Infrared bubbles provide a unique opportunity to study the interactions between massive stars and surrounding material.We conduct a multi-wavelength study on the environment and star formation around an infrared bubbl...Infrared bubbles provide a unique opportunity to study the interactions between massive stars and surrounding material.We conduct a multi-wavelength study on the environment and star formation around an infrared bubble N13.Three dust clumps and two molecular clumps are identified around N 13,which are all distributed on the layer.Young stellar objects(YSOs)are carefully searched using infrared colors and YSO candidates of WISE and Gaia DR2,and three Class I/II YSOs are found in N 13.In addition,four O-type stars identified in N 13 are probably the exciting stars.The dynamical and fragmentation ages of N 13 are 0.32-0.35 and 1.37-2.80 Myr respectively,which suggest that the radiation-driven implosion model may be dominant in N 13.By comparing the small-size bubble N 13(R~1.9 pc)and the larger-size bubble G15.684-0.29(R~15.7 pc)we found that star formation activity is more active in the large-size bubble.Brief comparisons of ten bubbles show that small-size bubbles have a small ratio of kinetic age versus the fragmentation time.Triggering star formation may be more active in bubbles with larger ratio between kinetic and fragmentation ages.Furthermore,the collect and collapse mechanism may play the dominant role in the large-size ones.展开更多
Double main phase process is applied to fabricate [(Pr, Nd)1 – xMMx]13.8FebalM1.5B5.9 (x = 0.5 and 0.7;M = Cu, Al, Co, and Nb) sintered magnets with high misch metal (MM) content. In comparison to the magnets by sing...Double main phase process is applied to fabricate [(Pr, Nd)1 – xMMx]13.8FebalM1.5B5.9 (x = 0.5 and 0.7;M = Cu, Al, Co, and Nb) sintered magnets with high misch metal (MM) content. In comparison to the magnets by single main phase process, the enhanced magnetic properties have been achieved. For magnets of x = 0.7, Hcj increases to 371.9 kA/m by 60.5%, and (BH)max is significantly enhanced to 253.3 kJ/m3 by 56.9%, compared with those of the single main phase magnets of the same nominal composition. In combination with minor loops and magnetic recoil curves, the property improvement of magnets with double main phase method is well explained. As a result, it is demonstrated that double main phase technology is an effective approach to improve the permanent magnetic properties of MM based sintered magnets.展开更多
The interface state of hydrogen-terminated(C-H)diamond metal-oxide-semiconductor field-effect transistor(MOSFET)is critical for device performance.In this paper,we investigate the fixed charges and interface trap stat...The interface state of hydrogen-terminated(C-H)diamond metal-oxide-semiconductor field-effect transistor(MOSFET)is critical for device performance.In this paper,we investigate the fixed charges and interface trap states in C-H diamond MOSFETs by using different gate dielectric processes.The devices use Al_(2)O_(3) as gate dielectrics that are deposited via atomic layer deposition(ALD)at 80℃and 300℃,respectively,and their C-V and I-V characteristics are comparatively investigated.Mott-Schottky plots(1/C2-VG)suggest that positive and negative fixed charges with low density of about 10^(11)cm^(-2) are located in the 80-℃-and 300-℃deposition Al2O3 films,respectively.The analyses of direct current(DC)/pulsed I-V and frequency-dependent conductance show that the shallow interface traps(0.46 eV-0.52 eV and 0.53 eV-0.56 eV above the valence band of diamond for the 80-℃and 300-℃deposition conditions,respectively)with distinct density(7.8×10^(13)eV^(-1)·cm^(-2)-8.5×10^(13)eV^(-1)·cm^(-2) and 2.2×10^(13)eV^(-1)·cm^(-2)-5.1×10^(13)eV^(-1)·cm^(-2) for the 80-℃-and 300-℃-deposition conditions,respectively)are present at the Al2O3/C-H diamond interface.Dynamic pulsed I-V and capacitance dispersion results indicate that the ALD Al_(2)O_(3) technique with 300-℃deposition temperature has higher stability for C-H diamond MOSFETs.展开更多
Young protoclusters （embedded stellar clusters） are responsible for the vast majority of star formation currently occurring in the Galaxy. Recent observations suggest a scenario in which filamen-tary structures in t...Young protoclusters （embedded stellar clusters） are responsible for the vast majority of star formation currently occurring in the Galaxy. Recent observations suggest a scenario in which filamen-tary structures in the interstellar medium represent the first step towards precluster clumps and even- tually star formation. Whether filaments continuously fuel the star formation process when the cluster accretes material is still an open question. In this paper, we present a case study of the famous ＇integral shaped filament＇ （ISF） in the Orion A molecular cloud and we seek to study the kinematics which is truly