Pub Date : 2024-06-30DOI: 10.1088/1674-1137/ad3c2d
Tianshu Wu, 天枢 吴, Yiqian Chen and 一千 陈
This paper investigates observable signatures of hot spots orbiting Reissner-Nordström (RN) black holes and naked singularities. For an RN black hole, we find two discernible lensing image tracks in time integrated images, capturing a complete orbit of hot spots and a image shadow within the critical curve where photons with a small impact parameter fall into the event horizon. Conversely, in RN singularities, additional image tracks can be found within the critical curve, originating from photons reflected by the infinitely high effective potential well. Moreover, we find incomplete and converging tracks from the time integrated images of hot spot orbiting RN singularities that have no photon sphere. The presence of these additional image tracks significantly influences temporal magnitudes at their local maxima, enabling us to differentiate between RN black holes and RN naked singularities.
{"title":"Distinguishing the observational signatures of hot spots orbiting Reissner-Nordström spacetime*","authors":"Tianshu Wu, 天枢 吴, Yiqian Chen and 一千 陈","doi":"10.1088/1674-1137/ad3c2d","DOIUrl":"https://doi.org/10.1088/1674-1137/ad3c2d","url":null,"abstract":"This paper investigates observable signatures of hot spots orbiting Reissner-Nordström (RN) black holes and naked singularities. For an RN black hole, we find two discernible lensing image tracks in time integrated images, capturing a complete orbit of hot spots and a image shadow within the critical curve where photons with a small impact parameter fall into the event horizon. Conversely, in RN singularities, additional image tracks can be found within the critical curve, originating from photons reflected by the infinitely high effective potential well. Moreover, we find incomplete and converging tracks from the time integrated images of hot spot orbiting RN singularities that have no photon sphere. The presence of these additional image tracks significantly influences temporal magnitudes at their local maxima, enabling us to differentiate between RN black holes and RN naked singularities.","PeriodicalId":10250,"journal":{"name":"中国物理C","volume":"42 1","pages":""},"PeriodicalIF":3.6,"publicationDate":"2024-06-30","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141165745","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2024-06-01DOI: 10.1088/1674-1137/ad361c
Jun-Qi Guo, Yu Hu, Pan-Pan Wang, Cheng-Gang Shao
We study the dynamics of the critical collapse of a spherically symmetric scalar field. Approximate analytic expressions for the metric functions and matter field in the large-radius region are obtained. In the central region, owing to the boundary conditions, the equation of motion for the scalar field is reduced to the flat-spacetime form.
{"title":"New results on the dynamics of critical collapse* * JQG is Supported by the Natural Science Foundation of Shandong Province, China (ZR2019MA068). YH, PPW and CGS are Supported by the National Natural Science Foundation of China (11925503)","authors":"Jun-Qi Guo, Yu Hu, Pan-Pan Wang, Cheng-Gang Shao","doi":"10.1088/1674-1137/ad361c","DOIUrl":"https://doi.org/10.1088/1674-1137/ad361c","url":null,"abstract":"We study the dynamics of the critical collapse of a spherically symmetric scalar field. Approximate analytic expressions for the metric functions and matter field in the large-radius region are obtained. In the central region, owing to the boundary conditions, the equation of motion for the scalar field is reduced to the flat-spacetime form.","PeriodicalId":10250,"journal":{"name":"中国物理C","volume":"7 1","pages":""},"PeriodicalIF":3.6,"publicationDate":"2024-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140830455","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2024-06-01DOI: 10.1088/1674-1137/ad34c2
Fan Huang, Yan-Chen Bi, Zhoujian Cao, Qing-Guo Huang
In the frequency band of the Laser Interferometer Space Antenna (LISA), extensive research has been conducted on the impact of foreground confusion noise generated by galactic binaries within the Milky Way Galaxy. Additionally, recent evidence of a stochastic signal, announced by the NANOGrav, EPTA, PPTA, CPTA, and InPTA, indicates that the stochastic gravitational-wave background (SGWB) generated by supermassive black hole binaries (SMBHBs) can contribute strong background noise within the LISA band. Given the presence of such strong noise, it is expected to have significant impacts on LISA's scientific missions. In this study, we investigate the impacts of the SGWB generated by SMBHBs on the detection of individual massive black hole binaries, verified galactic binaries, and extreme mass ratio inspirals in the context of LISA. We find it essential to resolve and eliminate the excess noise from the SGWB to guarantee the success of LISA's missions.
