This result has been achieved as a consequence of our improved capability in understanding and describing the physical behavior of stellar matter in the thermal regimes characteristic of the different stellar mass ranges and/or evolutionary stages. This notwithstanding, stellar models are still affected ...
This particularly luminous state is proceeded by evolutionary stages called the "Hayashi track" and the "Henyey track," which can be seen on the diagram below. This is a Hertzsprung Russell diagram that tracks the early evolution of the Sun from protostar to main sequence star. The evolution ...
Final Stages of Stellar Evolution EQUATION OF STATE OF DENSE MATTER AND MAXIMUM MASS OF NEUTRON STARSHaensel, P
ONE of the questions which the modern theory of stellar evolution fails to explain is why there are no stars rotating with extreme equatorial velocities. It is easy to see that the rotation of protostars is restricted because of the conservation of angular momentum during contraction, but if ...
The stellar evolution from the asymptotic giant branch (AGB) to planetary nebulae (PN) contains some of the most interesting physical and chemical processes in the Universe. Within a time period of one million years starting from the nucleosynthesis of carbon in the core, we witness the chemical...
We present a general overview of the structure and evolution of massive stars of masses ≥12 M ⊙ during their pre-supernova stages. We think it is worth... MFE Eid,LS The,BS Meyer - 《Space Science Reviews》 被引量: 27发表: 2009年 Iteration Stability for Simple Newtonian Stellar System...
Unraveling Mysteries in Late Stages of Stellar Evolution: The Enigma of the S-Type StarsS Stars: Stellar EvolutionWe report the results of an ongoing survey of S stars within 1 kpc of the Sun for emission from the J = 1 → 0 and J = 2 → 1 lines of CO. We derive mass loss ...
A T Tauri star is a stage in a star’s formation and evolution right before it becomes a main-sequence star. This phase occurs at the end of the protostar phase when the gravitational pressure holding the star together is the source of all its energy. T Tauri stars don’t have enough ...
In the last throes of their lives, how do low- and high-mass stars interact with their immediate surroundings? How does the circumstellar medium affect the shape of a nebula? How are supernovae affected by a dense medium? And what do we understand of how stellar winds interact with their...
In order to better understand stellar dynamics in merging systems, such asNGC 6240, we examine the evolution of central stellar velocity dispersion(\sig) in dissipative galaxy mergers using a suite of binary disk mergersimulations that include feedback from stellar formation and active galacticnuclei...