originated from the ISF. We firstly define the central ridge of the ISF with NHa, ^12CO, ^13CO and N2H^＋. Undulations are present in all the ridges. Moreover, a large scale offset is apparent in the ridges as derived by different tracers, which may be explained by the slingshot mechanism proposed by Stutz ＆ Gould. We fit the velocity field of the ISF and find the derived velocity gradient is about 0.7 km s^- 1 pc^- 1 which may come from an overall contraction. We propose a method to check the accretion flow along the ISF by using the velocity deviations of different molecular tracers, which is better than the common method of using the velocity distribution of one tracer alone. Using the velocity deviations, we also find that OMC-1 to 5 are located close to the local extrema of the fluctuations, which may demonstrate that gas flows toward each clump along the ISE展开更多
Here we present the study on chemical properties of massive star forming clumps using N2H^+(1-0),H^13CO+(1-0),HCN(1-0)and HN^13C(1-0)data from the literature[Astron.Astrophys.563,A97(2014)].We found that abundances of...Here we present the study on chemical properties of massive star forming clumps using N2H^+(1-0),H^13CO+(1-0),HCN(1-0)and HN^13C(1-0)data from the literature[Astron.Astrophys.563,A97(2014)].We found that abundances of H^13CO+ and HN^13C are a ected by H2 column densities.As the median values of these two abundances increase by nearly 10 times from stages A to B,H^13CO+and HN^13C are suitable for tracing the evolution of massive star forming clumps.The order of rapidity in growth of abundances of all the four studied molecules from stages A to B,is H^13CO^+,HCN,HN^13C,and N2H^+,from the highest to the lowest.Our results suggest that the observing optically thin molecular lines with high angular resolution are necessary to study the chemical evolution of massive star forming clumps.展开更多
We present large scale observations of C^18O （1-0） towards four massive star forming regions： MON R2, S156, DR17/L906 and M17/M18. The transitions of H2CO （110-111）, C^18O （1-0） and the 6cm continuum are compa...We present large scale observations of C^18O （1-0） towards four massive star forming regions： MON R2, S156, DR17/L906 and M17/M18. The transitions of H2CO （110-111）, C^18O （1-0） and the 6cm continuum are compared in these four regions. Our analysis of the observations and the results of the Non-LTE model shows that the brightness temperature of the formaldehyde absorption line is strongest in a background continuum temperature range of about 3 - 8 K. The excitation of the H2CO absorption line is affected by strong background continuum emission. From a comparison of H2CO and C^18O maps, we found that the extent of H2CO absorption is broader than that of C^18O emission in the four regions. Except for the DR17 region, the maximum in H2CO absorption is located at the same position as the C^18O peak. A good correlation between intensities and widths of H2CO absorption and C^18O emission lines indicates that the H2CO absorption line can trace the dense, warm regions of a molecular cloud. We find that N（H2CO） is well correlated with N（ C^18O） in the four regions and that the average ratio of column densities is （N（H2CO）/N（ClSO）） ～0.03.展开更多
We investigate the influence of fin architecture on linearity characteristics of AlGaN/GaNFinFET.It is found that the Fin FET with scaled fin dimensions exhibits much flatter Gm characteristics than the one with long ...We investigate the influence of fin architecture on linearity characteristics of AlGaN/GaNFinFET.It is found that the Fin FET with scaled fin dimensions exhibits much flatter Gm characteristics than the one with long fins as well as planar HEMT.According to the comparative study,we provide direct proof that source resistance rather than tri-gate structure itself dominates the Gm behavior.Furthermore,power measurements show that the optimized FinFET is capable of delivering a much higher output power density along with significant improvement in linearity characteristics than conventional planar HEMT.This study also highlights the importance of fin design in GaN-based FinFET for microwave power application,especially high-linearity applications.展开更多
We made the first CO（1-0） mapping to SNR G21.8-0.6 and SNR G32.8-0.1, both associated with OH 1720MHz maser. Based on the morphological correspondence and velocity and position agreement between the radio remnant an...We made the first CO（1-0） mapping to SNR G21.8-0.6 and SNR G32.8-0.1, both associated with OH 1720MHz maser. Based on the morphological correspondence and velocity and position agreement between the radio remnant and the CO clouds, we tentatively identify the clouds that are respectively interacting with the two SNRs.展开更多
