Background:Upper respiratory infections(URIs)are common infectious diseases worldwide.Accurate and timely assessment of the disease burden of URIs is crucial for governments to develop comprehensive prevention and con...Background:Upper respiratory infections(URIs)are common infectious diseases worldwide.Accurate and timely assessment of the disease burden of URIs is crucial for governments to develop comprehensive prevention and control strategies,and to allocate and utilize healthcare resources more efficiently.Methods:For URIs in Global Burden of Disease(GBD)2021 database,age-standardized incidence rates(ASIR),age-standardized prevalence rates(ASPR),age-standardized mortality rates(ASMR),disability-adjusted life-years(DALYs),and case numbers for incidence,prevalence,deaths,and DALYs across the globe,five socio-demographic index(SDI)regions,21 geographical regions,and 204 countries and territories were provided and analyzed.Trends from 1990 to 2021 were described using the average annual percentage change(AAPC),and future URIs burden was projected with a Bayesian age-period-cohort(BAPC)model.Results:From 1990 to 2021,there was a significant decline in global ASIR(APCC=-289.86,95%confidence interval[CI]:-298.59 to-281.12),ASPR(AAPC=-4.04,95%CI:-4.16 to-3.92),ASMR(AAPC=-0.02,95%CI:-0.02 to-0.03)and age-standardized DALY rate(AAPC=-0.75,95%CI:-0.76 to-0.74).The ASIR,ASPR,ASMR,and age-standardized DALY rate were high in elderly for both males and females,and both genders.Similarly,the number of incident cases,prevalence cases,deaths,and DALY cases for URIs was highest in children under five years.The ASMR and age-standardized DALY rate exhibited a negative correlation with SDI across 204 countries and territories in 2021.The ASIR and ASPR for URIs will show an upward trend from 2022 to 2050,while ASMR and age-standardized DALY rate are expected to decline.Low birth weight for gestation remains the leading contributor to deaths related to URIs.展开更多
The tropical Asian and Australasian floras have a close relationship,and is a vital distribution pattern of seed plants worldwide.As estimated,more than 81 families and 225 genera of seed plants distributed between tr...The tropical Asian and Australasian floras have a close relationship,and is a vital distribution pattern of seed plants worldwide.As estimated,more than 81 families and 225 genera of seed plants distributed between tropical Asia and Australasia.However,the evolutionary dynamics of two floras were still vague.Here,a total of 29 plant lineages,represented the main clades of seed plants and different habits,were selected to investigate the biotic interchange between tropical Asia and Australasia by integrated dated phylogenies,biogeography,and ancestral state reconstructions.Our statistics indicated that 68 migrations have occurred between tropical Asia and Australasia since the middle Eocene except terminal migrations,and the migration events from tropical Asia to Australasia is more than 2 times of the reverse.Only 12 migrations occurred before 15 Ma,whereas the remaining56 migrations occurred after 15 Ma.Maximal number of potential dispersal events(MDE) analysis also shows obvious asymmetry,with southward migration as the main feature,and indicates the climax of bi-directional migrations occurred after 15 Ma.We speculate that the formation of island chains after the Australian-Sundaland collision and climate changes have driven seed plant migrations since the middle Miocene.Furthermore,biotic dispersal and stable habitat may be crucial for floristic interchange between tropical Asia and Australasia.展开更多
The discovery of a planetary companion to the intermediate-mass late-type giant star HD173416 from precise Doppler surveys of G and K giants at Xinglong station and Okayama Astrophysical Observatory （OAO） is present...The discovery of a planetary companion to the intermediate-mass late-type giant star HD173416 from precise Doppler surveys of G and K giants at Xinglong station and Okayama Astrophysical Observatory （OAO） is presented in this letter. The planet has a minimum mass of 2.7 MJ, an eccentricity of 0.21, a semimajor axis of 1.16 AU and an orbital period of 324 days.展开更多
We aim at deriving accurate atmospheric parameters and chemical abundances of 19 barium（Ba） stars, including both strong and mild Ba stars, based on the high signal-to-noise ratio and high resolution Echelle spectra...We aim at deriving accurate atmospheric parameters and chemical abundances of 19 barium（Ba） stars, including both strong and mild Ba stars, based on the high signal-to-noise ratio and high resolution Echelle spectra obtained from the 2.16 m telescope at Xinglong station of National Astronomical Observatories, Chinese Academy of Sciences. The chemical abundances of the sample stars were obtained from an LTE, plane-parallel and line-blanketed atmospheric model by inputting the atmospheric parameters（effective temperatures Teff, surface gravities log g, metallicity [Fe/H] and microturbulence velocity ξt） and equivalent widths of stellar absorption lines. These samples of Ba stars are giants as indicated by atmospheric