The great Tancheng earthquake of M81/2 occurred in 1668 was the largest seismic event ever recorded in history in eastern China. This study determines the fault geometry of this earthquake by inverting seismological ...The great Tancheng earthquake of M81/2 occurred in 1668 was the largest seismic event ever recorded in history in eastern China. This study determines the fault geometry of this earthquake by inverting seismological data of present-day moderate-small earthquakes in the focal area. We relocated those earthquakes with the double-difference method and found focal mechanism solutions using gird test method. The inversion results are as follows： the strike is 21.6°, the dip angle is 89.5°, the slip angle is 170°, the fault length is about 160 km, the lower-boundary depth is about 32 km and the buried depth of upper boundary is about 4 km. This shows that the seismic fault is a NNE-trending upright right-lateral strike-slip fault and has cut through the crust. Moreover, the surface seismic fault, intensity distribution of the earthquake, earthquake-depth distribution and seismic-wave velocity profile in the focal area all verified our study result.展开更多
Based on the large field multicolor observations ofBeijing-Arizona-Taiwan-Connecticut (BATC) program, we obtain the spectral energy distribution (SED)for individual regions of M81. We study the structure and evolution...Based on the large field multicolor observations ofBeijing-Arizona-Taiwan-Connecticut (BATC) program, we obtain the spectral energy distribution (SED)for individual regions of M81. We study the structure and evolution of M81 with an evolutionarypopulation synthesis (EPS) model, PEGASE. We find that the exponentially deceasing star formationrate (SFR) with star formation scale 3 Gyr (hereafter Exp, τ = 3 Gyr) gives the best agreementbetween the model predictions and the observed SEDs. We then obtain the structure, age distributionand evolutionary history of M81. There is a clear age gradient between the central and outerregions. The populations in the central regions are older than 7 Gyr, those in the outer regions areyounger, at about 4.5 Gyr. The youngest components in the spiral arms have ages of about 2.5 Gyr orless.展开更多
It was found that advection-dominated accretion flow （ADAF）＋thin disk model calculations can reproduce the observed spectral energy distributions （SEDs） of two low-luminosity active galactic nuclei （AGNs）, prov...It was found that advection-dominated accretion flow （ADAF）＋thin disk model calculations can reproduce the observed spectral energy distributions （SEDs） of two low-luminosity active galactic nuclei （AGNs）, provided they are accreting at -0.01-0.03 Eddington rates and the thin disks are truncated to ADAFs at -100Rs （Rs is the Schwarzschild radius） for M81 and NGC 4579 （Quataert et al. 1999）. However, the black hole masses adopted in their work are about one order of magnitude lower than recent measurements on these two sources. Adopting the well estimated black hole masses, our ADAF＋thin disk model calculations can reproduce the observed SEDs of these two low- luminosity AGNs, if the black hole is accreting at 2.5×10^-4 Eddington rates with the thin disk truncated at Rtr=120Rs for M81（m= 3.3×10^-3 and Rtr=80Rs are required for NGC 4579）. The transition zones with temperature from the thin disk with ,-10^4- 10^5 to ,-10^9-10^10K in the ADAF will inevitably emit thermal X-ray lines, which provides a useful diagnosis of their physical properties. The observed widths of the thermal X-ray iron lines at -6.8 keV are consistent with Doppler broadening by Keplerian motion of the gases in the transition zones at ,-100Rs. We use the structure of the transition zone between the ADAF and the thin disk derived by assuming the turbulent diffusive heat mechanism to calculate their thermal X-ray line emission with the standard software package Astrophysical Plasma Emission Code （APEC）. Comparing them with the equivalent widths of the observed thermal X-ray iron lines in these two sources, we find that the turbulent diffusive heat mechanism seems to be unable to reproduce the observed thermal X-ray line emission. The test of the evaporation model for the accretion mode transition with the observed thermal X-ray line emission is briefly discussed.展开更多
We present metal abundance properties of 144 globular clusters associated with M81. These globulars represent the largest globular cluster sample in M81 till now. Our main results are： the distribution of metalliciti...We present metal abundance properties of 144 globular clusters associated with M81. These globulars represent the largest globular cluster sample in M81 till now. Our main results are： the distribution of metallicities is bimodal, with metallicity peaks at [Fe/H] -1.51 and -0.58, and the metal-poor globular clusters tend to be less spatially concentrated than the metal-rich ones; the metal-rich globular clusters in M81 do not demonstrate a centrally concentrated spatial distribution like the metalrich ones in M31 do; like our Galaxy and M31, the globular clusters in M81 have a small radial metallicity gradient. These results are consistent with those obtained from a small sample of M81 globular clusters. In addition, this paper shows that there is evidence that a strong rotation of the M81 globular cluster system around the minor axis exists, and that rotation is present in the metal-rich globular cluster subsample, but the metal-poor globular cluster subsample shows no evidence of rotation. The most significant difference between the rotation of the metal-rich and metal-poor globular clusters occurs at intermediate projected galactocentric radii. Our results confirm the conclusion of Schroder et al. that M81＇s metal-rich globular clusters at intermediate projected radii are associated with a thick disk of M81.展开更多
基金supported by the National Natural Science Foundation of China(No.90814002)the Natural Science Foundation of Shandong Province(No.Y2005E02)
文摘The great Tancheng earthquake of M81/2 occurred in 1668 was the largest seismic event ever recorded in history in eastern China. This study determines the fault geometry of this earthquake by inverting seismological data of present-day moderate-small earthquakes in the focal area. We relocated those earthquakes with the double-difference method and found focal mechanism solutions using gird test method. The inversion results are as follows： the strike is 21.6°, the dip angle is 89.5°, the slip angle is 170°, the fault length is about 160 km, the lower-boundary depth is about 32 km and the buried depth of upper boundary is about 4 km. This shows that the seismic fault is a NNE-trending upright right-lateral strike-slip fault and has cut through the crust. Moreover, the surface seismic fault, intensity distribution of the earthquake, earthquake-depth distribution and seismic-wave velocity profile in the focal area all verified our study result.