We performed an H20 maser survey towards 274 Bolocam Galactic Plane Survey （BGPS） sources with 85° 〈 1 〈 193° using the Nanshan 25 m radio telescope. We detected 25 H2O masers, and five of them are new d...We performed an H20 maser survey towards 274 Bolocam Galactic Plane Survey （BGPS） sources with 85° 〈 1 〈 193° using the Nanshan 25 m radio telescope. We detected 25 H2O masers, and five of them are new detections. The detection rate of H2O masers in our sample is 9% which is very low. The detection rate of H2O masers increases as the 1.1 mm flux density of BGPS sources increases, and both the peak flux density and luminosity of H2O masers increase as the sources evolve. The detection rate of H2O masers toward BGPS sources without HCO＋ emission is low. The BGPS sources associated with both H2O and CH3OH masers seem to be more compact than those only associated with H2O masers. This indicates that the sources with both masers may be in a relatively later evolutionary stage. The strongest H2O maser source G133.715＋01.217, also well known as W3 IRS 5 which has a flux density of 2.9 × 103 Jy, was detected at eight different nearby positions. By measuring the correlation between the flux densities of these H2O masers and their angular distance from the true source location, we get the influence radius r = 1/0.8 1og（F0/3rms）. For our observations, strong sources can be detected anywhere within this radius. It is helpful to determine whether or not a weak maser nearby the strong maser is a true detection.展开更多
The 110-111 formaldehyde （H2CO） absorption line and H110α radio recombination line （H RRL） are observed towards the giant HII region in cloud complex W43. The observations are obtained using the Nanshan 25 m sing...The 110-111 formaldehyde （H2CO） absorption line and H110α radio recombination line （H RRL） are observed towards the giant HII region in cloud complex W43. The observations are obtained using the Nanshan 25 m single dish operated by Urumqi Observatory, National Astronomical Observatories of China. A region about 30 × 30 is observed, which covers the whole HII region in W43. Except for the central 10 region, all the other seven points are first observed with the H2CO 110-111 absorption. The column density of the H2CO is calculated, and the H2CO density contours show some differences with the infrared image. Multiple features appear in the H2CO and H RRL which indicate complex structure. The intensities of the H2CO and the velocities of the H110α seem to present a linear correlation, which illustrates that the sphere of influence of the central WR/OB cluster may be much more extended than presently known, since the size is nearly 50 pc.展开更多
We collect 3249 OH maser sources from the literature published up to April 2007, and compile a new catalog of OH masers. We look for the exciting sources of these masers and their infrared properties from IRAS and MSX...We collect 3249 OH maser sources from the literature published up to April 2007, and compile a new catalog of OH masers. We look for the exciting sources of these masers and their infrared properties from IRAS and MSX data, and make a sta- tistical study. MSX sources associated with stellar 1612 MHz OH masers are located mainly above the blackbody line; this is caused by the dust absorption of stellar en- velopes, especially in the MSX_A band. The mid-IR sources associated with stellar OH masers are concentrated in a small region in an [A]-[D] vs.[A]-[E] diagram with a small fraction of contamination; this gives us a new criterion to search for new stellar OH masers and distinguish stellar masers from unknown types of OH masers. IR sources associated with 1612 MHz stellar OH masers show an expected result： the average flux of sources with F60 〉 F25 increases with increasing wavelength, while those with F60 〈 F25 vary little with wavelength, because the sources with F60 〈 F25 are much hotter than those with F60 〉 F25.展开更多
Injecting phase calibration （PCAL） signals to the feed horn of the observation system and analyzing the output response signals of the spectrometer, we measured the working performance of a 4096-channel digital auto...Injecting phase calibration （PCAL） signals to the feed horn of the observation system and analyzing the output response signals of the spectrometer, we measured the working performance of a 4096-channel digital autocalibration spectrometer. The results demonstrate that the spectrometer has a fine working performance： （1） the channels are distributed uniformly in the spectrometer; （2） line drift produces little effect on the observation results; （3） spectral resolution shows little changes with observation time. The distribution of the frequency resolution in an 80 MHz bandwidth was measured. A trial observation on the two molecular spectral lines of H2CO and H110α taken with this spectrometer is described.展开更多
