We present a study of the Galactic bubble N4 using the 13.7 m millimeterwave telescope, which is managed by Purple Mountain Observatory at Qinghai Station. N4 is one of the science demonstration regions where simultan...We present a study of the Galactic bubble N4 using the 13.7 m millimeterwave telescope, which is managed by Purple Mountain Observatory at Qinghai Station. N4 is one of the science demonstration regions where simultaneous observations of ^12CO （J = 1 - 0）, ^13CO （J = 1 - 0） and C^18O （J = 1 - 0） line emission towards N4 were carried out under the project Milky Way Imaging Scroll Painting （MWISP）. We analyze the spectral profile and the distribution of the molecular gas. Morphologically, the CO emissions correlate well with Spitzer IRAC 8.0 p-m emission. The channel map and velocity-position diagram show that N4 is more likely to be an inclined expanding ring rather than a spherical bubble. We calculated the physical parameters of N4 including mass, size, column density and optical depth. Some massive star candidates were discovered in the region of N4 using the （J, J-H） colormagnitude diagram. We found a candidate for the energy source driving the expansion of N4, a massive star with a mass of -15 M⊙ and an age of - 1Myr. There is the signature of infall motion in N4, which can be a good candidate for the infall area. Combining millimeter and infrared data, we suggest that triggered star formation can exist in N4.展开更多
The mutual interaction between cavitation bubbles plays an important role in the physical processes of cavitation. In this paper, a complete model is developed for modelling the mutual interaction between cavitation b...The mutual interaction between cavitation bubbles plays an important role in the physical processes of cavitation. In this paper, a complete model is developed for modelling the mutual interaction between cavitation bubbles with the effects of liquid compressibility fully included. It is found that the liquid compressibility is an important parameter in the determination of the direction of the force （the attraction or repulsion force）, as well as the magnitude of the force. The influences of the liquid compre- ssibility on the mutual interaction force can be categorized into three terms： the first is a new term added on the mutual interaction force in incompressible liquids and this term will vanish if the sizes of two bubbles are equal, the second is the radiation damping term, the third one can be considered as a correction of the mutual interaction force in incompressible liquids with a coefficient and this correction will be prominent for small bubbles and a high ambient pressure.展开更多
From the similarity theorem, an expression of bubble population is derived as a function of the air en-trainment rate, the turbulent kinetic energy (TKE) spectrum density and the surface tension. The bubble size spect...From the similarity theorem, an expression of bubble population is derived as a function of the air en-trainment rate, the turbulent kinetic energy (TKE) spectrum density and the surface tension. The bubble size spectrum that we obtain has a dependence of a?2.5+nd on the bubble radius, in which nd is positive and dependent on the form of TKE spectrum within the viscous dissipation range. To relate the bubble population with wave parameters, an expression about the air entrainment rate is deduced by intro-ducing two statistical relations to wave breaking. The bubble population vertical distribution is also derived, based on two assumptions from two typical observation results.展开更多
基金funded by the National Aeronautics and Space Administrationthe National Science Foundation+1 种基金supported by the National Natural Science Foundation of China (Grant Nos. 10873037, 10921063 and 11233007)supported by the National Basic Research Program of China (973 program, 2007CB815406)
文摘We present a study of the Galactic bubble N4 using the 13.7 m millimeterwave telescope, which is managed by Purple Mountain Observatory at Qinghai Station. N4 is one of the science demonstration regions where simultaneous observations of ^12CO （J = 1 - 0）, ^13CO （J = 1 - 0） and C^18O （J = 1 - 0） line emission towards N4 were carried out under the project Milky Way Imaging Scroll Painting （MWISP）. We analyze the spectral profile and the distribution of the molecular gas. Morphologically, the CO emissions correlate well with Spitzer IRAC 8.0 p-m emission. The channel map and velocity-position diagram show that N4 is more likely to be an inclined expanding ring rather than a spherical bubble. We calculated the physical parameters of N4 including mass, size, column density and optical depth. Some massive star candidates were discovered in the region of N4 using the （J, J-H） colormagnitude diagram. We found a candidate for the energy source driving the expansion of N4, a massive star with a mass of -15 M⊙ and an age of - 1Myr. There is the signature of infall motion in N4, which can be a good candidate for the infall area. Combining millimeter and infrared data, we suggest that triggered star formation can exist in N4.
基金Project supported by the National Natural Science Foun-dation of China(Grant Nos.51506051,51606221)
文摘The mutual interaction between cavitation bubbles plays an important role in the physical processes of cavitation. In this paper, a complete model is developed for modelling the mutual interaction between cavitation bubbles with the effects of liquid compressibility fully included. It is found that the liquid compressibility is an important parameter in the determination of the direction of the force （the attraction or repulsion force）, as well as the magnitude of the force. The influences of the liquid compre- ssibility on the mutual interaction force can be categorized into three terms： the first is a new term added on the mutual interaction force in incompressible liquids and this term will vanish if the sizes of two bubbles are equal, the second is the radiation damping term, the third one can be considered as a correction of the mutual interaction force in incompressible liquids with a coefficient and this correction will be prominent for small bubbles and a high ambient pressure.
文摘From the similarity theorem, an expression of bubble population is derived as a function of the air en-trainment rate, the turbulent kinetic energy (TKE) spectrum density and the surface tension. The bubble size spectrum that we obtain has a dependence of a?2.5+nd on the bubble radius, in which nd is positive and dependent on the form of TKE spectrum within the viscous dissipation range. To relate the bubble population with wave parameters, an expression about the air entrainment rate is deduced by intro-ducing two statistical relations to wave breaking. The bubble population vertical distribution is also derived, based on two assumptions from two typical observation results.
