A measure of entanglement on n qubits is defined in terms of Wigner-Yanase skew information. It is shown that the measure coincides essentially with the concurrence on two qubits. This uncovers the information-theoret...A measure of entanglement on n qubits is defined in terms of Wigner-Yanase skew information. It is shown that the measure coincides essentially with the concurrence on two qubits. This uncovers the information-theoretic meaning of the concurrence of entangled states.展开更多
Phenol,which belongs to the C_(6)H_(6)O isomeric group,is the simplest molecule in the family of alcohol of the aromatic series.Although phenol has yet to be detected in the interstellar medium,a tentative identificat...Phenol,which belongs to the C_(6)H_(6)O isomeric group,is the simplest molecule in the family of alcohol of the aromatic series.Although phenol has yet to be detected in the interstellar medium,a tentative identification was reported toward the Orion KL hot core using the IRAM-30 m line survey.To explore some more species of this isomeric group,we consider ten species to study the fate of their astronomical detection.It is noticed that phenol is the most energetically favorable isomer of this group.In contrast,propargyl ether is the least favorable(having relative energy~103kcal mol^(-1)compared to phenol)species of this group.So far,the studies associated with the formation of phenol are heavily concentrated on combustion chemistry.Here,we suggest a few key reactions(C_(6)H_(6)+OH→C_(6)H_(5)+H_(2)O,C_(6)H_(6)+O→C_(6)H_(5)OH,C_(6)H_(6)+H→C_(6)H_(5)+H_(2),and C_(6)H_(5)+OH→C_(6)H_(5)OH+hν)for the formation of phenol.All these pathways are included in a large gas-grain chemical network to study its formation in high mass star-forming regions and dark cloud environments.It is noticed that the phenyl(-C_(6)H_(5))formation by the ice-phase hydrogen abstraction reaction of benzene(i.e.,C_(6)H_(6)+OH→C_(6)H_(5)+H_(2)O if allowed at~10 K)could serve as the starting point for the formation of phenol in the gas phase by radiative association reaction C_(6)H_(5)+OH→C_(6)H_(5)OH+hν.The gasphase reaction C_(6)H_(6)+O→C_(6)H_(5)OH significantly contributes to the formation of phenol,when the ice-phase reaction C_(6)H_(6)+OH→C_(6)H_(5)+H_(2)O is not considered at low temperature.Band 4 ALMA archival data of a hot molecular core,G10.47+0.03,are analyzed.It yields an upper limit on phenol abundance of 5.19×10^(-9).Our astrochemical model delivers an upper limit on phenol abundance of~2.20×10^(-9)in the hot molecular core,whereas its production in the dark cloud is not satisfactory.展开更多
Recently,our group produced spin-polarized hydrogen(SPH)atoms at densities of at least 10^(19)cm^(-3)from the photodissociation of hydrogen halide molecules with circularly polarized UV light and measured them via mag...Recently,our group produced spin-polarized hydrogen(SPH)atoms at densities of at least 10^(19)cm^(-3)from the photodissociation of hydrogen halide molecules with circularly polarized UV light and measured them via magnetization-quantum beats with a pickup coil.These densities are approximately 7 orders of magnitude higher than those produced using conventional methods,opening up new fields of application,such as ultrafast magnetometry,the production of polarized MeV and GeV particle beams,such as electron beams with intensities approximately 10^(4)higher than current sources,and the study of polarized nuclear fusion,for which the reaction cross sections of D-T and D-(3)^He reactions are expected to increase by 50%for fully polarized nuclear spins.We review the production,detection,depolarization mechanisms,and potential applications of high-density SPH.展开更多
基金Supported by the National Natural Science Foundation of China under Grant No 10571176, the/National Basic Research Programme of China under Grant No 2001CB309309, and Chinese Academy of Sciences.
文摘A measure of entanglement on n qubits is defined in terms of Wigner-Yanase skew information. It is shown that the measure coincides essentially with the concurrence on two qubits. This uncovers the information-theoretic meaning of the concurrence of entangled states.
