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HD 49798: Its History of Binary Interaction and Future Evolution

Brooks, Jared and Kupfer, Thomas and Bildsten, Lars (2017) HD 49798: Its History of Binary Interaction and Future Evolution. Astrophysical Journal, 847 (1). Art. No. 78. ISSN 1538-4357. https://resolver.caltech.edu/CaltechAUTHORS:20170922-105845809

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Abstract

The bright subdwarf-O star (sdO) HD 49798 is in a 1.55 day orbit with a compact companion that is spinning at 13.2 s. Using the measurements of the effective temperature (T_(eff)), surface gravity (log g), and surface abundances of the sdO, we construct models to study the evolution of this binary system using Modules for Experiments in Stellar Astrophysics (MESA). Previous studies of the compact companion have disagreed on whether it is a white dwarf (WD) or a neutron star (NS). From the published measurements of the companion's spin and spin-up rate, we agree with Mereghetti and collaborators that an NS companion is more likely. However, since there remains the possibility of a WD companion, we use our constructed MESA models to run simulations with both WD and NS companions that help us constrain the past and future evolution of this system. If it presently contains an NS, the immediate mass transfer evolution upon Roche lobe filling will lead to mass transfer rates comparable to that implied in ultraluminous X-ray sources (ULXs). Depending on the rate of angular momentum extraction via a wind, the fate of this system is either a wide (P_(orb) ≈ 3 day) intermediate-mass binary pulsar (IMPB) with a relatively rapidly spinning NS (≈0.3 s) and a high mass WD (≈0.9 M_⊙), or a solitary millisecond pulsar (MSP).


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-4357/aa87b3DOIArticle
http://iopscience.iop.org/article/10.3847/1538-4357/aa87b3PublisherArticle
https://arxiv.org/abs/1708.06798arXivDiscussion Paper
ORCID:
AuthorORCID
Kupfer, Thomas0000-0002-6540-1484
Additional Information:© 2017 American Astronomical Society. Received 2017 July 26. Accepted 2017 August 7. Published 2017 September 22. We thank Jim Fuller, Sterl Phinney, and Josiah Schwab for their helpful conversations. This research is funded by the Gordon and Betty Moore Foundation through Grant GBMF5076, and was also supported by the National Science Foundation under grant PHY 11-25915. We acknowledge stimulating workshops at Sky House where these ideas germinated.
Funders:
Funding AgencyGrant Number
Gordon and Betty Moore FoundationGBMF5076
NSFPHY-1125915
Issue or Number:1
Record Number:CaltechAUTHORS:20170922-105845809
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20170922-105845809
Official Citation:Jared Brooks et al 2017 ApJ 847 78
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:81744
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:22 Sep 2017 19:57
Last Modified:03 Oct 2019 18:46

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