parameters, metallicities and kinematic analysis about UVW velocity. Chemical abundances of 17 elements were obtained for these Ba stars. Their Na, Al, α- and iron-peak elements（O, Na, Mg, Al, Si, Ca,Sc, Ti, V, Cr, Mn, Ni） are similar to the solar abundances. Our samples of Ba stars show obvious overabundances of neutron-capture（n-capture） process elements relative to the Sun. Their median abundances of[Ba/Fe], [La/Fe] and [Eu/Fe] are 0.54, 0.65 and 0.40, respectively. The Y I and Zr I abundances are lower than Ba, La and Eu, but higher than the α- and iron-peak elements for the strong Ba stars and similar to the iron-peak elements for the mild stars. There exists a positive correlation between Ba intensity and [Ba/Fe].For the n-capture elements（Y, Zr, Ba, La）, there is an anti-correlation between their [X/Fe] and [Fe/H]. We identify nine of our sample stars as strong Ba stars with [Ba/Fe]〉0.6 where seven of them have Ba intensity Ba=2-5, one has Ba=1.5 and another one has Ba=1.0. The remaining ten stars are classified as mild Ba stars with 0.17〈[Ba/Fe]〈0.54.展开更多
We present a study of the spectral line shape associated with a High Resolution Spectrograph on the 2.16 m telescope at the Xinglong Observing Station of National Astronomical Observatories, Chinese Academy of Science...We present a study of the spectral line shape associated with a High Resolution Spectrograph on the 2.16 m telescope at the Xinglong Observing Station of National Astronomical Observatories, Chinese Academy of Sciences. This measurement is based on modeling the instrumental line shape obtained by unresolved modes from a Yb-fiber mode-locked laser frequency comb. With the current repetition rate of 250 MHz and 26 GHz mode spacing on the spectrograph, we find the absolute variation of the line center, 0.0597 pixel in the direction of the CCDs, and 0.00275 pixel （～3 m s^-1） for relative variation in successive exposures on a short timescale. A novel double-Gaussian model is presented to improve the quality of the fit by a factor of 2.47 in a typical single exposure. We also use analysis with raw moments and central moments to characterize the change in line shape across the detector. A trend in charge transfer efficiency can be found on the E2V 4096 ×4096 CCD that provides a correction for wavelength calibration aiming to reach a level of precision for radial velocity below 1 m s^- 1.展开更多
Being one of the most fundamental physical parameter of astronomical objects,mass plays a vital role in the study of exoplanets,including their temperature structure,chemical composition,formation,and evolution.Howeve...Being one of the most fundamental physical parameter of astronomical objects,mass plays a vital role in the study of exoplanets,including their temperature structure,chemical composition,formation,and evolution.However,nearly a quarter of the known confirmed exoplanets lack measurements of their masses.This is particularly severe for those discovered via the radial velocity(RV)technique,which alone could only yield the minimum mass of planets.In this study,we use published RV data combined with astrometric data from a cross-calibrated Hipparcos-Gaia Catalog of Accelerations to jointly constrain the masses of 115 RV-detected substellar companions,by conducting full orbital fits using the public tool orvara.Among them,9 exoplanets with M_(p)sini<13.5M_(Jup)are reclassified to the brown dwarf(BD)regime,and 16 BD candidates(13.5≤Mp sini<80M_(Jup))turn out to be low-mass M dwarfs.We point out the presence of a transition in the BD regime as seen in the distributions of host star metallicity and orbital eccentricity with respect to planet masses.We confirm the previous findings that companions with masses below 42.5 M_(Jup)might primarily form in the protoplanetary disk through core accretion or disk gravitational instability,while those with masses above 42.5 M_(Jup)formed through the gravitational instability of a molecular cloud like stars.Selection effects and detection biases,which may affect our analysis to some extent,are discussed.展开更多
We report the discovery of a substellar companion around the intermediate- mass giant HD 175679. Precise radial velocity data of the star from the Xinglong Station and the Okayama Astrophysical Observatory revealed a ...We report the discovery of a substellar companion around the intermediate- mass giant HD 175679. Precise radial velocity data of the star from the Xinglong Station and the Okayama Astrophysical Observatory revealed a Keplerian velocity variation with an orbital period of 1366.8±5.7 d, a semiamplitude of 380.2±3.2 m s-1 and an eccentricity of 0.378± 0.008. Adopting a stellar mass of 2.7± 0.3 M, we obtain that the minimum mass of the HD 175679 b is 37.3± 2.8 M and the semimajor axis is 3.36±0.12 AU. This discovery is the second brown dwarf companion candidate from a joint planet-search program between China and Japan.展开更多
基金supported by the fund of Shanghai Natural Science Foundation(grant number 23ZR1464000)the Talent Fund of Longhua Hospital affiliated to Shanghai University of Traditional Chinese Medicine(grant number LH001.007).
