds of the pulsar and companion,where the shock shapes the eclipsing medium but had not been described in detail in previous works.The model is further used to explain the variations of the flux density and dispersion measure of three BW pulsars(i.e.,PSR B1957+20,J2055+3829,and J2051-0827)detected by the Five-hundred-meter Aperture Spherical radio Telescope.Consequently,we constrained the parameters of the three BW systems such as the inclination angles and true anomalies of the observer as well as the mass-loss rates and wind velocity of the companion stars.With the help of these constraints,it is expected that magnetic fields of companion stars and even masses of pulsars could further be determined as some extra observation can be achieved in the future.展开更多
文摘Previous simulations studying winds only focus on the line force due to photons from central active galactic nuclei.What properties of the winds will be when including the re-radiation force due to the scattered and reprocessed photons(i.e.,the re-radiation effect)?We perform simulations to study the large-scale dynamics of accretion disk winds driven by radiation line force and re-radiation force.For the fiducial run,we find that the re-radiation force drives stronger outflows during the early stages.When the flows get into the steadiness,the UV radiation due to spectral lines dominates total radiation and the re-radiation effect could be negligible.The opening angle of winds narrows as the initial gas density increases.The larger the gas density is,the stronger the re-radiation effect will be.For MBH=10^(6)M_(⊙),ε=0.3,the outflows do become much stronger with the re-radiation effect and the winds still cannot escape from gravitational potential.We find that the detection probability of ultra-fast outflows and the properties of the winds are both consistent with the observations.
基金supported by the National SKA program of China(2020SKA0120300)the National Key R&D Program of China(2021YFA0718500)+2 种基金the National Natural Science Foundation of China(grant Nos.11833003,12033001)the China Postdoctoral Science Foundation(No.2023T160410)the Opening Foundation of Xinjiang Key Laboratory(No.2021D04016)。
文摘Black widows(BWs)are millisecond pulsars ablating their companion stars.The out-flowing material from the companion can block the radio emission of the pulsar,resulting in eclipses.In this paper,we construct a model for the radio eclipse by calculating the geometry of the bow shock between the winds of the pulsar and companion,where the shock shapes the eclipsing medium but had not been described in detail in previous works.The model is further used to explain the variations of the flux density and dispersion measure of three BW pulsars(i.e.,PSR B1957+20,J2055+3829,and J2051-0827)detected by the Five-hundred-meter Aperture Spherical radio Telescope.Consequently,we constrained the parameters of the three BW systems such as the inclination angles and true anomalies of the observer as well as the mass-loss rates and wind velocity of the companion stars.With the help of these constraints,it is expected that magnetic fields of companion stars and even masses of pulsars could further be determined as some extra observation can be achieved in the future.