在激光干涉仪空间天线（LISA）的频段内，对银河系内银河双星产生的前景混淆噪声的影响进行了广泛的研究。此外，最近由 NANOGrav、EPTA、PPTA、CPTA 和 InPTA 公布的随机信号证据表明，超大质量黑洞双星（SMBHBs）产生的随机引力波背景（SGWB）会在 LISA 波段内产生强大的背景噪声。鉴于这种强噪声的存在，预计会对 LISA 的科学任务产生重大影响。在这项研究中，我们研究了 SMBHB 产生的 SGWB 对 LISA 检测单个大质量黑洞双星、验证星系双星和极端质量比吸气的影响。我们发现必须解决和消除来自 SGWB 的过量噪声，以保证 LISA 任务的成功。
{"title":"Impacts of gravitational-wave background from supermassive black hole binaries on the detection of compact binaries by LISA* * Supported by the NSFC (12250010, 11991052) and Key Research Program of Frontier Sciences, CAS, (ZDBS-LY-7009)","authors":"Fan Huang, Yan-Chen Bi, Zhoujian Cao, Qing-Guo Huang","doi":"10.1088/1674-1137/ad34c2","DOIUrl":"https://doi.org/10.1088/1674-1137/ad34c2","url":null,"abstract":"In the frequency band of the Laser Interferometer Space Antenna (LISA), extensive research has been conducted on the impact of foreground confusion noise generated by galactic binaries within the Milky Way Galaxy. Additionally, recent evidence of a stochastic signal, announced by the NANOGrav, EPTA, PPTA, CPTA, and InPTA, indicates that the stochastic gravitational-wave background (SGWB) generated by supermassive black hole binaries (SMBHBs) can contribute strong background noise within the LISA band. Given the presence of such strong noise, it is expected to have significant impacts on LISA's scientific missions. In this study, we investigate the impacts of the SGWB generated by SMBHBs on the detection of individual massive black hole binaries, verified galactic binaries, and extreme mass ratio inspirals in the context of LISA. We find it essential to resolve and eliminate the excess noise from the SGWB to guarantee the success of LISA's missions.","PeriodicalId":10250,"journal":{"name":"中国物理C","volume":"30 1","pages":""},"PeriodicalIF":3.6,"publicationDate":"2024-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140830698","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2024-06-01DOI: 10.1088/1674-1137/ad34be
Tao Zhong, Ya-Hong Dai, Hai-Bing Fu
Motivated by our previous study [Phys. Rev. D 104(1), 016021 (2021)] on the pionic leading-twist distribution amplitude (DA), we revisit the <italic toggle="yes">ρ</italic>-meson leading-twist longitudinal DA <inline-formula> <tex-math><?CDATA $ phi_{2;rho}^|(x,mu) $?></tex-math> <inline-graphic xlink:href="cpc_48_6_063108_M1.jpg" xlink:type="simple"></inline-graphic> </inline-formula> in this study. A model proposed by Chang based on the Dyson-Schwinger equations is adopted to describe the behavior of <inline-formula> <tex-math><?CDATA $ phi_{2;rho}^|(x,mu) $?></tex-math> <inline-graphic xlink:href="cpc_48_6_063108_M2.jpg" xlink:type="simple"></inline-graphic> </inline-formula>. However, the <italic toggle="yes">ξ</italic>-moments of <inline-formula> <tex-math><?CDATA $ phi_{2;rho}^|(x,mu) $?></tex-math> <inline-graphic xlink:href="cpc_48_6_063108_M3.jpg" xlink:type="simple"></inline-graphic> </inline-formula> are calculated with the QCD sum rules in the framework of the background field theory. The sum rule formulas for these moments are improved. More accurate values for the first five nonzero <italic toggle="yes">ξ</italic>-moments at the typical scale <inline-formula> <tex-math><?CDATA $ mu = (1.0, 1.4, 2.0, 3.0); {rm GeV} $?></tex-math> <inline-graphic xlink:href="cpc_48_6_063108_M4.jpg" xlink:type="simple"></inline-graphic> </inline-formula> are given, e.g., at <inline-formula> <tex-math><?CDATA $ mu = 1; {rm GeV} $?></tex-math> <inline-graphic xlink:href="cpc_48_6_063108_M5.jpg" xlink:type="simple"></inline-graphic> </inline-formula>, <inline-formula> <tex-math><?CDATA $ langlexi^2rangle_{2;rho}^| = 0.220(6) $?></tex-math> <inline-graphic xlink:href="cpc_48_6_063108_M6.jpg" xlink:type="simple"></inline-graphic> </inline-formula>, <inline-formula> <tex-math><?CDATA $ langlexi^4rangle_{2;rho}^| = 0.103(4) $?></tex-math> <inline-graphic xlink:href="cpc_48_6_063108_M7.jpg" xlink:type="simple"></inline-graphic> </inline-formula>, <inline-formula> <tex-math><?CDATA $ langlexi^6rangle_{2;rho}^| = 0.066(5) $?></tex-math> <inline-graphic xlink:href="cpc_48_6_063108_M8.jpg" xlink:type="simple"></inline-graphic> </inline-formula>, <inline-formula> <tex-math><?CDATA $ langlexi^8rangle_{2;rho}^| = 0.046(4) $?