Testing the Universal Structured Jet Models of Gamma-Ray Bursts by BATSE Observations

Assuming that the observed gamma-ray burst (GRB) rate as a function of redshift is proportional to a corrected star formation rate, we derive the empirical distribution of the viewing angles of long BATSE GRBs, $P^{\rm em}(\theta)$, and the distribution of these bursts in the plane of $\theta$ against redshift, $P^{\rm em}(\theta, z)$, by using a tight correlation between $E_{\gamma}$) and $E_{\rm p}^{'}$). Our results show that $P^{\rm em}(\theta)$ is well fitted by a log-normal distribution centering at $\log \theta/{\rm rad}=-0.76$ with a width of $\sigma_{\log \theta}=0.57$. We test different universal structured jet models by comparing model predictions with our empirical results. To make the comparisons reasonable, an "effective" threshold, which corresponds to the sample selection criteria of the long GRB sample, is used. We find that the predictions of a two-Gaussian jet model are roughly consistent with our empirical results. A brief discussion shows that cosmological effect on the $E_{\gamma}-E_{\rm p}^{'}$ relation does not significantly affect our results, but sample selection effects on this relationship might significantly influence our results.Comment: 5 pages, 6 figures, accepted for publication in A

Identification of Two categories of optically bright gamma-ray bursts

We present the results of a systematical analysis of the intrinsic optical afterglow light curves for a complete sample of gamma-ray bursts (GRBs) observed in the period from Feb. 1997 to Aug. 2005. These light curves are generally well-sampled, with at least four detections in the $R$ band. The redshifts of all the bursts in the sample are available. We derive the intrinsic $R$ band afterglow lightcurves (luminosity versus time within the cosmic proper rest frame) for these GRBs, and discover a fact that they essentially follow two universal tracks after 2 hours since the GRB triggers. The optical luminosities at 1 day show a clear bimodal distribution, peaking at 1.4*10^{46} ergs~s^{-1} for the luminous group and 5.3*10^{44} ergs~s^{-1} for the dim group. About 75% of the GRBs are in the luminous group, and the other 25% belong to the dim group. While the luminous group has a wide range of redshift distribution, the bursts in the dim group all appear at a redshift lower than 1.1.Comment: 10 pages, 2 figures, emulateapj style, accepted for publication by ApJ Letter

The Jet Composition of GRB 230307A: Poynting-Flux-Dominated Outflow?

The jet composition of GRB plays an important role in understanding the energy dissipation and radiation mechanisms in GRB physics, but it is poorly constrained from the observational data. Recently, an interesting long-duration GRB 230307A with redshift $z=$0.065 has attracted great attention. The lack of detected thermal emission and mini-structure of prompt emission lightcurve of this burst suggest that the outflow is Poynting-flux-dominated and point towards the ICMART model. In this paper, we invoke two independent methods to investigate the jet composition of GRB 230307A. The high magnetization parameter ($\sigma>7$ or ever large) for$R_0=10^{10}$ cm that is used to suppress thermal component, strongly suggests that a significant fraction of the outflow energy is likely in a Poynting flux entrained with the baryonic matter. Moreover, it is found that the radiation efficiency of this burst for typical values $\epsilon_e=0.1$ and $\epsilon_B=0.01$ can reach as high as $~50\%$ which disfavors the internal shock model, but is consistent with ICMART model. Finally, a possible unified picture to produce GRB 230307A originated from a compact star merger is also discussed.Comment: 6 pages, 2 figures, 1 table, updated references, and matched with the published veriso

Plant geographic phenotypic variation drives diversification in its associated community of a phytophagous insect and its parasitoids

