Six tektites from Guilin of Guangxi, Hainan, and Guangdong were analyzed for the abundances of major elements and 27 trace elements. All samples are splash-form tektites and have SiO2 contents ranging from 73.1wt% to 76.0wt% (74.6wt% on average). The chemical compositions, except Cr and Ni, of tektites from different areas, are similar. Guangdong tektite shows enrichments of Ni and Cr contents by a factor of 3, and has slightly higher MgO and FeO than Hainan and Guilin tektites. It indicates that the tektites were formed by mixing several target rocks. The major and trace element concentrations of southern China tektites closely resemble previously reported data for average splash-form and Muong Nong-type indochinites, indicating that they have the same source. (La/Lu)CI (7.99), Zr/Hf (35.45 on average), Ba/Rb (3.59 on average), and the rare earth element (REE) contents of tektites are similar to those of typical post Archean upper crustal rocks. This study suggests that the best fit for the target source of southern China tektites could be a combination of 41% shale, 2% sandstone, 20% greywacke, and 37% quartzite.
In the fireball model, it is more physically realistic that ganuna-ray burst （GRB） ejecta have a range of bulk Lorentz factors （assuming M ∝ Г^-8）. The low Lorentz factor part of the ejecta will catch up with the high Lorentz factor part when the latter is decelerated by the surrounding medium to a comparable Lorentz factor. Such a process will develop a long-lasting weak reverse shock until the whole ejecta are shocked. Meanwhile, the forward shocked materials are gradually supplied with energy from the ejecta that are catching-up, and thus the temporal decay of the forward shock emission will be slower than that without an energy supply. However, the reverse shock may be strong. Here, we extend the standard reverse-forward shock model to the case of radially nonuniform ejecta. We show that this process can be classified into two cases： the thick shell case and the thin shell case. In the thin shell case, the reverse shock is weak and the temporal scaling law of the afterglow is the same as that in Sad ＆ Meszaros （2000）. However, in the thick shell case, the reverse shock is strong and thus its emission dominates the afterglow in the high energy band. Our results also show slower decaying behavior of the afterglow due to the energy supply by low Lorentz factor materials, which may help the understanding of the plateau observed in the early optical and X-ray afterglows.
We present our 12CO and 13CO mapping observations of SNR IC 443 interacting with molecular clouds.It is the first largescale high-resolution 13CO mapping observation in the surrounding region.The morphologies of IC 443 in 12CO and 13 CO are compared with the optical,infrared,Spitzer far-infrared,X-ray,and neutral atomic gas(HI).We also make comparison and analysis in the kinematics,using the date-cubes of 12CO,13CO and HI,to help distinguish the complicated gas motions in the shocked regions.Based on the work of Wang & Scoville(1992),we present a new model to explain the coexistence of multiple shocks with different speeds in a pc-scale region at the central clump B.We test this new model by analyzing the HI and CO distribution in both velocity and space domain.We also establish the relationship between the dissociation rate of shocked molecular gas and the shock velocity in this region.Finally,we derive the optical depth of 12CO with the 13CO spectra in clump B,and discuss the validity of the assumption of optically thin emission for the shocked 12CO.
Combining the 12CO(1-0),13CO(1-0),and C18O(1-0) data with IRAS four band data,we here estimate the physical parameters such as size,viral mass,and CO J=1-0 isotopic and infrared luminosities for 29 dense molecular clouds from two published CO samples. We further analyze the various correlations between CO J=1-0 isotopic luminosities and infrared luminosity(star formation rate,SFR) and discuss the relationships between the molecular gas tracers and SFR. The results show that 12CO(1-0),13CO(1-0) and C18O(1-0) luminosities have tight correlations with each other. CO J=1-0 isotopic luminosities and SFR show weak correlations with larger scatter than the HCN-IR correlations of 47 dense cores in the Galaxy and 65 external star-forming galaxies. This might be interpreted as that both the SFR and star formation efficiency are mainly determined by the molecular gas at high volume density rather than high column density.
SUN Yan & GAO Yu Purple Mountain Observatory,Chinese Academy of Sciences,Nanjing 210008,China
GRB 080913,with a spectroscopically determined redshift of z=6.7,was the record holder for being the most remote stellar object before the discovery of the recent gamma-ray burst GRB 090423,whose redshift is about 8.2.The gradually accumulated high redshift GRB sample has shed light on the origin and physical properties of GRBs during the cosmic re-ionization epoch.Here,we present a detailed numerical fit to the multi-wavelength data of the optical afterglow of GRB 080913 and then constrain its circumburst environment and the other model parameters.We conclude that the late optical/X-ray plateau at about one day since the burst is due to the Poynting-flux dominated injection from the central engine which is very likely a massive spinning black hole with super strong magnetic fields.
