We present a statistical method to derive the stellar density profiles of the Milky Way from spectroscopic survey data, taking into account selection effects. We assume the selection function, which can be altered dur...We present a statistical method to derive the stellar density profiles of the Milky Way from spectroscopic survey data, taking into account selection effects. We assume the selection function, which can be altered during observations and data reductions, of the spectroscopic survey is based on photometric colors and magnitude. Then the underlying selection function for a line-of-sight can be recovered well by comparing the distribution of the spectroscopic stars in a color-magnitude plane with that of the photometric dataset. Subsequently, the stellar density profile along a line-of-sight can be derived from the spectroscopically measured stellar density profile multiplied by the selection function. The method is validated using Galaxia mock data with two different selection functions. We demonstrate that the derived stellar density profiles reconstruct the true ones well not only for the full set of targets, but also for sub-populations selected from the full dataset. Finally, the method is applied to map the density pro- files for the Galactic disk and halo, using the LAMOST RGB stars. The Galactic disk extends to about R = 19 kpc, where the disk still contributes about 10% to the total stellar surface density. Beyond this radius, the disk smoothly transitions to the halo without any truncation, bending or breaking. Moreover, no over-density corresponding to the Monoceros ring is found in the Galactic anti-center direction. The disk shows moderate north-south asymmetry at radii larger than 12 kpc. On the other hand, the R-Z tomographic map directly shows that the stellar halo is substantially oblate within a Galactocentric radius of 20 kpc and gradually becomes nearly spherical beyond 30 kpc.展开更多
Using the axially deformed relativistic Hartree-Fock-Bogoliubov(D-RHFB)model,we explore the mechanism behind the parity inversion and halo occurrence in^(11)Be,which are well reproduced by the RHF Lagrangian PKA1.It i...Using the axially deformed relativistic Hartree-Fock-Bogoliubov(D-RHFB)model,we explore the mechanism behind the parity inversion and halo occurrence in^(11)Be,which are well reproduced by the RHF Lagrangian PKA1.It is illustrated that evidently enhanced deformation effects by theπ-pseudo-vector andρ-tensor couplings in PKA1 are crucial for correctly describing both the even-parity ground state(GS)and the neutron halo of^(11)Be.Coupling with the deformation,the intrude 1d_(5/2)component largely enhances the couplings between the evenparity orbit 1/2_(2)^(+)and the nuclear core to ensure an even-parity GS,whereas the 2s_(1/2)component therein dominates the halo formation in^(11)Be.Moreover,the deformed halo in^(11)Be is found to be stabilized by the attractive inherent correlations between the 1d_(5/2)and 2s_(1/2)components of the halo orbit 1/2_(2)^(+),instead of pairing correlations,which paves a new way for understanding the halo pictures in deformed unstable nuclei.展开更多
The properties of neutron-rich boron isotopes are studied in the relativistic continuum Hartree-Bogoliubov theory in coordinate space with NL-SH,PK1 and TM2 effective interactions.Pairing corrections are taken into ac...The properties of neutron-rich boron isotopes are studied in the relativistic continuum Hartree-Bogoliubov theory in coordinate space with NL-SH,PK1 and TM2 effective interactions.Pairing corrections are taken into account by a density dependent force of zero range.The binding energies calculated for these nuclei agree with the experimental data quite well.The neutron-rich nucleus 17 B has been predicted to have a two-neutron halo structure in its ground state.The halo structure of 17 B is reproduced in a self-consistent way,and this halo is shown to be formed by the valence neutron level 2s 1/2.展开更多
The structure of Ne isotopes has been investigated by using deformed Skyrme-Hartree-Fock （SHF） method and BCS approximation. Especially the effect of tensor force on the halo structure of 29Ne and 31Ne is discussed....The structure of Ne isotopes has been investigated by using deformed Skyrme-Hartree-Fock （SHF） method and BCS approximation. Especially the effect of tensor force on the halo structure of 29Ne and 31Ne is discussed. To this end, the tensor contributions are considered to the energy density function and the single particle potential in SHF theory. For comparison, four Skyrme interactions are used： SLy5 and SGII without tensor force, and SLy5＋T and SGII＋ T with tensor force. The results indicate that the inclusion of tensor force shows a more pronounced halo structure for 31Ne.展开更多