A maser spectral line system is newly implemented on the Urumqi 25m Radio Telescope. The system consists mainly of a cooling receiver and a 4096 channels digital correlation spectrometer. The frequency resolution of t...A maser spectral line system is newly implemented on the Urumqi 25m Radio Telescope. The system consists mainly of a cooling receiver and a 4096 channels digital correlation spectrometer. The frequency resolution of the spectrometer at the maximum signal bandwidth of 80MHz is 19.5kHz. After careful calibrations observation at the 1665 MHz OH maser emission was made towards a number of sources, including W49N and W75N. The observed results demonstrate that the digital correlation spectrometer is suitable for astronomical spectral line observations.展开更多
The excitation of H2O masers usually needs very high density gas,hence it can serve as a marker of dense gas in HⅡ region. We selected a sample of H2O maser sources from Plume et al. （four with, and four without det...The excitation of H2O masers usually needs very high density gas,hence it can serve as a marker of dense gas in HⅡ region. We selected a sample of H2O maser sources from Plume et al. （four with, and four without detected CS（J = 7 - 6） emission）, and observed them in ^13CO（J=1-0） and C^18O （J=1-0）. C^18O （J=1-0） emission was detected only in three of the sources with detected CS（J=7-6） emission. An analysis combined with some data in the literature suggests that these dense cores may be located at different evolutionary stages. Multi-line observation study may provide us clues on the evolution of massive star forming regions and the massive stars themselves.展开更多
In this work,poly(3-hexylthiophene)(P3HT)ultrathin films(P3HT-T)were prepared by spin-coating a dilute P3HT solution(in a toluene:o-dichlorobenzene(Tol:ODCB)blend with a volume ratio of 80:20)with ultrasonication and ...In this work,poly(3-hexylthiophene)(P3HT)ultrathin films(P3HT-T)were prepared by spin-coating a dilute P3HT solution(in a toluene:o-dichlorobenzene(Tol:ODCB)blend with a volume ratio of 80:20)with ultrasonication and the addition of the nucleating agent bicycle[2.2.1]heptane-2,3-dicarboxylic acid disodium salt(HPN-68L)on glass,Si wafers and indium tin oxide(ITO)substrates.The electrical and mechanical properties of the P3HT-T ultrathin films were investigated,and it was found that the conductivity and crack onset strain(COS)were simultaneously improved in comparison with those of the corresponding pristine P3HT film(P3HT-0,without ultrasonication and nucleating agent)on the same substrate,regardless of what substrate was used.Moreover,the conductivity of P3HT-T ultrathin films on different substrates was similar(varying from 3.7 S·cm^(-1)to 4.4 S·cm^(-1)),yet the COS increased from 97%to 138%by varying the substrate from a Si wafer to ITO.Combining grazing-incidence wide-angle X-ray diffraction(GIXRD),UV-visible(UV-Vis)spectroscopy and atomic force microscopy(AFM),we found that the solid order and crystallinity of the P3HT-T ultrathin film on the Si wafer are highest,followed by those on glass,and much lower on ITO.Finally,the surface energy and roughness of three substrates were investigated,and it was found that the polar component of the surface energyγp plays a critical role in determining the crystalline microstructures of P3HT ultrathin films on different substrates.Our work indicates that the P3HT ultrathin film can obviously improve the stretchability and simultaneously retain similar electrical performance when a suitable substrate is chosen.These findings offer a new direction for research on stretchable CP ultrathin films to facilitate future practical applications.展开更多
Polypropylene(PP) sheets are cast with various chill roll temperatures and rates, which are studied with differential scanning calorimetry, wide angel X-ray diffraction, scanning electronic microscopy and dielectric w...Polypropylene(PP) sheets are cast with various chill roll temperatures and rates, which are studied with differential scanning calorimetry, wide angel X-ray diffraction, scanning electronic microscopy and dielectric withstand voltage test system. The results show that increasing the chill roll temperature and cast rate can promote the increase of crystallinity and the growth of β-form. The PP sheets have asymmetric skin layer structures. The lower the chill roll temperature, the thicker the skin layer, the smaller the spherulite size. The electric breakdown strength(Eb) of PP sheets is mainly affected by the crystallinity but not the morphology. The PP sheets are further stretched to prepare bi-axially oriented PP(BOPP) films with various heat setting time. Our results indicate that the structure of PP sheets affects the properties of BOPP films. The as prepared BOPP films from the sheets cast at high chill roll temperature and rate have the highest crystallinity and Eb. Heat setting time has profound effect on the crystallinity and Eb, which increase first and then decrease with the heat setting time. It is expected that our study can provide guidance for optimizing process parameters.展开更多
