Lei(Layla) Li

The first mitochondrial genome of Ophiocara porocephala was determined by the combination of next-generation sequencing (NGS) and Sanger sequencing methods. A complete circular mitogenome of O. porocephala (16,529 bp) consisted of 13 protein-coding genes, 22 transfer RNAs, two ribosomal RNAs, and two non-coding regions, including a control region (D-loop) and a light strand origin of replication (OL). Two start codons (ATG and GTG) and four stop codons (TAG, TAA, TA–, and T–) were used in all the PCGs. Except for ND6 and eight transfer RNAs (tRNAs), all the other genes were encoded in the heavy strand. Based on phylogenetic analysis, O. porocephala formed a clade with three other species in the subfamily Butinae, while the other 10 made a subfamily Eleotrinae clade.

GRB 230430A: A short GRB from a neutron star merger. - NASA/ADS Now on home page ads icon ads Enable full ADS view NASA/ADS GRB 230430A: A short GRB from a neutron star merger. Ruffini, R. ; Aimuratov, Y. ; Becerra, L. ; Bianco, CL ; Cherubini, C. ; Filippi, S. ; Karlica, M. ; Li, L. ; Moradi, R. ; Nia, FR ; Rueda, JA ; Sahakyan, N. ; Wang, Y. ; Xue, SS Abstract Publication: GRB Coordinates Network Pub Date: 2023 Bibcode: 2023GCN.33723....1R full text sources Publisher | © The SAO/NASA Astrophysics Data System adshelp[at]cfa.harvard.edu The ADS is operated by the Smithsonian Astrophysical Observatory under NASA Cooperative Agreement NNX16AC86A NASA logo Smithsonian logo Resources About ADS ADS Help What's New Careers@ADS Social @adsabs ADS Blog Project Switch to full ADS Is ADS down? (or is it just me...) Smithsonian Institution Smithsonian Privacy Notice Smithsonian Terms …

Callisto, the outermost of the four Galilean satellites, is a key body to answer present questions about the origin and the formation of the Jovian system. It appears to be the least differentiated and the least geologically evolved of the Galilean satellites, and therefore the one best reflecting the early ages of the Jovian system. The Tianwen-4 mission (CNSA) is in his early preparation stage to explore this system, and to go in orbit around Callisto.We perform a closed-loop simulation of spacecraft tracking (2-way Doppler), altimetry, and accelerometer data of a high inclination, low altitude orbiter. We first use Doppler data only to recover its precise orbit and Callisto’s geodetic parameters, eg, gravity field, rotation, and orientation parameters and the k2 tidal Love number. We consider several ways to mitigate the mismodeling of non-gravitational accelerations, such as using empirical accelerations and pseudo stochastic pulses, and we evaluate the benefits of an on-board accelerometer.

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Quantum-correlated D Dpairs collected by the BESIII experiment at the ψ (3770) resonance corresponding to an integrated luminosity of 2.93 fb− 1 are used to study the D 0→ K S 0 π+ π− π 0 decay mode. The C P-even fraction of D 0→ K S 0 π+ π− π 0 decays is determined to be 0.235±0.010±0.002, where the first uncertainty is statistical and the second is systematic.

Using data samples of e+ e− collisions collected with the BESIII detector at eight center-of-mass energy points between 3.49 and 3.67 GeV, corresponding to an integrated luminosity of 670 pb− 1, we present the upper limits of Born cross sections and the effective form factor for the process e+ e−→ Ω− Ω+. A fit to the cross sections using a perturbative QCD-derived energy-dependent function shows no significant threshold effect. The upper limit on the measured effective form factor is consistent with a theoretical prediction within the uncertainty of 1 σ. These results provide new experimental information on the production mechanism of Ω.

Localized increases in neuronal activity are supported by the hemodynamic response, which delivers oxygen to the brain tissue to support synaptic functions, action potentials and other neuronal processes. However, it remains unknown if changes in baseline neuronal activity, which are expected to reflect neuronal metabolic demand, alter the relationship between the local hemodynamic and oxygen behaviour. In order to better characterize this system, we examine here the relationship between brain tissue oxygen (PO2) and hemodynamic responses (BOLD functional MRI) under different levels of neuronal activity. By comparing the stimulus-evoked responses during different levels of baseline neuronal activity, the awake state vs isoflurane anesthesia, we were able to measure how a known change in neuronal demand affected tissue PO2 as well as the hemodynamic response to stimulation. We observed a high …

By analyzing an e+ e− data sample corresponding to an integrated luminosity of 2.93 fb− 1 taken at a center-of-mass energy of 3.773 GeV with the BESIII detector, we measure the branching fractions of the Cabibbo-favored hadronic decays D 0→ K− π+ η′, D 0→ K S 0 π 0 η′, and D+→ K S 0 π+ η′, which are determined to be (6.43±0.1 5 stat±0.3 1 syst)× 10− 3,(2.52±0.2 2 stat±0.1 5 syst)× 10− 3, and (1.90±0.1 7 stat±0.1 3 syst)× 10− 3, respectively. The precision of the branching fraction of D 0→ K− π+ η′ is significantly improved, and the processes D 0→ K S 0 π 0 η′ and D+→ K S 0 π+ η′ are observed for the first time.