></tex-math> <inline-graphic xlink:href="cpc_48_6_063108_M9.jpg" xlink:type="simple"></inline-graphic> </inline-formula> , and <inline-formula> <tex-math><?CDATA $ langlexi^{10}rangle_{2;rho}^| = 0.035(3) $?></tex-math> <inline-graphic xlink:href="cpc_48_6_063108_M10.jpg" xlink:type="simple"></inline-graphic> </inline-formula>. By fitting these values with the least squares method, the DSE model for <inline-formula> <tex-math><?CDATA $ phi_{2;rho}^|(x,mu) $?></tex-math> <inline-graphic xlink:href="cpc_48_6_063108_M11.jpg" xlink:type="simple"></inline-graphic> </inline-formula> is determined. By taking the left-handed current light-cone sum rule approach, we obtain the transition form factor in the large recoil region, <italic toggle="yes">i.e.</it
{"title":"ρ-meson longitudinal leading-twist distribution amplitude revisited and the D→ρ semileptonic decay* * Supported in part by the National Natural Science Foundation of China (12265009, 12265010, 12147102), the Project of Guizhou Provincial Department of Science and Technology (ZK[2021]024, ZK[2023]142), the Project of Guizhou Provincial Department of Education (KY[2021]030) and the Chongqing Graduate Research and Innovation Foundation (ydstd1912)","authors":"Tao Zhong, Ya-Hong Dai, Hai-Bing Fu","doi":"10.1088/1674-1137/ad34be","DOIUrl":"https://doi.org/10.1088/1674-1137/ad34be","url":null,"abstract":"Motivated by our previous study [Phys. Rev. D 104(1), 016021 (2021)] on the pionic leading-twist distribution amplitude (DA), we revisit the <italic toggle=\"yes\">ρ</italic>-meson leading-twist longitudinal DA <inline-formula>\u0000<tex-math><?CDATA $ phi_{2;rho}^|(x,mu) $?></tex-math>\u0000<inline-graphic xlink:href=\"cpc_48_6_063108_M1.jpg\" xlink:type=\"simple\"></inline-graphic>\u0000</inline-formula> in this study. A model proposed by Chang based on the Dyson-Schwinger equations is adopted to describe the behavior of <inline-formula>\u0000<tex-math><?CDATA $ phi_{2;rho}^|(x,mu) $?></tex-math>\u0000<inline-graphic xlink:href=\"cpc_48_6_063108_M2.jpg\" xlink:type=\"simple\"></inline-graphic>\u0000</inline-formula>. However, the <italic toggle=\"yes\">ξ</italic>-moments of <inline-formula>\u0000<tex-math><?CDATA $ phi_{2;rho}^|(x,mu) $?></tex-math>\u0000<inline-graphic xlink:href=\"cpc_48_6_063108_M3.jpg\" xlink:type=\"simple\"></inline-graphic>\u0000</inline-formula> are calculated with the QCD sum rules in the framework of the background field theory. The sum rule formulas for these moments are improved. More accurate values for the first five nonzero <italic toggle=\"yes\">ξ</italic>-moments at the typical scale <inline-formula>\u0000<tex-math><?CDATA $ mu = (1.0, 1.4, 2.0, 3.0); {rm GeV} $?></tex-math>\u0000<inline-graphic xlink:href=\"cpc_48_6_063108_M4.jpg\" xlink:type=\"simple\"></inline-graphic>\u0000</inline-formula> are given, e.g., at <inline-formula>\u0000<tex-math><?CDATA $ mu = 1; {rm GeV} $?></tex-math>\u0000<inline-graphic xlink:href=\"cpc_48_6_063108_M5.jpg\" xlink:type=\"simple\"></inline-graphic>\u0000</inline-formula>, <inline-formula>\u0000<tex-math><?CDATA $ langlexi^2rangle_{2;rho}^| = 0.220(6) $?></tex-math>\u0000<inline-graphic xlink:href=\"cpc_48_6_063108_M6.jpg\" xlink:type=\"simple\"></inline-graphic>\u0000</inline-formula>, <inline-formula>\u0000<tex-math><?CDATA $ langlexi^4rangle_{2;rho}^| = 0.103(4) $?></tex-math>\u0000<inline-graphic xlink:href=\"cpc_48_6_063108_M7.jpg\" xlink:type=\"simple\"></inline-graphic>\u0000</inline-formula>, <inline-formula>\u0000<tex-math><?CDATA $ langlexi^6rangle_{2;rho}^| = 0.066(5) $?></tex-math>\u0000<inline-graphic xlink:href=\"cpc_48_6_063108_M8.jpg\" xlink:type=\"simple\"></inline-graphic>\u0000</inline-formula>, <inline-formula>\u0000<tex-math><?CDATA $ langlexi^8rangle_{2;rho}^| = 0.046(4) $?></tex-math>\u0000<inline-graphic xlink:href=\"cpc_48_6_063108_M9.jpg\" xlink:type=\"simple\"></inline-graphic>\u0000</inline-formula> , and <inline-formula>\u0000<tex-math><?CDATA $ langlexi^{10}rangle_{2;rho}^| = 0.035(3) $?