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Abstract Outdoor trials were made to test the responses of male aphids to pheromone lures in fields with different host‐plants, in order to know whether host‐plants would affect catches of males to pheromone lures. In peach orchard, males of three aphid species, i.e. Myzus persicae, Hyalopterus amygdaliand Rhopalosiphum nymphaeae, were found in traps baited with aphid sex pheromone nepetalactone and nepetalactol. The most numerous numbers was M, persicaeand it was also attracted by plant‐derived nepetalactone alone in peach orchard and cabbage garden. Schizaphis graminummales were caught in water traps in wheat field. In apple orchard, males of two aphid species, Aphis cifricolaand Sappaphis sinipiricolawere caught in significantly larger numbers in the pheromone traps than in the control traps. Field study indicated that the sex pheromone of H. amygdulicomprises either one or both of nepetalactone and nepetalactol, and nepetalactone may be one component of sex pheromones of A cifricolaand S sinipiricolaAnother field trial had shown that catches were increased if volatiles from a steam‐distilled extract of peach leaves were released simultaneously with nepetalactone. Elec‐troantennograms (EAGs) were recorded from males of M. persicaeto volatiles of peach leaves and buds.

Strange quark matter, which is composed of u, d, and s quarks, could be the true ground state of matter. According to this hypothesis, compact stars may actually be strange quark stars, and there may even be stable strange quark dwarfs and strange quark planets. The detection of the binary neutron star merger event GW170817 provides us new clues on the equations of state of compact stars. In this study, the tidal deformabilities of strange quark planets and strange quark dwarfs are calculated. It is found to be smaller than that of normal matter counterparts. For a typical 0.6 M⊙ compact star, the tidal deformability of a strange dwarf is about 1.4 times less than that of a normal white dwarf. The difference is even more significant between strange quark planets and normal matter planets. Additionally, if the strange quark planet is a bare one (i.e., not covered by a normal matter curst), the tidal deformability will be extremely small, which means bare strange quark planets will hardly be distorted by tidal forces. Our study clearly proves the effectiveness of identifying strange quark objects via searching for strange quark planets through gravitational wave observations. [ABSTRACT FROM AUTHOR]

In this paper, we use the recent updated source properties of GW170817 to constrain the hybrid equation of state (EOS) constructed by a three-window modeling between the hadronic EOS and quark EOS. Specifically, the hadronic EOS is described by the NL3ωρ model whose corresponding pure neutron star (NS) is already excluded by the constraint of tidal deformability (TD) from GW170817, and the quark EOS is calculated with the 2+1 flavors Nambu-Jona-Lasinio (NJL) model. We also consider four other constraints on the hybrid EOS. As a result, we find the parameter set (B1/4,μ,Γ) can be well constrained, indicating the possible existence of the hybrid star (HS) with a crossover inside. The type of the two stars in the binary system for nine representative hybrid EOSs is shown in this paper too. Furthermore, the HSs restricted by five constraints do not suggest a pure quark core but a mixed phase in the center. [ABSTRACT FROM AUTHOR]