THE WHITE DWARF COMPANION OF A 2 M{sub sun} NEUTRON STAR
Abstract
We report the optical discovery of the companion to the 2 M{sub sun} millisecond pulsar PSR J1614-2230. The optical colors show that the 0.5 M{sub sun} companion is a 2.2 Gyr old He-CO white dwarf. We infer that M-dot during the accretion phase is <10{sup -2} M-dot{sub edd}. We show that the pulsar was born with a spin close to its current value, well below the rebirth line. The spin-down parameters, the mass of the pulsar, and the age of the system challenge the simple recycling model for the formation of millisecond pulsars.
- Authors:
-
- Department of Astronomy, California Institute of Technology, Pasadena, CA 91125 (United States)
- Publication Date:
- OSTI Identifier:
- 21562495
- Resource Type:
- Journal Article
- Journal Name:
- Astrophysical Journal Letters
- Additional Journal Information:
- Journal Volume: 737; Journal Issue: 1; Other Information: DOI: 10.1088/2041-8205/737/1/L1; Journal ID: ISSN 2041-8205
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; NEUTRON STARS; PULSARS; WHITE DWARF STARS; COSMIC RADIO SOURCES; DWARF STARS; STARS
Citation Formats
Bhalerao, Varun B, and Kulkarni, S R. THE WHITE DWARF COMPANION OF A 2 M{sub sun} NEUTRON STAR. United States: N. p., 2011.
Web. doi:10.1088/2041-8205/737/1/L1.
Bhalerao, Varun B, & Kulkarni, S R. THE WHITE DWARF COMPANION OF A 2 M{sub sun} NEUTRON STAR. United States. https://doi.org/10.1088/2041-8205/737/1/L1
Bhalerao, Varun B, and Kulkarni, S R. 2011.
"THE WHITE DWARF COMPANION OF A 2 M{sub sun} NEUTRON STAR". United States. https://doi.org/10.1088/2041-8205/737/1/L1.
@article{osti_21562495,
title = {THE WHITE DWARF COMPANION OF A 2 M{sub sun} NEUTRON STAR},
author = {Bhalerao, Varun B and Kulkarni, S R},
abstractNote = {We report the optical discovery of the companion to the 2 M{sub sun} millisecond pulsar PSR J1614-2230. The optical colors show that the 0.5 M{sub sun} companion is a 2.2 Gyr old He-CO white dwarf. We infer that M-dot during the accretion phase is <10{sup -2} M-dot{sub edd}. We show that the pulsar was born with a spin close to its current value, well below the rebirth line. The spin-down parameters, the mass of the pulsar, and the age of the system challenge the simple recycling model for the formation of millisecond pulsars.},
doi = {10.1088/2041-8205/737/1/L1},
url = {https://www.osti.gov/biblio/21562495},
journal = {Astrophysical Journal Letters},
issn = {2041-8205},
number = 1,
volume = 737,
place = {United States},
year = {Wed Aug 10 00:00:00 EDT 2011},
month = {Wed Aug 10 00:00:00 EDT 2011}
}
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