ABSTRACT
Gravitational waves from a merger of two neutron stars (NSs) were discovered for the first time in GW170817, together with diverse electromagnetic counterparts, providing a direct clue to ...the origin of short gamma-ray bursts (sGRBs). The associated sGRB 170817A was much fainter than typical, suggesting off-axis emission from a relativistic jet. However the observed prompt spectrum is inconsistent with the spectral (Amati) relation and causes the compactness problem in the simplest off-axis model. We suggest that this spectral and energetic puzzle of GRB170817A is explained if the origin of the off-axis emission arises from the off-centre jet. This emission location is generally created by the product of the rapidly declining (with angle) jet energy and the increasing beaming term. Hence the region of most luminous emission for an off-axis observer is neither the jet core around the primary axis, nor the line of sight at the viewing angle. The off-centre jet could be loaded with baryon or cocoon. The off-axis model predicts that roughly ${\sim } 10{{\ \rm per\ cent}}$ events are brighter at smaller viewing angles than sGRB 170817A, although the exact event rate sensitively depends on uncertainties of the off-centre structure. The model also predicts outliers to Amati relation, providing future tests to reveal the central engine activities.
It is generally known that the lymph nodes (LNs) are important tissues in cancer immunotherapy. Therefore, delivering immune functional compounds to LNs is a useful strategy for enhancing cancer ...immunotherapy. Lipid-based nanocarriers have been widely used as delivery systems that target LNs, but lipid nanoparticle (LNP) technology has recently attracted increased interest. High levels of nucleic acids can be efficiently loaded in LNPs, they can be used to actively deliver nucleic acids into the cytoplasm, and they can be produced on an industrial scale. The use of microfluidic devices has been particularly valuable for producing small-sized LNPs, thus paving the way for successful LN targeting. In the review, we focus on the potential of LNP technology for targeting LNs.
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For 0<a≤1/2, we define the quadrilateral zeta function Q(s,a) using the Hurwitz and periodic zeta functions and show that Q(s,a) satisfies Riemann's functional equation studied by Hamburger, Heck and ...Knopp. Moreover, we prove that for any 0<a≤1/2, there exist positive constants A(a) and T0(a) such that the number of zeros of the quadrilateral zeta function Q(s,a) on the line segment from 1/2 to 1/2+iT is greater than A(a)T whenever T≥T0(a).
ABSTRACT
We performed Population III (Pop III) binary evolution using population synthesis simulations for seven different models. We found that Pop III binaries tend to be binary black holes (BBHs) ...with chirp mass Mchirp ∼ 30 M⊙ and they can merge in the present day, due to a long merger time. The merger rate densities of Pop III BBHs at z = 0 are in the range 3.34–21.2 $\rm yr^{-1}\,Gpc^{-3}$ which is consistent with the Advanced Laser Interferometer Gravitational Wave Observatory (aLIGO)/Advanced Virgo (aVIRGO) result of 9.7–101 $\rm yr^{-1}\,Gpc^{-3}$. These Pop III binaries might contribute some portion of the massive BBH gravitational wave (GW) sources detected by aLIGO/aVIRGO. We also calculated the redshift dependence of Pop III BBH mergers. We found that Pop III low-spin BBHs tend to merge at low redshift, while Pop III high-spin BBHs merge at high redshift, which can be confirmed by future GW detectors such as Einstein Telescope (ET), Cosmic Explorer (CE), and DECi-hertz Interferometer Gravitational wave Observatory (DECIGO). These detectors can also check the redshift dependence of the BBH merger rate and spin distribution. Our results show that, except for one model, the mean effective spin 〈χeff〉 at z = 0 lies in the range 0.02–0.3, while at z = 10 it is 0.16–0.64. Therefore, massive stellar-mass BBH detection by GWs will be key for stellar evolution study in the early Universe.
For 0<a≤1, s,z∈C and 0<|z|≤1, the Hurwitz–Lerch zeta function is defined by Φ(s,a,z):=∑n=0∞zn(n+a)−s when σ:=ℜ(s)>1. In this paper, we show that Φ(σ,a,z)≠0 when σ∈(−1,0) if and only if I z=1 and ...(3−3)/6≤a≤1/2 or (3+3)/6≤a≤1, II z∈−1,1) and (1−z)(1−a)≤1, III z∉R and 0<a≤1. In addition, we give a new proof of the functional equation of Φ(s,a,z).
In the present paper, we give bounds for the Tornheim double zeta function T(s_1,s_2,s_3) when \lvert t_1 \rvert , \lvert t_2 \rvert , \lvert t_3 \rvert \ge 1, \lvert t_1 + t_2 \rvert , \lvert t_2 + ...t_3 \rvert , \lvert t_3 + t_1 \rvert \ge 1 and \lvert t_1 + t_2 + t_3 \rvert \ge 1 with \sigma _1 , \sigma _2, \sigma _3 > -K and \sigma _1 +\sigma _2, \sigma _2 + \sigma _3, \sigma _3 + \sigma _1 > 1-K, where K is a positive integer, from bounds for the Hurwitz zeta function which are shown by Bourgain’s bounds for exponential sums.
