Premium
The stability of tension stars
Author(s) -
Wolf C.
Publication year - 1993
Publication title -
astronomische nachrichten
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 0.394
H-Index - 63
eISSN - 1521-3994
pISSN - 0004-6337
DOI - 10.1002/asna.2113140606
Subject(s) - stars , physics , radius , stability (learning theory) , newtonian fluid , tension (geology) , square (algebra) , classical mechanics , configuration space , space (punctuation) , mechanics , astrophysics , geometry , mathematics , quantum mechanics , linguistics , philosophy , computer security , machine learning , computer science , moment (physics)
By studying the cylindrically symmetric solution for matter in 2+1 space‐time dimensions we arrive at stability criteria for such a configuration when the local energy density is proportional to the square of the tension (negative pressure). Our analysis demonstrates that to the post‐Newtonian approximation that such a configuration is stable provided it does not shrink below a certain radius. We find our model provides a reason for how stars form from a two‐dimensional configuration with both a maximum mass and a minimum radius.
Accelerating Research
Robert Robinson Avenue,
Oxford Science Park, Oxford
OX4 4GP, United Kingdom
Address
John Eccles HouseRobert Robinson Avenue,
Oxford Science Park, Oxford
OX4 4GP, United Kingdom