With an ideal dataset of many localized FRBs, how can the diffuse gas fraction in the IGM be constrained?
Why do some dwarf galaxies exhibit such old stellar populations? Perhaps simulations of reionization including radiative transfer can help to explain this peculiar trait.
Our gas giants spin slower than one might expect. Turns out gas giants outside of our solar system are also slower than originally what we might have thought! Today’s astrobite answers the question: What’s up with dat?
Astronomers have been finding planets around M dwarf stars for a while. Can we go even cooler and find planets around the diverse L and T spectral group?
Most Jupiter-like exoplanets go undetected. But do they leave a mark on the more easily detectable inner terrestrial worlds?
Millisecond pulsars haven’t been observed to spin faster than ~700 Hz — if they don’t fly apart until ~1 kHz, why haven’t we found any faster specimens?