Celotno besedilo
Dostopno za:
DOBA, IZUM, KILJ, NUK, PILJ, PNG, SAZU, SIK, UILJ, UKNU, UL, UM, UPUK
Using our population synthesis code, we found that the typical chirp mass defined by (m
1
m
2)3/5/(m
1 + m
2)1/5 of Population III (Pop III) binary black holes (BH–BHs) is ∼30 M⊙ with the total mass ...of ∼60 M⊙ so that the inspiral chirp signal as well as quasi-normal mode (QNM) of the merging black hole (BH) are interesting targets of KAGRA. The detection rate of the coalescing Pop III BH–BHs is ∼180 events yr− 1 (SFR
p/(10−2.5 M⊙ yr−1 Mpc−3))(f
b/(1 + f
b)/0.33)Err
sys in our standard model, where SFR
p, f
b and Err
sys are the peak value of the Pop III star formation rate, the binary fraction and the systematic error with Err
sys = 1 for our standard model, respectively. To evaluate the robustness of chirp mass distribution and the range of Err
sys, we examine the dependence of the results on the unknown parameters and the distribution functions in the population synthesis code. We found that the chirp mass has a peak at ∼30 M⊙ in most of parameters and distribution functions as well as Err
sys ranges from 0.046 to 4. Therefore, the detection rate of the coalescing Pop III BH–BHs ranges about 8.3-720 events yr− 1(SFR
p/(10− 2.5 M⊙ yr− 1 Mpc− 3))(f
b/(1 + f
b)/0.33). The minimum rate corresponds to the worst model which we think unlikely so that unless (SFR
p/(10− 2.5 M⊙ yr− 1 Mpc− 3))(f
b/(1 + f
b)/0.33) ≪ 0.1, we expect the Pop III BH–BHs merger rate of at least one event per year by KAGRA. Nakano, Tanaka & Nakamura show that if signal-to-noise ratio (S/N) of QNM is larger than 35, we can confirm or refute the general relativity (GR) more than 5σ level. In our standard model, the detection rate of Pop III BH–BHs whose S/N is larger than 35 is 3.2 events yr− 1 (SFR
p/(10− 2.5 M⊙ yr− 1 Mpc− 3))(f
b/(1 + f
b)/0.33)Err
sys. Thus, there is a good chance to check whether GR is correct or not in the strong gravity region.
Current status of zirconia restoration Miyazaki, Takashi; Nakamura, Takashi; Matsumura, Hideo ...
Journal of prosthodontic research,
10/2013, Letnik:
57, Številka:
4
Journal Article
Recenzirano
Odprti dostop
During the past decade, zirconia-based ceramics have been successfully introduced into the clinic to fabricate fixed dental prostheses (FDPs), along with a dental computer-aided/computer-aided ...manufacturing (CAD/CAM) system. In this article (1) development of dental ceramics, (2) the current status of dental CAD/CAM systems, (3) CAD/CAM and zirconia restoration, (4) bond between zirconia and veneering ceramics, (5) bond of zirconia with resin-based luting agents, (6) surface finish of zirconia restoration and antagonist enamel wear, and (7) clinical evaluation of zirconia restoration are reviewed.
Yttria partially stabilized tetragonal zirconia polycrystalline (Y-TZP) showed better mechanical properties and superior resistance to fracture than other conventional dental ceramics. Furthermore, ceria-stabilized tetragonal zirconia polycrystalline and alumina nanocomposites (Ce-TZP/A) had the highest fracture toughness and had resistance to low-temperature aging degradation. Both zirconia-based ceramics have been clinically available as an alternative to the metal framework for fixed dental prostheses (FDPs). Marginal adaptation of zirconia-based FDPs is acceptable for clinical application. The most frequent clinical complication with zirconia-based FDPs was chipping of the veneering porcelain that was affected by many factors. The mechanism for the bonding between zirconia and veneering ceramics remains unknown. There was no clear evidence of chemical bonding and the bond strength between zirconia and porcelain was lower than that between metal and porcelain.
There were two alternatives proposed that might avoid chipping of veneering porcelains. One was hybrid-structured FDPs comprising CAD/CAM-fabricated porcelain parts adhering to a CAD/CAM fabricated zirconia framework. Another option was full-contour zirconia FDPs using high translucent zirconia. Combined application of silica coating and/or silane coupler, and 10-methacryloyloxydecyl dihydrogen phosphate is currently one of the most reliable bonding systems for zirconia. Adhesive treatments could be applied to luting the restorations and fabricating hybrid-structured FDPs. Full-contour zirconia FDPs caused concern about the wear of antagonist enamel, because the hardness of Y-TZP was over double that of porcelain. However, this review demonstrates that highly polished zirconia yielded lower antagonist wear compared with porcelains. Polishing of zirconia is possible, but glazing is not recommended for the surface finish of zirconia.
Clinical data since 2010 are included in this review. The zirconia frameworks rarely got damaged in many cases and complications often occurred in the veneering ceramic materials. Further clinical studies with larger sample sizes and longer follow-up periods are required to investigate the possible influencing factors of technical failures.
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