We report on the discovery of an Earth-sized transiting planet (R p = 1.015 ± 0.051 R ⊕) in a P = 4.02 day orbit around K2-415 (EPIC 211414619), an M5V star at 22 pc. The planet candidate was first identified by analyzing the light-curve data obtained by the K2 mission, and it is here shown to exist in the most recent data from TESS. Combining the

Accretion disks around compact objects are expected to enter an unstable phase at high luminosity 1. One instability may occur when the radiation pressure generated by accretion modifies the disk viscosity, resulting in the cyclic depletion and refilling of the inner disk on short timescales 2. Such a scenario, however, has only been quantitatively

Cosmological constraints on the sum of the neutrino masses can be relaxed if the number density of active neutrinos is reduced compared to the standard scenario, while at the same time keeping the effective number of neutrino species N eff \approx 3 by introducing a new component of dark radiation. We discuss a UV complete model to realise this

We present a rapid timing analysis of optical (HiPERCAM and ULTRACAM) and X-ray (NICER) observations of the X-ray transient Swift J1858.6-0814 during 2018 and 2019. The optical light curves show relatively slow, large amplitude (~1 mag in g s) 'blue' flares (i.e. stronger at shorter wavelengths) on time-scales of ~minutes as well as fast, small

TOI-640 b is a hot, puffy Jupiter with a mass of 0.57 ± 0.02 M J and radius of 1.72 ± 0.05 R J, orbiting a slightly evolved F-type star with a separation of 6.33 −0.06 +0.07 R ⋆. Through spectroscopic in-transit observations made with the HARPS spectrograph, we measured the Rossiter-McLaughlin effect, analysing both in-transit radial velocities and

Numerical simulations within a cold dark matter (DM) cosmology form haloes whose density profiles have a steep inner slope ('cusp'), yet observations of galaxies often point towards a flat central 'core'. We develop a convolutional mixture density neural network model to derive a probability density function (PDF) of the inner density slopes of DM