基金the SVMCM scholarship,Government of West Bengalthe DST-INSPIRE Fellowship scheme for financial assistancethe CSIR fellowship。
文摘Phenol,which belongs to the C_(6)H_(6)O isomeric group,is the simplest molecule in the family of alcohol of the aromatic series.Although phenol has yet to be detected in the interstellar medium,a tentative identification was reported toward the Orion KL hot core using the IRAM-30 m line survey.To explore some more species of this isomeric group,we consider ten species to study the fate of their astronomical detection.It is noticed that phenol is the most energetically favorable isomer of this group.In contrast,propargyl ether is the least favorable(having relative energy~103kcal mol^(-1)compared to phenol)species of this group.So far,the studies associated with the formation of phenol are heavily concentrated on combustion chemistry.Here,we suggest a few key reactions(C_(6)H_(6)+OH→C_(6)H_(5)+H_(2)O,C_(6)H_(6)+O→C_(6)H_(5)OH,C_(6)H_(6)+H→C_(6)H_(5)+H_(2),and C_(6)H_(5)+OH→C_(6)H_(5)OH+hν)for the formation of phenol.All these pathways are included in a large gas-grain chemical network to study its formation in high mass star-forming regions and dark cloud environments.It is noticed that the phenyl(-C_(6)H_(5))formation by the ice-phase hydrogen abstraction reaction of benzene(i.e.,C_(6)H_(6)+OH→C_(6)H_(5)+H_(2)O if allowed at~10 K)could serve as the starting point for the formation of phenol in the gas phase by radiative association reaction C_(6)H_(5)+OH→C_(6)H_(5)OH+hν.The gasphase reaction C_(6)H_(6)+O→C_(6)H_(5)OH significantly contributes to the formation of phenol,when the ice-phase reaction C_(6)H_(6)+OH→C_(6)H_(5)+H_(2)O is not considered at low temperature.Band 4 ALMA archival data of a hot molecular core,G10.47+0.03,are analyzed.It yields an upper limit on phenol abundance of 5.19×10^(-9).Our astrochemical model delivers an upper limit on phenol abundance of~2.20×10^(-9)in the hot molecular core,whereas its production in the dark cloud is not satisfactory.
基金This work is supported by the Hellenic Foundation for Research and Innovation(HFRI)and the General Secretariat for Research and Technology(GSRT),grant agreement No.HFRI-FM17-3709(project NUPOL)and by the project"HELLASCHH(MIS 5002735)Which is implemented under the"Action for Strengthening Research and Innovation Infrastructures",funded by the Operational Programme"Competitiveness,Entrepreneurship and Innovation"(NSRF 2014-2020)cofinanced by Greece and the European Union(European Regional Development Fund).GK acknowledges funding from the Hellenic Foundation for Research and Innovation(HFRI)and the General Secretariat for Research and Technology(G5RT),under project HANDCORE grant agreem ent No 1789.Figure 5 is adapted with permission from Boulogiannis et al.,"Spin-polarized hydrogen depolarization rates at high hydrogen halide pressures:hyperfine depolarization via the HY-H complex",The Journal of Physical Chemistry A 123,8130-8134(2019)。
文摘Recently,our group produced spin-polarized hydrogen(SPH)atoms at densities of at least 10^(19)cm^(-3)from the photodissociation of hydrogen halide molecules with circularly polarized UV light and measured them via magnetization-quantum beats with a pickup coil.These densities are approximately 7 orders of magnitude higher than those produced using conventional methods,opening up new fields of application,such as ultrafast magnetometry,the production of polarized MeV and GeV particle beams,such as electron beams with intensities approximately 10^(4)higher than current sources,and the study of polarized nuclear fusion,for which the reaction cross sections of D-T and D-(3)^He reactions are expected to increase by 50%for fully polarized nuclear spins.We review the production,detection,depolarization mechanisms,and potential applications of high-density SPH.
