期刊
ASTROPHYSICAL JOURNAL LETTERS
卷 735, 期 2, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.1088/2041-8205/735/2/L30
关键词
binaries: eclipsing; stars: individual (CSS 41177); white dwarfs
资金
- Science and Technology Facilities Council (STFC) [ST/F002599/1]
- UK Science and Technology Facilities Council
- STFC [ST/G009465/1, ST/I001719/1, ST/G004269/1, ST/F002599/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/G004269/1, ST/I001719/1, ST/G009465/1, ST/F002599/1] Funding Source: researchfish
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [909182] Funding Source: National Science Foundation
Using Liverpool Telescope+RISE photometry we identify the 2.78 hr period binary star CSS 41177 as a detached eclipsing double white dwarf binary with a 21,100 K primary star and a 10,500 K secondary star. This makes CSS 41177 only the second known eclipsing double white dwarf binary after NLTT 11748. The 2 minute long primary eclipse is 40% deep and the secondary eclipse 10% deep. From Gemini+GMOS spectroscopy, we measure the radial velocities of both components of the binary from the Ha absorption line cores. These measurements, combined with the light curve information, yield white dwarf masses of M-1 = 0.283 +/- 0.064 M-circle dot and M-2 = 0.274 +/- 0.034 M-circle dot, making them both helium core white dwarfs. As an eclipsing, double-lined spectroscopic binary, CSS 41177 is ideally suited to measuring precise, model-independent masses and radii. The two white dwarfs will merge in roughly 1.1 Gyr to form a single sdB star.
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