></tex-math>\u0000<inline-graphic xlink:href=\"cpc_48_6_063108_M10.jpg\" xlink:type=\"simple\"></inline-graphic>\u0000</inline-formula>. By fitting these values with the least squares method, the DSE model for <inline-formula>\u0000<tex-math><?CDATA $ phi_{2;rho}^|(x,mu) $?></tex-math>\u0000<inline-graphic xlink:href=\"cpc_48_6_063108_M11.jpg\" xlink:type=\"simple\"></inline-graphic>\u0000</inline-formula> is determined. By taking the left-handed current light-cone sum rule approach, we obtain the transition form factor in the large recoil region, <italic toggle=\"yes\">i.e.</it","PeriodicalId":10250,"journal":{"name":"中国物理C","volume":"59 1","pages":""},"PeriodicalIF":3.6,"publicationDate":"2024-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140830663","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2024-06-01DOI: 10.1088/1674-1137/ad3943
Chunhua Li, Xijun Wang, Chen Wu
Particle was first observed by the Belle experiment in the invariant mass spectrum in the process and subsequently confirmed by the BaBar experiment. Both experiments reported the resonant parameters of this particle in the processes and assuming as an S-wave Breit-Wigner resonance. We performed a global fit to the distributions of invariant mass of measured by the Belle and BaBar experiments and additionally incorporated the measurements reported by the LHCb experiment to extract the mass and width of . We obtained MeV/ and MeV, which are consistent with the values from PDG within one standard deviation but with higher precision.
贝尔实验首次在过程中的不变质谱中观测到该粒子，随后巴巴尔实验证实了这一点。两次实验都报告了该粒子在过程中的共振参数，并假设为 S 波布雷特-维格纳共振。我们对 Belle 和 BaBar 实验所测得的该粒子的不变质量分布进行了全局拟合，并结合 LHCb 实验所报告的测量结果，提取了该粒子的质量和宽度。 我们得到了 MeV/ 和 MeV，与 PDG 的值一致，误差在一个标准差之内，但精度更高。
{"title":"Determination of the resonant parameters of with global fit* * Supported by National Natural Science Foundation of China (NSFC) (11805090)","authors":"Chunhua Li, Xijun Wang, Chen Wu","doi":"10.1088/1674-1137/ad3943","DOIUrl":"https://doi.org/10.1088/1674-1137/ad3943","url":null,"abstract":"Particle <inline-formula>\u0000<tex-math><?CDATA $ chi_{c0}(3915) $?></tex-math>\u0000<inline-graphic xlink:href=\"cpc_48_6_063001_M2.jpg\" xlink:type=\"simple\"></inline-graphic>\u0000</inline-formula> was first observed by the Belle experiment in the <inline-formula>\u0000<tex-math><?CDATA $ omega J/psi $?></tex-math>\u0000<inline-graphic xlink:href=\"cpc_48_6_063001_M3.jpg\" xlink:type=\"simple\"></inline-graphic>\u0000</inline-formula> invariant mass spectrum in the process <inline-formula>\u0000<tex-math><?CDATA $ Bto Komega J/psi $?></tex-math>\u0000<inline-graphic xlink:href=\"cpc_48_6_063001_M4.jpg\" xlink:type=\"simple\"></inline-graphic>\u0000</inline-formula> and subsequently confirmed by the BaBar experiment. Both experiments reported the resonant parameters of this particle in the processes <inline-formula>\u0000<tex-math><?CDATA $ gammagammatoomega J/psi $?></tex-math>\u0000<inline-graphic xlink:href=\"cpc_48_6_063001_M5.jpg\" xlink:type=\"simple\"></inline-graphic>\u0000</inline-formula> and <inline-formula>\u0000<tex-math><?CDATA $ Bto Komega J/psi $?></tex-math>\u0000<inline-graphic xlink:href=\"cpc_48_6_063001_M6.jpg\" xlink:type=\"simple\"></inline-graphic>\u0000</inline-formula> assuming <inline-formula>\u0000<tex-math><?CDATA $ chi_{c0}(3915) $?></tex-math>\u0000<inline-graphic xlink:href=\"cpc_48_6_063001_M7.jpg\" xlink:type=\"simple\"></inline-graphic>\u0000</inline-formula> as an <italic toggle=\"yes\">S</italic>-wave Breit-Wigner resonance. We performed a global fit to the distributions of invariant mass of <inline-formula>\u0000<tex-math><?CDATA $ omega J/psi $?></tex-math>\u0000<inline-graphic xlink:href=\"cpc_48_6_063001_M8.jpg\" xlink:type=\"simple\"></inline-graphic>\u0000</inline-formula> measured by the Belle and BaBar experiments and additionally incorporated the measurements reported by the LHCb experiment to extract the mass and width of <inline-formula>\u0000<tex-math><?CDATA $ chi_{c0}(3915) $?></tex-math>\u0000<inline-graphic xlink:href=\"cpc_48_6_063001_M9.jpg\" xlink:type=\"simple\"></inline-graphic>\u0000</inline-formula>. We obtained <inline-formula>\u0000<tex-math><?CDATA $ M=3920.9pm0.9 $?></tex-math>\u0000<inline-graphic xlink:href=\"cpc_48_6_063001_M10.jpg\" xlink:type=\"simple\"></inline-graphic>\u0000</inline-formula> MeV/<inline-formula>\u0000<tex-math><?CDATA $ c^2 $?