文摘Background:Upper respiratory infections(URIs)are common infectious diseases worldwide.Accurate and timely assessment of the disease burden of URIs is crucial for governments to develop comprehensive prevention and control strategies,and to allocate and utilize healthcare resources more efficiently.Methods:For URIs in Global Burden of Disease(GBD)2021 database,age-standardized incidence rates(ASIR),age-standardized prevalence rates(ASPR),age-standardized mortality rates(ASMR),disability-adjusted life-years(DALYs),and case numbers for incidence,prevalence,deaths,and DALYs across the globe,five socio-demographic index(SDI)regions,21 geographical regions,and 204 countries and territories were provided and analyzed.Trends from 1990 to 2021 were described using the average annual percentage change(AAPC),and future URIs burden was projected with a Bayesian age-period-cohort(BAPC)model.Results:From 1990 to 2021,there was a significant decline in global ASIR(APCC=-289.86,95%confidence interval[CI]:-298.59 to-281.12),ASPR(AAPC=-4.04,95%CI:-4.16 to-3.92),ASMR(AAPC=-0.02,95%CI:-0.02 to-0.03)and age-standardized DALY rate(AAPC=-0.75,95%CI:-0.76 to-0.74).The ASIR,ASPR,ASMR,and age-standardized DALY rate were high in elderly for both males and females,and both genders.Similarly,the number of incident cases,prevalence cases,deaths,and DALY cases for URIs was highest in children under five years.The ASMR and age-standardized DALY rate exhibited a negative correlation with SDI across 204 countries and territories in 2021.The ASIR and ASPR for URIs will show an upward trend from 2022 to 2050,while ASMR and age-standardized DALY rate are expected to decline.Low birth weight for gestation remains the leading contributor to deaths related to URIs.
基金supported by the National Natural Science Foundation of China (31670212,3206005631300181)+1 种基金the National Natural Science Foundation of China-Yunnan Joint Fund Project (U1802242)Guangxi Key Laboratory Construction Project (19-185-7)。
文摘The tropical Asian and Australasian floras have a close relationship,and is a vital distribution pattern of seed plants worldwide.As estimated,more than 81 families and 225 genera of seed plants distributed between tropical Asia and Australasia.However,the evolutionary dynamics of two floras were still vague.Here,a total of 29 plant lineages,represented the main clades of seed plants and different habits,were selected to investigate the biotic interchange between tropical Asia and Australasia by integrated dated phylogenies,biogeography,and ancestral state reconstructions.Our statistics indicated that 68 migrations have occurred between tropical Asia and Australasia since the middle Eocene except terminal migrations,and the migration events from tropical Asia to Australasia is more than 2 times of the reverse.Only 12 migrations occurred before 15 Ma,whereas the remaining56 migrations occurred after 15 Ma.Maximal number of potential dispersal events(MDE) analysis also shows obvious asymmetry,with southward migration as the main feature,and indicates the climax of bi-directional migrations occurred after 15 Ma.We speculate that the formation of island chains after the Australian-Sundaland collision and climate changes have driven seed plant migrations since the middle Miocene.Furthermore,biotic dispersal and stable habitat may be crucial for floristic interchange between tropical Asia and Australasia.
基金funded by the NSFC under grants 10803010 and 10521001Grants-in-Aid for Scientific Research (B) No.17340056 (H.A.)the Joint program on Search for Extra-solar planets between China and Japan (2008–2010) from the Japan Society for the Promotion of Science.
文摘The discovery of a planetary companion to the intermediate-mass late-type giant star HD173416 from precise Doppler surveys of G and K giants at Xinglong station and Okayama Astrophysical Observatory （OAO） is presented in this letter. The planet has a minimum mass of 2.7 MJ, an eccentricity of 0.21, a semimajor axis of 1.16 AU and an orbital period of 324 days.
