The Spionidae of southeastern Australia are described. Intertidal and subtidal collections come mostly from Victoria, New South Wales and southern Queensland. A few records from West Australia, South Australia, Tasmania and the Great Barrier Reef (Queensland) are also included. A total of 68 species in 19 genera have been identified. These include 4 new genera and 43 new species, with new synonyms and generic emendations also proposed. The genera with pointed prostomia include Scolelepis (9 species, 8 being new), Aonides (1 species) and Dispio (1 new species). Australospio trifida gen. et. sp. nov. is a unique spionid with both a distally pointed prostomium and lateral prostomial horns. The genera with frontal or lateral prostomial horns include Malacoceros (3 species, 2 being new), Rhynchospio (2 new species) and Scolecolepides (1 new species). The definition of Rhynchospio is expanded to include those species with branchiae free from dorsal lamellae. Laonice includes 3 new species, with 1 being a simultaneous hermaphrodite. Spiophanes includes 3 species, Spio with 3 species (2 being new) and Microspio with 1 new species. The genera of the Prionospio-compXex are reviewed and revised to include: Paraprionospio (1 species), Orthoprionospio gen. nov. (1 new species), Streblospio (not represented) and Prionospio (9 species, 5 being new). A generic revision of the Poly dora-comp\ex is presented with 6 genera recognized: Boccardia (3 species), Carazziella gen. nov. (4 new species), Polydora (15 species, 8 being new), Boccardiella gen. nov. (2 species, 1 being new), Tripolydora (not represented) and Pseudopolydora (5 species, 2 being new). Polydorella is synonymized with Pseudopolydora. Approximately I of the species reported herein are endemic to Australia; the remainder are species with more cosmopolitan distributions. Family Spionidae Grube, 1850 Diagnosis: Prostomium variable: anteriorly rounded or incised, anteriorly expanded to acutely pointed, with or without frontal horns. Occipital tentacle sometimes present on prostomial caruncle. A pair of long prehensile peristomial palps arising on either side of caruncle near junction of peristomium and setiger 1. Setiger 1 reduced to well-developed, often fused with peristomium. Parapodia biramous, with parapodial lobes conical, cirriform or foliose; posterior neuropodia often form low 16. Rhynchospio glycera sp. nov. 17. R. australiana sp. nov. 18. Scolecolepides aciculatus sp. nov. 1 9.

As an exoplanet orbits its host star it reflects and emits light, forming a distinctive phase curve 1,2 . By observing this light, we can study the atmosphere and surface of distant planets. The planets in our Solar System show a wide range of atmospheric phenomena, with stable wind patterns, changing storms, and evolving anomalies. Brown dwarfs also exhibit atmospheric variability 3,4 . Such temporal variability in the atmosphere of a giant exoplanet has not to date been observed. HAT-P-7 b is an exoplanet with a known offset in the peak of its phase curve 5,6 . Here we present variations in the peak offset ranging between -0.086 +0.033 -0.033 to 0.143 +0.040 -0.037 in phase, implying that the peak brightness repeatedly shifts from one side of the planet's substellar point to the other. The variability occurs on a timescale of tens to hundreds of days. These shifts in brightness are indicative of variability in the planet's atmosphere, and result from a changing balance of thermal emission and reflected flux from the planet's dayside. We suggest that variation in wind speed in the planetary atmosphere, leading to variable cloud coverage on the dayside and a changing energy balance, is capable of explaining the observed variation. Time (BJD-2454833)Peak Offset (Phase) Author ContributionsDJA obtained and detrended the data, developed and fit the phase curve models, implemented the atmospheric model, produced the figures and wrote the manuscript. EdM developed the discussion, contributed to the tests performed to check the results, and tested the results with his own models. HPO contributed to the phase curve model, and produced visual interpretations of the results. JBa developed the discussion of the atmospheric processes behind the peak offset variations. JBl provided the initial development of the phase curve model. NFS contributed to development of the figures. All authors commented on the manuscript.

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