></tex-math>\u0000<inline-graphic xlink:href=\"cpc_48_6_063001_M11.jpg\" xlink:type=\"simple\"></inline-graphic>\u0000</inline-formula> and <inline-formula>\u0000<tex-math><?CDATA $ Gamma=18.2pm2.4 $?></tex-math>\u0000<inline-graphic xlink:href=\"cpc_48_6_063001_M12.jpg\" xlink:type=\"simple\"></inline-graphic>\u0000</inline-formula> MeV, which are consistent with the values from PDG within one standard deviation but with higher precision.","PeriodicalId":10250,"journal":{"name":"中国物理C","volume":"15 1","pages":""},"PeriodicalIF":3.6,"publicationDate":"2024-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140830740","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2024-06-01DOI: 10.1088/1674-1137/ad34c0
Ye-Huang Pang, Xue Zhang, Qing-Guo Huang
Recently, the emergence of cosmological tension has raised doubts about the consistency of the ΛCDM model. To constrain the neutrino mass within a consistent cosmological framework, we investigate three massive neutrinos with normal hierarchy (NH) and inverted hierarchy (IH) in both the axion-like early dark energy (Axi-EDE) and AdS-EDE models. We use joint datasets including the cosmic microwave background power spectrum from Planck 2018, Pantheon of type Ia supernova, baryon acoustic oscillation, and data from SH0ES. For the νAxi-EDE model, we obtain < 0.152 eV and < 0.178 eV, whereas for the νAdS-EDE model, we find < 0.135 eV and < 0.167 eV. Our results exhibit a preference for NH in both the νAxi-EDE and νAdS-EDE models.
{"title":"Cosmological constraints on neutrino mass within consistent cosmological models* * We acknowledge the use of HPC Cluster of ITP-CAS. XZ is supported by the National Natural Science Foundation of China (12005183). QGH is supported by the National Natural Science Foundation of China (12250010, 11975019, 11991052, 12047503), and the Key Research Program of Frontier Sciences, CAS, (ZDBS-LY-7009)","authors":"Ye-Huang Pang, Xue Zhang, Qing-Guo Huang","doi":"10.1088/1674-1137/ad34c0","DOIUrl":"https://doi.org/10.1088/1674-1137/ad34c0","url":null,"abstract":"Recently, the emergence of cosmological tension has raised doubts about the consistency of the ΛCDM model. To constrain the neutrino mass within a consistent cosmological framework, we investigate three massive neutrinos with normal hierarchy (NH) and inverted hierarchy (IH) in both the axion-like early dark energy (Axi-EDE) and AdS-EDE models. We use joint datasets including the cosmic microwave background power spectrum from <italic toggle=\"yes\">Planck</italic> 2018, Pantheon of type Ia supernova, baryon acoustic oscillation, and <inline-formula>\u0000<tex-math><?CDATA $ H_0 $?></tex-math>\u0000<inline-graphic xlink:href=\"cpc_48_6_065102_M1.jpg\" xlink:type=\"simple\"></inline-graphic>\u0000</inline-formula> data from SH0ES. For the <italic toggle=\"yes\">ν</italic>Axi-EDE model, we obtain <inline-formula>\u0000<tex-math><?CDATA $sum m_{nu,mathrm{NH}}$?></tex-math>\u0000<inline-graphic xlink:href=\"cpc_48_6_065102_M2.jpg\" xlink:type=\"simple\"></inline-graphic>\u0000</inline-formula> < 0.152 eV and <inline-formula>\u0000<tex-math><?CDATA $sum m_{nu,mathrm{IH}}$?></tex-math>\u0000<inline-graphic xlink:href=\"cpc_48_6_065102_M3.jpg\" xlink:type=\"simple\"></inline-graphic>\u0000</inline-formula> < 0.178 eV, whereas for the <italic toggle=\"yes\">ν</italic>AdS-EDE model, we find <inline-formula>\u0000<tex-math><?CDATA $sum m_{nu,mathrm{NH}}$?></tex-math>\u0000<inline-graphic xlink:href=\"cpc_48_6_065102_M4.jpg\" xlink:type=\"simple\"></inline-graphic>\u0000</inline-formula> < 0.135 eV and <inline-formula>\u0000<tex-math><?CDATA $sum m_{nu,mathrm{IH}} $?></tex-math>\u0000<inline-graphic xlink:href=\"cpc_48_6_065102_M5.jpg\" xlink:type=\"simple\"></inline-graphic>\u0000</inline-formula> < 0.167 eV. Our results exhibit a preference for NH in both the <italic toggle=\"yes\">ν</italic>Axi-EDE and <italic toggle=\"yes\">ν</italic>AdS-EDE models.","PeriodicalId":10250,"journal":{"name":"中国物理C","volume":"45 1","pages":""},"PeriodicalIF":3.6,"publicationDate":"2024-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140830551","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