Callisto and Europa: a simulation study for gravity field determination from orbit tracking data Page 1 source: https://doi.org/10.48350/172535 | downloaded: 5.9.2022 Astronomical Institute University of Bern Callisto and Europa: a simulation study for gravity field determination from orbit tracking data (1) Astronomical Institute, University of Bern, Switzerland, (2) University of Maryland, Baltimore County, USA, (3) NASA Goddard Space Flight Center, (4) IRAP, CNRS-Université Paul Sabatier, Toulouse, France, (5) NSSC, Beijing, China, (6), European Space Agency W. Desprats (1), D. Arnold (1), S. Bertone (2,3), M. Blanc (4), A. Jäggi (1), M. Li (5), L. Lei (5), and O. Witasse (6) (william.desprats@aiub.unibe.ch) PSD.1: Satellite dynamics: new developments and challenged for Earth and solar system sciences Page 2 Slide 2 / 17 Astronomical Institute University of Bern Europa & Callisto Radius 1561 km 2410 km Mass …

The radiative hyperon decay Λ→ n γ is studied using (10087±44)× 10 6 J/ψ events collected with the BESIII detector operating at BEPCII. The absolute branching fraction of the decay Λ→ n γ is determined to be (0.832±0.03 8 stat±0.05 4 syst)× 10− 3, which is a factor of 2.1 lower and 5.6 standard deviations different than the previous measurement. By analyzing the joint angular distribution of the decay products, the first determination of the decay asymmetry α γ is reported with a value of− 0.16±0.1 0 stat±0.0 5 syst.

GRB 220101A, first detected by Swift (Tohuvavohu et al., GCN 31347) with redshift z= 4.618 (Fu et al 2022., GCN 31353; Fynbo et al 2022., GCN 31359) and energy of 3.7 E54 (J.-L. Atteia 2022, GCN 31365) is categorized as a BdHN I with the most powerful and the highest ever observed X-ray afterglow luminosity in 26 years, as well as the highest supernova rise (SN-rise) and the new neutron star rise (vNS-rise)(Ruffini et al. 2021 MNRAS, 504, 5301) see Fig. 1. There is evidence for the ultrarelativistic prompt emission (UPE) phase (Moradi et al. 2021 PRD 104, 063043). We encourage optical and radio observations to identify the corresponding UPE phase as well as the synchrotron emission originating from the spinning vNS. Fig. 1: http://www. icranet. org/figure1. pdf

Prognostic factor analysis refers to the adjustment of covariates when comparing treatments in a randomized clinical trial. This chapter covers various methodological issues related to prognostic factor analysis, including its importance to the randomization and primary analysis of the trial, statistical model building, selection of prognostic factors, and the study of interactions and subgroups, among others. Methodological discussion is illustrated with data examples, and some commonly made mistakes in statistical practice are identified and discussed. This chapter is intended to provide readers with practical advice on how to use prognostic factors in the design, analysis, and reporting of randomized clinical trials.

We confirm the results of our previous GCN (Ruffini et al. 2022, GCN 31465). Following the release of the X-ray afterglow (Tohuvavohu et al. 2022, GCN 31347) and the GeV data (Arimoto et al. 2022, GCN 31350) of this source, we can estimate the total (keV+ MeV+ GeV) isotropic energy (see eg Ruffini et al. 2021, MNRAS 504, 5301) to be~ 6E54 erg, making this GRB the most powerful GRB in 26 years (a" Petanova"). The period of the new neutron star (see eg Ruffini et al. 2021, MNRAS 504, 5301) generating the X-ray afterglow is~ 1 ms, the initial mass of the BH (see eg Ruffini et al. 2019 ApJ 886, 82) is 6.15 solar mass, the spin parameter is 0.95, and the irreducible mass is 4.98 solar masses (see Fig. 1). The peak of the bolometric flux of supernova is of the order of 1E-17 erg/s/cm^ 2 and will appear in 73+/-15 days after the GRB trigger, with emissions lasting~ one month peaking in different infrared bands. The …

In the binary-driven hypernova (BdHN) scenario, long gamma-ray bursts (GRBs) originate in a cataclysmic event that occurs in a binary system composed of a carbon-oxygen (CO) star and a neutron star (NS) companion in close orbit. The collapse of the CO star generates at its center a newborn NS (ν NS), and a supernova (SN) explosion. Matter from the ejecta is accreted both onto the ν NS because of fallback and onto the NS companion, leading to the collapse of the latter into a black hole (BH). Each of the ingredients of the above system leads to observable emission episodes in a GRB. In particular, the ν NS is expected to show up (hereafter ν NS− rise) in the early GRB emission, nearly contemporary or superimposed to the ultrarelativistic prompt emission (UPE) phase, but with a different spectral signature. Following the ν NS− rise, the ν NS powers the afterglow emission by injecting energy into the expanding …