基金funded by the CAS“Light of West China”Program under Grant No.2021-XBQNXZ-028the National Key R&D Program of China No.2022YFA1603103+5 种基金the National Natural Science Foundation of China(NSFC,Grant Nos.12103082,11973076,11903070 and 12173075)partially funded by the CAS“Light of West China”Program under Grant No.2020-XBQNXZ-017the CAS Presidents International Fellowship Initiative with Grant No.2022VMA0019the Natural Science Foundation of Xinjiang Uygur Autonomous Region under Grant No.2022D01E06the Project of Xinjiang Uygur Autonomous Region of China for Flexibly Fetching in Upscale Talentsthe support from Youth Innovation Promotion Association CAS。
文摘Infrared bubbles provide a unique opportunity to study the interactions between massive stars and surrounding material.We conduct a multi-wavelength study on the environment and star formation around an infrared bubble N13.Three dust clumps and two molecular clumps are identified around N 13,which are all distributed on the layer.Young stellar objects(YSOs)are carefully searched using infrared colors and YSO candidates of WISE and Gaia DR2,and three Class I/II YSOs are found in N 13.In addition,four O-type stars identified in N 13 are probably the exciting stars.The dynamical and fragmentation ages of N 13 are 0.32-0.35 and 1.37-2.80 Myr respectively,which suggest that the radiation-driven implosion model may be dominant in N 13.By comparing the small-size bubble N 13(R~1.9 pc)and the larger-size bubble G15.684-0.29(R~15.7 pc)we found that star formation activity is more active in the large-size bubble.Brief comparisons of ten bubbles show that small-size bubbles have a small ratio of kinetic age versus the fragmentation time.Triggering star formation may be more active in bubbles with larger ratio between kinetic and fragmentation ages.Furthermore,the collect and collapse mechanism may play the dominant role in the large-size ones.
基金Project supported by the National Natural Foundation of China(Grant Nos.51590880,11564030,and 51571126)the National Key Research Program of China(Grant No.2016YFB0700903)+3 种基金Fujian Institute of Innovation,Chinese Academy of Sciences(Grant No.FJCXY18040302)the Key Program of the Chinese Academy of Sciences(Grant No.KJZD-EW-M05-1)the Inner Mongolia Science and Technology Major Project of 2016,Chinathe Natural Science Foundation of Inner Mongolia,China(Grant Nos.2018LH05006 and 2018LH05011)。
文摘Double main phase process is applied to fabricate [(Pr, Nd)1 – xMMx]13.8FebalM1.5B5.9 (x = 0.5 and 0.7;M = Cu, Al, Co, and Nb) sintered magnets with high misch metal (MM) content. In comparison to the magnets by single main phase process, the enhanced magnetic properties have been achieved. For magnets of x = 0.7, Hcj increases to 371.9 kA/m by 60.5%, and (BH)max is significantly enhanced to 253.3 kJ/m3 by 56.9%, compared with those of the single main phase magnets of the same nominal composition. In combination with minor loops and magnetic recoil curves, the property improvement of magnets with double main phase method is well explained. As a result, it is demonstrated that double main phase technology is an effective approach to improve the permanent magnetic properties of MM based sintered magnets.
基金the National Natural Science Foundation of China(Grant No.61922021)the National Key Research and Development Project,China(Grant No.2018YFE0115500)the Fund from the Sichuan Provincial Engineering Research Center for Broadband Microwave Circuit High Density Integration,China.
文摘The interface state of hydrogen-terminated(C-H)diamond metal-oxide-semiconductor field-effect transistor(MOSFET)is critical for device performance.In this paper,we investigate the fixed charges and interface trap states in C-H diamond MOSFETs by using different gate dielectric processes.The devices use Al_(2)O_(3) as gate dielectrics that are deposited via atomic layer deposition(ALD)at 80℃and 300℃,respectively,and their C-V and I-V characteristics are comparatively investigated.Mott-Schottky plots(1/C2-VG)suggest that positive and negative fixed charges with low density of about 10^(11)cm^(-2) are located in the 80-℃-and 300-℃deposition Al2O3 films,respectively.The analyses of direct current(DC)/pulsed I-V and frequency-dependent conductance show that the shallow interface traps(0.46 eV-0.52 eV and 0.53 eV-0.56 eV above the valence band of diamond for the 80-℃and 300-℃deposition conditions,respectively)with distinct density(7.8×10^(13)eV^(-1)·cm^(-2)-8.5×10^(13)eV^(-1)·cm^(-2) and 2.2×10^(13)eV^(-1)·cm^(-2)-5.1×10^(13)eV^(-1)·cm^(-2) for the 80-℃-and 300-℃-deposition conditions,respectively)are present at the Al2O3/C-H diamond interface.Dynamic pulsed I-V and capacitance dispersion results indicate that the ALD Al_(2)O_(3) technique with 300-℃deposition temperature has higher stability for C-H diamond MOSFETs.