基金Supported by the National Natural Science Foundation of China
文摘Based on the large field multicolor observations ofBeijing-Arizona-Taiwan-Connecticut (BATC) program, we obtain the spectral energy distribution (SED)for individual regions of M81. We study the structure and evolution of M81 with an evolutionarypopulation synthesis (EPS) model, PEGASE. We find that the exponentially deceasing star formationrate (SFR) with star formation scale 3 Gyr (hereafter Exp, τ = 3 Gyr) gives the best agreementbetween the model predictions and the observed SEDs. We then obtain the structure, age distributionand evolutionary history of M81. There is a clear age gradient between the central and outerregions. The populations in the central regions are older than 7 Gyr, those in the outer regions areyounger, at about 4.5 Gyr. The youngest components in the spiral arms have ages of about 2.5 Gyr orless.
基金Supported by the National Natural Science Foundation of China
文摘It was found that advection-dominated accretion flow （ADAF）＋thin disk model calculations can reproduce the observed spectral energy distributions （SEDs） of two low-luminosity active galactic nuclei （AGNs）, provided they are accreting at -0.01-0.03 Eddington rates and the thin disks are truncated to ADAFs at -100Rs （Rs is the Schwarzschild radius） for M81 and NGC 4579 （Quataert et al. 1999）. However, the black hole masses adopted in their work are about one order of magnitude lower than recent measurements on these two sources. Adopting the well estimated black hole masses, our ADAF＋thin disk model calculations can reproduce the observed SEDs of these two low- luminosity AGNs, if the black hole is accreting at 2.5×10^-4 Eddington rates with the thin disk truncated at Rtr=120Rs for M81（m= 3.3×10^-3 and Rtr=80Rs are required for NGC 4579）. The transition zones with temperature from the thin disk with ,-10^4- 10^5 to ,-10^9-10^10K in the ADAF will inevitably emit thermal X-ray lines, which provides a useful diagnosis of their physical properties. The observed widths of the thermal X-ray iron lines at -6.8 keV are consistent with Doppler broadening by Keplerian motion of the gases in the transition zones at ,-100Rs. We use the structure of the transition zone between the ADAF and the thin disk derived by assuming the turbulent diffusive heat mechanism to calculate their thermal X-ray line emission with the standard software package Astrophysical Plasma Emission Code （APEC）. Comparing them with the equivalent widths of the observed thermal X-ray iron lines in these two sources, we find that the turbulent diffusive heat mechanism seems to be unable to reproduce the observed thermal X-ray line emission. The test of the evaporation model for the accretion mode transition with the observed thermal X-ray line emission is briefly discussed.
基金supported by the National Natural Science Foundation of China (Grant Nos. 10873016, 10633020, 10803007,11003021, 11173016 and 11073032)the National Basic Research Program of China (973 Program, 2007CB815403)
文摘We present metal abundance properties of 144 globular clusters associated with M81. These globulars represent the largest globular cluster sample in M81 till now. Our main results are： the distribution of metallicities is bimodal, with metallicity peaks at [Fe/H] -1.51 and -0.58, and the metal-poor globular clusters tend to be less spatially concentrated than the metal-rich ones; the metal-rich globular clusters in M81 do not demonstrate a centrally concentrated spatial distribution like the metalrich ones in M31 do; like our Galaxy and M31, the globular clusters in M81 have a small radial metallicity gradient. These results are consistent with those obtained from a small sample of M81 globular clusters. In addition, this paper shows that there is evidence that a strong rotation of the M81 globular cluster system around the minor axis exists, and that rotation is present in the metal-rich globular cluster subsample, but the metal-poor globular cluster subsample shows no evidence of rotation. The most significant difference between the rotation of the metal-rich and metal-poor globular clusters occurs at intermediate projected galactocentric radii. Our results confirm the conclusion of Schroder et al. that M81＇s metal-rich globular clusters at intermediate projected radii are associated with a thick disk of M81.