基金supported by the National Natural Science Foundation of China (NSFC) under grant Nos.11273011,U1231119,10973006,11003002,11273026,10933001 and 10973015the National Basic Research Program of China (973 Program,Grant Nos.2007CB815404,2007CB815403 and 2007CB815406)
文摘We aim at deriving accurate atmospheric parameters and chemical abundances of 19 barium（Ba） stars, including both strong and mild Ba stars, based on the high signal-to-noise ratio and high resolution Echelle spectra obtained from the 2.16 m telescope at Xinglong station of National Astronomical Observatories, Chinese Academy of Sciences. The chemical abundances of the sample stars were obtained from an LTE, plane-parallel and line-blanketed atmospheric model by inputting the atmospheric parameters（effective temperatures Teff, surface gravities log g, metallicity [Fe/H] and microturbulence velocity ξt） and equivalent widths of stellar absorption lines. These samples of Ba stars are giants as indicated by atmospheric parameters, metallicities and kinematic analysis about UVW velocity. Chemical abundances of 17 elements were obtained for these Ba stars. Their Na, Al, α- and iron-peak elements（O, Na, Mg, Al, Si, Ca,Sc, Ti, V, Cr, Mn, Ni） are similar to the solar abundances. Our samples of Ba stars show obvious overabundances of neutron-capture（n-capture） process elements relative to the Sun. Their median abundances of[Ba/Fe], [La/Fe] and [Eu/Fe] are 0.54, 0.65 and 0.40, respectively. The Y I and Zr I abundances are lower than Ba, La and Eu, but higher than the α- and iron-peak elements for the strong Ba stars and similar to the iron-peak elements for the mild stars. There exists a positive correlation between Ba intensity and [Ba/Fe].For the n-capture elements（Y, Zr, Ba, La）, there is an anti-correlation between their [X/Fe] and [Fe/H]. We identify nine of our sample stars as strong Ba stars with [Ba/Fe]〉0.6 where seven of them have Ba intensity Ba=2-5, one has Ba=1.5 and another one has Ba=1.0. The remaining ten stars are classified as mild Ba stars with 0.17〈[Ba/Fe]〈0.54.
基金supported by the National Natural Science Foundation of China (Grant Nos. 11233004 and 11390371)supported by the Specialized Research Fund for Shandong Provincial Key Laboratory
文摘We present a study of the spectral line shape associated with a High Resolution Spectrograph on the 2.16 m telescope at the Xinglong Observing Station of National Astronomical Observatories, Chinese Academy of Sciences. This measurement is based on modeling the instrumental line shape obtained by unresolved modes from a Yb-fiber mode-locked laser frequency comb. With the current repetition rate of 250 MHz and 26 GHz mode spacing on the spectrograph, we find the absolute variation of the line center, 0.0597 pixel in the direction of the CCDs, and 0.00275 pixel （～3 m s^-1） for relative variation in successive exposures on a short timescale. A novel double-Gaussian model is presented to improve the quality of the fit by a factor of 2.47 in a typical single exposure. We also use analysis with raw moments and central moments to characterize the change in line shape across the detector. A trend in charge transfer efficiency can be found on the E2V 4096 ×4096 CCD that provides a correction for wavelength calibration aiming to reach a level of precision for radial velocity below 1 m s^- 1.
基金supported by the National Key R&D Program of China Nos.2019YFA0405102 and 2019YFA0405502supported by the National Natural Science Foundation of China(NSFC,Grant Nos.12073044 and 11988101)。
文摘Being one of the most fundamental physical parameter of astronomical objects,mass plays a vital role in the study of exoplanets,including their temperature structure,chemical composition,formation,and evolution.However,nearly a quarter of the known confirmed exoplanets lack measurements of their masses.This is particularly severe for those discovered via the radial velocity(RV)technique,which alone could only yield the minimum mass of planets.In this study,we use published RV data combined with astrometric data from a cross-calibrated Hipparcos-Gaia Catalog of Accelerations to jointly constrain the masses of 115 RV-detected substellar companions,by conducting full orbital fits using the public tool orvara.Among them,9 exoplanets with M_(p)sini<13.5M_(Jup)are reclassified to the brown dwarf(BD)regime,and 16 BD candidates(13.5≤Mp sini<80M_(Jup))turn out to be low-mass M dwarfs.We point out the presence of a transition in the BD regime as seen in the distributions of host star metallicity and orbital eccentricity with respect to planet masses.We confirm the previous findings that companions with masses below 42.5 M_(Jup)might primarily form in the protoplanetary disk through core accretion or disk gravitational instability,while those with masses above 42.5 M_(Jup)formed through the gravitational instability of a molecular cloud like stars.Selection effects and detection biases,which may affect our analysis to some extent,are discussed.
基金the National Natural Science Foundation of China (Grant Nos. 10821061 and 10803010)the Japan Society for the Promotion of Science under grant 08032011-000184 in the framework of the Joint Research Project between China and Japan
文摘We report the discovery of a substellar companion around the intermediate- mass giant HD 175679. Precise radial velocity data of the star from the Xinglong Station and the Okayama Astrophysical Observatory revealed a Keplerian velocity variation with an orbital period of 1366.8±5.7 d, a semiamplitude of 380.2±3.2 m s-1 and an eccentricity of 0.378± 0.008. Adopting a stellar mass of 2.7± 0.3 M, we obtain that the minimum mass of the HD 175679 b is 37.3± 2.8 M and the semimajor axis is 3.36±0.12 AU. This discovery is the second brown dwarf companion candidate from a joint planet-search program between China and Japan.