基金funded by the CAS“Light of West China”Program(2015-XBQN-B-03)the National Natural Science Foundation of China(Grant Nos.11433008 and 11603063)+1 种基金supported by the National Natural Science Foundation of China(Grant Nos.11703073,117030734,11373062 and 11303081)Recruitment Program of High-end Foreign Experts(20166500004)
文摘Young protoclusters （embedded stellar clusters） are responsible for the vast majority of star formation currently occurring in the Galaxy. Recent observations suggest a scenario in which filamen-tary structures in the interstellar medium represent the first step towards precluster clumps and even- tually star formation. Whether filaments continuously fuel the star formation process when the cluster accretes material is still an open question. In this paper, we present a case study of the famous ＇integral shaped filament＇ （ISF） in the Orion A molecular cloud and we seek to study the kinematics which is truly originated from the ISF. We firstly define the central ridge of the ISF with NHa, ^12CO, ^13CO and N2H^＋. Undulations are present in all the ridges. Moreover, a large scale offset is apparent in the ridges as derived by different tracers, which may be explained by the slingshot mechanism proposed by Stutz ＆ Gould. We fit the velocity field of the ISF and find the derived velocity gradient is about 0.7 km s^- 1 pc^- 1 which may come from an overall contraction. We propose a method to check the accretion flow along the ISF by using the velocity deviations of different molecular tracers, which is better than the common method of using the velocity distribution of one tracer alone. Using the velocity deviations, we also find that OMC-1 to 5 are located close to the local extrema of the fluctuations, which may demonstrate that gas flows toward each clump along the ISE
基金the Open Program of the Key Laboratory of Xinjiang Uygur Autonomous Region(No.2019D04023)the National Natural Science foundation of China(No.11973076)+1 种基金the National Natural Science foundation of China(No.11433008,No.11603063,No.11703074 and No.11703073)the CAS"Light of West China"Program(No.2018-XBQNXZ-B-024,No.2016-QNXZB-23,and No.2016-QNXZ-B-22).
文摘Here we present the study on chemical properties of massive star forming clumps using N2H^+(1-0),H^13CO+(1-0),HCN(1-0)and HN^13C(1-0)data from the literature[Astron.Astrophys.563,A97(2014)].We found that abundances of H^13CO+ and HN^13C are a ected by H2 column densities.As the median values of these two abundances increase by nearly 10 times from stages A to B,H^13CO+and HN^13C are suitable for tracing the evolution of massive star forming clumps.The order of rapidity in growth of abundances of all the four studied molecules from stages A to B,is H^13CO^+,HCN,HN^13C,and N2H^+,from the highest to the lowest.Our results suggest that the observing optically thin molecular lines with high angular resolution are necessary to study the chemical evolution of massive star forming clumps.
基金funded by the National Natural Science Foundation of China (Grant Nos.10778703,11373062,11303081 and 10873025)partly supported by the National Basic Research Program of China (973 program,2012CB821800)
文摘We present large scale observations of C^18O （1-0） towards four massive star forming regions： MON R2, S156, DR17/L906 and M17/M18. The transitions of H2CO （110-111）, C^18O （1-0） and the 6cm continuum are compared in these four regions. Our analysis of the observations and the results of the Non-LTE model shows that the brightness temperature of the formaldehyde absorption line is strongest in a background continuum temperature range of about 3 - 8 K. The excitation of the H2CO absorption line is affected by strong background continuum emission. From a comparison of H2CO and C^18O maps, we found that the extent of H2CO absorption is broader than that of C^18O emission in the four regions. Except for the DR17 region, the maximum in H2CO absorption is located at the same position as the C^18O peak. A good correlation between intensities and widths of H2CO absorption and C^18O emission lines indicates that the H2CO absorption line can trace the dense, warm regions of a molecular cloud. We find that N（H2CO） is well correlated with N（ C^18O） in the four regions and that the average ratio of column densities is （N（H2CO）/N（ClSO）） ～0.03.