International audienceBackground: While the communities constituted by phytophageous insects and their parasites may represent half of all terrestrial animal species, understanding their diversification remains a major challenge. A neglected idea is that geographic phenotypic variation in a host plant may lead to heterogeneous evolutionary responses of the different members of the associated communities. This could result in diversification on a host plant by ecological speciation in some species, leading to geographic variation in community composition. In this study we investigated geographic variation of inflorescence receptacle size in a plant, Ficus hirta, and how the hymenopteran community feeding in the inflorescences has responded. Our predictions were:1) Inflorescence size variation affects wasp species differently depending on how they access oviposition sites.2) In some affected lineages of wasps, we may observe vicariant, parapatric species adapted to different inflorescence sizes.Results: We show that fig (the enclosed inflorescence of Ficus) wall thickness varies geographically. The fig-entering pollinating wasp was not affected, while the parasites ovipositing through the fig wall were. Two parapatric species of Philotrypesis, exhibiting strikingly different ovipositor lengths, were recorded. One species of Sycoscapter was also present, and it was restricted, like the shorter-ovipositor Philotrypesis, to the geographic zone where fig walls were thinner.Conclusions: Previous work on fig wasps suggested that parapatric geographic ranges among congenerics were due to adaptation to variation in abiotic factors, complemented by interspecific competition. Our results show that parapatric ranges may also result from adaptation to variation in biotic factors. Within an insect community, differences among species in their response to geographic phenotypic variation of their host plant may result in geographically heterogeneous community structure. Such heterogeneity leads to heterogeneous interaction networks among sites. Our results support the hypothesis that plant geographic phenotypic variation can be a driver of diversification in associated insect communities, and can complement other diversification processes

Influences of tilted thin accretion disks on the optical appearance of hairy black holes in Horndeski gravity

Research on the optical appearance of black holes, both in general relativity and modified gravity, has been in full swing since the Event Horizon Telescope Collaboration announced photos of M87$^{*}$ and Sagittarius A$^{*}$. Nevertheless, limited attention has been given to the impact of tilted accretion disks on black hole images. This paper investigates the $230$ GHz images of non-rotating hairy black holes illuminated by tilted, thin accretion disks in Horndeski gravity with the aid of a ray tracing method. The results indicate that reducing the scalar hair parameter effectively diminishes image luminosity and extends both the critical curve and the inner shadow. This trend facilitates the differentiation between hairy black holes and Schwarzschild black holes. Furthermore, we observe that the inclination of the tilted accretion disk can mimic the observation angle, consequently affecting image brightness and the morphology of the inner shadow. In specific parameter spaces, the disk inclination has the ability to shift the position of the light spot in the images of hairy black holes. This finding may provide potential theoretical evidence for the formation of three flares at different positions in the Sagittarius A$^{*}$ image. Additionally, by examining the images of hairy black holes surrounded by two thin accretion disks, we report the obscuring effect of the accretion environment on the inner shadow of the black hole.Comment: 26 pages, 14 figure

The progenitor and central engine of a peculiar GRB 230307A

Recently, a lack of supernova-associated long-duration gamma-ray burst (GRB 230307A) at such a low redshift $z=0.065$, but associated with a possible kilonova emission, has attracted great attention. Its heavy element nucleosynthesis and the characteristic of soft X-ray emission suggests that the central engine of GRB 230307A is magnetar which is originated from a binary compact star merger. The calculated lower value of $\varepsilon \sim 0.05$ suggests that the GRB 230307A seems to be with ambiguous progenitor. The lower value of $f_{\rm eff}=1.23$ implies that the GRB 230307A is not likely to be from the effect of "tip of iceberg". We adopt the magnetar central engine model to fit the observed soft X-ray emission with a varying efficiency and find that the parameters constraints of magnetar fall into a reasonable range, i.e., $B<9.4\times10^{15}$ G and $P<2.5$ ms for $\Gamma_{\rm sat} = 10^3$, and $B<3.6\times10^{15}$ G and $P<1.05$ ms for $\Gamma_{\rm sat} = 10^4$. Whether the progenitor of GBR 230307A is from the mergers of neutron star - white dwarf (NS - WD) or neutron star - neutron star (NS - NS) remains unknown.Comment: 7 pages, 1 table, 4 figures. Accepted for publication in ApJ Letters, 962:L27, 202