In this paper, we undertake a detailed study of real scalar inflation using LATTICEEASY simulations to investigate preheating phenomena. Generally, the scalar inflation potential with non-minimal coupling can be approximated using a quartic potential. We observe that the evolutionary behavior of this potential remains unaffected by the coupling coefficient. Furthermore, the theoretical predictions for the scalar spectral index ( ) and tensor-to-scalar power ratio (r) are independent of this coefficient. Consequently, the coefficients of this model are not constrained by Planck observations. Fortunately, the properties of preheating after inflation provide a viable approach to examining these coefficients. Through LATTICEEASY simulations, we trace the evolution of particle number density, scale factor, and energy density during the preheating process. Subsequently, we derive the parameters, such as the energy ratio (γ) and the e-folding number of preheating ( ), which facilitate further predictions of and r. We successfully validate real scalar inflation model using preheating in LATTICEEASY simulations based on the analytical relationship between preheating and inflation models.
{"title":"Constraints on real scalar inflation from preheating using LATTICEEASY*","authors":"Wei Cheng, 伟 程, Tong Qin, 通 秦, Jiujiang Jiang, 玖江 姜, Ruiyu Zhou and 瑞雨 周","doi":"10.1088/1674-1137/ad34bd","DOIUrl":"https://doi.org/10.1088/1674-1137/ad34bd","url":null,"abstract":"In this paper, we undertake a detailed study of real scalar inflation using LATTICEEASY simulations to investigate preheating phenomena. Generally, the scalar inflation potential with non-minimal coupling can be approximated using a quartic potential. We observe that the evolutionary behavior of this potential remains unaffected by the coupling coefficient. Furthermore, the theoretical predictions for the scalar spectral index ( ) and tensor-to-scalar power ratio (r) are independent of this coefficient. Consequently, the coefficients of this model are not constrained by Planck observations. Fortunately, the properties of preheating after inflation provide a viable approach to examining these coefficients. Through LATTICEEASY simulations, we trace the evolution of particle number density, scale factor, and energy density during the preheating process. Subsequently, we derive the parameters, such as the energy ratio (γ) and the e-folding number of preheating ( ), which facilitate further predictions of and r. We successfully validate real scalar inflation model using preheating in LATTICEEASY simulations based on the analytical relationship between preheating and inflation models.","PeriodicalId":10250,"journal":{"name":"中国物理C","volume":"38 1","pages":""},"PeriodicalIF":3.6,"publicationDate":"2024-05-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141194165","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2024-05-31DOI: 10.1088/1674-1137/ad33be
Xiu-Peng Yang, 秀鹏 杨, Bao-Fei Li, 瀑飞 李, Tao Zhu and 涛 朱
This study aims to investigate Lorentz/U(1) gauge symmetry-breaking electrodynamics in the framework of the standard-model extension and analyze the Hamiltonian structure for the theory with a specific dimension of Lorentz breaking operators. For this purpose, we consider a general quadratic action of the modified electrodynamics with Lorentz/gauge-breaking operators and calculate the number of independent components of the operators at different dimensions in gauge invariance and breaking. With this general action, we then analyze how Lorentz/gauge symmetry-breaking can change the Hamiltonian structure of the theories by considering Lorentz/gauge-breaking operators with dimension as examples. We show that the Lorentz-breaking operators with gauge invariance do not change the classes of the theory constrains and the number of physical degrees of freedom of the standard Maxwell electrodynamics. When U(1) gauge symmetry-breaking operators are present, the theories generally lack a first-class constraint and have one additional physical degree of freedom compared to the standard Maxwell electrodynamics.