Rationale & ObjectiveEvaluating repeated measures of estimated glomerular filtration rate (eGFR) and urinary protein-creatinine ratio (UPCR) over time may enhance our ability to understand the association between changes in kidney parameters and cardiovascular disease risk.Study DesignProspective cohort study.Setting & ParticipantsAnnual visit data from 2,438 participants in the Chronic Renal Insufficiency Cohort (CRIC).ExposuresAverage and slope of eGFR and UPCR in time-updated, 1-year exposure windows.OutcomesIncident heart failure, atherosclerotic cardiovascular disease events, death, and a composite of incident heart failure, atherosclerotic cardiovascular disease events, and death.Analytical ApproachA landmark analysis, a dynamic approach to survival modeling that leverages longitudinal, iterative profiles of laboratory and clinical information to assess the time-updated 3-year risk of adverse …

LM Gu (谷立民) 35 MH Gu (顾旻皓) 1, 50 C. Y Guan (关春懿) 1, 55 AQ Guo (郭爱强) 22 AQ Guo (郭爱强) 25 LB Guo (郭立波) 34 RP Guo (郭如盼) 41 YP Guo (郭玉萍) 9, f A. Guskov29, a TT Han (韩婷婷) 42 WY Han (韩文颖) 32 XQ Hao (郝喜庆) 15 FA Harris57 KK He (何凯凯) 47

Branching fraction and effective lifetime measurements of the rare decay B s 0→ μ+ μ− and searches for the decays B 0→ μ+ μ− and B s 0→ μ+ μ− γ are reported using proton-proton collision data collected with the LHCb detector at center-of-mass energies of 7, 8, and 13 TeV, corresponding to a luminosity of 9 fb− 1. The branching fraction B (B s 0→ μ+ μ−)=(3.0 9− 0.43− 0.11+ 0.46+ 0.15)× 10− 9 and the effective lifetime τ (B s 0→ μ+ μ−)= 2.07±0.29±0.03 ps are measured, where the first uncertainty is statistical and the second systematic. No significant signal for B 0→ μ+ μ− and B s 0→ μ+ μ− γ decays is found and upper limits B (B 0→ μ+ μ−)< 2.6× 10− 10 and B (B s 0→ μ+ μ− γ)< 2.0× 10− 9 at the 95% CL are determined, where the latter is limited to the range m μ μ> 4.9 GeV/c 2. The results are in agreement with the standard model expectations.

LHAASO observed more than 5000 very high energy (VHE) photons in GRB 221009A, with the highest energy reaching 18 TeV (GCN 32677). Previously, high energy TeV emissions were also observed in GRB 180720B (Abdalla et al. 2019), 190114C (MAGIC Collaboration 2019), 190829A (HESS Collaboration 2021) and 201216C (Blanch et al. GCN 29075). A common feature of these bursts is that the TeV light-curve follows a power-law decay with a similar index as the X-ray light-curve, and the TeV luminosity is tens of percent of the X-ray luminosity (see attached figure 1 and the references of Abdalla et al. 2019, MAGIC Collaboration 2019 and HESS Collaboration 2021, Ruffini et al. 2021, Rueda et al. 2022, Rastegarnia et al. 2022, Wang et al. 2022). Here we present the X-ray light-curve of GRB 221009A observed by Swift-XRT (GCN 32651), and the t0 is taken from the Fermi-GBM trigger time (GCN 32636 …

Mesons comprising a beauty quark and strange quark can oscillate between particle () and antiparticle () flavour eigenstates, with a frequency given by the mass difference between heavy and light mass eigenstates, Δms. Here we present a measurement of Δms using π+ decays produced in proton–proton collisions collected with the LHCb detector at the Large Hadron Collider. The oscillation frequency is found to be Δms = 17.7683 ± 0.0051 ± 0.0032 ps−1, where the first uncertainty is statistical and the second is systematic. This measurement improves on the current Δms precision by a factor of two. We combine this result with previous LHCb measurements to determine Δms = 17.7656 ± 0.0057 ps−1, which is the legacy measurement of the original LHCb detector.

GRB 220527A is observed by AGILE (Ursi et al. 2022, GCN 32129), Fermi (GCN 32130, Bissaldi et al. 2022, GCN 32131, Mangan et al. 2022, GCN 32133), Swift (B. Sbarufatti et al. 2022 GCN 32135, A. Tohuvavohu. 2022, GCN 32136), CALET (Yamaoka et al. 2022, GCN 32139), AstroSat (Gopalakrishnan et al. 2022, GCN 32140), and Konus-Wind (Lysenko et al. 2022, GCN 32152). With the redshift z= 0.857 of GRB 220527A (D. Xu et al. 2022, GCN 32141), the isotropic energy of this GRB in 10 keV-10 MeV, and 20 keV-16 MeV ranges are E_iso=(2.60+-0.14) x10^{53} erg, and E_iso= 1.22 (-0.06,+ 0.07) x10^{53} erg, respectively (A. Lysenko et al. 2022, GCN 32152). The ultra-relativistic prompt emission phase of this GRB, originating from the over-criticl electric field around the black hole (Moradi et al 2021, Phys. Rev. D 104, 063043) extends from rest-frame time of 3.7 s to 5.4 s. The UPE phase is best fitted by a …