基金Project supported by the National Natural Science Foundation of China(Grant Nos.61504125,61474101,and 61505181)
文摘We investigate the influence of fin architecture on linearity characteristics of AlGaN/GaNFinFET.It is found that the Fin FET with scaled fin dimensions exhibits much flatter Gm characteristics than the one with long fins as well as planar HEMT.According to the comparative study,we provide direct proof that source resistance rather than tri-gate structure itself dominates the Gm behavior.Furthermore,power measurements show that the optimized FinFET is capable of delivering a much higher output power density along with significant improvement in linearity characteristics than conventional planar HEMT.This study also highlights the importance of fin design in GaN-based FinFET for microwave power application,especially high-linearity applications.
基金Supported by the National Natural Science Foundation of China.
文摘We made the first CO（1-0） mapping to SNR G21.8-0.6 and SNR G32.8-0.1, both associated with OH 1720MHz maser. Based on the morphological correspondence and velocity and position agreement between the radio remnant and the CO clouds, we tentatively identify the clouds that are respectively interacting with the two SNRs.
基金funded by the National Natural Science Foundation of China under grant 11373062supported by the National Basic Research Program of China (973 program,2012CB821802)+1 种基金the National Natural Science Foundation of China under grant Nos.11433008,11303081 and 10873025the Program of the Light in China’s Western Region (LCRW) under grant Nos.RCPY201202 and XBBS-2014-24
文摘We performed an H20 maser survey towards 274 Bolocam Galactic Plane Survey （BGPS） sources with 85° 〈 1 〈 193° using the Nanshan 25 m radio telescope. We detected 25 H2O masers, and five of them are new detections. The detection rate of H2O masers in our sample is 9% which is very low. The detection rate of H2O masers increases as the 1.1 mm flux density of BGPS sources increases, and both the peak flux density and luminosity of H2O masers increase as the sources evolve. The detection rate of H2O masers toward BGPS sources without HCO＋ emission is low. The BGPS sources associated with both H2O and CH3OH masers seem to be more compact than those only associated with H2O masers. This indicates that the sources with both masers may be in a relatively later evolutionary stage. The strongest H2O maser source G133.715＋01.217, also well known as W3 IRS 5 which has a flux density of 2.9 × 103 Jy, was detected at eight different nearby positions. By measuring the correlation between the flux densities of these H2O masers and their angular distance from the true source location, we get the influence radius r = 1/0.8 1og（F0/3rms）. For our observations, strong sources can be detected anywhere within this radius. It is helpful to determine whether or not a weak maser nearby the strong maser is a true detection.
基金supported by the National Natural Science Foundation of China(Grant Nos. 10778703, 10873025)the Program of Light in China’s Western Region(LCWR,Nos. RCPY200605, RCPY200706)
文摘The 110-111 formaldehyde （H2CO） absorption line and H110α radio recombination line （H RRL） are observed towards the giant HII region in cloud complex W43. The observations are obtained using the Nanshan 25 m single dish operated by Urumqi Observatory, National Astronomical Observatories of China. A region about 30 × 30 is observed, which covers the whole HII region in W43. Except for the central 10 region, all the other seven points are first observed with the H2CO 110-111 absorption. The column density of the H2CO is calculated, and the H2CO density contours show some differences with the infrared image. Multiple features appear in the H2CO and H RRL which indicate complex structure. The intensities of the H2CO and the velocities of the H110α seem to present a linear correlation, which illustrates that the sphere of influence of the central WR/OB cluster may be much more extended than presently known, since the size is nearly 50 pc.
基金supported by the National Natural Science Foundation of China (Grant Nos. 10778703 and10873025) the Program of the Light in China’s Western Region (LCWR) (Nos. RCPY200605 and RCPY200706)
文摘We collect 3249 OH maser sources from the literature published up to April 2007, and compile a new catalog of OH masers. We look for the exciting sources of these masers and their infrared properties from IRAS and MSX data, and make a sta- tistical study. MSX sources associated with stellar 1612 MHz OH masers are located mainly above the blackbody line; this is caused by the dust absorption of stellar en- velopes, especially in the MSX_A band. The mid-IR sources associated with stellar OH masers are concentrated in a small region in an [A]-[D] vs.[A]-[E] diagram with a small fraction of contamination; this gives us a new criterion to search for new stellar OH masers and distinguish stellar masers from unknown types of OH masers. IR sources associated with 1612 MHz stellar OH masers show an expected result： the average flux of sources with F60 〉 F25 increases with increasing wavelength, while those with F60 〈 F25 vary little with wavelength, because the sources with F60 〈 F25 are much hotter than those with F60 〉 F25.
基金Supported by the National Natural Science Foundation of China.
