Hayashi limit

English Etymology Named after the Japanese astrophysicist Chushiro Hayashi. Noun en astrophysics A theoretical maximum radius of a star of given mass; the radius at which the inward force of gravity exactly balances the outward pressure of the gas of the star. en When a star is fully within hydrostatic equilibrium—a condition where the inward force of gravity is matched by the outward pressure of the gas—the star can not exceed the radius defined by the Hayashi limit.[Wikipedia] en 1977 Rudolf Kippenhahn; Walter Strohmeyer The Interaction of Variable Stars with Their Environment Remeis-Sternwarte https://books.google.com.au/books?id=WuE2AQAAIAAJ&q=%22Hayashi+limit%22%7C%22Hayashi+limits%22&dq=%22Hayashi+limit%22%7C%22Hayashi+limits%22&hl=en&newbks=1&newbks_redir=0&sa=X&ved=2ahUKEwjyvp_5nqD6AhWerpUCHYySD2QQ6AF6BAhbEAI 69 However, the approximate locations of the Hayashi limits point to remarkably low masses for the three T Tauri stars investigated here. It should be noted, that the Hayashi limits are valid only for stars in hydrostatic equilibrium. en 2006 Peter Eggleton Evolutionary Processes in Binary and Multiple Stars https://books.google.com.au/books?id=c7R9MYfAv7YC&pg=PA75&dq=%22Hayashi+limit%22%7C%22Hayashi+limits%22&hl=en&newbks=1&newbks_redir=0&sa=X&ved=2ahUKEwjyvp_5nqD6AhWerpUCHYySD2QQ6AF6BAgMEAI#v=onepage&q=%22Hayashi%20limit%22%7C%22Hayashi%20limits%22&f=false 75 w:Cambridge University Press Since the Hayashi limit approaches close to the main sequence at about 1 M⊙, the 'Hertzsprung gap' between the terminal main sequence and the Hayashi limit is much less marked than at high masses. en 2009 Donald Gerard Luttermoser; Beverly Joy Smith; Robert E. Stencel The Biggest, Baddest, Coolest Stars: Proceedings of a Workshop w:Astronomical Society of the Pacific https://books.google.com.au/books?id=iAdAAQAAIAAJ&q=%22Hayashi+limit%22%7C%22Hayashi+limits%22&dq=%22Hayashi+limit%22%7C%22Hayashi+limits%22&hl=en&newbks=1&newbks_redir=0&sa=X&ved=2ahUKEwjyvp_5nqD6AhWerpUCHYySD2QQ6AF6BAhhEAI 33 The latest-type RSGs[Red Supergiants] in the Magellanic Clouds are cooler than the current evolutionary tracks allow, occupying the region to the right of the Hayashi limit where stars are no longer in hydrostatic equilibrium. Related terms en Hayashi boundary en Hayashi track Translations theoretical upper limit of the radius of a hydrostatically stable star French: fr limite de Hayashi f German: de Hayashi-Limit n Italian: it limite di Hayashi m Further reading Hayashi track#Forbidden zone Hayashi track § Forbidden zone Eddington luminosity en Gravity Physical quantities en eponyms