期刊
ASTROPHYSICAL JOURNAL
卷 753, 期 2, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/753/2/174
关键词
binaries: eclipsing; gamma rays: stars; pulsars: individual (PSR J1816+4510); ultraviolet:stars; white dwarfs
资金
- NASA [NAS5-26555]
- NASA Office of Space Science [NNX09AF08G]
- NSF CAREER [09955929]
- PIRE [0968126]
- University of Wisconsin-Milwaukee Office of Undergraduate Research
- NSERC
- Division Of Physics
- Direct For Mathematical & Physical Scien [0955929] Funding Source: National Science Foundation
- Office Of The Director
- Office Of Internatl Science &Engineering [0968296] Funding Source: National Science Foundation
The energetic, eclipsing millisecond pulsar J1816+4510 was recently discovered in a low-frequency radio survey with the Green Bank Telescope. With an orbital period of 8.7 hr and a minimum companion mass of 0.16 M-circle dot, it appears to belong to an increasingly important class of pulsars that are ablating their low-mass companions. We report the discovery of the gamma-ray counterpart to this pulsar and present a likely optical/ultraviolet counterpart as well. Using the radio ephemeris, we detect pulsations in the unclassified gamma-ray source 2FGL J1816.5+4511, implying an efficiency of similar to 25% in converting the pulsar's spin-down luminosity into gamma-rays and adding PSR J1816+4510 to the large number of millisecond pulsars detected by Fermi. The likely optical/UV counterpart was identified through position coincidence (<0 ''.1) and unusual colors. Assuming that it is the companion, with R = 18.27 +/- 0.03 mag and effective temperature greater than or similar to 15,000 K, it would be among the brightest and hottest of low-mass pulsar companions and appears qualitatively different from other eclipsing pulsar systems. In particular, current data suggest that it is a factor of two larger than most white dwarfs of its mass but a factor of four smaller than its Roche lobe. We discuss possible reasons for its high temperature and odd size, and suggest that it recently underwent a violent episode of mass loss. Regardless of origin, its brightness and the relative unimportance of irradiation make it an ideal target for a mass, and hence a neutron star mass, determination.
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