文摘Injecting phase calibration （PCAL） signals to the feed horn of the observation system and analyzing the output response signals of the spectrometer, we measured the working performance of a 4096-channel digital autocalibration spectrometer. The results demonstrate that the spectrometer has a fine working performance： （1） the channels are distributed uniformly in the spectrometer; （2） line drift produces little effect on the observation results; （3） spectral resolution shows little changes with observation time. The distribution of the frequency resolution in an 80 MHz bandwidth was measured. A trial observation on the two molecular spectral lines of H2CO and H110α taken with this spectrometer is described.
基金Supported by the National Natural Science Foundation of China.
文摘A maser spectral line system is newly implemented on the Urumqi 25m Radio Telescope. The system consists mainly of a cooling receiver and a 4096 channels digital correlation spectrometer. The frequency resolution of the spectrometer at the maximum signal bandwidth of 80MHz is 19.5kHz. After careful calibrations observation at the 1665 MHz OH maser emission was made towards a number of sources, including W49N and W75N. The observed results demonstrate that the digital correlation spectrometer is suitable for astronomical spectral line observations.
基金Supported by the National Natural Science Foundation of China.
文摘The excitation of H2O masers usually needs very high density gas,hence it can serve as a marker of dense gas in HⅡ region. We selected a sample of H2O maser sources from Plume et al. （four with, and four without detected CS（J = 7 - 6） emission）, and observed them in ^13CO（J=1-0） and C^18O （J=1-0）. C^18O （J=1-0） emission was detected only in three of the sources with detected CS（J=7-6） emission. An analysis combined with some data in the literature suggests that these dense cores may be located at different evolutionary stages. Multi-line observation study may provide us clues on the evolution of massive star forming regions and the massive stars themselves.
基金supported by the National Natural Science Foundation of China(No.21975029)。
文摘In this work,poly(3-hexylthiophene)(P3HT)ultrathin films(P3HT-T)were prepared by spin-coating a dilute P3HT solution(in a toluene:o-dichlorobenzene(Tol:ODCB)blend with a volume ratio of 80:20)with ultrasonication and the addition of the nucleating agent bicycle[2.2.1]heptane-2,3-dicarboxylic acid disodium salt(HPN-68L)on glass,Si wafers and indium tin oxide(ITO)substrates.The electrical and mechanical properties of the P3HT-T ultrathin films were investigated,and it was found that the conductivity and crack onset strain(COS)were simultaneously improved in comparison with those of the corresponding pristine P3HT film(P3HT-0,without ultrasonication and nucleating agent)on the same substrate,regardless of what substrate was used.Moreover,the conductivity of P3HT-T ultrathin films on different substrates was similar(varying from 3.7 S·cm^(-1)to 4.4 S·cm^(-1)),yet the COS increased from 97%to 138%by varying the substrate from a Si wafer to ITO.Combining grazing-incidence wide-angle X-ray diffraction(GIXRD),UV-visible(UV-Vis)spectroscopy and atomic force microscopy(AFM),we found that the solid order and crystallinity of the P3HT-T ultrathin film on the Si wafer are highest,followed by those on glass,and much lower on ITO.Finally,the surface energy and roughness of three substrates were investigated,and it was found that the polar component of the surface energyγp plays a critical role in determining the crystalline microstructures of P3HT ultrathin films on different substrates.Our work indicates that the P3HT ultrathin film can obviously improve the stretchability and simultaneously retain similar electrical performance when a suitable substrate is chosen.These findings offer a new direction for research on stretchable CP ultrathin films to facilitate future practical applications.
基金financially supported by the State Key Laboratory of Advanced Power Transmission Technology (No.GEIRI-SKL2020-009)。
文摘Polypropylene(PP) sheets are cast with various chill roll temperatures and rates, which are studied with differential scanning calorimetry, wide angel X-ray diffraction, scanning electronic microscopy and dielectric withstand voltage test system. The results show that increasing the chill roll temperature and cast rate can promote the increase of crystallinity and the growth of β-form. The PP sheets have asymmetric skin layer structures. The lower the chill roll temperature, the thicker the skin layer, the smaller the spherulite size. The electric breakdown strength(Eb) of PP sheets is mainly affected by the crystallinity but not the morphology. The PP sheets are further stretched to prepare bi-axially oriented PP(BOPP) films with various heat setting time. Our results indicate that the structure of PP sheets affects the properties of BOPP films. The as prepared BOPP films from the sheets cast at high chill roll temperature and rate have the highest crystallinity and Eb. Heat setting time has profound effect on the crystallinity and Eb, which increase first and then decrease with the heat setting time. It is expected that our study can provide guidance for optimizing process parameters.
