We present an investigation of spin-orbit angles for planetary system candidates reported by Kepler. By combining the rotational period Ps inferred from the flux variation due to starspots and the projected rotational velocity Vsin Is and stellar radius obtained by a high-resolution spectroscopy, we...
When high-resolution (<10 km s−1) spectra of Cepheids are obtained throughout a pulsation cycle, the radial velocity curve constructed from these observations can be used to solve for the mean radius of the star. This is the Baade–Wesselink method. The change in the radius of the ...
The circles have a radius of 1″. The progenitor has dramatically faded in the optical but there is still faint near-IR emission. Reproduced from ref. (Adams et al., 2016a). (8b) N6946-BH1 light curves from HST (large circles), Spitzer Space telescope (SST, squares), Large Binocular...
We derive a reliable bolometric light curve that indicates that the shock breaks out from a dense layer with a radius substantially larger than typical supergiants. This is a preview of subscription content, access via your institution Access options Access through your institution Access Nature ...
whereNis the number of particles in the system. They have the structure of a Fokker–Planck equation involving a diffusion term and a drift term. The systematic drift of a vortex is the counterpart of the dynamical friction experienced by a star. At equilibrium, the diffusion and the drift ...
The high-cadence full-Sun view of SDO’s AIA revealed connections between activity in distant regions: filament eruptions or flux emergence in one location can deform the magnetic configuration sometimes more than a solar radius away. Combined with the full-Sun field models and STEREO EUVI observa...
It can be clearly seen that while the X-ray temperature is an order of magnitude higher, it is not enough to explain the observed UV/optical emission, suggesting physically distinct emission components at the two bands arising probably from different locations. The blackbody radius inferred from ...
of stellar oscillations is the possibility to infer the internalrotation rate of a star through the so-called rotational splittings. Such seismic measurements remained rather scarcefor hot B subdwarf (sdB) stars until the advent of space observations with theKeplerspacecraft. Nowadays, however,a ...
We discuss how recent advances in observations, theory and numerical simulations have allowed the stellar community to progress in its understanding of ste
The marginally bound radius Rmb is the minimum pericenter that avoids capture by the event horizon and is of order Rg (Bardeen et al. 1972). The online “Open TDE Catalog” https://tde.space/ is a useful resource for the observationally-curious reader. References P.A. Abell, J. Allison...