{"title":"Electrodynamics with violations of Lorentz and U(1) gauge symmetries and their Hamiltonian structures*","authors":"Xiu-Peng Yang, 秀鹏 杨, Bao-Fei Li, 瀑飞 李, Tao Zhu and 涛 朱","doi":"10.1088/1674-1137/ad33be","DOIUrl":"https://doi.org/10.1088/1674-1137/ad33be","url":null,"abstract":"This study aims to investigate Lorentz/U(1) gauge symmetry-breaking electrodynamics in the framework of the standard-model extension and analyze the Hamiltonian structure for the theory with a specific dimension of Lorentz breaking operators. For this purpose, we consider a general quadratic action of the modified electrodynamics with Lorentz/gauge-breaking operators and calculate the number of independent components of the operators at different dimensions in gauge invariance and breaking. With this general action, we then analyze how Lorentz/gauge symmetry-breaking can change the Hamiltonian structure of the theories by considering Lorentz/gauge-breaking operators with dimension as examples. We show that the Lorentz-breaking operators with gauge invariance do not change the classes of the theory constrains and the number of physical degrees of freedom of the standard Maxwell electrodynamics. When U(1) gauge symmetry-breaking operators are present, the theories generally lack a first-class constraint and have one additional physical degree of freedom compared to the standard Maxwell electrodynamics.","PeriodicalId":10250,"journal":{"name":"中国物理C","volume":"122 1","pages":""},"PeriodicalIF":3.6,"publicationDate":"2024-05-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140812351","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Cluster radioactivity is studied within the generalized liquid drop model (GLDM), in which the shell correction energy, pairing energy, and cluster preformation factor are considered. The calculations show significant improvements and can reproduce the experimental data within a factor of 8.04 after considering these physical effects. In addition, the systematic trend of the cluster preformation factors is discussed in terms of the scheme to study the influence of the valence proton-neutron interaction and shell effect on cluster radioactivity. It is found that is linearly related to . This is in agreement with a recent study [L. Qi et al., Phys. Rev. C 108, 014325 (2023)], in which , obtained using different theoretical models and treatment methods than those used in this study, also had a linear relationship with . Combined with the work by Qi et al., this study suggests that the linear relationship between and is model-independent and both the shell effect and valence proton-neutron interaction play essential roles in cluster radioactivity. An analytical formula is proposed to calculate the cluster preformation factor based on the scheme. In addition, the cluster preformation factors and the cluster radioactivity half-lives of some heavy nuclei are predicted, which can provide a reference for future experiments.
{"title":"Systematic study of cluster radioactivity within the generalized liquid drop model*","authors":"Jun-Gang Deng, 军刚 邓, Jun-Hao Cheng, 俊皓 程, Xiao-Jun Bao, 小军 包, Hong-Fei Zhang and 鸿飞 张","doi":"10.1088/1674-1137/ad30ef","DOIUrl":"https://doi.org/10.1088/1674-1137/ad30ef","url":null,"abstract":"Cluster radioactivity is studied within the generalized liquid drop model (GLDM), in which the shell correction energy, pairing energy, and cluster preformation factor are considered. The calculations show significant improvements and can reproduce the experimental data within a factor of 8.04 after considering these physical effects. In addition, the systematic trend of the cluster preformation factors is discussed in terms of the scheme to study the influence of the valence proton-neutron interaction and shell effect on cluster radioactivity. It is found that is linearly related to . This is in agreement with a recent study [L. Qi et al., Phys. Rev. C 108, 014325 (2023)], in which , obtained using different theoretical models and treatment methods than those used in this study, also had a linear relationship with . Combined with the work by Qi et al., this study suggests that the linear relationship between and is model-independent and both the shell effect and valence proton-neutron interaction play essential roles in cluster radioactivity. An analytical formula is proposed to calculate the cluster preformation factor based on the scheme. In addition, the cluster preformation factors and the cluster radioactivity half-lives of some heavy nuclei are predicted, which can provide a reference for future experiments.","PeriodicalId":10250,"journal":{"name":"中国物理C","volume":"103 1","pages":""},"PeriodicalIF":3.6,"publicationDate":"2024-05-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140812352","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
The full array of the Large High Altitude Air Shower Observatory (LHAASO) has been in operation since July 2021. For its kilometer-square array (KM2A), we optimized the selection criteria for very high and ultra-high energy γ-rays using data collected from August 2021 to August 2022, resulting in an improvement in significance of the detection in the Crab Nebula of approximately 15%, compared with that of previous cuts. With the implementation of these new selection criteria, the angular resolution was also significantly improved by approximately 10% at tens of TeV. Other aspects of the full KM2A array performance, such as the pointing error, were also calibrated using the Crab Nebula. The resulting energy spectrum of the Crab Nebula in the energy range of 10-1000 TeV are well fitted by a log-parabola model, which is consistent with the previous results from LHAASO and other experiments.
