text: 29,71,1427210696685756419,1425340957,Alex Haber,"We (Mark Alford, Ziyuan Yhang, Steven Harris and me) recently published a new paper on beta equilibration in neutron star mergers: <LINK> . What is it about? 1/n In a neutron star, weak interactions lead to various nucleonic reactions like neutron decay, electron capture and so on. These reactions change the chemical composition of the star, like the proton fraction (yes neutron stars do have some other particles, not only neutrons!) 2/n If you wait long enough, these reactions will balance and the chemical composition stays constant. Traditionally, we have always studied that at T=0. Although neutron stars are quite hot by traditional standards (10^6 K), in a particle physics context they are actually very cold. At T=0, the reactions balance each other when the chemical potential of the neutron equals the sum of the proton and electron chemical potential. But neutron star mergers require us to reexamine a lot of our prior assumptions and findings. 4/n Mergers are much hotter than isolated, old neutron stars. We find that in these conditions, the traditional beta equilibrium condition needs to be modified. The correction term reach magnitudes of more than 10 MeV. 5/n The corrected nucleonic rates change by up to an order of magnitude. How our results influence cooling or the outcome of neutron star mergers remains to be seen, but there is interesting work from @ProfNilsAnd and collaborators coming 6/6",https://arxiv.org/abs/2108.03324,"We calculate the nonzero-temperature correction to the beta equilibrium condition in nuclear matter under neutron star merger conditions, in the temperature range $1\,$MeV$ < T \lesssim 5\,$MeV. We improve on previous work by using a consistent description of nuclear matter based on the IUF and SFHo relativistic mean field models. This includes using relativistic dispersion relations for the nucleons, which we show is essential in these models. We find that the nonzero-temperature correction can be of order $10$ to $20\,$MeV, and plays an important role in the correct calculation of Urca rates, which can be wrong by factors of $10$ or more if it is neglected. ",Beta equilibrium under neutron star merger conditions,6,"['We (Mark Alford, Ziyuan Yhang, Steven Harris and me) recently published a new paper on beta equilibration in neutron star mergers: <LINK> . What is it about? 1/n', 'In a neutron star, weak interactions lead to various nucleonic reactions like neutron decay, electron capture and so on. These reactions change the chemical composition of the star, like the proton fraction (yes neutron stars do have some other particles, not only neutrons!) 2/n', 'If you wait long enough, these reactions will balance and the chemical composition stays constant. Traditionally, we have always studied that at T=0. Although neutron stars are quite hot by traditional standards (10^6 K), in a particle physics context they are actually very cold.', 'At T=0, the reactions balance each other when the chemical potential of the neutron equals the sum of the proton and electron chemical potential. But neutron star mergers require us to reexamine a lot of our prior assumptions and findings. 4/n', 'Mergers are much hotter than isolated, old neutron stars. We find that in these conditions, the traditional beta equilibrium condition needs to be modified. The correction term reach magnitudes of more than 10 MeV. 5/n', 'The corrected nucleonic rates change by up to an order of magnitude. How our results influence cooling or the outcome of neutron star mergers remains to be seen, but there is interesting work from @ProfNilsAnd and collaborators coming  6/6']",21,08,1424