Spectral representations of neutron-star equations of state
- Creators
- Lindblom, Lee
Abstract
Methods are developed for constructing spectral representations of cold (barotropic) neutron-star equations of state. These representations are faithful in the sense that every physical equation of state has a representation of this type and conversely every such representation satisfies the minimal thermodynamic stability criteria required of any physical equation of state. These spectral representations are also efficient, in the sense that only a few spectral coefficients are generally required to represent neutron-star equations of state quiet accurately. This accuracy and efficiency is illustrated by constructing spectral fits to a large collection of "realistic" neutron-star equations of state.
Additional Information
© 2010 The American Physical Society. Received 3 September 2010; published 18 November 2010. I thank Benjamin Owen, Benjamin Lackey, John Friedman, and Chris Vuille for helpful discussions about their work, B. O., B. L., and C.V. for useful comments on an earlier draft of this paper, and B. L and J. F. for providing tables of the various realistic equations of state used here. This research was supported in part by a grant from the Sherman Fairchild Foundation, by NSF Grant No. PHY-0601459, and by NASA Grant No. NNX09AF97G.Attached Files
Published - Lindblom2010p12103Phys_Rev_D.pdf
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Additional details
- Eprint ID
- 21373
- Resolver ID
- CaltechAUTHORS:20101215-091221587
- Sherman Fairchild Foundation
- PHY-0601459
- NSF
- NNX09AF97G
- NASA
- Created
-
2010-12-15Created from EPrint's datestamp field
- Updated
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2021-11-09Created from EPrint's last_modified field
- Caltech groups
- TAPIR