大型高空气流淋浴观测台（LHAASO）的全阵列已于 2021 年 7 月开始运行。对于其千米方阵（KM2A），我们利用2021年8月至2022年8月收集的数据优化了对极高能和超高能γ射线的选择标准，结果蟹状星云的探测显著性比以前的切割提高了约15%。随着这些新选择标准的实施，在数十 TeV 的角度分辨率也显著提高了约 10%。KM2A全阵列性能的其他方面，例如指向误差，也利用蟹状星云进行了校准。蟹状星云在10-1000 TeV能量范围内的能谱结果被对数抛物线模型很好地拟合，这与LHAASO和其他实验之前的结果是一致的。
{"title":"Optimization of performance of the KM2A full array using the Crab Nebula*","authors":"Zhen Cao, 臻 曹, F. Aharonian, Q. An, 琪 安, Axikegu, 克古 阿西, Y.X. Bai, 云翔 白, Y.W. Bao, 逸炜 包, D. Bastieri, X.J. Bi, 效军 毕, Y.J. Bi, 玉江 毕, J.T. Cai, 金庭 蔡, Q. Cao, 晴 曹, W.Y. Cao, 文羽 曹, Zhe Cao, 喆 曹, J. Chang, 进 常, J.F. Chang, 劲帆 常, A.M. Chen, 尚明 陈, E.S. Chen, 恩生 陈, Liang Chen, 亮 陈, Lin Chen, 林 陈, Long Chen, 龙 陈, M.J. Chen, 明君 陈, M.L. Chen, 玛丽 陈, Q.H. Chen, 起辉 陈, S.H. Chen, 素弘 陈, T.L. Chen, 天禄 陈, Y. Chen, 阳 陈, N. Cheng, 宁 程, Y.D. Cheng, 耀东 程, M.Y. Cui, 明阳 崔, S.W. Cui, 树旺 崔, X.H. Cui, 晓红 崔, Y.D. Cui, 昱东 崔, B.Z. Dai, 本忠 戴, H.L. Dai, 洪亮 代, Z.G. Dai, 子高 戴, Danzengluobu, 罗布 单增, D. della Volpe, X.Q. Dong, 绪强 董, K.K. Duan, 凯凯 段, J.H. Fan, 军辉 樊, Y.Z. Fan, 一中 范, J. Fang, 军 方, K. Fang, 堃 方, C.F. Feng, 存峰 冯, L. Feng, 莉 封, S.H. Feng, 少辉 冯, X.T. Feng, 晓婷 丰, Y.L. Feng, 有亮 冯, S. Gabici, B. Gao, 博 高, C.D. Gao, 川东 高, L.Q. Gao, 林青 高, Q. Gao, 启 高, W. Gao, 卫 高, W.K. Gao, 伟康 高, M.M. Ge, 茂茂 葛, L.S. Geng, 利斯 耿, G. Giacinti, G.H. Gong, 光华 龚, Q.B. Gou, 全补 苟, M.H. Gu, 旻皓 顾, F.L. Guo, 福来 郭, X.L. Guo, 晓磊 郭, Y.Q...","doi":"10.1088/1674-1137/ad2e82","DOIUrl":"https://doi.org/10.1088/1674-1137/ad2e82","url":null,"abstract":"The full array of the Large High Altitude Air Shower Observatory (LHAASO) has been in operation since July 2021. For its kilometer-square array (KM2A), we optimized the selection criteria for very high and ultra-high energy γ-rays using data collected from August 2021 to August 2022, resulting in an improvement in significance of the detection in the Crab Nebula of approximately 15%, compared with that of previous cuts. With the implementation of these new selection criteria, the angular resolution was also significantly improved by approximately 10% at tens of TeV. Other aspects of the full KM2A array performance, such as the pointing error, were also calibrated using the Crab Nebula. The resulting energy spectrum of the Crab Nebula in the energy range of 10-1000 TeV are well fitted by a log-parabola model, which is consistent with the previous results from LHAASO and other experiments.","PeriodicalId":10250,"journal":{"name":"中国物理C","volume":"64 1","pages":""},"PeriodicalIF":3.6,"publicationDate":"2024-05-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141059258","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":2,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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