基金supported by the Strategic Priority Research Program“The Emergence of Cosmological Structures”of the Chinese Academy of Sciences(Grant No.XDB09000000)the National Key Basic Research Program of China(2014CB845700)+1 种基金the National Natural Science Foundation of China(Grant Nos.11373032 and 11333003)a National Major Scientific Project built by the Chinese Academy of Sciences.Funding for the project has been provided by the project has been provided by the National Development and Reform Commission
文摘We present a statistical method to derive the stellar density profiles of the Milky Way from spectroscopic survey data, taking into account selection effects. We assume the selection function, which can be altered during observations and data reductions, of the spectroscopic survey is based on photometric colors and magnitude. Then the underlying selection function for a line-of-sight can be recovered well by comparing the distribution of the spectroscopic stars in a color-magnitude plane with that of the photometric dataset. Subsequently, the stellar density profile along a line-of-sight can be derived from the spectroscopically measured stellar density profile multiplied by the selection function. The method is validated using Galaxia mock data with two different selection functions. We demonstrate that the derived stellar density profiles reconstruct the true ones well not only for the full set of targets, but also for sub-populations selected from the full dataset. Finally, the method is applied to map the density pro- files for the Galactic disk and halo, using the LAMOST RGB stars. The Galactic disk extends to about R = 19 kpc, where the disk still contributes about 10% to the total stellar surface density. Beyond this radius, the disk smoothly transitions to the halo without any truncation, bending or breaking. Moreover, no over-density corresponding to the Monoceros ring is found in the Galactic anti-center direction. The disk shows moderate north-south asymmetry at radii larger than 12 kpc. On the other hand, the R-Z tomographic map directly shows that the stellar halo is substantially oblate within a Galactocentric radius of 20 kpc and gradually becomes nearly spherical beyond 30 kpc.
基金partly supported by the Strategic Priority Research Program of Chinese Academy of Sciences(XDB34000000)the National Natural Science Foundation of China(12275111)the Fundamental Research Funds for the Central Universities(lzujbky-2021–sp41,lzujbky-2021–sp36)。
文摘Using the axially deformed relativistic Hartree-Fock-Bogoliubov(D-RHFB)model,we explore the mechanism behind the parity inversion and halo occurrence in^(11)Be,which are well reproduced by the RHF Lagrangian PKA1.It is illustrated that evidently enhanced deformation effects by theπ-pseudo-vector andρ-tensor couplings in PKA1 are crucial for correctly describing both the even-parity ground state(GS)and the neutron halo of^(11)Be.Coupling with the deformation,the intrude 1d_(5/2)component largely enhances the couplings between the evenparity orbit 1/2_(2)^(+)and the nuclear core to ensure an even-parity GS,whereas the 2s_(1/2)component therein dominates the halo formation in^(11)Be.Moreover,the deformed halo in^(11)Be is found to be stabilized by the attractive inherent correlations between the 1d_(5/2)and 2s_(1/2)components of the halo orbit 1/2_(2)^(+),instead of pairing correlations,which paves a new way for understanding the halo pictures in deformed unstable nuclei.
基金Supported by National Natural Science Foundation of China (11075133,10205019,11075190)Fundamental Research Funds for the Central Universities (XDJK2010D005,XDJK2010C049)+1 种基金Knowledge Innovation Program of Chinese Academy of Sciences(KJCX2-YW-N44)Open Research Program at Large Scale Facility of Chinese Academy of Sciences (O903010YKF)
文摘The properties of neutron-rich boron isotopes are studied in the relativistic continuum Hartree-Bogoliubov theory in coordinate space with NL-SH,PK1 and TM2 effective interactions.Pairing corrections are taken into account by a density dependent force of zero range.The binding energies calculated for these nuclei agree with the experimental data quite well.The neutron-rich nucleus 17 B has been predicted to have a two-neutron halo structure in its ground state.The halo structure of 17 B is reproduced in a self-consistent way,and this halo is shown to be formed by the valence neutron level 2s 1/2.
基金Supported by National Natural Science Foundation of China under Grant Nos.10975116 and 11275160
文摘The structure of Ne isotopes has been investigated by using deformed Skyrme-Hartree-Fock （SHF） method and BCS approximation. Especially the effect of tensor force on the halo structure of 29Ne and 31Ne is discussed. To this end, the tensor contributions are considered to the energy density function and the single particle potential in SHF theory. For comparison, four Skyrme interactions are used： SLy5 and SGII without tensor force, and SLy5＋T and SGII＋ T with tensor force. The results indicate that the inclusion of tensor force shows a more pronounced halo structure for 31Ne.