LIU XueWen,WU XueFeng & LU Tan Purple Mountain Observatory,Chinese Academy of Sciences,Nanjing 210008,China
We report results of petrologic and mineralogical studies of 25 unequili- brated ordinary chondrites （19 Chinese Antarctic meteorites） using electron microprobe, scanning electron microscopy （SEM） and energy-dispersive X-ray spectrometry （EDS） techniques. With increasing degree of thermal metamorphism, chemical zoning of olivine was erased; plessite was transformed into intergrowths of coarsergrained kamacite and Ni-rich metal; Cr exsolved from ferroan olivine, produced needie-like crystals and coarsened into equant chromite grains; and feldspar crystallized during devitrification of glass and recrystallization of matrix. These features can help to identify different metamorphic grades. Based on the scheme by Sears et al （1982）, we subdivided type 3 Chinese Antarctic ordinary chondrites into petrologic type 3.3 to 4 （3 type 3.3, 3 type 3.4, 1 type 3.5, 2 type 3.6, 2 type 3.7, 5 type 3.8, 3 type 4 ）. This classification scheme is a quite effective way to subdivide Antarctic meteorites. Additionally, we propose to revise the chemical groups of GRV 020032 and GRV 020104 to L and H, respectively.
We study the global star formation law,the relation between the gas and star formation rate (SFR) in a sample of 130 local galaxies with infrared (IR) luminosities spanning over three orders of magnitude (10 9-10 12 L),which includes 91 normal spiral galaxies and 39 (ultra)luminous IR galaxies [(U)LIRGs].We derive their total (atomic and molecular) gas and dense molecular gas masses using newly available HI,CO and HCN data from the literature.The SFR of galaxies is determined from total IR (8-1000 m) and 1.4 GHz radio continuum (RC) luminosities.The galaxy disk sizes are defined by the de-convolved elliptical Gaussian FWHM of the RC maps.We derive the galaxy disk-averaged SFRs and various gas surface densities,and investigate their relationships.We find that the galaxy disk-averaged surface density of dense molecular gas mass has the tightest correlation with that of SFR (scatter ～0.26 dex),and is linear in log-log space (power-law slope of N=1.03±0.02) across the full galaxy sample.The correlation between the total gas and SFR surface densities for the full sample has a somewhat larger scatter (～0.48 dex),and is best fit by a power-law with slope 1.45±0.02.However,the slope changes from ～1 when only normal spirals are considered,to ～1.5 when more and more (U)LIRGs are included in the fitting.When different CO-to-H 2 conversion factors are used to infer molecular gas masses for normal galaxies and (U)LIRGs,the bi-modal relations claimed recently in CO observations of high-redshift galaxies appear to also exist in local populations of star-forming galaxies.
We present results of 13CO（1-0）,C18O（1-0）,and HCO＋（1-0） map observations and N2H＋（1-0） single point observations directed towards a sample of nine low-luminosity 6.7-GHz masers.N2H ＋ line emission has been detected from six out of nine sources,C18O line emission has been detected from eight out of nine sources,and HCO ＋ and 13CO emission has been detected in all sources.In particular,a ＂blue profile＂ of the HCO ＋ spectrum,a signature of inflow,is found towards one source.From integrated intensity emission maps,we identified 17 cores in the sample.Among them,nine cores are closely associated with low-luminosity methanol masers.For these cores,we derive the column densities,core sizes,masses and molecular abundances.Comparison of our results with similar molecular line surveys towards the southern sky methanol masers indicates that linewidths of our sample,including only the low-luminosity masers,are smaller than the sample that includes both lowand high-luminosity masers.For the maser associated cores,their gas masses have the same order of magnitude as their virial masses,indicating that these cores are gravitationally bound systems.In addition,we have found from our observations that the low-luminosity methanol masers tend to coexist with H2O masers and outflows rather than with OH masers.
Yuan-Wei Wu,Ye Xu and Ji Yang Purple Mountain Observatory,Chinese Academy of Sciences,Nanjing 210008,China
